- Cosmo-torun - cosmo.torun.pl

COSMO 04 Second Circular (fwd)
by boud 18 Mar '04

18 Mar '04

---------- Forwarded message ---------- > Date: Wed, 17 Mar 2004 19:58:26 -0500 (EST) > From: conference <cosmo04(a)cita.utoronto.ca> > To: conference <cosmo04(a)cita.utoronto.ca> > Subject: COSMO 04 Second Circular COSMO 04 Second Circular ============== Dear Colleague, Thank you for your interest in Cosmo04. Online registration and abstract submission are now open at: http://www.cita.utoronto.ca/~cosmo04/ Accomodation details can also be found on the web site. We will be updating the site regularly with additional information such as session program, list of speakers, and travel information. We look forward to seeing you in Toronto, Cosmo04 Organizing Committee

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low multipoles from Oort cloud?
by Boud Roukema 17 Mar '04

17 Mar '04

http://adjani.astro.uni.torun.pl:9673/zwicky/CosmoNews -> AstroPh:0403353 low multipoles from Oort cloud (outer solar system)? "Is the low-l microwave background cosmic?" - Dominik J. Schwarz (CERN), Glenn D. Starkman (CERN, Case Western Reserve University), Dragan Huterer (CWRU), Craig J. Copi

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bazanski - soft@ mailing list
by Boud Roukema 13 Mar '04

13 Mar '04

Dear Bazański, You have requested to join a private email list ("soft") for a cosmology computer at the TCfA, UMK, for discussing system admin. My guess is this is probably an error - you are most welcome to join any of our lists for discussing cosmology - it would be nice to introduce yourself briefly on cosmo-torun, just for us to get to know each other. My guess from your email address is that you're in physics at UW. :) Probably cosmo-torun and shape-univ are most used right now: http://www.astro.uni.torun.pl/sympa/ regards boud

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A&A impact factor: the danger of productivist ideology
by Boud Roukema 09 Mar '04

09 Mar '04

http://arxiv.org/abs/astro-ph/0403184 Authors: Aa. Sandqvist (Stockholm Observatory, AlbaNova, Stockholm, Sweden) Comments: 4 pages, to be published in A. Heck (ed.) "Organizations and Strategies in Astronomy, Vol. 5" (Kluwer, 2004) There is a widespread impression that the scientific journal "Astronomy & Astrophysics" (A&A) has a smaller impact, as measured by citations to articles, than some of the other major astronomy journals. This impression was apparently supported - and probably created - by the Journal Citation Report (JCR), which is prepared annually by the Institute of Scientific Information (ISI) Web of Knowledge. The published poor impact factor of A&A was in fact wrong and was due to a serious flaw in the method used by ISI Web of Knowledge to determine it. The resulting damage inflicted upon A&A by the JCR is incalculable.

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mirror matter + DAMA/NaI => CDM solved ?
by Boud Roukema 08 Mar '04

08 Mar '04

http://arxiv.org/abs/astro-ph/0403043 Exploring the mirror matter interpretation of the DAMA experiment: Has the dark matter problem been solved? Authors: R.Foot Comments: About 10 pages The self consistency between the impressive DAMA annual modulation signal and the measured recoil energy spectrum is identified as an important test for dark matter candidates. Mirror matter-type dark matter passes this test while other dark matter candidates, including standard WIMPs and mini-electric charged particle dark matter, fail. We argue that the unique properties of mirror matter-type dark matter seem to be just those required to fully explain the data, suggesting that the dark matter problem has finally been solved.

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CMB energy
by Jarek Rzepecki 25 Feb '04

25 Feb '04

Hi all, CMB photons are red-shifted due to Universe expansion -> this means that the whole CMB energy gets smaller... where does it go? pozdrawiam Jarek

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poprawienie do listy uczestnikow ,,Wszechswiat: globalisci vs antyglobalisci"
by Boud Roukema 24 Feb '04

24 Feb '04

Witam, Jak rozumiem, nasze propozycja dla dyskusji panelowej o temat kosmologii byli akceptowany dla Festiwału Nauki: http://adjani.astro.uni.torun.pl/cgi-bin/twiki/view/Cosmo/FestiwalNauki2004 Proszę do mąlego poprawki: Pisaliśmy że Michał Frąckowiak chce uczestniczyć, ale prawdziwie on nie chce uczestniczyć. Proszę usunuj swoj nazwa od listy uczestników na baz danych Festiwału. Pozdrawiam serdecznie Boud Roukema (Centrum Astronomii UMK)

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festiwal nauki
by Boud Roukema 24 Feb '04

24 Feb '04

hi - i updated the Festiwal Nauki page: http://adjani.astro.uni.torun.pl/cgi-bin/twiki/view/Cosmo/FestiwalNauki2004 Please correct, update, modify... i guess it's now obvious why there was silly bureaucracy - there's money (150 zl) paid to official speakers (and if i understood the small print, "students" cannot be paid, though doktoranci are OK) - this is not a "grassroots" festival by scientists... Missing info: how much time do we have? One hour? Two hours? And is this time schedule definitely fixed? Staszek Krawczyk and A Strobel seem to be the official contacts so i'm cc-ing them here. boud

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Cosmo parameters according to VSA
by Andrzej Marecki 20 Feb '04

20 Feb '04

Paper: astro-ph/0402466 Title: Cosmological parameter estimation using Very Small Array data out to l=1500 Authors: Rafael Rebolo, Richard A. Battye, Pedro Carreira, Kieran Cleary, et al. We estimate cosmological parameters using data obtained by the Very Small Array (VSA) in its extended configuration, in conjunction with a variety of other CMB data and external priors. Within the flat $\Lambda$CDM model, we find that the inclusion of high resolution data from the VSA modifies the limits on the cosmological parameters as compared to those suggested by WMAP alone, while still remaining compatible with their estimates. [...]

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Re: wewnetrzny grant UMK
by Boud Roukema 18 Feb '04

18 Feb '04

hi everyone, Attached are two equivalent copies of the draft application (pdf to help a certain person who uses micro$oft ;) Any substantial comments, criticisms? (Or trivial ones?) Given that it's for pedagogical purposes, i haven't put anything about a specific "research project". i put my title as "dr" since i presume i don't officially have "hab" until the central committee confirms it. i can expect the bureaucrats may complain that the format is slightly changed, but that's their fault for using micro$oft. They're here to support us, we're not here to work for them doing trivia. pozd boud

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UMK grants by Sat 21 Feb for Wydzial Fizyki
by Boud Roukema 18 Feb '04

18 Feb '04

For UMK grant applications http://www.uni.torun.pl/badania/finansowanie/granty/umk/

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wewnetrzny grant UMK
by Boud Roukema 18 Feb '04

18 Feb '04

hi Andrzej (Kus), Apparently we need to spend 5kPLN of an internal UMK grant money/application and decide by tomorrow? IMHO this would be best spent on improving the computing facilities in the student room in KRA. If formally speaking this should be for a research project, that's no problem - the whole existence of the internet means that students can get a taste of research and be motivated to study questions of which the answers are not yet known. As the students get to learn how to program, find theoretical information and observational data, and analyse it in ways they understand, they also will start contributing to research (hopefully). i meant to have a look at the computers with Roman before the new semester started, i didn't realise it had already started. i remember some students claiming not many of the terminals/computers were working properly, but i didn't get around to checking specifically. ** It could certainly not hurt to buy another computer, which we can put as cosmic topology research - or for Bartek and my dark matter projects - but which i can set up for secondary usage by the students who i'm sure can always use more cpu and disk space. ** Maybe also a DAT drive + a few dozen DAT tapes (to last several years) for backups so that all the students can have a decent amount of backed up disk space. KA&A seems to have more or less good student support but we clearly are pushing the limits with the larger numbers of students. pozd boud

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final grant proposal (boud+bartek)
by Boud Roukema 26 Jan '04

26 Jan '04

witam, It's now too late (in practice) to change any of the grant proposals, but here is what bartek and i came up with. The discussion that bartek and i had about the relative importance (or non-importance) of having visitors ("consultants" in business English), who stay either a week or a month and help generate ideas for new research projects, make criticisms from alternative points of view on methods, results, theory, reminded me of one of the reasons why the KBN grant system is a bad system (as opposed to simply giving the money directly to institutes and having scientists at an institute discuss funding decisions by some open method with a reasonable chance of arriving at decisions - in principle, any visitor wanting to use this money is tied to an extremely narrow scientific subject, and what's probably worse, is that depending which "team" gets the money, the decisions on which visitors get funding risks become personalised and visitors have to become "friends" of the "director" of the project in order to get funding. Anyway, enough rant from me ;), at least our grant is on the archive so if we get it we can hopefully use an open system of decision-making on how to spend it... pozd boud %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \documentclass[12pt]{article} \newcommand\engpol[2]{#1} % version for english %\newcommand\engpol[2]{#2} % version for polish \usepackage[polish]{babel} \usepackage[T1]{fontenc} \usepackage[latin2]{inputenc} \usepackage{calc} \usepackage{hyperref} \usepackage{setspace} \usepackage{multicol} \usepackage[normalem]{ulem} \usepackage{color} \usepackage{polski} \hyphenation{po-czy-nio-nych} \newcommand\NIPTCfA{ xxx-xxx-xx-xx } \newcommand\REGONTCfA{ xxxxxxxxx } \newcommand\bankTCfA{ XXXXXXXXXXXXXXXXXXXXXX \\ xxx xxxxxxx xxxxx xxxxx xxxxxx} %\newcommand\peselmagda{ xxxxxxxxxxx } %\newcommand\peselandrzej{ xxxxxxxxxxx } \newcommand\nipboud{ \fbox{\rule{3cm}{0cm}\rule{0cm}{1.5ex}} } \newcommand\peselbartek{ \fbox{\rule{3cm}{0cm}\rule{0cm}{1.5ex}} } \newcommand\adresboud{ XXXXXX xx, XXXXXX xx-xxx, (xxx)-xxx-xxxx, XXXX } \newcommand\symbolrodzaju{ D } %\usepackage{prywatny} %\setlength{\oddsidemargin}{0.500000in-1in} %\setlength{\textwidth}{\paperwidth - 0.500000in-0.500000in} \setlength{\oddsidemargin}{0.5in-1in} \setlength{\textwidth}{\paperwidth - 1.0in -0.2in} \setlength{\textheight}{24cm} \setlength{\topmargin}{0cm} \setlength{\headheight}{-1cm} %%%%%%%%%%%%%%%%%%% %%% personal definitions \newcommand\noin{\noindent} \def\pub #1;;#2;;#3;;#4;;#5 {#1. {\it#2, }{\ \it#3, } {\bf#4, }#5} % PUBLISHED REFERENCE-- #1 AUTHORSHIP, YEAR; #2 TITLE; #3 JOURNAL; % #4 VOLUME; #5 PAGE. \newcommand\revinvit{ %%{\\ \bf (invited review)} { } } %\def\apj{Ap.J.} %\def\mnras{MNRAS} \def\apj{Astrophysical Journal} \def\mnras{Monthly Notices of the Royal Astronomical Society} \def\AandA{Astronomy \& Astrophysics} \def\AASupp{Astronomy \& Astrophysics Supplement} \def\cqg{Classical and Quantum Gravity} \def\jaf{Journal des astronomes fran\c{c}ais} \def\asr{Advances in Space Research} \def\dans{ in } \renewcommand\PLdateending{r.} \newcommand\datepolski{ { \number\day~\ifcase\month \or stycznia\or lutego\or marca\or kwietnia\or maja\or czerwca\or lipca\or sierpnia\or wrzenia\or padziernika\or listopada\or grudnia\fi \space\number\year \PLdateending} } \newcommand\Omm{\Omega_{\mbox{\rm m}}} \newcommand\Omtot{\Omega_{\mbox{\rm tot}}} %%%%%hardwired !!!! %\renewcommand\datepolski{31 stycznia 2004~r.} \newcommand\mdcitem[0]{\item } \newcounter{monthsone} \setcounter{monthsone}{12} \newcommand\monthsone{\arabic{monthsone}} \newcounter{monthstwo} \setcounter{monthstwo}{12} \newcommand\monthstwo{\arabic{monthstwo}} \newcounter{monthsthree} \setcounter{monthsthree}{12} \newcommand\monthsthree{\arabic{monthsthree}} \newcounter{monthstotal} \setcounter{monthstotal}{\monthsone+\monthstwo+\monthsthree} \newcommand\monthstotal{\arabic{monthstotal}} \newcounter{salrate} \setcounter{salrate}{11800} \newcommand\salrate{\arabic{salrate}} %\setcounter{x}{?} \renewcommand\x{\arabic{x}} \newcounter{x} \setcounter{x}{12} \newcommand\x{\arabic{x}} \newcounter{z} \setcounter{z}{12} \newcommand\z{\arabic{z}} \newcounter{w} \setcounter{w}{12} \newcommand\w{\arabic{w}} \newcounter{y} \setcounter{y}{12} \newcommand\y{\arabic{y}} %\setcounter{y}{?} \renewcommand\y{\arabic{y}} \newcounter{persontotal} \setcounter{persontotal}{12} \newcommand\persontotal{\arabic{dummy}} \newcounter{boudeffective} \setcounter{boudeffective}{50} \newcommand\boudeffective{\arabic{boudeffective}} %\setcounter{persontotal}{(100+(1*50))} \setcounter{persontotal}{(\boudeffective +(1*50))} \renewcommand\persontotal{\arabic{persontotal}} \newcounter{saltotalyear} \setcounter{saltotalyear}{(\salrate *\persontotal)/100} \newcommand\saltotalyear{\arabic{saltotalyear}} \newcounter{scsi} \setcounter{scsi}{5}%kPLN \newcommand\scsi{\arabic{scsi}} \newcounter{perso} \setcounter{perso}{7} %kPLN \newcommand\perso{\arabic{perso}} \newcounter{clusterperso} \setcounter{clusterperso}{7} %kPLN \newcommand\clusterperso{\arabic{clusterperso}} \newcounter{cluster} \setcounter{cluster}{4*\clusterperso} %kPLN \newcommand\cluster{\arabic{cluster}} \newcounter{ups} \setcounter{ups}{1600} %PLN \newcommand\ups{\arabic{ups}} \newcounter{nups} \setcounter{nups}{2} %PLN \newcommand\nups{\arabic{nups}} \newcounter{upstotal} \setcounter{upstotal}{\nups*\ups} %PLN \newcommand\upstotal{\arabic{upstotal}} \newcounter{sober} \setcounter{sober}{700} \newcommand\sober{\arabic{sober}} \newcounter{portable} \setcounter{portable}{10} %kPLN \newcommand\portable{\arabic{portable}} \newcounter{equip} \setcounter{equip}{1000*(1+7+2+ \cluster + (\upstotal/1000) + \perso*2 + \portable) } \newcommand\equip{\arabic{equip}} \newcounter{consultrate} \setcounter{consultrate}{4500} \newcommand\consultrate{\arabic{consultrate}} \newcounter{consultpm} % personmonths \setcounter{consultpm}{12} \newcommand\consultpm{\arabic{consultpm}} \newcounter{consult} \setcounter{consult}{\consultrate * \consultpm} \newcommand\consult{\arabic{consult}} \newcounter{confperyear} \setcounter{confperyear}{2} \newcommand\confperyear{\arabic{confperyear}} \newcounter{oneconfer} \setcounter{oneconfer}{6500} \newcommand\oneconfer{\arabic{oneconfer}} \newcounter{allconferyear} \setcounter{allconferyear}{(\oneconfer *\confperyear * \persontotal)/100} \newcommand\allconferyear{\arabic{allconferyear}} \newcounter{allconfer} \setcounter{allconfer}{\allconferyear * \monthstotal /12} \newcommand\allconfer{\arabic{allconfer}} \newcounter{subone} \setcounter{subone}{\saltotalyear + \equip + \consult/(\monthstotal/12) + \allconferyear} \newcommand\subone{\arabic{subone}} \newcounter{suboneequip} \setcounter{suboneequip}{\saltotalyear + 0 + \consult/(\monthstotal/12) + \allconferyear} \newcommand\suboneequip{\arabic{suboneequip}} \newcounter{subtwo} \setcounter{subtwo}{\saltotalyear + 0 + \consult/(\monthstotal/12) + \allconferyear} \newcommand\subtwo{\arabic{subtwo}} \newcounter{subthree} \setcounter{subthree}{\saltotalyear + 0 + \consult/(\monthstotal/12) + \allconferyear} \newcommand\subthree{\arabic{subthree}} \newcounter{suball} \setcounter{suball}{\subone+\subtwo+\subthree} \newcommand\suball{\arabic{suball}} \newcounter{adminone} % \setcounter{adminone}{\subone /4} WRONG \setcounter{adminone}{(\suboneequip *3)/10} \newcommand\adminone{\arabic{adminone}} \newcounter{admintwo} \setcounter{admintwo}{(\subtwo *3)/10} \newcommand\admintwo{\arabic{admintwo}} \newcounter{adminthree} \setcounter{adminthree}{(\subthree *3)/10} \newcommand\adminthree{\arabic{adminthree}} \newcounter{adminall} \setcounter{adminall}{\adminone+\admintwo+\adminthree} \newcommand\adminall{\arabic{adminall}} \newcounter{totalone} \setcounter{totalone}{\subone + \adminone} \newcommand\totalone{\arabic{totalone}} \newcounter{totaltwo} \setcounter{totaltwo}{\subtwo + \admintwo} \newcommand\totaltwo{\arabic{totaltwo}} \newcounter{totalthree} \setcounter{totalthree}{(\subthree + \adminthree} \newcommand\totalthree{\arabic{totalthree}} \newcounter{totalall} \setcounter{totalall}{\totalone+\totaltwo+\totalthree} \newcommand\totalall{\arabic{totalall}} \newcounter{grandtotal} \setcounter{grandtotal}{\totalall} \newcommand\grandtotal{\arabic{grandtotal}} \newcounter{dummy} \setcounter{dummy}{12} \newcommand\dummy{\arabic{dummy}} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{document} \begin{flushleft} \textcolor[rgb]{1.000,1.000,1.000}{{\footnotesize{} }} \textbf{\textcolor[rgb]{1.000,1.000,1.000}{Zacznik nr 15}} \end{flushleft} \begin{center} \end{center} \begin{center} \end{center} \begin{center} \textbf{WNIOSEK} \end{center} \begin{center} \textbf{o finansowanie projektu badawczego} \end{center} \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{Tytuł projektu} {\bf \centerline{\underline{Modelowanie procesów powstawania galaktyk i ograniczenia na}} \centerline{\underline{profile rozkładu ciemnej materii w galaktykach i gromadach galaktyk.}}} \smallskip \centerline{(Galaxy formation modelling and constraints on Dark Matter Profiles in Galaxies and Galaxy Clusters)} \end{flushleft} \vspace {0.5cm} \begin{flushleft} \textbf{A. DANE WNIOSKODAWCY} \end{flushleft} \begin{flushleft} %Wypenia Komitet Bada Naukowych {\em 1. Nazwa i adres jednostki, w której będzie realizowany projekt}\\ Centrum Astronomiczne Uniwersytetu Mikołaja Kopernika (CA-UMK)\\ ul. Gagarina, 11, 87-100 Toruń \end{flushleft} \begin{flushleft} 2. NIP \NIPTCfA \\ REGON \REGONTCfA \end{flushleft} \begin{flushleft} {\em 3. Nazwa banku, numer rachunku} \\ \bankTCfA \end{flushleft} \begin{flushleft} {\em 4. Kierownik projektu\textit{ }(tytuł i stopień naukowy, imię nazwisko, adres prywatny, telefon miejsce zatrudnienia --- w przypadku uczelni podać także wydział, instytut, katedrę lub zakład --- telefon, e-mail) Numer rejestracyjny projektu} \end{flushleft} dr Boudewijn Roukema, \adresboud \begin{flushleft} {\em Data założenia} \end{flushleft} \datepolski %31 stycznia 2004 \begin{flushleft} {\em Zesp Komitetu} \end{flushleft} PO3D \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{B. DANE OGÓLNE} \end{flushleft} \begin{flushleft} {\em 1. Planowany okres realizacji projektu. {\bf \monthstotal}.. miesięcy (01.2004 -- 12.2006)} \end{flushleft} \begin{flushleft} {\em 2. Liczba osób przewidzianych do udziału w realizacji projektu} {\bf 2} \end{flushleft} \begin{flushleft} {\em 3. Rodzaj projektu: \textbf{własny} - %\rule[0.5ex]{48mm}{0.2ex}\hspace{-45mm} \sout{promotorski -- zamawiany Nr} wg ogłoszenia (niepotrzebne skreślić.}\\ \end{flushleft} \begin{flushleft} {\em 4. Propozycja skierowania wniosku: (symbol lub nazwa sekcji specjalistycznej Komitetu)} \end{flushleft} {\bf P03D: Astronomia i astrofizyka} \begin{flushleft} {\em 5. Planowane nakłady {\rm \grandtotal~PLN} (w z) ogółem} \end{flushleft} \begin{flushleft} {\em w tym w latach } 2005: \totalone~PLN; 2006: \totaltwo~PLN, 2007: \totalthree~PLN \end{flushleft} \begin{flushleft} {\em 6. Słowa kluczowe} \end{flushleft} kosmologia obserwacyjna, formowanie galaktyki, ciemna materia, galaktyki karłowaty, gromady galaktyk \clearpage \begin{flushleft} {\bf 7. Streszczenie projektu} \\ (streszczenie może być upowszechnione przez Komitet po zakwalifikowaniu projektu do finansowania) \end{flushleft} \begin{centering} %{\underline{Poszukiwanie soczewkowania topologicznego}} %{\underline{w aktywnych galaktykach czynnych radiowo i gromadach galaktyk}} {\underline{Modelowanie procesów powstawania galaktyk i ograniczenia na }} \\ {\underline{profile rozkładu ciemnej materii w galaktykach i gromadach galaktyk}} \smallskip \end{centering} \smallskip Przesłanki obserwacyjne dotyczące wartości lokalnych parametrów kosmologicznych -- nierelatywistycznej gęstości materii ($\Omm$), stałej kosmologicznej ($\Omega_\Lambda$), oraz ich sumy - parametru całkowitej gęstości ($\Omtot$), w skalach odległości od dziesiątek kiloparseków do dziesiątek gigaparseków --- obecnie zbiegły się wskazując że około 25\% całkowitej gęstości materii-energii składa się z nie barionowej ciemnej materii. Istnieje wiele koncepcji rozwijanych w ramach fizyki cząstek elementarnych, dotyczących natury owej ciemnej materii oraz reprezentujących ją potencjalnych kandydatów, takich jak aksjony, wprowadzone jako bozony odpowiedzialne za łamanie symetrii CP, czy też najlżejsze supersymetryczne cząstki (LSP) wprowadzane w supersymetrycznych rozszerzeniach standardowego modelu cząstek, oraz cały szereg eksperymentów poświęconych ich detekcji. Astrofizyczną wskazówką dotyczącą natury ciemnej materii jest jednoznaczna rozbieżność pomiędzy zaobserwowanymi, a teoretycznie (bądź semianalitycznie) przewidywanymi profilami gęstości ciemnej materii zwłaszcza w galaktykach karłowatych, oraz w gromadach galaktyk. W skrócie problem polega na tym, iż profile teoretyczne powinny być bardziej strome niż zaobserwowane (patrz na przykład McGaugh, Barker \& de Blok, ApJ, 584, 566, 2003). W projekcie proponujemy użyć i dalej rozwijać istniejące narzędzia służące do modelowania powstawania galaktyk - w szczególności oprogramowanie {\sc ArFus} (Roukema, Ninin, Devriendt, Bouchet, Guiderdoni \& Mamon 2001; dostępne pod adresem: \url{http://adjani.astro.uni.torun.pl/~boud/ArFus/}) jak również przesłanki obserwacyjne, aby spróbować rozwiązać zaobserwowaną rozbieżność. Rozwiązanie to może uwzględniać zarówno błędy w teoretycznej analizie, błędy w dotychczasowej analizie obserwacji, jak również nie standardowe właściwości ciemnej materii. Przewiduje się, że cząstki ciemnej materii, poza oddziaływaniami grawitacyjnymi biorą również udział w oddziaływaniach słabych i tego typu koncepcje mogą być badane w ramach hipotez o samooddziałującej ciemnej materii. (SIDM - self-interacting dark matter). Przykładowo, Totani (arXiv:astro-ph/0401140) wprowadza anihilację neutralin, jako dodatkowe źródło energii w centrach gromad galaktyk, wystarczające dla wypłaszczenia wewnętrznych części profili gęstości. Planujemy prześledzić każdą z tych możliwości, bez zakładania jakichkolwiek koncepcji, która z nich jest poprawna. Ponieważ gorąca ciemna materia (HDM) (na przykład masywne neutrina) może reprezentować jedynie małą część całej ciemnej materii, z powodu zaobserwowanego widma mocy fluktuacji gęstości, planujemy rozważać jedynie hipotezy dotyczące zimnej ciemnej materii (CDM). Techniki modelowania formowania się galaktyk, takie jak zawarte w pakiecie {\sc ArFus} umożliwiają stworzenie statystyk które mogą być porównane bezpośrednio z obserwacjami. Oczywistym problemem w obserwacjach ciemnej materii jest niemożliwość zaobserwowania jej bezpośrednio. To co jest obserwowane to gwiazdy w galaktyce (bądź neutralny wodór) oraz ich ruch. Hipotezy dotyczące natury (właściwości) ciemnej materii mogą być testowane poprzez modelowanie powstawania galaktyk, począwszy od warunków początkowych, aż do poszukiwanych obserwabli, poprzez uwzględnianie różnego typu przesłanek obserwacyjnych oraz postulowanych założeń. Na przestrzeniu ostatnich siedemdziesięciu lat wiele pracy włożono w poznawanie natury ciemnej materii. Jednakże, pomimo (bądź z powodu) ogromnej ilości danych obserwacyjnych sytuacja wciąż pozostaje bardzo nie jasna. Co więcej rozwikłanie problemu powstawania galaktyk jest również jednym z podstawowych problemów w polu obserwacyjnej kosmologii. % % this is too long - it's one page on this point. % %Dlatego też, potencjał zagadek związanych z naturą ciemnej materii daje tego typu badania wśród problemów o najwyższej randze %i priorytecie w zagadnieniach dzisiejszej obserwacyjnej kosmologii. % Rwnania Hilberta--Einsteina s niewystarczajce do opisania geometrii % Wszechwiata, poniewa nakadaj one ograniczenia tylko na pewn waciwoďż˝% lokalnej geometrii, mianowicie jej krzywiznďż˝ Pene poznanie geometrii % przestrzeni, jeli w ogle moliwe, wymaga take pomiaru topologii % Wszechwiata. Od czasu kiedy temat ten by poruszony w 1900r. przez % Schwarzschilda, prby obserwacyjne zmierzenia oglnej topologii byy rzadkie % w cigu caego XX. wieku, a wzmoone zostay dopiero w latach 90-tych w % rezultacie gwatownego wzrostu liczby obserwacji znacznej czďż˝i % obserwowalnego Wszechwiata. % % Fizyczne zaoenia pomiaru topologii Wszechwiata s cakiem proste z % teoretycznego (naiwnego?) punktu widzenia: wystarczy (,,tylko''!) znaleďż˝% {\bf wielokrotne obrazy} obiektw pozagalaktycznych, ktrych wiato biegnie % do obserwatora po liniach prostych (geodezyjnych) w rnych kierunkach, tzn. % promieniowanie z obiektw przemierza Wszechwiat rnymi drogami tak, i % dociera ono do obserwatora z rnych kierunkw, albo wiďż˝ej ni jeden raz. % Niezalenie zatem od tego, jaka teoria bďż˝zie w przyszoci opisywaďż˝oglny % ksztat Wszechwiata, termin ,,soczewkowanie topologiczne'' stanie siďż˝% prawdopodobnie rozszerzeniem Oglnej Teorii Wzglďż˝noci (OTW). I podobnie % jak soczewkowanie grawitacyjne polegajce na tym, e widzimy wiele obrazw % tego samego pojedynczego obiektu o duym przesuniďż˝iu ku czerwieni, jest % testem dla OTW, tak soczewkowanie topologiczne naoy warunki dla przyszej % (prawdopodobnie kwantowej) teorii grawitacji. % % W praktyce, podobnie zreszt jak to ma miejsce w przypadku wyznaczania % lokalnych parametrw kosmologicznych takich, jak parametr gďż˝toci materii, % staa kosmologiczna czy staa Hubble'a, ktre okazao siďż˝znacznie % trudniejsze ni pocztkowo siďż˝spodziewano, obserwowane waciwoci obiektw % pozagalaktycznych --- tak indywidualne jak i statystyczne --- sprawiaj, % e poszukiwanie zjawiska soczewkowania topologicznego jest trudne. % Najbardziej obiecujce obiekty o duych przesuniďż˝iach ku czerwieni nadajce % siďż˝do poszukiwania soczewkowania grawitacyjanego to te, ktre widzimy w % znacznych ilociach i w duych obszarach przestrzeni kosmicznej, a mianowicie: % (1) aktywne jdra galaktyk (AGN) i (2) gromady galaktyk. % % Podjďż˝ie tego typu bada w Centrum Astronomii UMK w Toruniu bďż˝zie % moliwe dziďż˝i sprzďż˝niu nastďż˝ujcych okolicznoci: % % \begin{list}{(\roman{enumi})}{\usecounter{enumi}} % {\item \parskip=-4pt % w CA-UMK od wielu lat prowadzi siďż˝badania nad radiowo % czynnymi AGN-ami (ze szczeglnym uwzglďż˝nieniem ich ewolucji), co w % szczeglnoci oznacza doskonae opanowanie metod i wyksztacenie zespou % (Marecki, Kunert, Gawroski) % \item w CA-UMK, w oparciu o posiadany 32-m radioteleskop, realizowny jest % projekt OCRA (One-cm Receiver Array), dziďż˝i ktremu mamy nadziejďż˝otrzymaďż˝% wkrtce (w oparciu o efekt Suniajewa-Zeldowicza) katalog tysiďż˝y gromad % galaktyk o duym przesuniďż˝iu ku czerwieni (Soberski); % \item kierownik projektu (B. Roukema) ma wietnie opanowane podstawy % teoretyczne w dziedzinie kosmologii i topologii Wszechwiata, a take % rozwin strategie obserwacyjne pozwalajce j badaďż˝ % }\end{list} % % \vspace{-10pt} % Mamy zatem doskona okazjďż˝ aby zesp CA-UMK skadajcy niniejszy wniosek % przyczyni siďż˝do rozwoju tej tematyki badawczej. W naszych badaniach % zamierzamy skupiďż˝siďż˝na analizie radiowo czynnych AGN-w (RLAGN) i gromad % galaktyk, jednakowo znajomoďż˝najnowszych bada waciwoci kosmicznego % promieniowania ta (CMB) bďż˝zie miaa kluczowe znaczenie dla niezalenego % sprawdzenia powanych kandydatw na zjawisko soczewkowania topologicznego. % Fortunn zatem okolicznoci jest doczenie do naszej grupy osoby % specjalizujcej siďż˝w badaniach kosmicznego promieniowania ta, mianowicie % studenta Bartosza Lwa, ktry --- mamy nadziejďż˝--- otrzyma w 2003 r. tytu % magistra i podejmie studia doktoranckie w CA-UMK. \clearpage \begin{flushleft} \textbf{C. INFORMACJE O WYKONAWCACH} \end{flushleft} \begin{flushleft} {\em 1. Oświadczenia} \end{flushleft} \begin{quote} {Przyjmuję warunki udziału w konkursie projektów badawczych, określone w przepisach w sprawie kryteriów i trybu przyznawania i rozliczania środków finansowych ustalanych w budżecie państwa na naukę oraz wyrażam zgodę na zamieszczenie moich danych osobowych zawartych we wniosku w zbiorze danych Komitetu Badań Naukowych oraz na przetwarzanie tych danych zgodnie z przepisami ustawy z dnia 29 sierpnia 1997 r. o ochronie danych osobowych (Dz. U. Nr 133, poz. 883 z pn. zm.).} \end{quote} \begin{flushleft} {\em 2. Wykaz wykonawców} \begin{tabular}{c|l|r|c|c} \hline \\ Lp. & \multicolumn{1}{c|}{Charakter udziału w realizacji projektu,} & Udział w & Symbol & {~~Podpis~~} \\ & \multicolumn{1}{c|}{tytuł i stopień naukowy, imię nazwisko, nr PESEL} & realizacji &\multicolumn{1}{c|}{rodzaju} & \\ &\multicolumn{1}{c|}{miejsce zatrudnienia, stanowisko} & projektu&&\\ 1 & Kierownik projektu - dr Boudewijn Roukema & \boudeffective\% & \symbolrodzaju\\ & CA-UMK, adiunkt \nipboud &&& \\ 6& Wykonawca - mgr. Bartosz Lew \peselbartek & 50\% &\symbolrodzaju\\ & CA-UMK &&& \\ &&&&\\ \hline \end{tabular} $^{\mathrm{1/}}$ należy wpisać, P''- umowa o pracę mianowanie, ,,Z''- umowa zlecenie, ,,D''- umowa o dzieło \end{flushleft} %%% end table %%%% \begin{flushleft} {\em 3. Ankieta dorobku naukowego kierownika projektu i najważniejszych wykonawców projektu} \end{flushleft} \begin{flushleft} {\em 1) Imię i nazwisko} \end{flushleft} dr Boudewijn Roukema \begin{flushleft} {\em 2) Przebieg pracy naukowej: nazwa szkoły wyższej, instytutu lub innej jednostki organizacyjnej specjalność} \end{flushleft} \begin{flushleft} {\em data uzyskania tytułu zawodowego, tytułu lub stopnia naukowego} \end{flushleft} \begin{flushleft} doktora \end{flushleft} 1989-93: Doktorat z Filozofii w Astronomii i Astrofizyce, Mt Stromlo and Siding Spring Observatories (M.S.S.S.O.), Australian National University (A.N.U.), Canberra. 1985-88: Bachelor of Science (Hons), Australian National University, Canberra, Australia \begin{flushleft} {\em 3) Informacje o pracach wykonanych w okresie ostatnich 4 lat przed zgłoszeniem wniosku} \end{flushleft} \begin{flushleft} {\em (wykaz najważniejszych publikacji - maksimum 10 pozycji, podać miejsce i datę publikacji; opracowane nowe technologie; najważniejsze osiągnięcia poznawcze, aplikacyjne).} \end{flushleft} Główne Tematy Badawcze %{Main Research Interests} (i) {\em Kosmologia obserwacyjna} i (ii) {\em Formowanie się galaktyk}: (i) Obserwacyjne ograniczenia nakładane na statystyki wielkoskalowych struktur i lokalne parametry kosmologiczne (takie jak parametr gęstości czy stała kosmologiczna) i programy obserwacyjne mające na celu określenie ogólnych parametrów kosmologicznych; (ii) Modele formowania się galaktyk w kontekście kosmologicznym i porównanie ich ze statystyką obserwowanych galaktyk. { \begin{list}{\arabic{enumi}}{\usecounter{enumi}} \parskip=-2pt \item \pub \underline{Roukema, B.F.} \& Bajtlik, S., 1999;;Transverse Galaxy Velocities from Multiple Topological Images;;\mnras;;308;;309 \ (arXiv:astro-ph/9903038) %% CAMK, IAP, IUCAA %art \item \pub \underline{Roukema, B.F.}, 2000a;;COBE and Global Topology: An Example of the Application of the Circles Principle;;\mnras;;312;;712 \ (arXiv:astro-ph/9910272) %% IUCAA %ftp blacksci 15/10/99 %art \mdcitem %\item \pub \underline{Roukema, B.F.} \& Mamon, G.A., 2000;;Tangential Large Scale Structure as a Standard Ruler: Curvature Parameters from Quasars;;\AandA;;358;;395 \ (arXiv:astro-ph/9911413) %art %%395-408 %\item \mdcitem \pub \underline{Roukema, B.F.}, 2000b;;A Counterexample to Claimed COBE Constraints on Compact Toroidal Universe Models;;\cqg;;17;;3951 \ (arXiv:astro-ph/0007140) \item \pub \underline{Roukema, B.F.}, 2000c;;The Topology of the Universe;;Bulletin of the Astronomical Society of India;;28;;483 \ (arXiv:astro-ph/0010185) \revinvit \item \pub \underline{Roukema, B.F.} \& Mamon, G.A., 2001;;Lifting cosmic degeneracy within a single data set;;{\AandA};;366;;1 \ (arXiv:astro-ph/0010511) \item \pub \underline{Roukema, B.F.}, 2001b;;How to distinguish a nearly flat Universe from a flat Universe using the orientation independence of a standard ruler;;{\AandA};;369;;729 \ (arXiv:astro-ph/0102095) %art \item \pub \underline{Roukema, B.F.}, 2001d;;On the comoving distance as an arc-length in four dimensions;;{\mnras};;325;;138 \ (arXiv:astro-ph/0102099)%art \item \pub \underline{Roukema, B.F.}, Ninin, S., Devriendt, J., Bouchet, F.B., Guiderdoni, B., Mamon, G.A., 2001;;Star Formation Losses Due to Tidal Debris in Hierarchical Galaxy Formation;;\AandA;;373;;494 \ (arXiv:astro-ph/0105152) %art \item \pub \underline{Roukema, B.F.}, Mamon, G.A., \& Bajtlik, S., 2002;;The Cosmological Constant and Quintessence from a Correlation Function Comoving Fine Feature in the 2dF Quasar Redshift Survey;;{\AandA};;382;;397 \ (arXiv:astro-ph/0106135) \end{list} } \begin{flushleft} {\em 4) Wykonane i aktualnie wykonywane projekty badawcze finansowane ze środków budżetowych na naukę - numery projektów - charakter udziału przy realizacji projektu oraz czy uzyskał lub uzyskuje z tego tytułu wynagrodzenie (tak, nie). } \end{flushleft} \begin{flushleft} {\em 5) Doświadczenia naukowe zdobyte w kraju i za granicą (kraj, instytucja, rodzaj pobytu, okres pobytu).} \end{flushleft} \noin od 2002: adiunkt, Toruń Centre for Astronomy, Uniwersytet Mikołaja Kopernika, Toru\'n, Poland \noin 2001: konsultant, DARC/LUTH (Laboratoire de l'Univers et ses Th\'eories), Observatoire de Meudon, France \noin 1998--2000: postdoctoral fellow, Inter-University Centre for Astronomy \& Astrophysics, Pune, India \noin Feb--July 1998: konsultant, CAMK, Warszawa %\noin May-Sep 1997: konsultant, Institut d'Astrophysique % de Paris, CNRS, France %(R) %\noin April 1997: konsultant, Beijing %Astronomical Observatory, Beijing, P.R.China %(R) \noin 1996--1997: Centre of Excellence foreign visiting fellow, NAOJ, % Mitaka, Tokyo, %181, Japan %(R) %\smallskip \noin 1994--1995: postdoctoral research fellow, Astronomy Centre, University of Sussex, U.K. %(RT) %United Kingdom %\smallskip %\noin Aug/Sep 1994: Visitor, Dept of Astronomy, Bandung Institute of %Technology, Bandung, Indonesia %(T) %\smallskip \noin Jan/Feb 1994: konsultant, Institute of Astronomy, University of Cambridge, United Kingdom %(R) %\smallskip \noin 1993: postdoctoral fellow, Institut d'Astrophysique de Paris, CNRS, France %(R) \begin{flushleft} {\em 6) Najważniejsze międzynarodowe i krajowe wyróżnienia wynikające z prowadzenia badań naukowych lub prac rozwojowych (rodzaj wyróżnienia, miejsce i data).} \end{flushleft} %\begin{flushleft} % %\end{flushleft} % %\begin{flushleft} % %\end{flushleft} % \begin{flushleft} Miejscowość i data \rule{2cm}{0ex} Podpisy osób wypełniających ankietę\end{flushleft} \bigskip %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{flushleft} \textbf{\newpage } \end{flushleft} \begin{flushleft} \textbf{D. OPIS PROJEKTU BADAWCZEGO, METODYKA BADAŃ ORAZ CHARAKTERYSTYKA OCZEKIWANYCH WYNIKÓW} \end{flushleft} \begin{flushleft} {\em 1. Cel naukowy projektu --- jaki problem wnioskodawca podejmuje się rozwiązać, co jest jego istotą, co uzasadnia podjęcie tego problemu w Polsce, jakie przesłanki skłaniają wnioskodawcę do podjęcia proponowanego tematu?} \end{flushleft} Postawiony problem polega na porównaniu roli jaką zgodnie z teorią może grać nie barionowa ciemna materia w procesie formowania się galaktyk, z obserwacyjnymi obwarowaniami, w kontekście profili gęstości nie barionowej ciemnej materii w galaktykach i gromadach galaktyk. Opisany problem przedsięwzięto ponieważ około 25\% gęstości materii-energii we Wszechświecie składa się z przynajmniej jednego typu cząstek, który jak dotąd nigdy jeszcze nie został wykryty w żadnym laboratorium. Ta nie barionowa ciemna materia została wykryta poprzez jej grawitacyjny wpływ na astrofizyczne obiekty w szerokim zakresie skal odległości i jest całkiem prawdopodobne, że lepsze symulacje procesów formowania się galaktyk mogą nałożyć dalsze ograniczenia na własności tej nieznanej cząstki (cząstek). Te badania powinny zostać przeprowadzone w Polsce gdyż właśnie tutaj historia głównych odkryć astronomicznych ma swoje silne korzenie i chcielibyśmy ją dalej budować. \begin{flushleft} {\em 2. Istniejący stan wiedzy w zakresie tematu badań --- jaki oryginalny wkład wniesie rozwiązanie postawionego problemu do dorobku danej dyscypliny naukowej w świecie i w Polsce, czy w kraju i w świecie jest to problem nowy czy kontynuowany i w jakim zakresie weryfikuje utarte poglądy i dotychczasowy stan wiedzy?} \end{flushleft} Obecny stan wiedzy dotyczący profili gęstości ciemnej materii w galaktykach i gromadach galaktyk, na podstawie wielu obserwacji wykazuje, że ich wewnętrzne części są bardziej płaskie (mniej skoncentrowane) niż by to wynikało z klasycznego profilu Navarro, Frenk \& White (ApJ, 462, 563, 1996): \begin{equation} {\delta(r) \over \delta_{\mbox{crit}}} = {\delta_c \over (r/r_s) (1+ r/r_s)^2} \nonumber \end{equation} otrzymanego z symulacji wielu ciał, gdzie ${r_s = r_{200}/c}$ jest promieniem zależnym od zwirializowanego promienia $r_{200}$, $c$ jest parametrem koncentracji, natomiast $\delta_c$ bezpośrednio zależy od $c$ bez żadnych wolnych parametrów. Chociaż nachylenie profilu jest tutaj bardziej strome w centrum niż w zewnętrznych regionach, jest ono i tak dużo bardziej strome w porównaniu z obserwacjami. Nie wiemy z góry czy projekt potwierdzi czy podważy teoretycznie oczekiwane profile gęstości. Mamy nadzieje, że projekt przyczyni się do przyspieszenia odkrycia, oraz lepszego rozumienia procesu powstawania struktur, poprzez wyjaśnienie natury i przyczyn przedstawionej rozbieżności pomiędzy teorią a obserwacją profili gęstości, jak również że da on pewne wskazówki na temat tego jak właściwości cząstek ciemnej materii --- jak dotąd nie zarejestrowanych w naziemnych laboratoriach --- mogą zawęzić pole poszukiwań obserwacyjnych. Wynikiem mogą być wskazówki dotyczące natury nie barionowej ciemnej materii, które są komplementarne do tych które mogą być otrzymane poprzez bezpośrednie metody detekcji w dedykowanych eksperymentach (przekrój czynny na różnego rodzaju procesy i masa cząstki) jak na przykład gęstość ciemnej materii w galaktykach i gromadach galaktyk. Problem ciemnej materii generalnie sięga wstecz około siedemdziesięciu lat, jednakże problem centralnych zagęszczeń istnieje dopiero od około połowy dekady. (Główną rolę w tej dziedzinie stanowią profile gęstości z 1996r. autorstwa Navarro-Frenk-White) \begin{flushleft} {\em 3. Metodyka badań --- co stanowi podstawę naukowego warsztatu wnioskodawcy i jak zamierza rozwiązać postawiony problem, na czym będzie polegać analiza i opracowanie wyników badań, jakie urządzenia (aparatura) zostaną wykorzystane w badaniach, czy wnioskodawca ma do nich bezpośredni dostęp i umiejętność obsługi?} \end{flushleft} Zaproponowana metodologia polega na dalszym rozwijaniu pakietu {\sc ArFus} ``hybrid'' - oprogramowania służącemu formowaniu się galaktyk (dostępnego pod adresem:\\ \url{http://adjani.astro.uni.torun.pl/~boud/ArFus/}), oraz na sprawdzeniu różnych teoretycznych koncepcji. Nie ma gwarancji, że problem zostanie rozwiązany, jednakże jest prawdopodobne, że zostanie poczynionych kilka kroków we właściwym kierunku. Wymagany sprzęt obejmuje wydajne zasoby obliczeniowe, zarówno pod względem sprzętowym jak i oprogramowania. Posiadamy jedną wersje pakietu ({\sc ArFus}), możemy również użyć innych. Podczas gdy posiadamy już sprzęt aby zacząć projekt, ubiegamy się o zakup czterech komputerów w celu zbudowania komputera klastrowego i zwiększenia w ten sposób możliwości mocy obliczeniowej dla symulacji. Boudewijn Roukema posiada rozległe doświadczenie w zakresie dedykowanego oprogramowania {\sc ArFus}, natomiast Bartosz Lew posiada ogólne doświadczenie w symulacjach komputerowych w systemach wielozadaniowych w szczególności z analiz danych kosmicznego promieniowania tła dostarczonych przez satelitę WMAP. \begin{flushleft} {\em 4. Co będzie wymiernym, udokumentowanym efektem podjętego problemu --- zakładany sposób przekazu i upowszechnienia wyników (publikacje naukowe oraz referaty na konferencjach w kraju i za granicą, monografie naukowe, rozprawy doktorskie i habilitacyjne, nowe patenty i ,,know-how'', nowe metody i urządzenia badawcze)?} \end{flushleft} Przewidywanymi rezultatami mogą być rozwiązanie problemu profili gęstości, na przykład stwierdzenie teoria źle przewiduje wysoce skoncentrowane profile gęstości z powodu zbytniego uproszczenia zakładanych w modelu zachodzących procesów fizycznych bądź potwierdzenie samego problemu oraz wytłumaczenie jakie właściwości cząstek ciemnej materii prowadzą do zgodności z obserwacją. Prace z wynikami oczywiście będą opublikowane w recenzowanych żurnalach i prezentowane na konferencjach. Zarówno profesjonaliści jak i amatorzy będą mogli śledzić rozwój (i może również partycypować) w badaniach poprzez nasze strony internetowe na ogólnych zasadach budowania kultury internetowej, w postaci na przykład archiwizowanej, publicznie dostępnej listy dyskusyjnej. \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{E. W ODNIESIENIU DO PROJEKTÓW ZAMAWIANYCH -- INFORMACJA O SPEŁNIENIU OKREŚLONYCH PRZEZ KOMITET WARUNKÓW UCZESTNICZENIA W KONKURSIE, W SZCZEGÓLNOŚCI DOTYCZĄCYCH WSPÓŁPRACY Z PARTNERAMI ZAGRANICZNYMI} \end{flushleft} \clearpage \begin{flushleft} \textbf{F. }\textbf{ HARMONOGRAM WYKONANIA PROJEKTU BADAWCZEGO -- PLAN ZADAŃ} \end{flushleft} %\begin{center} %Lp.Nazwa i opis zadaniaTermin realizacji %\\(m-c, rok)Przewidywane koszty\\(z)1234Razem %\end{center} %\begin{flushleft} %\textbf{F. PROJECT} \textbf{SCHEDULE} \textbf{- ANTICIPATED TASKS} %\end{flushleft} \setcounter{x}{(\saltotalyear) /2} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *6} \renewcommand\y{\arabic{y}} \setcounter{z}{\consult /3} \renewcommand\z{\arabic{z}} \setcounter{w}{\y + \equip + \z*3 +\allconfer + \adminone+ \admintwo+ \adminthree } \renewcommand\w{\arabic{w}} \usecounter{enumi} \begin{center} \begin{tabular}{clrr} \hline \\ Lp. & Nazwa i opis zadania %Termin realizacji %&(m-c, rok)Przewidywane koszty %&(z)1234Razem & \multicolumn{1}{c}{Termin} & \multicolumn{1}{c}{Przewidywane} \\ %Expected cost (z) \\ & & \multicolumn{1}{c}{realizacji} & \multicolumn{1}{c}{koszty (z)} \\ & & \multicolumn{1}{c}{(m-c, rok)} & \\ \\ \addtocounter{enumi}{1} \arabic{enumi} & aktualizacja {\sc ArFus} do pracy na komputerze klastrowym %and evolution effects of multiple images & 6/2005 & \x~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & profile gęstości w galaktykach karłowatych % application to individual candidate pairs & 12/2005 & \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} % & zakup komputerów i peryferiów %purchase computer items & 12/2005 & \equip~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & międzynarodowe konsultacje kosmologiczne % international cosmology consultants & 12/2005 & \z~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & konferencje, public relations & 12/2005 & \allconferyear~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & koszty pośrednie & 12/2005 & \adminone~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & modelowanie profili ciemnej materii w gromadach galaktyk %predictions of further images & 6/2006 & \x~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & udoskonalanie ``obserwacyjnych'' wyników z pakietu {\sc ArFus} %statistical analysis of RLAGN catalogues & 12/2006 & \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & międzynarodowe konsultacje kosmologiczne %international cosmology consultants & 12/2006 & \z~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & konferencje, public relations & 12/2006 & \allconferyear~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & koszty pośrednie & 12/2006 & \admintwo~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & oprogramowanie samooddziałującej ciemnej materii w pakiecie {\sc ArFus} & 6/2007& \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} &analiza hipotezy samooddziałującej ciemnej materii %predictions of further images & 12/2007 & \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & międzynarodowe konsultacje kosmologiczne %international cosmology consultants & 12/2007 & \z~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & konferencje, public relations & 12/2007 & \allconferyear~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & koszty pośrednie & 12/2007 & \adminthree~PLN % % \\ \hline & & Razem & \w~PLN \\ \hline \end{tabular} \end{center} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{flushleft} {\footnotesize{}\newpage } \end{flushleft} \begin{flushleft} \textbf{G. KOSZTORYS PROJEKTU BADAWCZEGO} \end{flushleft} \begin{flushleft} {\em 1. Poszczególne pozycje kosztorysu w cenach bieżących (w zł)} \end{flushleft} % \begin{center} % Lp.Treďż˝lanowane koszty w roku budżetowym %Razem12345671Koszty bezpośrednie, w tym: %1/ Wynagrodzenia z pochodnymi 2/ Koszty zakupu aparatury naukowo - %badawczej 3/ Inne koszty realizacji projektu2Koszty pośrednie %3Koszty ogółem finansowane ze środkw na naukę˝(1+2) % \end{center} \begin{center} \begin{spacing}{1.24} \setcounter{y}{\saltotalyear + \saltotalyear + \saltotalyear} \renewcommand\y{\arabic{y}} \setcounter{z}{\consult /3} \renewcommand\z{\arabic{z}} \begin{tabular}{llrrr|r} \hline Lp. & Treść˝& \multicolumn{3}{c}{Planowane koszty} & \\ & & \multicolumn{3}{c}{w roku budżetowym (z)} & \\ %1 1/ 2/ Koszty zakupu aparatury naukowo - badawczej %3/ Inne koszty realizacji projektu2Koszty porednie3Koszty %ogem finansowane ze rodkw na naukę˝(1+2) %No. Item & \multicolumn{3}{c}{Funds for each budget year (z)} % & Total \\ & & 2005 & 2006 & 2007 & Razem \\ % 1&2&3&4&5&6 \\ {\bf 1} & Koszty bezpośrednie, w tym: &&&& \\ {\footnotesize{}1/ } & Wynagrodzenia z pochodnymi %Salaries and benefits & \saltotalyear & \saltotalyear & \saltotalyear & \y~PLN \\ % % {\footnotesize{}2/} &Koszty zakupu aparatury naukowo - badawczej %Equipment & \equip & & & \equip~PLN\\ % {\footnotesize{}3/} &Inne koszty realizacji projektu %Other direct costs &&&&\\ % &mięďzynarodowe konsultacje kosmologiczne %international cosmology consultants & \z &\z &\z & \consult~PLN \\ % &konferencje, public relations & %conferences, public relations & \allconferyear &\allconferyear &\allconferyear & \allconfer~PLN \\ \hline % &{\bf 1} Razem & \subone & \subtwo& \subthree & \suball~PLN \\ &&&&\\ {\bf 2} & \multicolumn{4}{l|}{ Koszty pośrednie (koszty admin UMK -- 30\% 1/ + 3/)} %Indirect costs %(admin costs to UMK - 25\% 1st yr; 30\% 2nd, 3rd yrs)} &\\ && \adminone & \admintwo & \adminthree & \adminall~PLN \\ \hline {\bf 3} &Koszty ogółem finansowane ze &&&& \\ &środków na naukę({\bf 1+2}) & \totalone &\totaltwo &\totalthree& \totalall~PLN \\ \hline \end{tabular} \end{spacing} \end{center} \begin{flushleft} {\em 2. Kalkulacja poszczególnych pozycji kosztorysu} \end{flushleft} \begin{flushleft} {\em 1) Wynagrodzenia z pochodnymi} \end{flushleft} \setcounter{w}{(\boudeffective*\monthstotal)/100} \renewcommand\w{\arabic{w}} \setcounter{x}{(\salrate *50)/100} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *3} \renewcommand\y{\arabic{y}} \begin{flushleft} {\em Kierownika projektu - liczba osobomiesięcy udziału w projekcie: {\bf \w} , forma wynagrodzenia, } \end{flushleft} Według reguł KBN, 100\% \salrate{}PLN/rok dla kierownika projektu jeśli dr., 75\% dla innych wykonawców jeśli dr., 50\% \salrate{}PLN/rok dla innych wykonawców jeśli mgr. Jednakże, dla tego projektu, postanawiamy dać takie samo wynagrodzenie obu uczestnikom. Więc: \begin{list}{(\roman{enumi})}{\usecounter{enumi}} %\setcounter{x}{\salrate *3} \renewcommand\x{\arabic{x}} \item dr Boudewijn Roukema \x{}~PLN *3 = \y~PLN \end{list} \setcounter{x}{(\monthstotal *(\persontotal-\boudeffective))/100} \renewcommand\x{\arabic{x}} \begin{flushleft} {\em Wykonawców projektu - liczba osobomiesięcy udziału w projekcie: {\bf \x} , forma wynagrodzenia.} \end{flushleft} \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \addtocounter{enumi}{1} \setcounter{x}{(\salrate *67)/100} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *3} \renewcommand\y{\arabic{y}} % %\item dr Andrzej Marecki \x~PLN *3 = \y~PLN % \setcounter{x}{(\salrate *50)/100} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *3} \renewcommand\y{\arabic{y}} % \item mgr Bartosz Lew \x~PLN *3 = \y~PLN \end{list} \setcounter{x}{(\salrate *(\monthstotal/12)*(\persontotal))/100} \renewcommand\x{\arabic{x}} Razem: \x~PLN \begin{flushleft} {\em 2) Opis planowanych zakupów lub wytworzenia aparatury naukowo- badawczej (podaż nazwa zakupu, planowany koszt, planowany miesiąc i rok zakupu oraz merytoryczne uzasadnienie zakupu).} \end{flushleft} %\prefixing Uzasadnienie: Modelowanie formowania się galaktyk oraz wyznaczanie roli ciemnej materii w centrach galaktyk wymaga dużej mocy obliczeniowej. Potrzebujemy również komputera w celu prezentowania rezultatów na seminariach, konferencjach bądź innych działalnościach związanych z udostępnianiem i rozpowszechnianiem wyników pracy. \newcommand\oldequipjustification{ {\bf COMMENT OUT THE LINE {$\backslash$}oldequipjustification TO HIDE THIS} Uzasadnienie: Wymienione zespoły komputerów i podzespoły są potrzebne dla syntezy i analizy danych doświadczalnych, oraz dla stworzenia sumarycznego rezultatu w postaci wyników projektu (prezentacja i dostępność wyników). Porwnywanie par obiektw w duych katalogach jest operacj czasochonn (jak $N^2$), wymagajc duej mocy obliczeniowej. Mona j przyspieszyďż˝poprzez wprowadzenie odgrnych zaoe. Jednake, historia astronomii pokazuje, e przyjmowanie ,,rozsdnych'', ale {\it de facto} zych zaoe, czďż˝to prowadzi do przeoczenia prawdziwego sygnau, tak wiďż˝ posiadanie duej mocy obliczeniowej byoby z korzyci dla projektu. } %\oldequipjustification Planowane zakupy na rok 2005: \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \item komputer klaster do symulacji - cztery komputery \item {\nups} jednostki ,,uninterrupted power supply'' (UPS), obie \ups~PLN, razem= \upstotal~PLN \item komputer do analizy (B. Lew) % - AMD Athlon, 2GHz, 512Mb RAM, 100Gb hard disk, %CD burner, ethernet card, 19'' screen + 3 letnie ubezpieczenie przed kradzieżą itd. \perso~kPLN \item komputer do analizy (B. Roukema) % - AMD Athlon, 2GHz, 512Mb RAM, %100Gb hard disk, CD burner, ethernet card, 19'' screen + 3 letnie ubezpieczenie przed kradzieżą itd. \perso~kPLN \item przenośny komputer (dla wszystkich członków grupy) + 3 letnie ubezpieczenie przed kradzieżą itd. \portable~kPLN \item inkjet drukarka atramentowa/skaner/fotokopiarka + 3 letnie ubezpieczenie przed kradzieżą itd. (np. inkjet PSC 750 kosztuje 900PLN; odzyskane pojemniki na tusze kosztują około 35~PLN B/W, 50~PLN kolorowe) 1~kPLN \item drukarka laserowa/skaner/fotokopiarka + 3 letnie ubezpieczenie przed kradzieżą itd. 7~kPLN \item papier + tuszy dla drukarki 2~kPLN \end{list} Razem: \equip~PLN \smallskip \begin{flushleft} {\em 3) Uzasadnienie wysokości planowanych innych kosztów realizacji projektu (wymienić rodzaj kosztów, wysokość oraz ich powiązanie z planem zadań projektu).} \end{flushleft} Koszty te odnoszą się do planu projektu w tym sensie, iż projekt jest jednym rozwijanych na świecie kierunkiem badań więc (1) potrzebni są zagraniczni konsultanci dla umożliwienia wymiany poglądów, konstruktywnej krytyki oraz wglądu do naszej strategii, jak również (2) musimy mieć możliwość prezentacji naszych wyników na międzynarodowych konferencjach i konsultacji ze światowymi ekspertami w ich placówkach badawczych. \smallskip (1) Konkurowanie z innymi tego typu projektami na świecie wymaga konsultacji ze światowymi ekspertami w okresie od 1~tygodnia do kilku miesięcy. Trzy osoby każda po jednym miesiącu i cztery osoby każda po jednym tygodniu w ciągu jednego roku daje w sumie {\consultpm}~osobo-miesięćy w okresie 3~lat trwania projektu. Koszt \consultrate PLN/miesiąc na opłacenie zagranicznych konsultantów z dziedziny kosmologii daje razem: {\consult}~PLN. \smallskip (2) W celu prezentacji naszych wyników na konferencjach i innych spotkaniach naukowych, uczestnictwo na dwóch międzynarodowych konferencjach na osobę na rok byłoby zgodne z światowymi standardami. Koszt konferencji: typowy przejazd pociągiem klasy drugiej (lub lot samolotem) w Europie lub podróż samolotem do USA średnio wynosi 2000 PLN; międzykontynentalny lot (economy class) (Indie/Japonia/Australia) nie przekracza 10000 PLN; tak więc średnio 3.5 kPLN jest bezpiecznym kompromisem. Tygodniowe zakwaterowanie i dieta w Europie/USA/Japonii/Australii (2kPLN) + opłaty rejestracyjne (1 kPLN) $\Rightarrow$ \oneconfer~PLN. Tak więc dwie konferencje rocznie dla wszystkich osób znajdują się w zalecanych granicach wydatków. \setcounter{x}{\persontotal/100} \renewcommand\x{\arabic{x}} \setcounter{y}{\persontotal-100*(\persontotal/100)} \renewcommand\x{\arabic{x}} Dwie konferencje rocznie na efektywną osobę oraz \x{}.\y{} efektywnej osoby w okresie trzech lat daje: Razem: \allconfer~PLN \smallskip W celu zwiększenia przejrzystości i odpowiedzialności oraz zyskania elastyczności, wszyscy członkowie komisji są mile widziani w naszej archiwizowanej, publicznie dostępnej liście dyskusyjnej, ze wszystkimi naukowo przydatnymi komentarzami, sugestiami lub/i krytyką: \\ \url{http://www.astro.uni.torun.pl/sympa/cosmo-torun} \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{H. OŚWIADCZENIA I PODPISY} \end{flushleft} \begin{flushleft} 1. Oświadczam, że zapoznałem się z wnioskiem o finansowanie projektu badawczego pt.: {\bf Modelowanie procesów powstawania galaktyk i ograniczenia na profile rozkładu ciemnej materii w galaktykach i gromadach galaktyk. {\em (Galaxy formation modelling and constraints on Dark Matter Profiles in Galaxies and Galaxy Clusters) }} \end{flushleft} \begin{flushleft} 2. W przypadku przyjęcia projektu badawczego do finansowania jednostka zobowiązuje się do: \end{flushleft} \begin{flushleft} - włączenia projektu do planu zadaniowo-finansowego jednostki, \end{flushleft} \begin{flushleft} - udostępnienia lokalu, aparatury i obsługi administracyjno-finansowej, \end{flushleft} \begin{flushleft} - zatrudnienia pracowników niezbędnych do realizacji projektu, zgodnie z wnioskiem, na podstawie umowy o pracę, umowy o dzieło lub umowy zlecenia, \end{flushleft} \begin{flushleft} - sprawowania nadzoru nad prawidłowością wydatkowania środków finansowych przeznaczonych na realizację projektu, a w przypadku stwierdzenia nieprawidłowości --- do niezwłocznego powiadomienia Komitetu. \end{flushleft} \begin{flushleft} 3. Oświadczam, że jednostka nie może zapewnić dostępu do urządzeń wymienionych w wykazie aparatury w dziale G ust. 2 pkt 2. \end{flushleft} \begin{flushleft} 4. Oświadczam, że wniosek nie obejmuje doświadczeń na ludziach lub zwierzętach $^{\mathrm{2)}}$. % \sout comes from \usepackage{ulem} \sout{Do wniosku dołączono zgodę właściwej komisji etycznej na przeprowadzenie doświadczeń na zwierzętach lub na przeprowadzenie innych badań objętych właściwością komisji.} $^{\mathrm{2)}}$ \end{flushleft} \begin{flushleft} 5. Oświadczam, że zgodnie z moją wiedzą przygotowany wniosek o finansowanie projektu badawczego nie narusza praw osób trzecich. \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} $^{\mathrm{2) }}$Niepotrzebna skreślić. \end{flushleft} \begin{flushleft} \end{flushleft} \clearpage \begin{flushleft} Wniosek sporządzono w dniu: \datepolski %31 stycznia 2004 \end{flushleft} \vspace {1.5cm} \begin{flushleft} \begin{tabular}{cccc} {\em Pieczęć jednostki} & Kierownik jednostki & Kwestor & Kierownik projektu \\ & Prorektor ds. Nauki i Współpracy\\ & z Zagranic\c{a} \\ & prof dr. hab. Marek Zaidlewicz & mgr Henryk Heldt & dr Boudewijn Roukema \\ \\ \\ \\ & podpis i pieczęć & podpis i pieczęć & podpis \end{tabular} \end{flushleft} \begin{center} \end{center} \setlength{\oddsidemargin}{0.472222in-1in} \setlength{\textwidth}{\paperwidth - 0.472222in-0.472222in} \begin{center} \end{center} \begin{flushleft} \end{flushleft} \end{document} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

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from the French PNC - conférences (fwd)
by Boud Roukema 26 Jan '04

26 Jan '04

---------- Forwarded message ---------- > Date: Mon, 26 Jan 2004 09:45:18 +0100 (CET) > From: Programme National de Cosmologie <pnc at iap.fr> > To: diffusion PNC <pnc at iap.fr> > Subject: [iso-8859-1] conférences --------------------------------------------------------------------------- PNC PNC PNC http://www.iap.fr/pnc/ PNC PNC PNC PNC --------------------------------------------------------------------------- message # 207 26 janvier 2004 1. STScI May Symposium - 3-6 mai 2004 - Baltimore (Maryland) Planets to Cosmology: Essential Science in Hubble's Final Years 2. Vth Marseille International Cosmology Conference Marseille - 21-25 juin 2004 3. 20th IAP colloquium on CMB physics and observation IAP - 28 juin 2004 / 2 juillet 2004 4. COSMO 04 - CITA (Toronto, Canada) - 17-21 septembre 2004 --------------------------------------------------------------------------- PNC PNC PNC http://www.iap.fr/pnc/ PNC PNC PNC PNC --------------------------------------------------------------------------- 1. STScI May Symposium - 3-6 mai 2004 - Baltimore (Maryland) Planets to Cosmology: Essential Science in Hubble's Final Years Dear Colleague, This is the Second Announcement of the upcoming Symposium at the Space Telescope Science Institute. Additional information can be found on the Symposium's web page at: http://sd.stsci.edu/Planets_to_Cosmology/index.html WE ARE SOLICITING CONTRIBUTED TALKS. IF YOU ARE INTERESTED IN PRESENTING SUCH A TALK, PLEASE SEND A TITLE AND AN ABSTRACT TO THE SYMPOSIUM'S ADMINISTRATIVE COORDINATOR, QUIN GRYCE (gryce(a)stsci.edu) BY FEBRUARY 15, 2004. PLANETS TO COSMOLOGY: ESSENTIAL SCIENCE IN HUBBLE'S FINAL YEARS _______________________________________________________________ The upcoming STScI May Symposium will take place May 3-6, 2004, with registration and a reception on May 2.The Symposium will concentrate on the most recent science to have been accomplished by HST and other observatories and on potential future advances. A broad range of topics will be covered, with sessions devoted to: - Planets (both in the solar system and extrasolar); - Star Formation (in the Local Group, in clusters); - Black Holes (at galaxy centers, potential existence in globular clusters); - The ISM and the IGM (the baryon content, feedback); - Galaxy Formation and Evolution (mass assembly, morphological evolution); - Cosmology (the nature of dark energy, high-z suprenovae, gravitational lensing); - The Hubble Ultra Deep Field. The Program will be composed primarily of invited talks, with a small number of contributed talks. We are soliciting contributed talks. If you are interested in presenting such atalk, please send a title and an abstract to the Symposium's Administrative Coordinator, Quin Gryce (gryce(a)stsci.edu), by February 15, 2004. If you intend to present a poster, please indicate so on the registration form. ORGANIZING COMMITTEE --------------------- Mario Livio (Chair), Daniela Calzetti, Stefano Casertano, Harry Ferguson, Ron Gilliland, Sangeeta Malhotra, Bruce Margon, Adam Riess, Massimo Robberto, Ken Sembach, Rachel Somerville, William Sparks, Massimo Stiavelli. PRELIMINARY LIST OF CONFIRMED TALKS ----------------------------------- Opening Talk, Motivation - John Bahcall (1) Planets ____________ Transits and Atmospheres- Dave Charbonneau Direct Planet Detections - Mark Clampin Solar System - Mike A'Hearn (2) Star Formation in the Local Universe __________________________________________ Open Questions in Star Formation - Cathie Clarke Star Formation in the Locaol Group - Eva Grebel Star Formation in Clusters - Soeren Larsen (3) AGN, Black Holes _____________________ Black Holes in Galaxy Centers and Globular Clusters - Laura Ferrarese Galaxy Centers - Tim de Zeeuw Quasar Hosts - Kim McLeod (4) Galaxy Formation and Evolution __________________________________ Morphological Evolution - Marijn Franx Galaxy Assembly - Eric Bell Reionization - Zoltan Haiman (5) IGM, ISM, Feedback ________________________ IGM and Feedback - Alice Shapley The Baryon Content - Mike Shull ISM - Blair Savage (6) The Hubble Ultra Deep Field _________________________________ The Hubble Ultra Deep Field - Steve Beckwith The HUDF with NICMOS - Rodger Thompson (7) Cosmology _______________ Dark Energy from Supernovae - John Tonry The Nature of Dark Energy - David Weinberg Cosmology from Gravitational Lensing - Bhuvnesh Jain Summary Talk - John Huchra --------------------------------------------------------------------------- PNC PNC PNC http://www.iap.fr/pnc/ PNC PNC PNC PNC --------------------------------------------------------------------------- 2. Vth Marseille International Cosmology Conference Marseille - 21-25 juin 2004 Vth MARSEILLE INTERNATIONAL COSMOLOGY CONFERENCE http://www.oamp.fr/marseille2005 Tuesday, 21 June 2005 - Saturday, 25 June 2005 The Fabulous Destiny of Galaxies:Bridging Past and Present Ten years after the first deep redshift surveys, the Lyman-break galaxies and the Hubble Deep Field, cosmic star formation rate, mass assembly, re-ionization, feedback, ... have become usual words. They all convey a desire for a global view on the fate of matter in the Universe even though observations are difficult and discordant in some instances. Time is ripe to look at these difficulties in a proper perspective and under the light of a number of recent surveys or missions (GOODS, COSMOS, HUDF, VVDS, GALEX, SIRTF, to name a few). They are expected to provide larger time scale, larger space coverage and better homogeneity in connecting the past and present Universe. --------------------------------------------------------------------------- PNC PNC PNC http://www.iap.fr/pnc/ PNC PNC PNC PNC --------------------------------------------------------------------------- 3. 20th IAP colloquium on CMB physics and observation IAP - 28 juin 2004 / 2 juillet 2004 Dear colleagues, We are pleased to announce the 20th IAP colloquium on Cosmic Microwave Background physics and observation, to be held at the Institut d'Astrophysique de Paris, from Monday June 28 to Friday July 2d 2004. This meeting will conclude the successful European network CMBNET, and we hope it will serve as a kick-off meeting of its successor, CMB-Planet, in case it is funded. After a series of observational results that culminated in the WMAP results of last year, CMB observations have dramatically sharpened our view of the Universe in the last five years. In the mean time, the recently discovered CMB polarization, bearing new cosmological information, is getting increasing attention, and indeed most of the upcoming CMB experiments are targetting polarization. The second release of WMAP is also now imminent. It should be a good time to assess what we have learnt as of today, both from the theoretical and experimental points of view, from this very rich period; to discuss the likely stumbling block on the way forward, and new physics that the future CMB experiments will be able to help reveal, and the new experimental and data-processing techniques that need to be developped in their context. The meeting will focus namely on the following topics: Early Universe theory and CMB physics, main CMB experiments (past and future), cosmological parameters extraction, Sunyaev-Zeldovich effect, CMB and gravitational lensing, Integrated Sachs-Wolf detection, reionisation, Galactic and extragalactic foregrounds, data processing methods and experimental developments. Schedule: - Web site opening at http://www.iap.fr February 1st - Registration deadline: April 1st Scientific Organizing Committee: D. Bond, F. R. Bouchet (Chair), M. Demianski, R. Durrer, G. Efstathiou, D. Egret, E. Martinez-Gonzalez, J. Peebles, A. Starobinski, J. Silk, D. Spergel, R. Sunyaev, N. Vittorio --------------------------------------------------------------------------- PNC PNC PNC http://www.iap.fr/pnc/ PNC PNC PNC PNC --------------------------------------------------------------------------- 4. COSMO 04 - CITA (Toronto, Canada) - 17-21 septembre 2004 COSMO 04 FIRST ANNOUNCEMENT ============== Dear Colleague, As you may know this year's edition of the annual Cosmo International Conference on Particle Physics and Cosmology -- Cosmo04 -- will be hosted by the Canadian Institute for Theoretical Astrophysics in Toronto between Friday September 17 till Tuesday September 21, 2004. The conference will take place at the downtown campus of the University of Toronto. Cosmo-04 will be the eighth in the Cosmo series after Ambleside, UK 97 and 03; Asilomar, US 98; Trieste, Italy 99; Cheju Island, Korea 2K; Rovaniemi, Finland 01, Chicago, US 02. The Cosmo series is one of the major venues of interaction between cosmologists and particle physicists. The Conference will be devoted to the modern interfaces between Fundamental and Phenomenological Particle Physics and Physical Cosmology and Astronomy. The topics covered at the meeting will include: - Supertsring/Brane/Extra dimension cosmology; - Inflation; Cosmological Fluctuations; - Baryon/Leptogenesis; - Astroparticle physics; Neutrino astrophysics; - Dark Matter; Cosmological Constant; - Cosmological parameters; CMB - Large Scale Structure; Weak Lensing. The format of the Conference will be the traditional one for the Cosmo series with about 25 invited 30 minute plenary talks and contributed 15-20 minute talks as selected by the chairs of the several parallel sessions which will run concurrently in the afternoons. Poster sessions will also be available. A web site for the conference can be found at the following address: http://www.cita.utoronto.ca/~cosmo04/index.shtml Detailed information and application forms for registration, conference fee, travel and accommodation, and applications for contributed talks/presentations and a list of topics/speakers will be available by the end of January 2004. The site will also be linked from CITA's main web site; http://www.cita.utoronto.ca/ To assist us with the organization, please reply to: cosmo04(a)cita.utoronto.ca and let us know if you a) are coming b) are tentatively coming and would like to remain on the email list for future communication. We would also appreciate if you could further propagate this announcement. We hope to see you all in Toronto in September. Organizing Committee, Lev Kofman (Chair), Dick Bond, Carlo Contaldi, Andrei Frolov, Margaret Fukunaga, Johannes Martin, Rob Myers, Marco Peloso, Dmitry Podolsky, Erich Poppitz, Pascal Vaudrevange

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What is the mechanism generating the astrophysical jets?
by Andrzej Marecki 21 Jan '04

21 Jan '04

What is the mechanism generating the astrophysical jets? The answer is: we still don't know. Even worse, we know "less than before". What we know now is that: " [...] the generation of highly relativistic outflows does not require properties that are unique to blackholes, such as an event horizon." said Fender et al., (15 Jan 2004) Nature 427, 222. It means that the famous Blanford-Znajek mechanism is in big trouble. See also a pop-science coverage: http://serwisy.gazeta.pl/nauka/1,34136,1876751.html -- Andrzej

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Re: new grant form .tex file?
by Andrzej Marecki 19 Jan '04

19 Jan '04

> Bartek and i are going to try to apply for a grant. > > Motyl thinks that there's a new form for the KBN - do you have a latex > template for this? No, nothing has changed. For the templates (.doc unfortunately) plus some useful info (in polish) go to: http://www.uni.torun.pl/badania/finansowanie/grkbn/ A. Cc: Bartek

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interesting
by Bartosz Lew 16 Jan '04

16 Jan '04

science development participation by country plot, see: http://arxiv.org/PS_cache/astro-ph/pdf/0401/0401228.pdf bartek

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Re: your mail
by Bartosz Lew 12 Jan '04

12 Jan '04

> i'm not sure if it helps for a research project... if the project is about getting some clues about DM halo density profile then the first question is, what dataset to use, which is related to what we want do calculate. as I understand it's like: for distances < 50kpc Hi claudls can be used, and stellar kinematics, for distances < 100 kpc gravitational lensing is in use for dist. < 1Mpc study of that sattelite galaxies mae be used. (SDSS etc.) oh and there is also that X-ray flux approach for whole clusters of galaxies. (but don't know how this works, some assumptions about flux - mass or luminosity - mass must be made) all of the above techniques require powerfull cpu consuming simulations and involve gaz/hyrdo/sometimes magneto/radiative and DM dyanamics stuff. otherwise I see (if only gravity is involved) no way to solve momentum problem in galaxy disk formation. the cusps etc seem to be more vast problem: \rho ~ r^-x - this is the general law - N-body simulations (with CDM) give density profiles which have x=1 - 1.5 - only disk stellar density declines exponentially or with x close to 0.25 (for bluge) - flat rotation curve (so distances from about 10 to 50 kpc) constraint give x=2 so - obserwations velocity fields give (for these distances) x higher (contrary to smoothed central cusp idea) and even higher x=3 for very periphial galactic regions > 100 kpc - but obserwations of dwarf galaxies give a flat density cores (so it's for very small distances from the galaxy center) totanisan's paper is also intersting to me. but it seems it's just the idea of self interacting DM (SIDM) which has been studied in simulations to fit density profile to obserwations. > - it seems that the long expected cooling flows in g clusters do not exist the cooling does not exist (because the disks of galaxies would be too small then observed with simulated high cooling rate) unless there are additional heating sources (agn, SIDM, UV background, starbursts ,etc, second reionisation :)) bartek

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0401140: nonexistent cooling flows: AGNs vs DM from neutralino annihilations
by Boud Roukema 12 Jan '04

12 Jan '04

http://de.arXiv.org/abs/astro-ph/0401140 - it seems that the long expected cooling flows in g clusters do not exist - Totani-san proposes neutralino annihilation (where DM = neutralinos) as a better source for heating than AGNs Seems interesting to me. b

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0401094: fine-structure constant evolution (-0.06\pm0.06)e-5
by Boud Roukema 09 Jan '04

09 Jan '04

The IUCAA/IAP group have a constraint on (\Delta \alpha/\alpha) evolution with redshift which makes it look like the Webb et al results are only as significant as cosmic topology detections :( http://de.arxiv.org/abs/astro-ph/0401094 \Delta\alpha / \alpha = (-0.06\pm0.06)e-5 The individual values range from -1e-5 to +1e-5 - see Fig.15 on p22 In other words, we should keep checking, but not yet get too excited. pozd boud

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nice paper by joe silk on DM 0401032
by Boud Roukema 06 Jan '04

06 Jan '04

http://de.arxiv.org/abs/astro-ph/0401032 Some Current Issues in Galaxy Formation conclude with a description of the prospects for observing one of the most important ingredients in galaxy formation theory, namely cold dark matter.

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Grav. lensing caused by a very massive object
by Andrzej Marecki 18 Dec '03

18 Dec '03

Paper: astro-ph/0312427 From: Masamune Oguri <oguri(a)utap.phys.s.u-tokyo.ac.jp> Title: A Gravitationally Lensed Quasar with Quadruple Images Separated by 14.62 Arcseconds Journal-ref: Nature 426 (2003) 810-812 [...] Here we report the discovery of a lensed quasar, SDSS J1004+14112, which has a maximum separation between the components of 14.62 arcsec. Such a large separation means that the lensing object must be dominated by dark matter. Our results are fully consistent with theoretical expectations based on the cold-dark-matter model. \\ ( http://arXiv.org/abs/astro-ph/0312427 , 364kb) ----- End of forwarded message from send mail ONLY to astro-ph ----- -- Andrzej

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Doubt cast over dark energy?
by Andrzej Marecki 17 Dec '03

17 Dec '03

NEWSALERT: Saturday, December 13, 2003 @ 2327 GMT --------------------------------------------------------------------- The latest news from Astronomy Now and Spaceflight Now HAS XMM-NEWTON CAST DOUBT OVER DARK ENERGY? ------------------------------------------- In a survey of distant clusters of galaxies, European Space Agency's XMM-Newton observatory has found puzzling differences between today's clusters of galaxies and those present in the Universe around seven thousand million years ago. Alain Blanchard of the Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrenees and his team use the results to calculate how the abundance of galaxy clusters changes with time. Blanchard, knowing that this conclusion will be highly controversial, said: "To account for these results you have to have a lot of matter in the Universe and that leaves little room for dark energy." http://spaceflightnow.com/news/n0312/12darkenergy/ [...] ----- End of forwarded message from NewsAlert ----- -- Andrzej

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jarek - grant application?
by Boud Roukema 16 Dec '03

16 Dec '03

hi Jarek (Rzepecki), Would you like to be included in our next grant application, on the assumption that you are likely to start a PhD in cosmo at CAMK-Toruń (or TCfA) next academic year? The SZ stuff can certainly be counted as useful for topology in the sense that more precise SZ modelling can lead to better values of the curvature parameters (via mass function evolution a la Blanchard et al) and so constrain, e.g. the Poincare dodecahedral model. You can see the discussion on our previous grant application here: http://www.astro.uni.torun.pl/sympa/cosmo-torun/2003-01/thrd1.html http://www.astro.uni.torun.pl/sympa/cosmo-torun/2003-02/thrd1.html We're about to start discussing our next application this week, since the deadline is (probably) the end of Jan 2004 and there's a lot of paperwork to be filled out. Anyone else who would like to be included (or excluded) from the application? As i said in my previous email, IMHO this is astropolitics which does not provide efficient positive/negative feedbacks (for example, magister and PhD students cannot provide positive/negative feedback despite their obvious scientific qualification, while senior scientists who know less of the subject than students can provide feedback based on intuition without having any public record of their arguments or lack of arguments). But anyway, i think the consensus is that it's better to apply for grants than not to. pozd boud

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grant proposal???
by Boud Roukema 15 Dec '03

15 Dec '03

Hi Sebastian, It's getting time for the cosmo/extragalactic group to prepare our next grant application. Some of the others feel that your interests are probably more in the polarisation project (where i think you are part of the grant) rather than in AGN death/rebirth studies, hybrid morphology studies, and using AGNs and the CMB for cosmic topology. At least so far your collaboration with the rest of us has not been that active. Would you feel it is reasonable for you *not* to be included in our next grant proposal? i'm sure you're doing some interesting stuff with Peter Wilkinson, but at the moment it would seem a bit artificial to include you in our grant proposal. i personally think that grant proposals are an *ineffective* way of providing negative and positive feedback to the quality of scientific research, and contribute more to astropolitics than to science. The money would be better distributed evenly (to stipends and salaries) and feedback mechanisms such as wiki pages on research projects would provide faster and much more open and constructive methods of both negative feedback (criticising "bad science" or scientific errors) and positive feedback (encouraging "good science"). However, for the moment we still have to live with grants and the related politics. :( So please tell us what you think. pozdrawiam boud

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Re: information request
by Boud Roukema 04 Dec '03

04 Dec '03

[pl] Witam - kolegy interesowane na tym dyskusji, proszę do http://www.astro.uni.torun.pl/sympa/cosmo-media/ Chciałbym że dyskusja jest publiczna, ale nie chcę spamować w po francusku... ;) [fr] Cher David, (Tu peux m'appeler Boud - mes travaux sont valables ou erronés indépendamment de mes titres officiels. Et j'en ai marre du vousvoyage, c'est pire encore en polonais avec "Monsieur pense-t-il ?"...) On Tue, 2 Dec 2003, dlarousserie wrote: > I am a french journalist working in a scientific magazine called > Sciences et Avenir (about 250 000 ex. monthly). I am writing a > paper on the shape of the universe ; Because of the recent paper Génial ! :))) > from Luminet et al. in Nature (9 ocotber 2003). I know that you > were, but perhaps are still, involved in this field. Then I have a > few questions. Je m'y intéresse toujours :)). Il y a maintenant une équipe de cosmologie à Toruń (Pologne) en train de se former, et la topologie cosmique est une de nos priorités. > In 1997, you have annouced that three galaxy cluster were in fact the same. Pas tout à fait. Alastair Edge et moi avons annoncé que trois amas de galaxies se trouvaient localisés dans l'espace d'une façon qui donnent à penser qu'ils soient trois images topologiques d'un seul amas. En traitant cette idée comme *hypothèse de travail*, Alastair Edge, Stanisław Bajtlik et moi avons essayé de la réfuter, vu qu'une quelconque hypothèse de topologie cosmique (comme celle de Luminet et al. dans Nature) devrait être solidement testée empiriquement avant qu'elle puisse être prise comme élément clé de la cosmologie moderne. * http://fr.arxiv.org/abs/astro-ph/9706166 - Roukema, Edge - premier article sur l'hypothèse spécifique * http://fr.arxiv.org/abs/astro-ph/9903038 - Roukema, Bajtlik - analyse photométrique des cartes de ciel - une tentative d'identifier des galaxies individuelles lentillées entre les deux images de l'amas à grand redshift, et ainsi d'en déduire leurs vitesses dans le plan du ciel, donne un résultat raisonnable (nous espérions trouver une incohérence et ainsi réfuter l'hypothèse) * http://fr.arxiv.org/abs/astro-ph/9910272 - Roukema - analyse du rayonnement de fond cosmologique (COBE) - hypothèse réfutée à une confiance de 94% (ce qui n'est pas très fort), à condition d'ignorer l'effet d'une constante cosmologique non-nulle. Or, aujourd'hui, quasiment tous les observateurs (sauf l'équiipe d'Alain Blanchard à Toulouse ;), et les partisans du modèle steady state comme Jayant Narlikar, Jean-Claude Pecker, ...) sont convaincus que la constante cosmologique est non-nulle. > Is it right ? Did you received confirmation ? La réponse courte est : « Je ne sais pas. » Je préfère distinguer mon intuition des calculs clairs et nets. Mon *intuition* est que cette hypothèse est probablement incohérente avec les observations du fond diffus cosmologique du satellite WMAP, et je travaille en priorité sur d'autres hypothèses. Or, mon intuition n'est pas une preuve qui enterre définitivement l'hypothèse. Lors de ma visite chez nous, à l'Obs de P-Meudon, Dominique Proust (maintenant dans le département « GePi » de l'Obs P-M) nous a aidé dans la préparation de demandes de temps aux télescopes au Chili et à l'Hawaï pour tester l'hypothèse. Or, nous n'avons jamais reçu de réponse positive des comités d'allocation de temps... :( Ce qui ne dit pas que notre hypothèse soit la bonne, elle dit plutôt qu'elle n'entre pas dans la pensée de productivisme à court terme. > What was the name of the three clusters ? Les trois amas sont: * l'amas de Coma * RX J1347-1145 * CL 09104+4109 Vous pourriez profiter des articles publiés librement (voir le fr.arXiv.org ci-dessus). > Do yo know if someone has observed the same similarity in galaxy > clusters or another objects ? Le travail le plus proche que je connais est celui de G.I. Gomero, mais je ne trouve plus de version publique de ces articles. En tous les cas, les résumés sont toujours publiques: * http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2003CQGra..20.4775G * http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2002IJMPA..17.4281G > What is your opinion on the work from Luminet et al. ? Voir http://adjani.astro.uni.torun.pl/cgi-bin/twiki/view/Cosmo/CommuniqueDePress… pour le point de vue de notre équipe. Je n'ai pas de monopole sur la sagesse, mieux regarder nos points de vue intégrées (en autres mots, mes propres points de vue corrigés par les critiques de mes collègues). > Do you have your own "shape" of the universe ? I mean, how do you > see our Universe ? Tout simplement je ne sais pas quelle est la forme de l'Univers. Je voudrais bien la savoir, et c'est pour cette raison que j'y travaille avec mes collègues... > When I speak about this subject, people ask me what is the interest >of such a research. What can I answer ? Why is it interesting to know >the shape of the universe ? Du point de vue des Lumières, l'intérêt principal est culturel : (quasiment) tout le monde a envie de comprendre et de savoir. Savoir quel est la forme de l'objet dans lequel nous vivons est fondamental. Du point de vue mercantile (genre Matra-Hachette-Lagardère, Messier, Bouygues, etc) et des politiques (genre Osama bin Laden, Jacques Chirac, Tony Blair, Saddam Hussein, Nicolas Sarkozy, George Bush), du point de vue de chacun-pour-soi, l'intérêt est que la recherche fondamentale motivée par la curiosité, sans aucune justification « productiviste » a régulièrement sorti des surprises qui plus tôt ou plus tard sont utilisées pour les buts technologiques. Voilà donc du fric et du pouvoir. Les ordinateurs avec lesquels nous communiquons sont en grande partie le fruit de réflexions sur la nature de la logique même. Mais pensez aussi à la radioactivité, à la relativité restreinte (« la théorie de Poincaré et d'Einstein), à la mécanique quantique, aux lasers, ... Evidemment, comme toute découverte scientifique peut être utilisée dans son application technologique tant pour violer les droits humains ainsi que pour les soutenir (en règle générale), la conséquence des découvertes cosmoloqiues pourraient, éventuellement, être de loin plus dévastateurs que les découvertes de la radioactivité et de la relativité restreinte, plus catastrophiques que les découvertes empiriques dans la psychologie et leur application dans les méthodes de propagande modernes et malheureusement légales et meurtrières, et plus répressives que les méthodes de torture dans les camps de la Guantanamo Bay qui pulvérisent le contenu humain du cerveau tout en gardant le corps en bon état. > What is your own motivation ? Tout simplement, j'ai envie de comprendre l'Univers :). Et les risques que je viens d'énoncer, alors ? J'en les assume. Je suis conscient des risques que je vient d'énoncer, et si les résultats soient catastrophiques, j'aurai ma part de blâme (bien qu'il n'y aurait peut-être pas ni moi ni aucun autre humain pour en parler...). Or, les arguments énergétiques et les mécanismes décisionnels qui permettent quelques éléments de démocratie dans notre société globale suggèrent que le plus grand risque actuel vient de l'Empéreur Bush et son Régent Dick Cheney plutôt que de la communauté des physiciens. Néanmoins, pour que *toutes les sciences et technologies* soient plus gérables par les cityon-ne-s, je suis aussi motivé dans le développement de plus de participation dans la recherche scientifique, les miennes incluses. J'essais de promouvoir la science ouverte, non au sens de mots vides, mais dans le sens de l'usage des technologies de l'internet pour non seulement permettre une participation du genre « les croyants peuvent lire ce que disent les sages » mais pour raccourcir les distances entre les fans et les experts. En jetant un coup d'oeil sur nos pages http://adjani.astro.uni.torun.pl/cosmo tu verrais que je commence en encourageant la transparence de relations entre étudiants (1ère, 2ème et 3ème cycles universitaires) et chercheurs, et j'espère pouvoir développer des logiciels qui peuvent être utilisés au sein s'un système ouvert comme GNU/linux afin que l'utilisateur moyen avec un savoir scientifique de base (niveau bac) puisse en profiter. Certaines parties des travaux astronomiques/cosmologiques sont très ouvertes, d'autres sont à moitié fermés comme certains logiciels « open source » qui non sont pas « libres » au sens du GNU GPL/LPG GNU (http://www.april.org), et encore il y a toujours des données empiriques ou logiciels complêtement fermés. Nous avons encore une longue distance entre nos pratiques actuelles et celles de la communauté GNU/Linux... > Do you think we could answer to this question ? When ? Is the Planck > observer the last hope ? Les prévisions du futur sont très peu fiables dans ce genre de domaine. Mieux regarder dans http://www.bdl.fr pour voir quelles seront les dates d'éclipse en 2007 ou 2008 ou 2010 plutôt que prédire le résultat d'une recherche scientifique de fond. :) > According to you who are the leader in this field ? Je ne crois pas trop au mythe des « stars » dans la recherche. Néanmoins, vu que les chercheurs actifs dans ce domaine qui reçoivent le moins de publicité sont ceux de l'Amérique du Sud et du Japon, pour des raisons nombriliques traditionnelles aux USA et en France, il faut que je vous les disent leurs noms: Helio FAGUNDES, Germán GOMERO (german à ift.unesp.br), M.J. REBOUCAS, et Kaiki Taro INOUE (ex http://fr.arxiv.org/abs/astro-ph/0103158, tinoue à yukawa.kyoto-u.ac.jp) > That's all for this time... N'hésite pas à répondre sur mailto:cosmo-media à astro.uni.torun.pl > Best regards, > > Larousserie David > 00 33 1 55 35 56 27 Bien à vous :) Que le savoir avance ! boud

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IV Torunski Festiwal N .i Sz. (fwd)
by Boud Roukema 04 Dec '03

04 Dec '03

Witam, Andrzej Kus już proponował że zrobimy debat panelowy na tym Festiwał. Widocznie, ktoś w Administracji był bardzo zadowolony z artykuł w Rzeczpospolicie... Niezależny od mediów, zgadzam się że byłoby fajny pomysł zrobić jakiś prezentacja rozmaity punkt widzenia - dla inflacji, dla możliwość mierzyć topologia Wszechświat. Dokładnie format możemy dyskutować kilka dni przed Festiwał, ale chyba potrzebujemy: - tytuł - abstrakt - nazywa kto będzi mówić (ale oczywiści, moźemy zmienić na ostatniu minut, tylko nie będzi Twoja nazywa drukowana na reklama etc.) Tu propozycja: http://adjani.astro.uni.torun.pl/cgi-bin/twiki/view/Cosmo/FestiwalNauki2004 Staszek mówił że potrzeba być propozycja do jutrze czw 4 grudnia (jest trochę absurdalny, dać tylko jeden dzień dla decydować, ale nie ma sprawy), więc będę dać jej do Andrzeja Strobela jutro (czw 4 grud) w popołudniu. Oczywiście, ja nie mogę kontrolować co będzie na reklamów ofycjalny, ale chyba w praktyce możesz myśleć w czasie następne kilka miesięce... Proszę poprawiuj ten stron! http://adjani.astro.uni.torun.pl/cgi-bin/twiki/view/Cosmo/FestiwalNauki2004 pozd boud > > ---------- Forwarded message ---------- > Date: Wed, 3 Dec 2003 09:50:36 +0100 (CET) > From: Stanislaw Krawczyk <Stanislaw.Krawczyk at astri.uni.torun.pl> > To: staff at astri.uni.torun.pl > Subject: IV Torunski Festiwal N .i Sz. > > Zgodnie z ustaleniami na ostatniej Radzie Centrum bardzo prosze o > skladanie propozycji uczestnictwa w Festiwalu ( tematy prelekcji lub > innych imprez) na ręce pana prof. A. Strobla do dnia 4 grudnia 2003. > Na wyklady zarezerwowana jest wstepnie sala wykladowa w Instytucie Chemii > na Bielanach w kazdym dniu Festiwalu (22-25 kwietnia 2004) w godz. 18-20. > Formularze zgłoszeniowe jak i więcej informacji o przyszłorocznym > festiwalu mozna znalzc na stronie www.festiwal.torun.pl badz w biurze > Centrum Promocji i Informacji UMK (tel. 611 46 57, 611 48 74) > Podobnie jak w roku ubieglym organizowac bedziemy zwiedzanie Centrum i > pokazy nieba przez teleskop i w miare odpowiednich warunkow projekcje > filmow astronomicznych w "letnim kinie". Prosze takze o deklaracje > uczestnictwa w tym rutynowym przedsiewzieciu bezposrednio do mnie > badz do prof. A.Strobla. > Z gory dziekuje za pomoc w promocji naszego Centrum na Festiwalu. > S. Krawczyk >

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Fine structure constant vs. quintessence
by Andrzej Marecki 02 Dec '03

02 Dec '03

NEWSALERT: Thursday, November 27, 2003 @ 1442 GMT --------------------------------------------------------------------- The latest news from Astronomy Now and Spaceflight Now [...] Light signals from quasars seem to indicate that the bond between electrons and protons was weaker in the early universe. Luis Anchordoqui and Haim Goldberg of the Department of Physics at Northeastern University in Boston, Mass., propose that the apparent change in the fine structure constant is coupled to "quintessence." The fine structure constant was measurably weaker ten billion years ago, but as quintessence assumed dominance about eight billion years ago, the force between electrons and protons became stronger and "more constant." http://spaceflightnow.com/news/n0311/25nature/ ----- End of forwarded message from NewsAlert ----- -- Andrzej

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magister course 2003/2004
by Boud Roukema 12 Nov '03

12 Nov '03

Proposal for Supervising Masters (Magister) projects at TCfA for Nov 2003 - Sep 2004 Supervisor: B. Roukema (boud at astro.uni.torun.pl) Number of students: up to 3-4 students is possible Title: Observational Constraints on Cosmological Parameters Description: There are many possible projects which could be done as a master's thesis project, in using publicly available archival data from observational surveys to constrain one or more of the local or global cosmological parameters, either those related to shape (curvature, topology) or maybe also those unrelated to shape ("dark energy"). The precise projects would be chosen in discussion with the masters students during Nov-Dec 2003. One example would be further development and application of the "Dark Energy" software package which has been worked on during the "Shape of the Universe" monograph course: http://www.astro.uni.torun.pl/sympa/shape-univ/ Requirements: - basic knowledge in astronomy, physics, mathematics, computing skills - desire to measure something about the shape of the Universe - willingness both to learn from and to teach others interested in observational cosmology at TCfA - willingness to learn the following practical skills: touch-typing, emacs, \LaTeX, usage of mailing lists and wikis for communication - participation in the "Shape of the Universe" monograph course and/or Bronek Rudak's semester 9 "Kosmologia" course: http://www.ncac.torun.pl/~bronek/KOS.html - nie ma problemu jeśli student magisterowy (jeszcze) nie dobrze mówi po angielsku

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Re: prosba o komentarz
by szajtan odwieczny 03 Nov '03

03 Nov '03

> > > > What I think we can say for sure is that, although we're not sure about > > > > the actual curvature of our obserwable universe, and thus we're not sure > > > > if the space go on and on to infinity, it seems that it's quite sure that > > > > our universe is accelerating (q<0), and from this point of view we can say > > > > that if we send out a probe into the space even at the velocity of light, > > > > it's likely that it will never return regardelss of the the curvature > > > > of the universe, because it just won't overpass the expantion rate of the > > > > universe unless there is some nontrivial topology involved. The Big Crunch > > > > never happens in area where q<0 on Omega_l, Omega_m plane. So from our > > > > point of view we can say the spacetime is infinite if we're thinking in a > > > > > > We can't say "the spacetime is infinite". What you mean is > > > why not ? > > Because "x is infinite" means that > "for every y \in {Real numbers}, x > y". > > If the Universe has positive curvature with curvature radius R_C (and > is a perturbed FLRW model, as we think), then there exists a maximal > length spatial geodesic X_s and a maximal length space-time geodesic > X_st . okok but if we set k=1 the solution of geodesic equation in FLRW metric for distance is something like arcsine function of comoving distance times S(t). So it's closed solution and space is finite. but when additionaly we set for example Omega_l > Omega_cdm then S(t) has no maximum (as is had in closed model with zero cosmological constant) and it grows with time to infinity. hmm it sounds simple ;) however infinity doen't appear anywhere in flormula. What I said was that I think the data are suffucient to say that the photon once sent in some direction will never return no matter what curvature the universe has because of S(t). So from the point of view of that photon the universe will be infinite > Then, there exist y \in {Real numbers} greater than these values and > there are no longer any x in the Universe greater than y. So it's not > infinite. > > > > event horizon accounts for all evolution of expantion according to assumed > > model. if it's less than the curent curvature radius then we won't see the > > probe, if it's bigger we mae but not must see it, for the curvature > > radius is changing in time. > > i'll let you do the calculations here, but they are irrelevant for the > question of infinity. > > > the fundamental nature of the model is that going in space we also move in > > time. > > This is extremely confusing language. What do you mean by "going in > space", "moving in time" and "we"? If you mean there's a second time > variable representing the time variable of a thought experiment, then > it makes sense. Or if you're talking about a physical particle, then > two different time variables are the local (proper) time of the particle > and the cosmological time. > > But it's perfectly possible to imagine comoving space without needing > any time variable to "go" through it (though having a local psychological > time variable is convenient). well, comoving space without remembering of time. how would you describe how it comoves then ? ;) it wouldn't differ from galileo's static space. > > > eg. Imagine that that space is closed, and expands slow enough that > > a photon emited from your flashlight can round it, but as the time passes > > expansion rate mae grow up, event horizon falls, (say cosmological > > constant starts dominate) and the photon won't make it eventually. > > IMHO this is a different theme to the universe being infinite or not why ? this is right the core of this probelm. if we consider only the spatial part of of the solution of geodesic equation, fine, but it's multiplied by S(t) which has no bounds because the time dimension in our universe has no bounds (no upper limit) so the whole distance (to something) relation has no bounds in spacetime interpretation, if I can say so. So here I recall the question why can't we say the spacetime is infinite, which reduces just to what's the maximal length of your X_st ? > > > > If you can think of an alternative model which only models our past > > > time cone, fine. > > btw. > > if the accurate model predict things in the past, I see no reason why > > it should not predict also things in the future. > > You can't predict things in the past. Astronomers doing models often talk about > "predicting" observations already made, but this is just astropolitics. > > The reality is that you can only postdict the past, and that if you make > predictions they will usually be wrong. Moreover, you're more likely to > get observing time/grants if you postdict the past (and say that you're > predicting it) rather than if you make real predictions. > > As for accuracy, the model below is extremely accurate, by definition. > > > below this this point I don't follow ;) > > Another way of describing the model is that the Universe the inside of a > 6k-light-year sphere and that initial (and continuing) boundary conditions > on the sphere have been designed in such a way that people trying to > understand them conclude with a series of simple (but wrong) physical > laws. Initial conditions throughout the sphere were also set up with > the same intention (e.g. fossils, distribution of continents, genetic > mixes of people and other animals, isotopic ratios of uranium etc...) > > Maybe another way of describing it is that we live inside a planetarium > of radius 6kly and that The Designer is pretty good at designing fun > models with just enough clues that we remain interested and think we > can understand the model represented in the planetarium. > > > > It's a model which perfectly fits all cosmological observations, > > > including those of WMAP. ;) The Universe in this model is the inside > > > > gash, does it says about CMB fluctuations ? > > No: but since human beings have interpreted these in terms of a simple > set of physical laws, the Christian fundamentalist model is satisfied > - there are simply a new set of boundary conditions designed to make > physicists interpret them this way. >

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Re: prosba o komentarz
by szajtan odwieczny 29 Oct '03

29 Oct '03

> > On Tue, 28 Oct 2003, szajtan odwieczny wrote: > > > What I think we can say for sure is that, although we're not sure about > > the actual curvature of our obserwable universe, and thus we're not sure > > if the space go on and on to infinity, it seems that it's quite sure that > > our universe is accelerating (q<0), and from this point of view we can say > > that if we send out a probe into the space even at the velocity of light, > > it's likely that it will never return regardelss of the the curvature > > of the universe, because it just won't overpass the expantion rate of the > > universe unless there is some nontrivial topology involved. The Big Crunch > > never happens in area where q<0 on Omega_l, Omega_m plane. So from our > > point of view we can say the spacetime is infinite if we're thinking in a > > We can't say "the spacetime is infinite". What you mean is why not ? event horizon accounts for all evolution of expantion according to assumed model. if it's less than the curent curvature radius then we won't see the probe, if it's bigger we mae but not must see it, for the curvature radius is changing in time. > "the http://www.wikipedia.org/wiki/Event_horizon is less than > 2 \pi times the radius of curvature even if comoving space is a hypersphere". last time I checked the page expired so don't know what was there, but did anyone said something about the relation of the event horizon to the curvature ratius.? (this should be calculated) > > This is true even when \Omega_\Lambda = 0 - the Big Crunch happens > before we can see the back of our head. > even better - another reason for which we will never see the sent signal (probe), but with CDM=.3 and DE=.7 or anything close to it we have no big crunch at all. > > way of traveling in it. If we think just of a space as a slice in some > > moment of time the quiestion is still open, but what is use of thinking > > i think you mean here "in some spatial section at constant cosmological time". yes > > about space this way - it just cannot be separated from time right ? > > It's the fundamental nature of the model, so we ought to think about it. the fundamental nature of the model is that going in space we also move in time. eg. Imagine that that space is closed, and expands slow enough that a photon emited from your flashlight can round it, but as the time passes expansion rate mae grow up, event horizon falls, (say cosmological constant starts dominate) and the photon won't make it eventually. > > If you can think of an alternative model which only models our past > time cone, fine. btw. if the accurate model predict things in the past, I see no reason why it should not predict also things in the future. below this this point I don't follow ;) > But personally this reminds me of the Christian > fundamentalist cosmology model where the Unvierse is only 6000 years > old, as written in the Bible. > > It's a model which perfectly fits all cosmological observations, > including those of WMAP. ;) The Universe in this model is the inside gash, does it says about CMB fluctuations ? meaybe I should review the bible instead of Peebles, etc :) > of a sphere of radius 6000 light-years, on which EM radiation of all > sorts of wavelengths (and we could add other particles) was generated > 6000 years ago on this surface, emitted in the direction of the Sun > (and it continues to be generated) in such a way to reproduce a > "naive" model that makes it (more or less) easy for human beings to > interpret these in terms of simple laws of physics. The being "God/Bóg" > which generates the emission wants human beings to have an easily > interpretable Universe, he/she/it is extremely intelligent and able > to generate such complex emission patterns of radiation. Just like > he/she/it set up species of animals 6000 years ago in a way that > makes biologists think there must have been lots of evolution... > > Personally i find the model ridiculous, but it perfectly fits all the > observations and avoids "extrapolation" into times with which we have > no written contact (prehistorical), and the Universe is only 6000 > years old. pozdrawiam bartek.

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Re: prosba o komentarz
by szajtan odwieczny 28 Oct '03

28 Oct '03

What I think we can say for sure is that, although we're not sure about the actual curvature of our obserwable universe, and thus we're not sure if the space go on and on to infinity, it seems that it's quite sure that our universe is accelerating (q<0), and from this point of view we can say that if we send out a probe into the space even at the velocity of light, it's likely that it will never return regardelss of the the curvature of the universe, because it just won't overpass the expantion rate of the universe unless there is some nontrivial topology involved. The Big Crunch never happens in area where q<0 on Omega_l, Omega_m plane. So from our point of view we can say the spacetime is infinite if we're thinking in a way of traveling in it. If we think just of a space as a slice in some moment of time the quiestion is still open, but what is use of thinking about space this way - it just cannot be separated from time right ? bart.

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multipole vectors - another hint for topology?
by Boud Roukema 21 Oct '03

21 Oct '03

http://de.arxiv.org/abs/astro-ph/0310511 ...We find that the result from comparing the oriented area of planes defined by these vectors between multipole pairs 2 <= l1 != l2 <= 8 is inconsistent with the isotropic Gaussian hypothesis at the 98.8% level for the ILC map and at 99.6% level for the cleaned map of Tegmark et al. A particular correlation is suggested between the l=3 and l=8 multipoles, as well as several other pairs. This effect is entirely different from the now familiar planarity and alignment of the quadrupole and octupole: while the aforementioned is fairly unlikely, the multipole vectors indicate correlations not expected in Gaussian random skies that make them unusually likely. ... If it's not topology, it's something else weird (politically incorrect ;) that happened on near-horizon scales... pozd boud

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--- SPAM --- Confidential
by joseph mobutu 20 Oct '03

20 Oct '03

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Re: ksztalt Wszechswiata i media kontrolowane
by Andrzej Kus 16 Oct '03

16 Oct '03

Boud, Please ask someone from the group to correct polish in the > http://adjani.astro.uni.torun.pl/cgi-bin/twiki/view/Cosmo/OswiadczeniePraso… Some parts, as it is for the press, are not clear, perhaps Andrzej Marecki can do the job. This is very interesting and important development ! Cheers Andrzej K.

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prosba o komentarz (fwd)
by Boud Roukema 16 Oct '03

16 Oct '03

hi everyone, i definitely think we should respond to this - but i would prefer it to be a collective response - there's no reason why only my name should be cited - e.g., we could at least have the official "team" who was on the grant (amr + motyl + magda + bartek + sebastian + me), but if someone else wants to participate (i guess we can call this an official "press release" (oświadczenie prasowe)) that would be good, especially someone from CAMK to show that we work together despite the bureaucratic difference between CA-UMK and CAMK. As i understand it, Łukasz is in a hurry - he'll ring back at 15.00 - so i'll try to get a draft to the list within the next half hour or so. pozd boud > ---------- Forwarded message ---------- > Date: Tue, 14 Oct 2003 12:07:10 +0200 > From: Lukasz Kaniewski <l.kaniewski at rzeczpospolita.pl> > To: boud at astro.uni.torun.pl > Subject: prosba o komentarz > > Szanowny Panie doktorze! W zeszlym tygodniu w "Nature" ukazaly sie > wyniki badan dotyczacych ksztaltu i rozmiaru Wszechswiata. > > http://www.eurekalert.org/pub_releases/2003-10/ns-dtu100803.php > > Czy moglby Pan wyslac mi swaja opinie na temat tych wynikow? Prosze o > kilka lub kilkanascie zdan - mailem, bylbym wdzieczny za szybka > odpowiedz. > Sprobuje zadzwonic jeszcze do Pan okolo trzeciej. > Dziekuje - Lukasz Kaniewski, dziennik "Rzeczpospolita". >

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Re: prosba o komentarz
by Boud Roukema 16 Oct '03

16 Oct '03

Dear Łukasz, We have a draft version of a text here: http://adjani.astro.uni.torun.pl/cgi-bin/twiki/view/Cosmo/OswiadczeniePraso… but clearly the po polsku is not yet correct. It would probably be better that one of us corrects the po polsku in order to avoid introducing scientific errors, but it is unlikely that this will be ready by 18.00 today. If you can wait till later in the evening, then maybe we will have a better version ready for you. Alternatively, you could just click on "Register" on that page and make yourself your own username + password, then return to the page and click on Edit. Make the language corrections, click Preview and Save when you're happy. I (and maybe some of the others) will check later this evening to see if the scientific meaning is still correct after the corrections, but I'll be offline for the next few hours. Feel free to reply directly to our mailing list (cosmo-torun at astro.uni.torun.pl). *** Please keep the URLs (http links), at least you may shift them as references to the end of the article if you don't like them in the middle of the sentence - the aim of an article about cosmology in a major newspaper should not only be to "inform" readers, but also to give the power to readers to *inform themselves*. By including URLs - even in the paper version - some fraction (10-20%) of the readers will be able to explore further and will have some independence both from Rzeczpospolita editors/writers and from CA-UMK/CAMK scientists. Maybe only 1% will really do this, but the principle of giving maximum power to the reader is a fundamental part of intellectual freedom. pozdrawiam boud On Tue, 14 Oct 2003, Lukasz Kaniewski wrote: > Szanowny Panie doktorze! W zeszlym tygodniu w "Nature" ukazaly sie > wyniki badan dotyczacych ksztaltu i rozmiaru Wszechswiata. > > http://www.eurekalert.org/pub_releases/2003-10/ns-dtu100803.php > > Czy moglby Pan wyslac mi swaja opinie na temat tych wynikow? Prosze o > kilka lub kilkanascie zdan - mailem, bylbym wdzieczny za szybka > odpowiedz. > Sprobuje zadzwonic jeszcze do Pan okolo trzeciej. > Dziekuje - Lukasz Kaniewski, dziennik "Rzeczpospolita".

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Dodecahedral space topology
by Andrzej Marecki 10 Oct '03

10 Oct '03

----- Forwarded message from NatureAlert ----- [...] Dodecahedral space topology as an explanation for weak wide-angle temperature correlations in the cosmic microwave background JEAN-PIERRE LUMINET, JEFFREY R. WEEKS, ALAIN RIAZUELO, ROLAND LEHOUCQ & JEAN-PHILIPPE UZAN http://info.nature.com/cgi-bin24/DM/y/eMJG0BfWLH0Ch0EeW0Ay [...] ----- End of forwarded message from NatureAlert ----- Nature's politics require embargo for articles before they are in the current issue on Nature so the authors couldn't post it on astro-ph but hope they'll do so. ;-) A.M.

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No topological signal detected in WMAP data
by Andrzej Marecki 10 Oct '03

10 Oct '03

Paper: astro-ph/0310233 From: Neil J. Cornish <cornish(a)physics.montana.edu> Date: Wed, 8 Oct 2003 20:27:22 GMT (16kb) Title: Constraining the Topology of the Universe Authors: Neil J. Cornish, David N. Spergel, Glenn D. Starkman and Eiichiro Komatsu Comments: Submitted to PRL \\ The first year data from the Wilkinson Microwave Anisotropy Probe are used to place stringent constraints on the topology of the Universe. We search for pairs of circles on the sky with similar temperature patterns along each circle. We restrict the search to back-to-back circle pairs, and to nearly back-to-back circle pairs, as this covers the majority of the topologies that one might hope to detect in a nearly flat universe. We do not find any matched circles with radius greater than 25 degrees. For a wide class of models, the non-detection rules out the possibility that we live in a universe with topology scale smaller than 24 Gpc. ------------------------------------------------------------------------------

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double double-lobed FR IIs
by Boud Roukema 03 Oct '03

03 Oct '03

http://arxiv.org/abs/astro-ph/0310045 Double-double radio galaxies: remnants of merger of supermassive binary black holes Sounds like a model from what andrzej presented yesterday.

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EARA workshop at IAP (fwd)
by boud 30 Sep '03

30 Sep '03

> ---------- Forwarded message ---------- > Date: Mon, 29 Sep 2003 16:02:13 +0200 (CEST) > From: Caroline Terquem <terquem at iap.fr> > Subject: EARA workshop at IAP > > > Dear colleague, > > The IAP will host an EARA workshop entitled: > > The interplay between galaxy interactions, black holes, starbursts > and galaxy formation > > The dates (which we set from people's preferences and local constraints > with other meetings in Paris) are: > > December 4 and 5, 2003 (Thursday & Friday) > > You are invited to attend and present your work. > > Please let us know if you can attend as soon as possible, and send us a title. > > all the best > > Gary Mamon > Andrea Cattaneo > Bruno Guiderdoni > Avishai Dekel

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Re: A Big Rip instead of Big Crunch?
by Jaroslaw Rzepecki 30 Aug '03

30 Aug '03

>About 3 months before the end the solar >system would become undone. About 30 minutes before that the Earth >would explode. And about 10^-19 seconds before the ultimate >moment of doom, atoms would be pulled apart Hi! I never quite understood this... what do you mean by 3 months, 30 min, 10^-19s? Is this the time measured by my local clock? General question is: What would happen to time dimension in such a fast accelerating universe? Cheers Jarek

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A Big Rip instead of Big Crunch?
by Andrzej Marecki 29 Aug '03

29 Aug '03

----- Forwarded message from physnews(a)aip.org ----- PHYSICS NEWS UPDATE The American Institute of Physics Bulletin of Physics News Number 651 August 28, 2003 by Phillip F. Schewe, Ben Stein, and James Riordon THE BIG RIP: A NEW COSMIC DOOMSDAY scenario takes the present acceleration of the expansion of the universe to new extremes. Dartmouth physicist Robert Caldwell and his colleagues Marc Kamionkowski and Nevin Weinberg at Caltech have determined that if the supposed dark energy responsible for the acceleration is potent enough not only will the space between galaxies continue to increase but that the galaxies themselves will fly apart as will, at successive times stars, planets, and even atoms and nuclei. Since the acceleration idea became established with astronomers a few years ago in the wake of observations of distant supernovae, it has been conventional to apportion the supposed energy inventory of the universe as follows: 5% in the form of conventional baryon matter (out of which atoms are made), 25% in the form of dark matter, and the biggest part, 70%, in the form of dark energy. Not a lot is known about dark matter, and even less about dark energy. Cosmologists have taken to discussing the enigmatic properties of the dark energy with the use of a new parameter, w, which is the ratio of its average pressure to energy density. The degree of this runaway expansion impulse is expressed by w. What is the nature of dark energy and how does it overcome the attractive pull of gravitation in order to speed up the cosmic expansion, and what is the proper value of w? In the best known model, the "cosmological constant" in Einstein's famous equations of general relativity corresponds to energy and pressure of the universal quantum vacuum, and is constant in space and time. Here the value of w is -1. In a second popular model, the "quintessence"model, the dark energy is associated with a universal quantum field relaxing towards some final state. Here the energy density and pressure of the dark energy are slowly decreasing with time, and the value of w is somewhere between -1/3 and -1 (w must be smaller than -1/3 in order for cosmic acceleration to occur). In Caldwell's "phantom energy" model, there is no stable vacuum quantum state and the energy density and the expansionary pressure exerted on the universe seems to increase even as the spacetime itself expands (with ordinary gases, pressure falls with expansion). In this scenario w is less than -1. The implications of this new type of cosmology are that bound systems should in the course of time be ripped up (see figure at http://www.aip.org/mgr/png/2003/200.htm ). For example, at a w value of -1.5 the universe would last for 35 billion years before being ripped apart. About 60 million years before the end, the Milky Way would be torn apart. About 3 months before the end the solar system would become undone. About 30 minutes before that the Earth would explode. And about 10^-19 seconds before the ultimate moment of doom, atoms would be pulled apart. Caldwell (robert.r.caldwell(a)dartmouth.edu, 603-646-2742) suggests that deciding between this model and the others might be possible in coming years with much better data coming from microwave background, supernovae, and galaxy measurements. (Caldwell et al., Physical Review Letters, 15 August 2003; text at www.aip.org/physnews/select) [...] ----- End of forwarded message from physnews(a)aip.org -----

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open zwicky proposal - deadline Mon 7 July 2003
by boud 30 Jun '03

30 Jun '03

Hi everyone, I think people have had enough time to see how wiki pages work internally http://adjani.astro.uni.torun.pl:9673/zwicky/ and how they work externally where anybody at all with internet access can modify pages http://pl.wikipedia.org So I think it's time to have some open zwiki (or other wiki software) pages on adjani for organising things like: - cosmic topology research - cosmic standard ruler stuff - OCRA coordination - other research projects - cosmo/extragalactic session at http://www.pta.edu.pl/zjazd - other conferences where there's no point creating a new password for everyone who might want to make a comment or change something. So this is my proposal. Please provide comments, a modified, improved version of the proposal, or if you really think this goes against the purpose of why we are here - observational cosmology research - then you may *block* the proposal, but in that case you take responsibility for having blocked. (This is the style of consensus decision-making, for anyone who forgot...) pozdrawiam boud ********************************************************************** PROPOSAL for open (z)wiki pages. DECISION DEADLINE Mon 7 July 2003 It is proposed to have some wiki pages, separate from the present pages http://adjani.astro.uni.torun.pl:9673/zwicky/ For example, with a name http://adjani.astro.uni.torun.pl:9673/open/ to make it clear that it's an open zwiki. The purpose will be to organise things like - cosmic topology research - cosmic standard ruler stuff - OCRA coordination - other research projects - cosmo/extragalactic session at http://www.pta.edu.pl/zjazd - other conferences where cosmologists (faculty, postdocs, students) from outside of TCfA will be able to contribute to pages, update them, etc. Although hypothetically this means that web surfers might write rubbish on the pages, in practice there will hopefully be enough real cosmology users on the pages that any rubbish will quickly be removed by the real users. The example of http://pl.wikipedia.org shows that this is possible and practical, with good results. **********************************************************************

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H0=75km/s/Mpc
by Andrzej Marecki 12 Jun '03

12 Jun '03

----- Forwarded message from send mail ONLY to astro-ph ----- [...] Paper: astro-ph/0306216 From: L.V.E. Koopmans <leon(a)astro.rug.nl> Date: Wed, 11 Jun 2003 01:59:39 GMT (350kb) Title: The Hubble Constant from the Gravitational Lens B1608+656 Authors: L.V.E. Koopmans (Caltech/STScI), T. Treu (Caltech), C.D. Fassnacht (UC Davis), R.D. Blandford (Caltech), G. Surpi (Caltech) Comments: 16 pages, 6 figures, 5 tables; submitted to ApJ \\ We present a refined gravitational lens model of the four-image lens system B1608+656 based on new and improved observational constraints: [...] A combined gravitational-lens and stellar dynamical analysis leads to a value of the Hubble Constant of H_0=75(+7/-6) km/s/Mpc (68 percent CL; Omega_m=0.3, Omega_Lambda=0.7. [...] ----- End of forwarded message from send mail ONLY to astro-ph ----- It's important to note that originally the same group claimed that H0 might be as low as... 61 km/s/Mpc, see: Fassnacht et al. (2002) ApJ, 581, 823 -- Andrzej

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unofficial unofficial grant results :(
by Boud Roukema 10 Jun '03

10 Jun '03

Hi everyone (on the grant proposal), The unofficial unofficial grants results are negative, sorry. :( The official unofficial results should be found as Konkurs XXV here within a few days: http://www.astrouw.edu.pl/~kst/konkursy.html And the official official results probably within 3-4 weeks. i'll be in Blois next week: http://blois.in2p3.fr/2003/pages/inform2.html but in July and August i'll be more or less in Toruń/Piwnice, though probably working from home more often than from my office. i'm not eager to do the paperwork again, but i guess the funding arithmetic can be the same, we only need to change the scientific plan and translate it to po polsku. IMHO, it's probably not worth trying again in topology, i think we should consider a plan which is more or less: ArFus - galaxy formation modelling + SMBH merger models for inducing AGN formation => RLAGN birth, youth and death observational (phenomenological) population constraints Nothing will stop us doing topology anyway, and this sort of work is something i think we should do anyway - it's the obvious way of combining our best observational and theoretical experience on a subject where it is certain that the objects of interest exist! The difficult question is how Bartek can fit into this. Bartek: any ideas? How about something like the reionisation epoch, around z=10-20? Since WMAP, people are coming up with all sorts of stuff on this. Hmmm... How about predictions for SKA? http://www.skatelescope.org/ That should find star-forming galaxies at redshifts anywhere around z=5-20, and SMBH and AGN formation around then should certainly be affected by when and how reionisation happened, making the link with RLAGN evolution modelling. Anyway, please say what you think, is it realistic to do this during July - including Polish translation etc etc - when everyone would rather be doing theoretical cosmology in the warm sunshine outside? pozd boud

1 0

PTA wrzesnia - can we have a cosmo session?
by boud 10 Jun '03

10 Jun '03

Cześć, Would it be possible for the cosmologists in Poland to organise a session during the PTA in September? Since many of us may be attending anyway, we might as well do this in an organised and open way rather than just as a random meeting among friends who already know each other... My idea would be to use the mailing list cosmo-pl(a)astro.uni.torun.pl so that everybody from Toruń, Warszawa, Kraków and other cosmologists with Polish connections can coordinate, decide on a programme, etc. I would be happy to facilitate (moderować) the discussions. I guess the questions to the LKO would be: (1) How much time can we have in total? half-a-day? a few hours? (2) Would a meeting in the full session be best, or would a parallel session be better? But they would have to evolve depending on how much interest there is to Polish cosmologists. For the moment I'm only cc-ing this to cosmo-torun, so that we have some "local" coordination first, before PL level coordination. I'm not yet a member of the PTA, but of course I would be happy to become a member. pozdrawiam Boud PS: Is there an http: reference to the meeting details?

2 1

SZ - OCRA paper - Battye Weller
by Boud Roukema 30 May '03

30 May '03

http://de.arxiv.org/abs/astro-ph/0305568

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Dark matter - yes, MOND - no.
by Andrzej Marecki 23 May '03

23 May '03

----- Forwarded message from physnews(a)aip.org ----- THE CONVENTIONAL THEORY OF DARK MATTER just got some potent support from a new batch of observations to be reported by scientists from the Sloan Digital Sky Survey (SDSS) this week at a meeting in the Canary Islands. One of the main reasons for believing in the existence of non-luminous matter is that the motions of galaxies within galaxy clusters and the motions of matter around individual galaxies seems to defy conventional celestial mechanics. Either plenty of extra (but unconventional) mass must lurk in the vicinity of the galaxies (the dark matter theory) or the known laws of physics might be in need of amendment (the theory known as modified Newtonian dynamics, or MOND). Scrutinizing a subset of 3000 galaxies (from Sloan's inventory of 250,000 galaxies) with satellite galaxies in tow, the researchers' profile of satellite velocities supported the dark matter theory and discounted the MOND idea. (See the Sloan website at www.sdss.org ) ----- End of forwarded message from physnews(a)aip.org ----- -- Andrzej

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Weyssenhoff fluid article - Szydlowski & Krawiec
by Boud Roukema 21 May '03

21 May '03

Cześć Adam (z Krakowie), Zobaczyłem twoj artykuł z Marekem Szydłowskiego: http://de.arxiv.org/abs/astro-ph/0305364 Chyba już znasz, ale w Toruniu próbujemy rozwijać komunikacji między kosmologów i ekstragalaktyków w Polsce - możesz napisać się na lista mejla cosmo-pl małpa astro.uni.torun.pl tutaj: http://www.astro.uni.torun.pl/sympa/cosmo-pl/index.html SUBSCRIBE: email to sympa(a)astro.uni.torun.pl with "subscribe cosmo-pl" W tej chwili nie są wiele mejlów (ryzyko spam jest bardzo niski, oprócz spam od mnie :), ale kiedy ktoś chce używać ta lista, może być użyteczny. Mniej-więcej są osób z Toruniu + Wwie + Krakowie + kilka na granicą (Bohdan P, Radek Stompor, Krz Górski). Najaktywne listy mejla u nas chyba są http://www.astro.uni.torun.pl/sympa/cosmo-torun/index.html http://www.astro.uni.torun.pl/sympa/shape-univ/index.html i stron Zwicky: http://adjani.astro.uni.torun.pl:9673/zwicky/TCfACosmology Chyba teraz najłatwiejszy okazja dla spotka kosmo w Polsce będzie spotka PTA w Toruniu, widocznie: 8-10.09.2003 http://www.phys.uni.torun.pl/phys/KONFERENCJE/konf-w2003.html ale wiem że potrzebuję iść do Krakowie dla spotykać z wasz... pozdrawiam boud

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Nowe czasopismo on line (fwd)
by Andrzej Marecki 08 May '03

08 May '03

----- Forwarded message from Biblioteka CA UMK ----- Delivered-To: astro.staff(a)astri.uni.torun.pl Date: Thu, 8 May 2003 09:35:29 +0200 (MET DST) From: Biblioteka CA UMK <cfalib(a)newton.astro.uni.torun.pl> To: staff(a)astro.uni.torun.pl cc: staff(a)astri.uni.torun.pl Subject: Nowe czasopismo on line Szanowni Czytelnicy! To jest oferta nowego czasopisma on-line. Do konca roku mamy dostep za darmo ale od nowego roku zaproponuja oplate. Prosze przejrzec ta oferte i zdecydowac czy warto sie tym zainteresowac. O ewentualnej prenumeracie elektronicznej na rok 2004 musze wiedziec do konca maja. pozdrawiam Karolina Wojtkowska ------- Forwarded message follows ------- Date sent: 8 May 2003 00:00:53 -0000 To: Dominika.Czyzak(a)bu.uni.torun.pl (Dominika Czyzak) From: andrew.wray(a)iop.org Send reply to: karen.brixey(a)iop.org Subject: Free offer from Journal of Cosmology and Astroparticle Physics (3/415) We're delighted to introduce a major new electronic-only publication, the Journal of Cosmology and Astroparticle Physics (JCAP). JCAP is published in partnership between the Institute of Physics Publishing (IOP) and the International School for Advanced Studies (SISSA) and will follow a similar trajectory to that of its sister journal Journal of High Energy Physics (JHEP). JCAP brings together cutting-edge research in all aspects of cosmology as well as astrophysics and particle physics. The journals remit encompasses theoretical, observational and experimental areas as well as computation and simulation. The first papers appeared online in March 2003. Access to the full text is free to all until the end of 2003. Beginning January 2004 a low annual subscription will be introduced for institutions. For more information or to place your order, please visit http://ej.iop.org/pdf/jcap.pdf to download an order form. JCAP will be included in Packs A, B and Z as well as the new Package H for 2004. With this new addition there has never been a better time to upgrade to an IOP journal package! Please contact your regional representative for more information on how you can save money on your subscriptions. A full list of representatives is available at www.iop.org/EJ/enquiries or e-mail custserv(a)iop.org for more information. We have also produced a colourful A3 poster to enable you to publicise this exciting new journal to your end users and I am delighted to offer you a complimentary copy for your institution. If you would like to receive a copy, please reply to this email, indicating to whom the parcel should be addressed. I look forward to hearing from you soon Kind regards Dr Andrew Wray Senior Publisher Institute of Physics Publishing Dirac House, Temple Back, Bristol BS1 6BE, UK ------- End of forwarded message ------- ***************************************************************************** ----- End of forwarded message from Biblioteka CA UMK -----

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Re: Nowe czasopismo on line
by Andrzej Marecki 08 May '03

08 May '03

[...] > Access to the full text is free to all until the end of 2003. Beginning January > 2004 a low annual subscription will be introduced for institutions. ^^^ Hope it's going to be truly low. ;) Anyway, let's go for it! A.M.

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The Extragalactic Distance Scale
by Andrzej Marecki 28 Apr '03

28 Apr '03

Paper: astro-ph/0304427 From: Joseph B. Jensen <jjensen(a)gemini.edu> Date: Wed, 23 Apr 2003 23:52:07 GMT (67kb) Title: The Extragalactic Distance Scale Authors: Joseph B. Jensen (Gemini), John L. Tonry (Hawaii), John P. Blakeslee (JHU) Comments: 18 pages, 1 figure; contribution to Measuring and Modeling the Universe, Carnegie Observatories Astrophysics Series Vol. 2, ed. W. L. Freedman \\ Significant progress has been made during the last 10 years toward resolving the debate over the expansion rate of the Universe. [...] We discuss remaining systematic uncertainties, particularly related to the Cepheid calibration, and identify where improvements are likely to be made in the next few years. \\ ( http://de.arXiv.org/abs/astro-ph/0304427 , 67kb) ------------------------------------------------------------------------------ [...] ----- End of forwarded message from astro-ph -----

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"projective sphere" (fwd)
by boud 01 Apr '03

01 Apr '03

hi, i received this from a friend. The projective sphere is the 2-sphere S^2 where each point is identified with its opposite point. So the fundamental polygon is a hemisphere. Geodesics only intersect once in the projective sphere. > Hi Boud, > what an irony, but I am looking for your help with Polish !!! > Could you or your collaborators on topology in Torun > enlighten me with Polish term for "projective sphere" ? > Thanks in advance, Can anyone help? boud

2 1

topology - WMAP - urgent
by boud 19 Mar '03

19 Mar '03

Witam, Micha³, Bartek, anyone else interested. Now that there's some big time media coverage, anyone interested in working together on this? IMHO it's urgent to do the analysis ourselves. I haven't fully understand Marek's comments, but I think he's just playing safe ;) - no harm there. Anyone who sees signs that our North/South American and or European colleagues have done something concrete on this, please say and point to the URL! Boud amr wrote: > Artyku³ o odkryciu ("odkryciu" ?) Tegmarka: > http://www.gazeta.pl/nauka/1,34148,1376101.html > Krytyka Marka Demiañskiego: > http://www1.gazeta.pl/nauka/1,34148,1376526.html ---------- Forwarded message ---------- > Date: Wed, 19 Mar 2003 12:57:53 +0100 (MET) > From: Programme National de Cosmologie <pnc at iap.fr> > To: diffusion PNC <pnc at iap.fr> > Subject: divers ... --------------------------------------------------------------------------- PNC PNC PNC http://www.iap.fr/pnc/ PNC PNC PNC PNC --------------------------------------------------------------------------- 4. Extraits d'un article du New-York Times du 11 mars 2003 "Universe as Doughnut: New Data, New Debate" The New York Times March 11, 2003 Universe as Doughnut: New Data, New Debate By DENNIS OVERBYE Long ago in the dawn of the computer age, college students often whiled away the nights playing a computer game called Spacewar. It consisted of two rocket ships attempting to blast each other out of the sky with torpedoes while trying to avoid falling into a star at the center of the screen. Although cartoonish in appearance, the game was amazingly faithful to the laws of physics, complete with a gravitational field that affected both the torpedoes and the rockets. Only one feature seemed outlandish: a ship that drifted off the edge of the screen would reappear on the opposite side. Real space couldn't work that way. Or could it? Imagine that the Spacewar screen is wrapped around to form a cylinder or a section of a doughnut so that the two edges meet. That is the picture of space, some cosmologists say, that has been suggested by a new detailed map of the early universe. Their analysis of this map has now provided a series of hints though only hints that the universe may have a more complicated shape than astronomers presumed. ... This mirror game is not limited to cubes and doughnuts. Over the years mathematicians, particularly Dr. William Paul Thurston, now at the University of California at Davis, and Dr. Jeffrey Weeks, an independent mathematician, have speculated about universes composed of various polyhedrons glued together in various ways. In 1996 the French astronomer Dr. Jean-Pierre Luminet of the Paris Observatory and his colleagues Dr. Roland Lehoucq and Dr. Marc Lachieze-Rey, both of the Center for Astrophysical Studies in Saclay, France, developed a method called "cosmic crystallography," using galaxy statistics to detect and diagnose the repeating periodic patterns that would be created in the sky by light going around and around in differently shaped universe. Finite or Infinite? Problems Are Posed For Favored Theory ...

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astro-ph/0302496 - T^1 model in WMAP data? - compare astro-ph/0007140
by Boud Roukema 13 Mar '03

13 Mar '03

1 0

final polski version of grant application
by Boud Roukema 19 Feb '03

19 Feb '03

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\adminthree} \newcommand\totalthree{\arabic{totalthree}} \newcounter{totalall} \setcounter{totalall}{\totalone+\totaltwo+\totalthree} \newcommand\totalall{\arabic{totalall}} \newcounter{grandtotal} \setcounter{grandtotal}{\totalall} \newcommand\grandtotal{\arabic{grandtotal}} \newcounter{dummy} \setcounter{dummy}{12} \newcommand\dummy{\arabic{dummy}} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{document} \begin{flushleft} \textcolor[rgb]{1.000,1.000,1.000}{{\footnotesize{} }} \textbf{\textcolor[rgb]{1.000,1.000,1.000}{Za\l{}ącznik nr 15}} \end{flushleft} \begin{center} \end{center} \begin{center} \end{center} \begin{center} \textbf{WNIOSEK} \end{center} \begin{center} \textbf{o finansowanie projektu badawczego} \end{center} \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{Tytu\l{} projektu} {\bf \centerline{\underline{Poszukiwanie soczewkowania topologicznego}} \centerline{\underline{wśród aktywnych radiogalaktyk (AGNs) i gromad galaktyk}} } \smallskip \centerline{(Search for Topological Lensing of Radio-Loud Active Galactic Nuclei and Galaxy Clusters)} \end{flushleft} \begin{flushleft} \textbf{A. DANE WNIOSKODAWCY} \end{flushleft} \begin{flushleft} Wype\l{}nia Komitet Bada\'n Naukowych {\em 1. Nazwa i adres jednostki, w której będzie realizowany projekt} \end{flushleft} \begin{flushleft} {\em (w przypadku uczelni poda\'c tak\.ze: wydzia\l{}, instytut, katedrę lub zak\l{}ad)} \end{flushleft} Centrum Astronomiczne Uniwersytet Mikolaja Kopernika (CA-UMK), %Toru\'n Centre for Astronomy, Nicolas Copernicus University, ul. Gagarina, 11, Toru\'n 87-100; director prof. hab. dr Andrzej Kus \begin{flushleft} {\em 2. NIP} \NIPTCfA \\ {\em REGON} \REGONTCfA \end{flushleft} \begin{flushleft} {\em 3. Nazwa banku, numer rachunku} \\ \bankTCfA \end{flushleft} \begin{flushleft} {\em 4. Kierownik projektu\textit{ }(tytu\l{} i stopie\'n naukowy, imię, nazwisko, adres prywatny, telefon; miejsce zatrudnienia - w przypadku uczelni poda\'c tak\.ze: wydzia\l{}, instytut, katedrę lub zak\l{}ad - telefon, e-mail)Numer rejestracyjny projektu} \end{flushleft} dr Boudewijn Roukema, \adresboud \begin{flushleft} {\em Data z\l{}o\.zenia} \end{flushleft} \datepolski \begin{flushleft} {\em Zespó\l{} Komitetu} \end{flushleft} PO3D \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{B. DANE OGÓLNE} \end{flushleft} \begin{flushleft} {\em 1. Planowany okres realizacji projektu. {\bf \monthstotal}.. miesięcy (01.2004 -- 12.2006)} \end{flushleft} \begin{flushleft} {\em 2. Liczba osób przewidzianych do udzia\l{}u w realizacji projektu} {\bf 6} \end{flushleft} \begin{flushleft} {\em 3. Rodzaj projektu: \textbf{w\l{}asny} - %\rule[0.5ex]{48mm}{0.2ex}\hspace{-45mm} \sout{promotorski -- zamawiany Nr} wg og\l{}oszenia (niepotrzebne skre\'sli\'c).}\\ \end{flushleft} \begin{flushleft} {\em 4. Propozycja skierowania wniosku: (symbol lub nazwa sekcji specjalistycznej Komitetu)} \end{flushleft} {\bf P03D: Astronomia i astrofizyka} \begin{flushleft} {\em 5. Planowane nak\l{}ady {\rm \grandtotal~PLN} (w z\l{}) ogó\l{}em} \end{flushleft} \begin{flushleft} {\em w tym w latach } 2004: \totalone~PLN; 2005: \totaltwo~PLN, 2006: \totalthree~PLN \end{flushleft} \begin{flushleft} {\em 6. S\l{}owa kluczowe} \end{flushleft} kosmologia obserwacyjna, topologia kosmiczna, aktywne jądra radiogalaktyk, gromady galaktyk \clearpage \begin{flushleft} {\bf 7. Streszczenie projektu} \end{flushleft} \begin{flushleft} (streszczenie mo\.ze by\'c upowszechnione przez Komitet po zakwalifikowaniu projektu do finansowania) \end{flushleft} \begin{centering} {\underline{Poszukiwanie soczewkowania topologicznego}} {\underline{wśród aktywnych radiogalaktyk (AGNs) i gromad galaktyk}} \smallskip (Search for Topological Lensing of Radio-Loud Active Galactic Nuclei and Galaxy Clusters) \end{centering} \smallskip % Równania Hilberta-Einsteina są niewystarczające do opisania geometrii % Wszechświata, ponieważ dotyczą tylko lokalnej geometrii: krzywizny. % Ogólna wiedza na temat geometrii przestrzeni, jeśli w ogóle możliwa, % wymagać będzie pomiaru topologii Wszechświata. % Od czasu kiedy temat ten był dyskutowany przez Schwarzschilda (1900), % próby obserwacyjnego zmierzenia ogólnej topologii były rzadkie. % Przyspieszeniu uległy dopiero w latach 1990-tych wskutek gwałtownego % wzrostu obserwacji The Hilbert-Einstein equations are insufficient to describe the geometry of the Universe, as they only constrain a local geometrical property: curvature. A global knowledge of the geometry of space, if possible, would require measurement of the topology of the Universe. Since the subject was discussed in 1900 by Schwarzschild, observational attempts to measure global topology have been rare for most of this century, but have accelerated in the 1990's due to the rapidly increasing amount of observations of non-negligible fractions of the observational sphere. The basic physical test for measuring the topology of the Universe is simple from a na\"{\i}ve theoretical point of view: it is sufficient to see multiple images of extragalactic objects whose light travels to the observer via straight lines (geodesics) in different directions, or in other words that crosses the Universe from different directions or more than once. Hence, the term ``topological lensing'', since whatever theory might in the future explain the global shape of the Universe will presumably be an extension of general relativity, and just as general relativity is tested by gravitational lensing, where single objects such as high redshift galaxies are seen several times, the future theory (probably a theory of quantum gravity) should be constrained by topological lensing. In practice, just as the individual and statistical observational properties of extragalactic objects have made determination of local cosmological parameters (such as the matter density parameter, the cosmological constant and the Hubble constant) much more difficult than was hoped, their properties make the search for topological lensing difficult. The most promising objects at high redshifts for detecting topological lensing are those we can see in large numbers and across large volumes of space: (1) active galactic nuclei (AGNs) and (2) clusters of galaxies. In the Toru\'n Centre for Astronomy, we have a combination of \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \item existing observational expertise in radio-loud AGNs (RLAGNs) including the study of the evolution of RLAGNs (Marecki, Kunert, Gawro\'nski); and \item with the OCRA (One-cm Receiver Array) project, we hope to soon obtain a catalogue of thousands of clusters of galaxies at high redshifts via the Sunyaev-Zel'dovich Effect (Soberski); and \item the PI (Roukema) has developed observational strategies for investigating cosmic topology. \end{list} For this reason, we have an excellent opportunity at TCfA to excel in this field. Although our focus will be on the use of RLAGNs and clusters of galaxies, knowledge of cosmic microwave background (CMB) observational analyses will be crucial for independently checking any serious candidates for topological lensing. We are fortunate to have the presence in our group of an expert in CMB data, Bartosz Lew, who we expect to achieve the status of Magister during 2003. \clearpage \begin{flushleft} \textbf{C. INFORMACJE O WYKONAWCACH} \end{flushleft} \begin{flushleft} {\em 1. O\'swiadczenia} \end{flushleft} \begin{quote} {Przyjmuję warunki udzia\l{}u w konkursie projektów badawczych, okre\'slone w przepisach w sprawie kryteriów i trybu przyznawania i rozliczania \'srodków finansowych ustalanych w bud\.zecie pa\'nstwa na naukę oraz wyra\.zam zgodę na zamieszczenie moich danych osobowych zawartych we wniosku w zbiorze danych Komitetu Bada\'n Naukowych oraz na przetwarzanie tych danych zgodnie z przepisami ustawy z dnia 29 sierpnia 1997 r. o ochronie danych osobowych (Dz. U. Nr 133, poz. 883 z pó\'zn. zm.).} \end{quote} \begin{flushleft} {\em 2. Wykaz wykonawców} \begin{tabular}{c|l|r|c|c} \hline \\ Lp. & \multicolumn{1}{c|}{Charakter udzia\l{}u w realizacji projektu,} & Udział w & Symbol & {~~Podpis~~} \\ & \multicolumn{1}{c|}{tytu\l{} i stopie\'n naukowy, imię, nazwisko, nr PESEL} & realizacji &\multicolumn{1}{c|}{rodzaju} & \\ &\multicolumn{1}{c|}{miejsce zatrudnienia, stanowisko} & projektu&&\\ 1 & Kierownik projektu - dr Boudewijn Roukema & 100\% & \symbolrodzaju\\ & CA-UMK, adiunkt \fbox{\rule{3cm}{0cm}\rule{0cm}{1.5ex}} &&& \\ 2& Wykonawca - dr Andrzej Marecki \protect\fbox{\rule{3cm}{0cm}\rule{0cm}{1.5ex}}& 67\% &\symbolrodzaju& \\ & CA-UMK, adiunkt &&& \\ 3& Wykonawca - mgr Magdalena Kunert \fbox{ \peselmagda } & 50\% & \symbolrodzaju&\\ & CA-UMK, doktorant &&& \\ 4& Wykonawca - mgr Marcin Gawro\'nski \fbox{\rule{3cm}{0cm}\rule{0cm}{1.5ex}}& 50\% & \symbolrodzaju&\\ & CA-UMK, doktorant&&& \\ 5& Wykonawca - mgr Sebastian Soberski \fbox{\rule{3cm}{0cm}\rule{0cm}{1.5ex}}& 50\% &\symbolrodzaju& \\ & CA-UMK, doktorant &&& \\ 6& Wykonawca - (2003 mgr) Bartosz Lew \fbox{\rule{3cm}{0cm}\rule{0cm}{1.5ex}}& 50\% &\symbolrodzaju\\ & CA-UMK &&& \\ &&&&\\ \hline \end{tabular} $^{\mathrm{1/}}$ nale\.zy wpisa\'c ,,P''- umowa o pracę, mianowanie, ,,Z''- umowa zlecenia, ,,D''- umowa o dzie\l{}o \end{flushleft} %%% end table %%%% \begin{flushleft} {\em 3. Ankieta dorobku naukowego kierownika projektu i najwa\.zniejszych wykonawców projektu} \end{flushleft} \begin{flushleft} {\em 1) Imię i nazwisko} \end{flushleft} dr Boudewijn Roukema \begin{flushleft} {\em 2) Przebieg pracy naukowej: nazwa szko\l{}y wy\.zszej, instytutu lub innej jednostki organizacyjnej specjalno\'s\'c } \end{flushleft} \begin{flushleft} {\em data uzyskania tytu\l{}u zawodowego, tytu\l{}u lub stopnia naukowego} \end{flushleft} \begin{flushleft} doktora \end{flushleft} 1989-93: Doktorat z Filozofii w Astronomii i Astrofizyce, Mt Stromlo and Siding Spring Observatories (M.S.S.S.O.), Australian National University (A.N.U.), Canberra. 1985-88: Bachelor of Science (Hons), Australian National University, Canberra, Australia \begin{flushleft} {\em 3) Informacje o pracach wykonanych w okresie ostatnich 4 lat przed zg\l{}oszeniem wniosku} \end{flushleft} \begin{flushleft} {\em (wykaz najwa\.zniejszych publikacji - maksimum 10 pozycji, poda\'c miejsce i datę publikacji; opracowane nowe technologie; najwa\.zniejsze osiągnięcia poznawcze, aplikacyjne).} \end{flushleft} Główne Tematy Badawcze %{Main Research Interests} (i) {\em Observational Cosmology} and (ii) {\em Galaxy Formation}: (i) Observational constraints on statistics of ``large scale'' structure, observational constraints on local cosmological parameters (such as the density parameter and the cosmological constant), and observational programmes to try to constrain global cosmological parameters; (ii) Merging-history-tree based galay formation models in a cosmological context and their comparison with observational galaxy statistics. \begin{list}{\arabic{enumi}}{\usecounter{enumi}} \item \pub \underline{Roukema, B.F.} \& Bajtlik, S., 1999;;Transverse Galaxy Velocities from Multiple Topological Images;;\mnras;;308;;309 \ (arXiv:astro-ph/9903038) %% CAMK, IAP, IUCAA %art \item \pub \underline{Roukema, B.F.}, 2000a;;COBE and Global Topology: An Example of the Application of the Circles Principle;;\mnras;;312;;712 \ (arXiv:astro-ph/9910272) %% IUCAA %ftp blacksci 15/10/99 %art \mdcitem %\item \pub \underline{Roukema, B.F.} \& Mamon, G.A., 2000;;Tangential Large Scale Structure as a Standard Ruler: Curvature Parameters from Quasars;;\AandA;;358;;395 \ (arXiv:astro-ph/9911413) %art %%395-408 %\item \mdcitem \pub \underline{Roukema, B.F.}, 2000b;;A Counterexample to Claimed COBE Constraints on Compact Toroidal Universe Models;;\cqg;;17;;3951 \ (arXiv:astro-ph/0007140) \item \pub \underline{Roukema, B.F.}, 2000c;;The Topology of the Universe;;Bulletin of the Astronomical Society of India;;28;;483 \ (arXiv:astro-ph/0010185) \revinvit \item \pub \underline{Roukema, B.F.} \& Mamon, G.A., 2001;;Lifting cosmic degeneracy within a single data set;;{\AandA};;366;;1 \ (arXiv:astro-ph/0010511) \item \pub \underline{Roukema, B.F.}, 2001b;;How to distinguish a nearly flat Universe from a flat Universe using the orientation independence of a standard ruler;;{\AandA};;369;;729 \ (arXiv:astro-ph/0102095) %art \item \pub \underline{Roukema, B.F.}, 2001d;;On the comoving distance as an arc-length in four dimensions;;{\mnras};;325;;138 \ (arXiv:astro-ph/0102099)%art \item \pub \underline{Roukema, B.F.}, Ninin, S., Devriendt, J., Bouchet, F.B., Guiderdoni, B., Mamon, G.A., 2001;;Star Formation Losses Due to Tidal Debris in `Hierarchical' Galaxy Formation;;\AandA;;373;;494 \ (arXiv:astro-ph/0105152) %art \item \pub \underline{Roukema, B.F.}, Mamon, G.A., \& Bajtlik, S., 2002;;The Cosmological Constant and Quintessence from a Correlation Function Comoving Fine Feature in the 2dF Quasar Redshift Survey;;{\AandA};;382;;397 \ (arXiv:astro-ph/0106135) \end{list} \begin{flushleft} {\em 4) Wykonane i aktualnie wykonywane projekty badawcze finansowane ze \'srodków bud\.zetowych na naukę - numery projektów - charakter udzia\l{}u przy realizacji projektu oraz czy uzyska\l{} lub uzyskuje z tego tytu\l{}u wynagrodzenie (tak, nie). } \end{flushleft} \begin{flushleft} {\em 5) Do\'swiadczenia naukowe zdobyte w kraju i za granicą (kraj, instytucja, rodzaj pobytu, okres pobytu).} \end{flushleft} \noin od 2002: adiunkt, Toru\'n Centre for Astronomy, Uniwersytet Miko\l{}aja Kopernika, Toru\'n, Poland \noin 2001: konsultant, DARC/LUTH (Laboratoire de l'Univers et ses Th\'eories), Observatoire de Meudon, France \noin 1998--2000: postdoctoral fellow, Inter-University Centre for Astronomy \& Astrophysics, Pune, India \noin Feb--July 1998: konsultant, CAMK, Warszawa %\noin May-Sep 1997: konsultant, Institut d'Astrophysique % de Paris, CNRS, France %(R) %\noin April 1997: konsultant, Beijing %Astronomical Observatory, Beijing, P.R.China %(R) \noin 1996--1997: Centre of Excellence foreign visiting fellow, NAOJ, % Mitaka, Tokyo, %181, Japan %(R) %\smallskip \noin 1994--1995: postdoctoral research fellow, Astronomy Centre, University of Sussex, U.K. %(RT) %United Kingdom %\smallskip %\noin Aug/Sep 1994: Visitor, Dept of Astronomy, Bandung Institute of %Technology, Bandung, Indonesia %(T) %\smallskip \noin Jan/Feb 1994: konsultant, Institute of Astronomy, University of Cambridge, United Kingdom %(R) %\smallskip \noin 1993: postdoctoral fellow, Institut d'Astrophysique de Paris, CNRS, France %(R) \begin{flushleft} {\em 6) Najwa\.zniejsze międzynarodowe i krajowe wyró\.znienia wynikające z prowadzenia bada\'n naukowych lub prac rozwojowych (rodzaj wyró\.znienia, miejsce i data).} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} Miejscowo\'s\'c i data \rule{2cm}{0ex} Podpisy osób wype\l{}niających ankietę \end{flushleft} \bigskip \begin{flushleft} {\em 3. Ankieta dorobku naukowego kierownika projektu i najwa\.zniejszych wykonawców projektu} \end{flushleft} \begin{flushleft} {\em 1) Imię i nazwisko} \end{flushleft} dr Andrzej Marecki \begin{flushleft} {\em 2) Przebieg pracy naukowej: nazwa szko\l{}y wy\.zszej, instytutu lub innej jednostki organizacyjnej specjalno\'s\'c } \end{flushleft} \begin{flushleft} {\em data uzyskania tytu\l{}u zawodowego, tytu\l{}u lub stopnia naukowego} \end{flushleft} \begin{flushleft} doktora \end{flushleft} 1980 Magister (astronomia) UMK, Toru\'n 1992 Doktor (astronomia) UMK, Toru\'n \begin{flushleft} {\em 3) Informacje o pracach wykonanych w okresie ostatnich 4 lat przed zg\l{}oszeniem wniosku} \end{flushleft} \begin{flushleft} {\em (wykaz najwa\.zniejszych publikacji - maksimum 10 pozycji, poda\'c miejsce i datę publikacji; opracowane nowe technologie; najwa\.zniejsze osiągnięcia poznawcze, aplikacyjne).} \end{flushleft} Krótki odpis projektów naukowych: %Brief description of research projects: %Interferometryczne obserwacje radiowo głośny AGN (RLAGN) Interfermetric observations of radio-loud AGN (RLAGN) aimed to reveal structures of compact i.e. {\it young} objects. Selection and observations (MERLIN, VLBI) of a new sample of faint compact objects. Measurements of the velocities of the components in such radio structures. \begin{list}{\arabic{enumi}}{\usecounter{enumi}} \item \underline{Marecki, A.}, Falcke H., Niezgoda J. Garrington, S.T., Patnaik A.R. (1999) "Gigahertz Peaked Spectrum sources from the Jodrell Bank-VLA Astrometric Survey" A\&AS 135, 273 \item Fanti, C. ... \underline{Marecki, A.}, et al. (2000) "ISO observations of a sample of CSS and GHz Peaked Spectrum radio galaxies", A\&A 358, 499 \item Browne, I. W. \underline{Marecki, A.}, et al. (2000) "OCRA: a one-centimeter receiver array" SPIE 4015, 299 \item \underline{Kunert, M.}, \underline{Marecki, A.} et al. (2002) "FIRST-based survey of Compact Steep Spectrum sources. I. MERLIN images of arc-second scale objects" A\&A 391, 47 \item \underline{Marecki, A.} et al. (2003) "Location of Weak CSS Sources on the Evolutionary Path of Radio-Loud AGN", PASA 20, in press (astro-ph/0211253) \item \underline{Marecki, A.} et al. (2003) "Weak CSS Sources from the FIRST Survey", PASA 20, in press (astro-ph/0211249) \item \underline{Marecki, A.} et al. (2003) "1245+676 - a CSO/GPS source being an extreme case of a double-double" PASA 20, in press (astro-ph/0209212) \end{list} \begin{flushleft} {\em 4) Wykonane i aktualnie wykonywane projekty badawcze finansowane ze \'srodków bud\.zetowych na naukę - numery projektów - charakter udzia\l{}u przy realizacji projektu oraz czy uzyska\l{} lub uzyskuje z tego tytu\l{}u wynagrodzenie (tak, nie). } \end{flushleft} \begin{flushleft} {\em 5) Do\'swiadczenia naukowe zdobyte w kraju i za granicą (kraj, instytucja, rodzaj pobytu, okres pobytu).} \end{flushleft} od 1992 adiunkt, Centrum Astronomii, UMK, Toru\'n \begin{flushleft} {\em 6) Najwa\.zniejsze międzynarodowe i krajowe wyró\.znienia wynikające z prowadzenia bada\'n naukowych lub prac rozwojowych (rodzaj wyró\.znienia, miejsce i data).} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} Miejscowo\'s\'c i data \rule{2cm}{0ex} Podpisy osób wype\l{}niających ankietę \end{flushleft} \begin{flushleft} \end{flushleft} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{flushleft} \textbf{\newpage } \end{flushleft} \begin{flushleft} \textbf{D. OPIS PROJEKTU BADAWCZEGO, METODYKA BADA\'N ORAZ CHARAKTERYSTYKA OCZEKIWANYCH WYNIKÓW} \end{flushleft} \begin{flushleft} {\em 1. Cel naukowy projektu - jaki problem wnioskodawca podejmuje się rozwiąza\'c, co jest jego istotą, co uzasadnia podjęcie tego problemu w Polsce, jakie przes\l{}anki sk\l{}aniają wnioskodawcę do podjęcia proponowanego tematu?} \end{flushleft} The problem being posed is to try to measure the shape of the Universe. This is important because the Universe is the object in which we live and it is of obvious scientific and cultural interest to be aware of the shape of the object in which we live. It should be undertaken here because we have a combination of present and developing observational expertise in radio-loud active galactic nuclei (RLAGNs) and clusters of galaxies via the Sunyaev-Zel'dovich Effect respectively, plus expertise in the development of observational strategies for measuring cosmic topology. Poland has obvious historical precedents in showing that the Earth is not the centre of the Universe, and that planets around other stars exist. It would clearly be good to continue the tradition on a much larger length scale (Gigaparsecs). \begin{flushleft} {\em 2. Istniejący stan wiedzy w zakresie tematu bada\'n -jaki oryginalny wk\l{}ad wniesie rozwiązanie postawionego problemu do dorobku danej dyscypliny naukowej w \'swiecie i w Polsce, czy w kraju i w \'swiecie jest to problem nowy czy kontynuowany i w jakim zakresie weryfikuje utarte poglądy i dotychczasowy stan wiedzy?} \end{flushleft} It is clear that topological lensing on scales of a few hundred Megaparsecs is extremely unlikely. Attempted constraints on scales from 1 Gigaparsec (1$h^{-1}$Gpc) to the horizon diameter of about 20$h^{-1}$Gpc (comoving) are much weaker and generally very model dependent. This project will use RLAGNs and clusters of galaxies up to redshifts of about $z\sim2-3$ as tracers, covering a volume of about half the diameter of the observable Universe, i.e. about 10$h^{-1}$Gpc. It will advance discovery and understanding by using these tracers as realistically as possible given understanding of their evolution and properties. This problem dates back to the pre-relativistic era (Schwarzschild 1900), but has only been tackled non-trivially since the early 1990s. Work on this theme is still in the pioneering stage. \begin{flushleft} {\em 3. Metodyka bada\'n - co stanowi podstawę naukowego warsztatu wnioskodawcy i jak zamierza rozwiąza\'c postawiony problem, na czym będzie polega\'c analiza i opracowanie wyników bada\'n, jakie urządzenia (aparatura) zostaną wykorzystane w badaniach, czy wnioskodawca ma do nich bezpo\'sredni dostęp i umiejętno\'s\'c obs\l{}ugi?} \end{flushleft} The methodology is to use a range of methods, from studies of individual objects to statistical studies of large catalogues, and to parametrise understanding of the properties of the tracers in order to make these methods as observationally correct and precise as possible. Just as the supernova type Ia method was only one among many methods proposed for measuring local cosmological parameters, but happened to be the most dramatically successful, it is impossible to predict beforehand which specific method for measuring topological lensing will first yield highly significant results. Although the TCfA 32m telescope will be used for part of the general understanding of RLAGNs and for the OCRA project, which should in the long term yield large numbers of high-redshift clusters of galaxies, use of existing public catalogues such as those available at the Centre de Donn\'ees astronomiques de Strasbourg (CDS) and the information processing analysis requires the use of computers and computer peripherals. We do have access to these telescopes and databases and have experience managing computer resources. \begin{flushleft} {\em 4. Co będzie wymiernym, udokumentowanym efektem podjętego problemu - zak\l{}adany sposób przekazu i upowszechnienia wyników (publikacje naukowe oraz referaty na konferencjach w kraju i za granicą, monografie naukowe, rozprawy doktorskie i habilitacyjne, nowe patenty i ,,know-how'', nowe metody i urządzenia badawcze)?} \end{flushleft} This is a {\bf research} project, not a {\bf development} project, and the required theory which goes beyond general relativity has not yet been developed, so while we would hope to detect topological lensing, the results cannot be predicted before they are found. Articles on the results will of course be published in refereed journals, presented at conferences, and professionals and non-professionals will be able to follow (and maybe participate) in the research on our web pages via the normal methods of internet culture such as publicly archived mailing lists and wiki pages. \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{E. W ODNIESIENIU DO PROJEKTÓW ZAMAWIANYCH -- INFORMACJA O SPE\L{}NIENIU OKRE\'SLONYCH PRZEZ KOMITET WARUNKÓW UCZESTNICZENIA W KONKURSIE, W SZCZEGÓLNO\'SCI DOTYCZĄCYCH WSPÓ\L{}PRACY Z PARTNERAMI ZAGRANICZNYMI} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{F. }\textbf{ HARMONOGRAM WYKONANIA PROJEKTU BADAWCZEGO -- PLAN ZADA\'N} \end{flushleft} %\begin{center} %Lp.Nazwa i opis zadaniaTermin realizacji %\\(m-c, rok)Przewidywane koszty\\(z\l{})1234Razem %\end{center} %\begin{flushleft} %\textbf{F. PROJECT} \textbf{SCHEDULE} \textbf{- ANTICIPATED TASKS} %\end{flushleft} \setcounter{x}{(\saltotalyear) /2} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *6} \renewcommand\y{\arabic{y}} \setcounter{z}{\consult /3} \renewcommand\z{\arabic{z}} \setcounter{w}{\y + \equip + \z*3 +\allconfer + \adminone+ \admintwo+ \adminthree } \renewcommand\w{\arabic{w}} \usecounter{enumi} \begin{center} \begin{tabular}{clrr} \hline \\ Lp. & Nazwa i opis zadania %Termin realizacji %&(m-c, rok)Przewidywane koszty %&(z\l{})1234Razem & \multicolumn{1}{c}{Termin} & \multicolumn{1}{c}{Przewidywane} \\ %Expected cost (z\l{}) \\ & & \multicolumn{1}{c}{realizacji} & \multicolumn{1}{c}{koszty (zł)} \\ & & \multicolumn{1}{c}{(m-c, rok)} & \\ \\ \addtocounter{enumi}{1} \arabic{enumi} & parametryczne modelowanie efektów rzutowania %parametric modelling of projection \\ & i ewolucji wielokrotnych obrazów %and evolution effects of multiple images & 6/2004 & \x~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & zastosowania do poszczególnych par kandydatów % application to individual candidate pairs & 12/2004 & \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} % & zakup komputerów i periferiów %purchase computer items & 12/2004 & \equip~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & międzynarodowe konsultacje kosmologiczne % international cosmology consultants & 12/2004 & \z~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & konferencje, public relations & 12/2004 & \allconferyear~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & koszty pośrednie & 12/2004 & \adminone~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & poszukiwania przewidywanych obrazów topologicznych %predictions of further images & 6/2005 & \x~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & statystyczna analiza katalogów RLAGN'ów %statistical analysis of RLAGN catalogues & 12/2005 & \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & międzynarodowe konsultacje kosmologiczne %international cosmology consultants & 12/2005 & \z~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & konferencje, public relations & 12/2005 & \allconferyear~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & koszty pośrednie & 12/2005 & \admintwo~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & statystyczna analiza katalogów gromad galaktyk, %statistical analysis of cluster catalogues, \\ & przewidywania obrazów topologicznych dla OCRA & 6/2006& \x~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & poszukiwania przewidywanych obrazów topologicznych %predictions of further images & 12/2006 & \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & międzynarodowe konsultacje kosmologiczne %international cosmology consultants & 12/2006 & \z~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & konferencje, public relations & 12/2006 & \allconferyear~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & koszty pośrednie & 12/2006 & \adminthree~PLN % % \\ \hline & & Razem & \w~PLN \\ \hline \end{tabular} \end{center} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{flushleft} {\footnotesize{}\newpage } \end{flushleft} \begin{flushleft} \textbf{G. KOSZTORYS PROJEKTU BADAWCZEGO} \end{flushleft} \begin{flushleft} {\em 1. Poszczególne pozycje kosztorysu w cenach bie\.zących (w z\l{})} \end{flushleft} % \begin{center} % Lp.Tre\'s\'cPlanowane koszty w roku bud\.zetowym %Razem12345671Koszty bezpo\'srednie, w tym: %1/ Wynagrodzenia z pochodnymi 2/ Koszty zakupu aparatury naukowo - %badawczej 3/ Inne koszty realizacji projektu2Koszty po\'srednie %3Koszty ogó\l{}em finansowane ze \'srodków na naukę (1+2) % \end{center} \begin{center} \begin{spacing}{1.24} \setcounter{y}{\saltotalyear + \saltotalyear + \saltotalyear} \renewcommand\y{\arabic{y}} \setcounter{z}{\consult /3} \renewcommand\z{\arabic{z}} \begin{tabular}{llrrr|r} \hline Lp. & Tre\'s\'c & \multicolumn{3}{c}{Planowane koszty} & \\ & & \multicolumn{3}{c}{w roku bud\.zetowym (zł)} & \\ %1 1/ 2/ Koszty zakupu aparatury naukowo - badawczej %3/ Inne koszty realizacji projektu2Koszty po\'srednie3Koszty %ogó\l{}em finansowane ze \'srodków na naukę (1+2) %No. Item & \multicolumn{3}{c}{Funds for each budget year (z\l{})} % & Total \\ & & 2004 & 2005 & 2006 & Razem \\ % 1&2&3&4&5&6 \\ {\bf 1} & Koszty bezpo\'srednie, w tym: &&&& \\ {\footnotesize{}1/ } & Wynagrodzenia z pochodnymi %Salaries and benefits & \saltotalyear & \saltotalyear & \saltotalyear & \y~PLN \\ % % {\footnotesize{}2/} &Koszty zakupu aparatury naukowo - badawczej %Equipment & \equip & & & \equip~PLN\\ % {\footnotesize{}3/} &Inne koszty realizacji projektu %Other direct costs &&&&\\ % &międzynarodowe konsultacje kosmologiczne %international cosmology consultants & \z &\z &\z & \consult~PLN \\ % &konferencje, public relations & %conferences, public relations & \allconferyear &\allconferyear &\allconferyear & \allconfer~PLN \\ \hline % &{\bf 1} Razem & \subone & \subtwo& \subthree & \suball~PLN \\ &&&&\\ {\bf 2} & \multicolumn{4}{l|}{ Koszty pośrednie (koszty admin UMK -- 30\% 1/ + 3/)} %Indirect costs %(admin costs to UMK - 25\% 1st yr; 30\% 2nd, 3rd yrs)} &\\ && \adminone & \admintwo & \adminthree & \adminall~PLN \\ \hline {\bf 3} &Koszty ogółnem finansowane ze &&&& \\ &środków na naukę ({\bf 1+2}) & \totalone &\totaltwo &\totalthree& \totalall~PLN \\ \hline \end{tabular} \end{spacing} \end{center} \begin{flushleft} {\em 2. Kalkulacja poszczególnych pozycji kosztorysu} \end{flushleft} \begin{flushleft} {\em 1) Wynagrodzenia z pochodnymi} \end{flushleft} \begin{flushleft} {\em Kierownika projektu - liczba osobomiesięcy udzia\l{}u w projekcie: {\bf \monthstotal} , forma wynagrodzenia, } \end{flushleft} Według regułe KBN, 100\% \salrate{}PLN/rok dla kierownika projektu jeśli dr., 75\% dla innych wykanowców jeśli dr., 50\% \salrate{}PLN/rok dla innych wykanowców jeśli mgr. Więc: \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \setcounter{x}{\salrate *3} \renewcommand\x{\arabic{x}} \item dr Boudewijn Roukema \salrate{}PLN *3 = \x~PLN \end{list} \setcounter{x}{(\monthstotal *(\persontotal-100))/100} \renewcommand\x{\arabic{x}} \begin{flushleft} {\em Wykonawców projektu - liczba osobomiesięcy udzia\l{}u w projekcie: {\bf \x} , forma wynagrodzenia.} \end{flushleft} \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \addtocounter{enumi}{1} \setcounter{x}{(\salrate *67)/100} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *3} \renewcommand\y{\arabic{y}} % \item dr Andrzej Marecki \x~PLN *3 = \y~PLN % \setcounter{x}{(\salrate *50)/100} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *3} \renewcommand\y{\arabic{y}} % \item mgr Magdalena Kunert \x~PLN *3 = \y~PLN \item mgr Sebastian Soberski \x~PLN *3 = \y~PLN \item mgr Marcin Gawro\'nski \x~PLN *3 = \y~PLN \item (2003 mgr) Bartosz Lew \x~PLN *3 = \y~PLN \end{list} \setcounter{x}{(\salrate *(\monthstotal/12)*(\persontotal))/100} \renewcommand\x{\arabic{x}} Razem: \x~PLN \begin{flushleft} {\em 2) Opis planowanych zakupów lub wytworzenia aparatury naukowo- badawczej (poda\'c nazwę zakupu, planowany koszt, planowany miesiąc i rok zakupu oraz merytoryczne uzasadnienie zakupu).} \end{flushleft} %\prefixing Uzasadnienie: Wymienione zespoły komputerów i podzespoły są potrzebne dla syntezy i analizy danych doświadczalnych, oraz dla stworzenia sumarycznego rezultatu w postaci wyników projektu (prezentacja i dostępność wyników). Porównywanie par obiektów w dużych katalogach jest operacją czasochłonną (jak $N^2$), wymagającą dużej mocy obliczeniowej. Można ją przyspieszyć poprzeż wprowadzenie odgórnych założeń. Jednakże, historia astronomii pokazuje że przyjmowanie rozsądnych, ale złych zalożen często prowadzi do przeoczenia prawdziwego sygnału, więc posiadanie dużej mocy obliczeniowej byłoby dużym zyskiem dla projektu. Planowane zakupy na rok 2004: \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \item komputer (M. Gawro\'nski) % - AMD Athlon, 2GHz, 512Mb RAM, 100Gb hard disk, %CD burner, ethernet card, 19'' screen + 3 letnie ubezpieczenie przed kradzieżą itd \perso~kPLN \item komputer (B. Lew) % - AMD Athlon, 2GHz, 512Mb RAM, 100Gb hard disk, %CD burner, ethernet card, 19'' screen + 3 letnie ubezpieczenie przed kradzieżą itd \perso~kPLN \item komputer (M. Kunert) % - AMD Athlon, 2GHz, 512Mb RAM, %100Gb hard disk, CD burner, ethernet card, 19'' screen + 3 letnie ubezpieczenie przed kradzieżą itd \perso~kPLN \item periferia (A. Marecki) - 2 SCSI dyski 73Gb lub więcej + 3 letnie ubezpieczenie przed kradzieżą itd \scsi~kPLN \item komputer peripheral (S. Soberski) - nagrywarka CD 200~PLN, 512Mb RAM 500~PLN, %- CD burner 200~PLN, 512Mb RAM 500~PLN, razem \sober~PLN \item przenośny komputer (dla wszystkich członków grupy) + 3 letnie ubezpieczenie przed kradzieżą itd \portable~kPLN \item inkjet drukarka atramentowa/skaner/fotokopiarka + 3 letnie ubezpieczenie przed kradzieżą itd (np. inkjet PSC 750 kosztuje 900PLN; odzyskane pojemniki na tusze kosztują około 35~PLN B/W, 50~PLN kolorowe) 1~kPLN \item drukarka laserowa/skaner/fotokopiarka + 3 letnie ubezpieczenie przed kradzieżą itd 7~kPLN \end{list} Razem: \equip~PLN \smallskip \begin{flushleft} {\em 3) Uzasadnienie wysoko\'sci planowanych innych kosztów realizacji projektu (wymieni\'c rodzaj kosztów, wysoko\'s\'c oraz ich powiązanie z planem zada\'n projektu).} \end{flushleft} Koszta te odnoszą się do planu projektu w tym sensie iz, projekt jest konkurującym z innymi miedzynarodowymi, programem tak więc: (1) potrzebni są zagraniczni konsultanci dla zapewnienia wglądu do teoretycznych i doświadczalnych strategii, dotyczących sposobów dzięki którym RLAGN i gromady galaktyk mogą być używane jako obiekty soczewkowane topologicznie, jak również (2) potrzebujemy mieć możliwość prezentacji naszych wyników na miedzynarodowych konferencjach i konsultacji ze swiatowymi ekspertami w ich własnych placowkach badawczych. \smallskip (1) Środowisko naukwe, dla projektu konkurującego z innymi tego typu projektami na świecie, wymaga konsultacji ze światowymi ekspertami w okresie od 1 tygodnia do kilku miesięcy. Trzech ludzi, każdy po jednym miesiącu i czterech ludzi każdy po jednym tygodniu, w ciagu jednego roku, daje w sumie 12 osobo-miesiecy w okresie 3 lat trwania projektu. Koszt 5100 PLN/miesiąc na zagranicznych konsultantów z dziedziny kosmologii daje razem: 61200 PLN. \smallskip (2) W celu prezentacji naszych wyników na konferencjach i innych spotkaniach naukowych, uczestnictwo na dwóch międzynarodowych konferencjach na cząstkową osobe na rok byłoby zgodne z światowymi standardami Pojedyncza konferencja: międzynarodowy (Europa, Stany Zjednoczone) typowy przejazd pociągiem klasy drugiej (lub lot samolotem) w Europie, lub podróż samolotem do USA średnio wynosi 2000 PLN; miedzykontynentalny lot (economy class) (Indie/Japonia/Australia) nie przekracza 10000 PLN; tak więc średnio 3.5 kPLN jest bezpiecznym kompromisem. Tygodniowe zakwaterowanie i dniówka w Europie/USA/Japoni/Australii (2kPLN) + oplaty rejesracyjne (1 kPLN) $\Rightarrow$ 14000 kPLN. Tak więc dwie konferencje rocznie dla wszystkich osób znajdują się w zalecanych granicach wydatkow. Dwie konferencje rocznie na efektywną osobę, oraz 3.67 efektywnej osoby w okresie trzech lat daje: Razem: 154140 PLN \smallskip W celu zwiększenia przejżystości i odpowiedzialności, zyskania elastyczność, wszyscy członkowie komisji są mile widziani w naszej archiwizowanej publicznie dostepnej liscie dyskusyjnej, ze wszystkimi naukowo przydatnymi komentarzami, sugestiami lub/i krytyką: \\ \url{http://www.astro.uni.torun.pl/sympa/cosmo-torun} \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{H. O\'SWIADCZENIA I PODPISY} \end{flushleft} \begin{flushleft} 1. O\'swiadczam, \.ze zapozna\l{}em się z wnioskiem o finansowanie projektu badawczego pt.: {\bf Poszukiwanie soczewkowania topologicznego wśród aktywnych radiogalaktyk (AGNs) i gromad galaktyk (Search for Topological Lensing of Radio-Loud Active Galactic Nuclei and Galaxy Clusters)} \end{flushleft} \begin{flushleft} 2. W przypadku przyjęcia projektu badawczego do finansowania jednostka zobowiązuje się do: \end{flushleft} \begin{flushleft} - w\l{}ączenia projektu do planu zadaniowo-finansowego jednostki, \end{flushleft} \begin{flushleft} - udostępnienia lokalu, aparatury i obs\l{}ugi administracyjno-finansowej, \end{flushleft} \begin{flushleft} - zatrudnienia pracowników niezbędnych do realizacji projektu, zgodnie z wnioskiem, na podstawie umowy o pracę, umowy o dzie\l{}o lub umowy zlecenia, \end{flushleft} \begin{flushleft} - sprawowania nadzoru nad prawid\l{}owo\'scią wydatkowania \'srodków finansowych przeznaczonych na realizację projektu, a w przypadku stwierdzenia nieprawid\l{}owo\'sci - do niezw\l{}ocznego powiadomienia Komitetu. \end{flushleft} \begin{flushleft} 3. O\'swiadczam, \.ze jednostka nie mo\.ze zapewni\'c dostępu do urządze\'n wymienionych w wykazie aparatury w dziale G ust. 2 pkt 2. \end{flushleft} \begin{flushleft} 4. O\'swiadczam, \.ze wniosek nie obejmuje do\'swiadcze\'n na ludziach lub zwierzętach $^{\mathrm{2)}}$. % \sout comes from \usepackage{ulem} \sout{Do wniosku do\l{}ączono zgodę w\l{}a\'sciwej komisji etycznej na przeprowadzenie do\'swiadcze\'n na zwierzętach lub na przeprowadzenie innych bada\'n objętych w\l{}a\'sciwo\'scią komisji.} $^{\mathrm{2)}}$ \end{flushleft} \begin{flushleft} 5. O\'swiadczam, \.ze zgodnie z moją wiedzą przygotowany wniosek o finansowanie projektu badawczego nie narusza praw osób trzecich. \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} $^{\mathrm{2) }}$Niepotrzebna skre\'sli\'c. \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} Wniosek sporządzono w dniu \end{flushleft} \datepolski \begin{flushleft} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \begin{tabular}{cccc} {\em Pieczęć jednostki} & Kierownik jednostki & Kwestor & Kierownik projektu \\ & Prorektor ds Nauki i Wsp\'o\l{}pracy\\ & z Zagranic\c{a} \\ & prof dr. hab. Marek Zaidlewicz & mgr Henryk Heldt & dr Boudewijn Roukema \\ \\ \\ \\ & podpis i pieczęć & podpis i pieczęć & podpis \end{tabular} \end{flushleft} \begin{center} \end{center} \setlength{\oddsidemargin}{0.472222in-1in} \setlength{\textwidth}{\paperwidth - 0.472222in-0.472222in} \begin{center} \end{center} \begin{flushleft} \end{flushleft} \end{document}

3 2

(fwd) WMAP results
by Andrzej Marecki 18 Feb '03

18 Feb '03

-- forwarded message -- Newsgroups: sci.astro.research Path: mat.uni.torun.pl!news.man.torun.pl!news.man.poznan.pl!news-fra1.dfn.de!news.tele.dk!news.tele.dk!small.news.tele.dk!skynet.be!skynet.be!peer.news.eu-x.com!server2.netnews.ja.net!bath.ac.uk!unknown From: ebunn(a)lfa221051.richmond.edu Subject: WMAP results Approved: sci.astro.research-request(a)slimy.greenend.org.uk (mjh) Sender: unknown(a)hercules.star.bris.ac.uk (Address not verified) Organization: A poorly-installed InterNetNews site Message-ID: <mt2.0-19184-1045046860(a)star.bris.ac.uk> X-Posting-Tool: modtool v2.0 Date: Wed, 12 Feb 2003 10:47:41 GMT Lines: 78 Xref: mat.uni.torun.pl sci.astro.research:2262 MAP (now WMAP -- see below) had its press conference and has released a bunch of papers on the first-year sky maps. Technical papers are at http://map.gsfc.nasa.gov/m_mm/pub_papers/firstyear.html and a pretty picture and less-technical explanation of the results is at http://map.gsfc.nasa.gov/m_mm.html The most exciting thing about the results is that there are no big surprises! The angular power spectrum, which is the primary bit of science you get out of a microwave background sky map, is very consistent with what has become the "standard model" of cosmology: a flat inflation-based model containing dark matter and dark energy. The power spectrum is well measured past the second acoustic peak and into the third one. The temperature-polarization cross-correlation signal was also seen at about the expected level. Although surprises in the data would have been fun, the lack of surprises is actually extremely remarkable, considering (a) how strange the "standard model" is and (b) how recently cosmology has become a mature scientific discipline. I haven't read the papers yet -- there are 13 of them, some quite long! But here are a couple of highlights from scanning abstracts and figures: 1. The data let you constrain cosmological parameters much more precisely than before. In particular, the age of the Universe is 13.7 +/- 0.2 Gyr. (Not that long ago, we couldn't say more than "12 to 20 Gyr"!) The Universe is flat: Omega total is 1.02 +/- 0.02. The densities of various forms of matter and energy are pinned down quite well too. One reason WMAP is such an improvement over previous data is that it's a single data set covering both large and small scales. To get limits on parameters from previous data, you had to stitch together COBE on large scales with other experiments on small scales. Since each experiment has its own calibration errors, that means you don't measure the heights of the peaks all that well. 2. The TE polarization correlation showed up as expected. This strongly confirms that the initial fluctuations were adiabatic. That matters, because adiabatic fluctuations are a strong prediction of inflation, and large-scale adiabatic fluctuations are hard to produce in any way other than inflation. 3. The large-angular-scale polarization gives information about the way the Universe reionized after the time of decoupling. This is an area about which very little was known before now: reionization had to have happened some time, but the data didn't say when. Now we know: the optical depth to reionization is 0.17 +/- 0.04, which means that the Universe reionized at an age of about 200000 years. This is presumably when the first stars formed -- their UV radiation is what presumably reionized the Universe. 4. There is a hint that the spectral index may vary with scale, from n>1 on large scales to n<1 on small scales. That is, the primordial spectrum of fluctuations may not have been a pure power law. That's only significant at the 2-sigma level, so it may go away. If it's true, it gives useful information on discriminating between specific inflationary models. That's all I'll say for now. There's a ton of information in this data set, and people will be poring over it for a long time to come, but those are the main things that jumped out at me after a quick look. On a non-scientific note, they changed MAP to WMAP. The W stands for Wilkinson, a member of the MAP team who died last year. David Wilkinson was a leader in observational cosmology for decades, and this is a very fitting tribute to him. -Ted -- [E-mail me at name(a)domain.edu, as opposed to name(a)machine.domain.edu.] -- end of forwarded message -- -- ----------------------------------------------------------------------------- Andrzej Marecki | Torun Centre for Astronomy | e-mail: amr(a)astro.uni.torun.pl N. Copernicus University | WWW: http://www.astro.uni.torun.pl ul. Gagarina 11 | tel: +48 56 6113032 PL-87-100 Torun, POLAND | fax: +48 56 6113009 -----------------------------------------------------------------------------

2 2

Cosmo params from MAP
by Andrzej Marecki 12 Feb '03

12 Feb '03

Paper: astro-ph/0302209 From: Robert S. Hill <bhill(a)map.gsfc.nasa.gov> Date: Tue, 11 Feb 2003 20:59:59 GMT (273kb) Title: First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters Authors: D. N. Spergel [...] et al. (see also: astro-ph/0302207 and astro-ph/0302208) -- Andrzej

1 0

MAP data
by Andrzej Marecki 12 Feb '03

12 Feb '03

----- Forwarded message from NASA Science News ----- Date: Tue, 11 Feb 2003 17:12:03 -0600 Subject: The Oldest Light in the Universe Content-Type: text NASA Science News for February 11, 2003 A NASA satellite has taken a picture of the Big Bang's ancient afterglow. Scientists have analyzed the data and learned that the universe is 13.7 billon years old (plus or minus 1 percent)and that the first stars appeared only 200 million years after the Big Bang. These results are a milestone in cosmology, says the NASA director of astronomy and physics. FULL STORY at http://science.nasa.gov/headlines/y2003/11feb_map.htm?list13497 [...] ----- End of forwarded message from NASA Science News -----

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CMBEASY - C++ C_l spectrum code
by Boud Roukema 10 Feb '03

10 Feb '03

Witam, i haven't looked at this yet - if it's GPL it might be very interesting... http://de.arXiv.org/abs/astro-ph/0302138 http://www.cmbeasy.org boud

1 0

(fwd) MAP data release now Feb 11
by Andrzej Marecki 07 Feb '03

07 Feb '03

-- forwarded message -- Newsgroups: sci.astro.research Path: mat.uni.torun.pl!news.man.torun.pl!news.man.poznan.pl!news.supermedia.pl!news.nask.pl!newsfeed.gazeta.pl!newsfeed.tpinternet.pl!newsfeed01.sul.t-online.de!t-online.de!newsfeed.stueberl.de!logbridge.uoregon.edu!server3.netnews.ja.net!south.jnrs.ja.net!server2.netnews.ja.net!bath.ac.uk!unknown From: jgraber(a)mailaps.org (Jim Graber) Subject: MAP data release now Feb 11 Approved: sci.astro.research-request(a)slimy.greenend.org.uk (mjh) Sender: unknown(a)hercules.star.bris.ac.uk (Address not verified) Organization: http://groups.google.com/ Message-ID: <mt2.0-24947-1044533939(a)star.bris.ac.uk> X-Posting-Tool: modtool v2.0 Date: Thu, 6 Feb 2003 12:19:01 GMT Lines: 4 Xref: mat.uni.torun.pl sci.astro.research:2241 MAP website http://map.gsfc.nasa.gov/m_mm/ms_status.html now says "Tuesday February 11, 2:00 pm EST at NASA Headquarters". Coming soon. Jim Graber -- end of forwarded message -- -- ----------------------------------------------------------------------------- Andrzej Marecki | Torun Centre for Astronomy | e-mail: amr(a)astro.uni.torun.pl N. Copernicus University | WWW: http://www.astro.uni.torun.pl ul. Gagarina 11 | tel: +48 56 6113032 PL-87-100 Torun, POLAND | fax: +48 56 6113009 -----------------------------------------------------------------------------

1 0

(fwd) MAP data release NOT on 6 February!!!!!!
by Andrzej Marecki 06 Feb '03

06 Feb '03

-- forwarded message -- Newsgroups: sci.astro.research Path: mat.uni.torun.pl!news.man.torun.pl!news.man.poznan.pl!news-fra1.dfn.de!eusc.inter.net!mephistopheles.news.clara.net!news.clara.net!server3.netnews.ja.net!bath.ac.uk!unknown From: ebunn(a)lfa221051.richmond.edu Subject: MAP data release NOT on 6 February!!!!!! Approved: sci.astro.research-request(a)slimy.greenend.org.uk (mjh) Sender: unknown(a)hercules.star.bris.ac.uk (Address not verified) Organization: A poorly-installed InterNetNews site Message-ID: <mt2.0-22300-1044472201(a)star.bris.ac.uk> X-Posting-Tool: modtool v2.0 References: <mt2.0-27782-1042888051(a)star.bris.ac.uk> <mt2.0-15914-1043793431(a)star.bris.ac.uk> <mt2.0-5569-1043853434(a)star.bris.ac.uk> <mt2.0-668-1043871004(a)star.bris.ac.uk> Date: Wed, 5 Feb 2003 19:10:01 GMT Lines: 14 Xref: mat.uni.torun.pl sci.astro.research:2239 Note the change in the subject line. According to http://map.gsfc.nasa.gov/m_mm/ms_status.html the release is scheduled for "Early 2003." Rumor has it that it'll be delayed for only a week or two, because NASA is obviously preoccupied with other matters right now, but I don't know that for sure. -Ted -- [E-mail me at name(a)domain.edu, as opposed to name(a)machine.domain.edu.] -- end of forwarded message -- -- ----------------------------------------------------------------------------- Andrzej Marecki | Torun Centre for Astronomy | e-mail: amr(a)astro.uni.torun.pl N. Copernicus University | WWW: http://www.astro.uni.torun.pl ul. Gagarina 11 | tel: +48 56 6113032 PL-87-100 Torun, POLAND | fax: +48 56 6113009 -----------------------------------------------------------------------------

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habilitation
by boud 05 Feb '03

05 Feb '03

Witam, Any comments, negative, postive, or whatever on my habilitation thesis are welcome. The 6 articles are available on http://cdsads.u-strasbg.fr http://de.arXiv.org Cześć boud

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1st MAP data release
by Andrzej Marecki 28 Jan '03

28 Jan '03

Feb. 2003 First Data Release, Feb. 6, 1 pm EST. NASA Headquarters. A NASA Space Science Update press conference will release the initial findings of the full sky survey. see: http://map.gsfc.nasa.gov/m_mm/ms_status.html -- Andrzej

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RL/RQ quasar dichotomy
by Andrzej Marecki 28 Jan '03

28 Jan '03

Paper: astro-ph/0301526 From: Cirasuolo Michele <ciras(a)sissa.it> Date: Mon, 27 Jan 2003 09:52:07 GMT (391kb) Title: The Radio Loud / Radio Quiet dichotomy: news from the 2dF QSO Redshift Survey Authors: M. Cirasuolo, M. Magliocchetti, A. Celotti, L. Danese Comments: 11 pages, 14 figures, accepted by MNRAS [...] ----- End of forwarded message from send mail ONLY to astro-ph ----- This paper uses the modern surveys: FIRST and 2dF to show (or rather confirm): 1. SMBH mass is _not_ responsible for the radio loudness. 2. The alleged RL/RQ dichotomy is a selection effect - there is a continuum of possible levels of radio loudness. My 0.03 PLN: I will still like the term "radio-loud" for those AGN which occupy the particular part (side) of that radio loudness continuum. -- Andrzej

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grant appln revised: deadline wtorek 28.01 poludniu! more comments?
by boud 27 Jan '03

27 Jan '03

%% ==================================================================== %% This LaTeX file was created by AbiWord. %% AbiWord is a free, Open Source word processor. %% You may obtain more information about AbiWord at http://www.abisource.com %% ====================================================================== \documentclass[12pt]{article} \usepackage[T1]{fontenc} \usepackage{calc} %\usepackage{hyperref} \usepackage{setspace} \usepackage{multicol} \usepackage[normalem]{ulem} \usepackage{color} \setlength{\oddsidemargin}{0.984028in-1in} \setlength{\textwidth}{\paperwidth - 0.984028in-0.984028in} \setlength{\textheight}{23cm} %%%%%%%%%%%%%%%%%%% %%% personal definitions \newcommand\noin{\noindent} \def\pub #1;;#2;;#3;;#4;;#5 {#1. {\it#2, }{\ \it#3, } {\bf#4, }#5} % PUBLISHED REFERENCE-- #1 AUTHORSHIP, YEAR; #2 TITLE; #3 JOURNAL; % #4 VOLUME; #5 PAGE. \newcommand\revinvit{ %%{\\ \bf (invited review)} { } } %\def\apj{Ap.J.} %\def\mnras{MNRAS} \def\apj{Astrophysical Journal} \def\mnras{Monthly Notices of the Royal Astronomical Society} \def\AandA{Astronomy \& Astrophysics} \def\AASupp{Astronomy \& Astrophysics Supplement} \def\cqg{Classical and Quantum Gravity} \def\jaf{Journal des astronomes fran\c{c}ais} \def\asr{Advances in Space Research} \def\dans{ in } \newcommand\mdcitem[0]{\item } %%%%%%%%%%%%%%%%%%% \begin{document} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% %% budget %%%%%%%%% \begin howto do integer arithmetic with \usepackage{calc} %%%% %% %%% declare variable as a ``counter'' %%\newcounter{testvariable} %%\newcommand\testvariable{\arabic{testvariable}} %% %%% do arithmetic using constants and counters converted to commands %%\setcounter{testvariable}{31415} %% %%% to print its value %%\arabic{testvariable} %% %%% convert counter to command so that it can be used in arithmetic %%\renewcommand\testvariable{\arabic{testvariable}} %% %%% do arithmetic using constants and counters converted to commands %%\setcounter{testvariable}{(\testvariable + 31415)*10} %% %%% to print its value %%\arabic{testvariable} %% %%%%%%%%% \end howto do integer arithmetic with \usepackage{calc} %%%%% \newcounter{monthsone} \setcounter{monthsone}{12} \newcommand\monthsone{\arabic{monthsone}} \newcounter{monthstwo} \setcounter{monthstwo}{12} \newcommand\monthstwo{\arabic{monthstwo}} \newcounter{monthsthree} \setcounter{monthsthree}{12} \newcommand\monthsthree{\arabic{monthsthree}} \newcounter{monthstotal} \setcounter{monthstotal}{\monthsone+\monthstwo+\monthsthree} \newcommand\monthstotal{\arabic{monthstotal}} \newcounter{salrate} \setcounter{salrate}{11800} \newcommand\salrate{\arabic{salrate}} %\setcounter{x}{?} \renewcommand\x{\arabic{x}} \newcounter{x} \setcounter{x}{12} \newcommand\x{\arabic{x}} \newcounter{z} \setcounter{z}{12} \newcommand\z{\arabic{z}} \newcounter{w} \setcounter{w}{12} \newcommand\w{\arabic{w}} \newcounter{y} \setcounter{y}{12} \newcommand\y{\arabic{y}} %\setcounter{y}{?} \renewcommand\y{\arabic{y}} \newcounter{persontotal} \setcounter{persontotal}{12} \newcommand\persontotal{\arabic{dummy}} \setcounter{persontotal}{(100+67+(4*50))} \renewcommand\persontotal{\arabic{persontotal}} \newcounter{saltotalyear} \setcounter{saltotalyear}{(\salrate *\persontotal)/100} \newcommand\saltotalyear{\arabic{saltotalyear}} \newcounter{scsi} \setcounter{scsi}{5}%kPLN \newcommand\scsi{\arabic{scsi}} \newcounter{perso} \setcounter{perso}{7} %kPLN \newcommand\perso{\arabic{perso}} \newcounter{sober} \setcounter{sober}{700} \newcommand\sober{\arabic{sober}} \newcounter{portable} \setcounter{portable}{10} %kPLN \newcommand\portable{\arabic{portable}} \newcounter{equip} \setcounter{equip}{1000*(1+7+ \perso*3 + \scsi + \portable) + \sober} \newcommand\equip{\arabic{equip}} \newcounter{consultrate} \setcounter{consultrate}{5100} \newcommand\consultrate{\arabic{consultrate}} \newcounter{consultpm} % personmonths \setcounter{consultpm}{12} \newcommand\consultpm{\arabic{consultpm}} \newcounter{consult} \setcounter{consult}{\consultrate * \consultpm} \newcommand\consult{\arabic{consult}} \newcounter{confperyear} \setcounter{confperyear}{2} \newcommand\confperyear{\arabic{confperyear}} \newcounter{oneconfer} \setcounter{oneconfer}{6500*\confperyear} \newcommand\oneconfer{\arabic{oneconfer}} \newcounter{allconferyear} \setcounter{allconferyear}{(\oneconfer * \persontotal)/100} \newcommand\allconferyear{\arabic{allconferyear}} \newcounter{allconfer} \setcounter{allconfer}{\allconferyear * \monthstotal /12} \newcommand\allconfer{\arabic{allconfer}} \newcounter{subone} \setcounter{subone}{\saltotalyear + \equip + \consult/(\monthstotal/12) + \allconferyear} \newcommand\subone{\arabic{subone}} \newcounter{subtwo} \setcounter{subtwo}{\saltotalyear + 0 + \consult/(\monthstotal/12) + \allconferyear} \newcommand\subtwo{\arabic{subtwo}} \newcounter{subthree} \setcounter{subthree}{\saltotalyear + 0 + \consult/(\monthstotal/12) + \allconferyear} \newcommand\subthree{\arabic{subthree}} \newcounter{suball} \setcounter{suball}{\subone+\subtwo+\subthree} \newcommand\suball{\arabic{suball}} \newcounter{adminone} \setcounter{adminone}{\subone /4} \newcommand\adminone{\arabic{adminone}} \newcounter{admintwo} \setcounter{admintwo}{(\subtwo *3)/10} \newcommand\admintwo{\arabic{admintwo}} \newcounter{adminthree} \setcounter{adminthree}{(\subthree *3)/10} \newcommand\adminthree{\arabic{adminthree}} \newcounter{adminall} \setcounter{adminall}{\adminone+\admintwo+\adminthree} \newcommand\adminall{\arabic{adminall}} \newcounter{totalone} \setcounter{totalone}{\subone + \adminone} \newcommand\totalone{\arabic{totalone}} \newcounter{totaltwo} \setcounter{totaltwo}{\subtwo + \admintwo} \newcommand\totaltwo{\arabic{totaltwo}} \newcounter{totalthree} \setcounter{totalthree}{(\subthree + \adminthree} \newcommand\totalthree{\arabic{totalthree}} \newcounter{totalall} \setcounter{totalall}{\totalone+\totaltwo+\totalthree} \newcommand\totalall{\arabic{totalall}} \newcounter{grandtotal} \setcounter{grandtotal}{\totalall} \newcommand\grandtotal{\arabic{grandtotal}} \newcounter{dummy} \setcounter{dummy}{12} \newcommand\dummy{\arabic{dummy}} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{State Committee for Scientific Research -- KBN }{\footnotesize{}For KBN use only} \end{flushleft} \begin{flushleft} \textbf{00-529 Warszawa Nr.} \end{flushleft} \begin{flushleft} \textbf{ul. Wsp\'olna 1/3 Group} \end{flushleft} \begin{flushleft} \textbf{POLAND} \\ \end{flushleft} \begin{center} \textbf{GRANT APPLICATION} \end{center} \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{Project Title:} \centerline{\underline{Search for Topological Lensing}} \\ \centerline{\underline{of Radio-Loud Active Galactic Nuclei and Galaxy Clusters}} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{A. APPLICANT DATA} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} {\em 1. Name and address of the organization where work will be performed (include department, institute, laboratory, and chair, as applicable): } \end{flushleft} Toru\'n Centre for Astronomy, Nicolas Copernicus University, ul. Gagarina, 11, Toru\'n 87-100; director prof. hab. dr Andrzej Kus \begin{flushleft} {\em 2. Principal Investigator (include title, first name, last name): } \end{flushleft} dr Boudewijn Roukema \begin{flushleft} {\em 3. Principal Investigator's employer, if different from above organization (include department, institute, laboratory, and chair, as applicable): } \end{flushleft} (same as above) \begin{flushleft} \textbf{B. GENERAL DATA} \end{flushleft} \begin{flushleft} {\em 1. Funding period: } {\bf \monthstotal}..months (01.2004 -- 12.2006) \end{flushleft} \begin{flushleft} {\em 2. Number of personnel involved in the project:} {\bf 6} \end{flushleft} \begin{flushleft} {\em 3. Type of project (pick one):} \textbf{Individual Project} \end{flushleft} \begin{flushleft} {\em 4. Requested funding amount (in Polish z\l{}otys{\footnotesize{} Polish z\l{}oty annual 2002 mid - rate against the euro is estimated at 3,95 (Ministry of Finance - draft budget for the Year 2002)} - z\l{}):} \end{flushleft} \grandtotal~PLN \begin{flushleft} {\em 5. Keywords:} \end{flushleft} observational cosmology, cosmic topology, radio-loud active galactic nuclei, clusters of galaxies \clearpage \begin{flushleft} 6. \textbf{Project summary} (not to exceed 1 page; may be published by KBN if grant is awarded): \end{flushleft} \begin{centering} {\underline{Search for Topological Lensing of Radio-Loud Active Galactic Nuclei and Galaxy Clusters}} \end{centering} The Hilbert-Einstein equations are insufficient to describe the geometry of the Universe, as they only constrain a local geometrical property: curvature. A global knowledge of the geometry of space, if possible, would require measurement of the topology of the Universe. Since the subject was discussed in 1900 by Schwarzschild, observational attempts to measure global topology have been rare for most of this century, but have accelerated in the 1990's due to the rapidly increasing amount of observations of non-negligible fractions of the observational sphere. The basic physical test for measuring the topology of the Universe is simple from a na\"{\i}ve theoretical point of view: it is sufficient to see multiple images of extragalactic objects whose light travels to the observer via straight lines (geodesics) in different directions, or in other words that crosses the Universe from different directions or more than once. Hence, the term ``topological lensing'', since whatever theory might in the future explain the global shape of the Universe will presumably be an extension of general relativity, and just as general relativity is tested by gravitational lensing, where single objects such as high redshift galaxies are seen several times, the future theory (probably a theory of quantum gravity) should be constrained by topological lensing. In practice, just as the individual and statistical observational properties of extragalactic objects have made determination of local cosmological parameters (such as the matter density parameter, the cosmological constant and the Hubble constant) much more difficult than was hoped, their properties make the search for topological lensing difficult. The most promising objects at high redshifts for detecting topological lensing are those we can see in large numbers and across large volumes of space: (1) active galactic nuclei (AGNs) and (2) clusters of galaxies. In the Toru\'n Centre for Astronomy, we have a combination of \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \item existing observational expertise in radio-loud AGNs (RLAGNs) including the study of the evolution of RLAGNs (Marecki, Kunert, Gawro\'nski); and \item with the OCRA (One-cm Receiver Array) project, we hope to soon obtain a catalogue of thousands of clusters of galaxies at high redshifts via the Sunyaev-Zel'dovich Effect (Soberski); and \item the PI (Roukema) has developed observational strategies for investigating cosmic topology. \end{list} For this reason, we have an excellent opportunity at TCfA to excel in this field. Although our focus will be on the use of RLAGNs and clusters of galaxies, knowledge of cosmic microwave background (CMB) observational analyses will be crucial for independently checking any serious candidates for topological lensing. We are fortunate to have the presence in our group of an expert in CMB data, Bartosz Lew, who we expect to achieve the status of Magister during 2003. \clearpage \begin{flushleft} \textbf{C. STAFF INFORMATION} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} {\em For the Principal Investigator and each senior staff member, provide the following biographical information:} \end{flushleft} \begin{flushleft} 1. {\em Name} \end{flushleft} dr Boudewijn Roukema \begin{flushleft} 2. {\em Educational history including, for each degree, the field, institution, and date obtained} \end{flushleft} 1989-93: Doctor of Philosophy (Ph.D.) in Astronomy and Astrophysics, Mt Stromlo and Siding Spring Observatories (M.S.S.S.O.), Australian National University (A.N.U.), Canberra. 1985-88: Bachelor of Science (Hons), Australian National University, Canberra, Australia (awarded National Undergraduate Scholarship for this degree ) \begin{flushleft} 3. {\em Academic and professional appointments, in reverse chronological order} \end{flushleft} \noin since 2002: adiunkt, Toru\'n Centre for Astronomy, Uniwersytet Miko\l{}aja Kopernika, Toru\'n, Poland \noin 2001: visitor, DARC/LUTH (Laboratoire de l'Univers et ses Th\'eories), Observatoire de Meudon, France \noin 1998--2000: postdoctoral fellow, Inter-University Centre for Astronomy \& Astrophysics, Pune, India \noin Feb--July 1998: visitor, CAMK, Warszawa %\noin May-Sep 1997: Visitor, Institut d'Astrophysique % de Paris, CNRS, France %(R) %\noin April 1997: Visitor, Beijing %Astronomical Observatory, Beijing, P.R.China %(R) \noin 1996--1997: Centre of Excellence foreign visiting fellow, NAOJ, % ďźĺ˝çŤĺ¤Šćĺ°ďź Mitaka, Tokyo, %181, Japan %(R) %\smallskip \noin 1994--1995: postdoctoral research fellow, Astronomy Centre, University of Sussex, U.K. %(RT) %United Kingdom %\smallskip %\noin Aug/Sep 1994: Visitor, Dept of Astronomy, Bandung Institute of %Technology, Bandung, Indonesia %(T) %\smallskip \noin Jan/Feb 1994: visitor, Institute of Astronomy, University of Cambridge, United Kingdom %(R) %\smallskip \noin 1993: postdoctoral fellow, Institut d'Astrophysique de Paris, CNRS, France %(R) \begin{flushleft} 4. {\em Brief descriptions of research projects completed in the last four years, including up to 10 publications (provide publication data).} \end{flushleft} {Main Research Interests} (i) {\em Observational Cosmology} and (ii) {\em Galaxy Formation}: (i) Observational constraints on statistics of ``large scale'' structure, observational constraints on local cosmological parameters (such as the density parameter and the cosmological constant), and observational programmes to try to constrain global cosmological parameters; (ii) Merging-history-tree based galaxy formation models in a cosmological context and their comparison with observational galaxy statistics. \begin{list}{\arabic{enumi}}{\usecounter{enumi}} \item \pub \underline{Roukema, B.F.} \& Bajtlik, S., 1999;;Transverse Galaxy Velocities from Multiple Topological Images;;\mnras;;308;;309 \ (arXiv:astro-ph/9903038) %% CAMK, IAP, IUCAA %art \item \pub \underline{Roukema, B.F.}, 2000a;;COBE and Global Topology: An Example of the Application of the Circles Principle;;\mnras;;312;;712 \ (arXiv:astro-ph/9910272) %% IUCAA %ftp blacksci 15/10/99 %art \mdcitem %\item \pub \underline{Roukema, B.F.} \& Mamon, G.A., 2000;;Tangential Large Scale Structure as a Standard Ruler: Curvature Parameters from Quasars;;\AandA;;358;;395 \ (arXiv:astro-ph/9911413) %art %%395-408 %\item \mdcitem \pub \underline{Roukema, B.F.}, 2000b;;A Counterexample to Claimed COBE Constraints on Compact Toroidal Universe Models;;\cqg;;17;;3951 \ (arXiv:astro-ph/0007140) \item \pub \underline{Roukema, B.F.}, 2000c;;The Topology of the Universe;;Bulletin of the Astronomical Society of India;;28;;483 \ (arXiv:astro-ph/0010185) \revinvit \item \pub \underline{Roukema, B.F.} \& Mamon, G.A., 2001;;Lifting cosmic degeneracy within a single data set;;{\AandA};;366;;1 \ (arXiv:astro-ph/0010511) \item \pub \underline{Roukema, B.F.}, 2001b;;How to distinguish a nearly flat Universe from a flat Universe using the orientation independence of a standard ruler;;{\AandA};;369;;729 \ (arXiv:astro-ph/0102095) %art \item \pub \underline{Roukema, B.F.}, 2001d;;On the comoving distance as an arc-length in four dimensions;;{\mnras};;325;;138 \ (arXiv:astro-ph/0102099)%art \item \pub \underline{Roukema, B.F.}, Ninin, S., Devriendt, J., Bouchet, F.B., Guiderdoni, B., Mamon, G.A., 2001;;Star Formation Losses Due to Tidal Debris in `Hierarchical' Galaxy Formation;;\AandA;;373;;494 \ (arXiv:astro-ph/0105152) %art \item \pub \underline{Roukema, B.F.}, Mamon, G.A., \& Bajtlik, S., 2002;;The Cosmological Constant and Quintessence from a Correlation Function Comoving Fine Feature in the 2dF Quasar Redshift Survey;;{\AandA};;382;;397 \ (arXiv:astro-ph/0106135) \end{list} \begin{flushleft} 5. {\em Awards received} \end{flushleft} \begin{flushleft} 1. {\em Name} \end{flushleft} dr Andrzej Marecki \begin{flushleft} 2. {\em Educational history including, for each degree, the field, institution, and date obtained} \end{flushleft} 1980 MSc (astronomy) UMK, Toru\'n 1992 PhD (astronomy) UMK, Toru\'n \begin{flushleft} 3. {\em Academic and professional appointments, in reverse chronological order} \end{flushleft} since 1992 adiunkt, Centrum Astronomii, UMK, Toru\'n \begin{flushleft} 4. {\em Brief descriptions of research projects completed in the last four years, including up to 10 publications (provide publication data).} \end{flushleft} Brief description of research projects: Interfermetric observations of radio-loud AGN (RLAGN) aimed to reveal structures of compact i.e. {\it young} objects. Selection and observations (MERLIN, VLBI) of a new sample of faint compact objects. Measurements of the velocities of the components in such radio structures. \begin{list}{\arabic{enumi}}{\usecounter{enumi}} \item \underline{Marecki, A.}, Falcke H., Niezgoda J. Garrington, S.T., Patnaik A.R. (1999) "Gigahertz Peaked Spectrum sources from the Jodrell Bank-VLA Astrometric Survey" A\&AS 135, 273 \item Fanti, C. ... \underline{Marecki, A.}, et al. (2000) "ISO observations of a sample of CSS and GHz Peaked Spectrum radio galaxies", A\&A 358, 499 \item Browne, I. W. \underline{Marecki, A.}, et al. (2000) "OCRA: a one-centimeter receiver array" SPIE 4015, 299 \item \underline{Kunert, M.}, \underline{Marecki, A.} et al. (2002) "FIRST-based survey of Compact Steep Spectrum sources. I. MERLIN images of arc-second scale objects" A\&A 391, 47 \item \underline{Marecki, A.} et al. (2003) "Location of Weak CSS Sources on the Evolutionary Path of Radio-Loud AGN", PASA 20, in press (astro-ph/0211253) \item \underline{Marecki, A.} et al. (2003) "Weak CSS Sources from the FIRST Survey", PASA 20, in press (astro-ph/0211249) \item \underline{Marecki, A.} et al. (2003) "1245+676 - a CSO/GPS source being an extreme case of a double-double" PASA 20, in press (astro-ph/0209212) \end{list} \begin{flushleft} 5. {\em Awards received} \end{flushleft} \begin{flushleft} \textbf{D. PROJECT DESCRIPTION, METHODOLOGY, AND EXPECTED RESULTS} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \textbf{ }{\em What problem is being proposed and why? Why should this work be undertaken in Poland?} \end{flushleft} The problem being posed is to try to measure the shape of the Universe. This is important because the Universe is the object in which we live and it is of obvious scientific and cultural interest to be aware of the shape of the object in which we live. It should be undertaken here because we have a combination of present and developing observational expertise in radio-loud active galactic nuclei (RLAGNs) and clusters of galaxies via the Sunyaev-Zel'dovich Effect respectively, plus expertise in the development of observational strategies for measuring cosmic topology. Poland has obvious historical precedents in showing that the Earth is not the centre of the Universe, and that planets around other stars exist. It would clearly be good to continue the tradition on a much larger length scale (Gigaparsecs). \begin{flushleft} {\em What is the present state of knowledge in the field, and to what extent does this project verify it? How will the project advance discovery and understanding in its field or across fields? Is this a new or a continued problem? } \end{flushleft} It is clear that topological lensing on scales of a few hundred Megaparsecs is extremely unlikely. Attempted constraints on scales from 1 Gigaparsec (1$h^{-1}$Gpc) to the horizon diameter of about 20$h^{-1}$Gpc (comoving) are much weaker and generally very model dependent. This project will use RLAGNs and clusters of galaxies up to redshifts of about $z\sim2-3$ as tracers, covering a volume of about half the diameter of the observable Universe, i.e. about 10$h^{-1}$Gpc. It will advance discovery and understanding by using these tracers as realistically as possible given understanding of their evolution and properties. This problem dates back to the pre-relativistic era (Schwarzschild 1900), but has only been tackled non-trivially since the early 1990s. Work on this theme is still in the pioneering stage. \begin{flushleft} {\em What is the proposed methodology? How will it solve the problem? What equipment will be used? Does the applicant have the required equipment skills and access?} \end{flushleft} The methodology is to use a range of methods, from studies of individual objects to statistical studies of large catalogues, and to parametrise understanding of the properties of the tracers in order to make these methods as observationally correct and precise as possible. Just as the supernova type Ia method was only one among many methods proposed for measuring local cosmological parameters, but happened to be the most dramatically successful, it is impossible to predict beforehand which specific method for measuring topological lensing will first yield highly significant results. Although the TCfA 32m telescope will be used for part of the general understanding of RLAGNs and for the OCRA project, which should in the long term yield large numbers of high-redshift clusters of galaxies, use of existing public catalogues such as those available at the Centre de Donn\'ees astronomiques de Strasbourg (CDS) and the information processing analysis requires the use of computers and computer peripherals. We do have access to these telescopes and databases and have experience managing computer resources. \begin{flushleft} {\em What are the expected results of this project (``know-how'', patents, methods, equipment), and how will they be disseminated (publications, conference presentations, PhD theses)?} \end{flushleft} This is a {\bf research} project, not a {\bf development} project, and the required theory which goes beyond general relativity has not yet been developed, so while we would hope to detect topological lensing, the results cannot be predicted before they are found. Articles on the results will of course be published in refereed journals, presented at conferences, and professionals and non-professionals will be able to follow (and maybe participate) in the research on our web pages via the normal methods of internet culture such as publicly archived mailing lists and wiki pages. \begin{flushleft} \textbf{E.} \textbf{SOLICITED PROJECTS ONLY: DOES THE APPLICANT MEET THE CALL CRITERIA, PARTICULARLY THOSE CONCERNING INTERNATIONAL COOPERATION?} \end{flushleft} N/A \begin{flushleft} \textbf{F. PROJECT} \textbf{SCHEDULE} \textbf{- ANTICIPATED TASKS} \end{flushleft} \setcounter{x}{(\saltotalyear) /2} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *6} \renewcommand\y{\arabic{y}} \setcounter{z}{\consult /3} \renewcommand\z{\arabic{z}} \setcounter{w}{\y + \equip + \z*3 +\allconfer} \renewcommand\w{\arabic{w}} \usecounter{enumi} \begin{center} \begin{tabular}{clrr} \hline \\ No. & Name and description of task & \multicolumn{1}{c}{Expected} & Expected cost (z\l{}) \\ & & \multicolumn{1}{c}{completion} \\ & & \multicolumn{1}{c}{date (mm/yy)} \\ \\ \addtocounter{enumi}{1} \arabic{enumi} & parametric modelling of projection \\ & and evolution effects of multiple images & 6/2004 & \x~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & application to individual candidate pairs & 12/2004 & \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} % & purchase computer items & 12/2004 & \equip~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & international cosmology consultants & 12/2004 & \z~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & conferences, public relations & 12/2004 & \allconferyear~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & predictions of further images & 6/2005 & \x~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & statistical analysis of RLAGN catalogues & 12/2005 & \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & international cosmology consultants & 12/2005 & \z~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & conferences, public relations & 12/2005 & \allconferyear~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & statistical analysis of cluster catalogues, \\ & OCRA predictions & 6/2006& \x~PLN % \\ \addtocounter{enumi}{1} \arabic{enumi} & predictions of further images & 12/2006 & \x~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & international cosmology consultants & 12/2006 & \z~PLN \\ \addtocounter{enumi}{1} \arabic{enumi} & conferences, public relations & 12/2006 & \allconferyear~PLN % % \\ \hline Total & & & \w~PLN \\ \hline \end{tabular} \end{center} \smallskip \begin{flushleft} \textbf{G. PROPOSED BUDGET} \end{flushleft} \begin{center} \begin{spacing}{1.24} \setcounter{y}{\saltotalyear + \saltotalyear + \saltotalyear} \renewcommand\y{\arabic{y}} \setcounter{z}{\consult /3} \renewcommand\z{\arabic{z}} \begin{tabular}{lrrr|r} \hline No. Item & \multicolumn{3}{c}{Funds for each budget year (z\l{})} & Total \\ & 2004 & 2005 & 2006 \\ % {\bf 1} Direct costs, including: &&&& \\ {\footnotesize{}1/ }Salaries and benefits & \saltotalyear & \saltotalyear & \saltotalyear & \y~PLN \\ % % {\footnotesize{}2/} Equipment & \equip & & & \equip~PLN\\ % {\footnotesize{}3/} Other direct costs &&&&\\ % international cosmology consultants & \z &\z &\z & \consult~PLN \\ % conferences, public relations & \allconferyear &\allconferyear &\allconferyear & \allconfer~PLN \\ \hline % Subtotal: & \subone & \subtwo& \subthree & \suball~PLN \\ &&&&\\ \multicolumn{4}{l|}{{\bf 2} Indirect costs (admin costs to UMK - 25\% 1st yr; 30\% 2nd, 3rd yrs)} &\\ & \adminone & \admintwo & \adminthree & \adminall~PLN \\ \hline {\bf 3} Total costs (1+2) & \totalone &\totaltwo &\totalthree& \totalall~PLN \\ \hline \end{tabular} \end{spacing} \end{center} \begin{flushleft} \begin{spacing}{1.24} Details of direct cost items \end{spacing} \end{flushleft} \begin{flushleft} 1) {\em Salaries and benefits} \end{flushleft} \begin{flushleft} {\em Principal Investigator {\bf \monthstotal} person-months} \end{flushleft} Based on KBN guidelines, 100\% of \salrate{}PLN/annum for the principal investigator if dr., 75\% for other investigators if dr., 50\% of \salrate{}PLN/annum for other investigators if mgr. Hence: \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \setcounter{x}{\salrate *3} \renewcommand\x{\arabic{x}} \item dr Boudewijn Roukema \salrate{}PLN *3 = \x~PLN \end{list} \begin{flushleft} \setcounter{x}{(\monthstotal *(\persontotal-100))/100} \renewcommand\x{\arabic{x}} {\em Staff {\bf \x} person-months} \end{flushleft} \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \addtocounter{enumi}{1} \setcounter{x}{(\salrate *67)/100} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *3} \renewcommand\y{\arabic{y}} % \item dr Andrzej Marecki \x~PLN *3 = \y~PLN % \setcounter{x}{(\salrate *50)/100} \renewcommand\x{\arabic{x}} \setcounter{y}{\x *3} \renewcommand\y{\arabic{y}} % \item mgr Magdalena Kunert \x~PLN *3 = \y~PLN \item mgr Sebastian Soberski \x~PLN *3 = \y~PLN \item mgr Marcin Gawro\'nski \x~PLN *3 = \y~PLN \item (2003 mgr) Bartosz Lew \x~PLN *3 = \y~PLN \end{list} \setcounter{x}{(\salrate *(\monthstotal/12)*(\persontotal))/100} \renewcommand\x{\arabic{x}} Total: \x~PLN \smallskip \begin{flushleft} 2) {\em Equipment (type, estimated cost, planned month of purchase, and justification)} \end{flushleft} Justification: These computing facilities are needed for synthesis and analysis of empirical data, and for creating added value of the scientific products of the project (presenting and communicating results). Comparison of pairs of objects in a large catalogue is an $N^2$ operation, i.e. it is CPU intensive. It can be speeded up by making introducing prior assumptions. However, the history of astronomy shows that making reasonable, but wrong, assumptions often leads to missing a real signal, so having good CPU power would be an advantage to the project. Purchases are planned for 2004. \begin{list}{(\roman{enumi})}{\usecounter{enumi}} \item inkjet scanner/copier/printer + 3yrs insurance (loss/theft/etc.) (an inkjet PSC 750 costs 900PLN; recycled cartridges cost about 35~PLN B/W, 50~PLN colour) 1~kPLN \item colour laserwriter/scanner/copier + 3yrs insurance (loss/theft/etc.) 7~kPLN \item computer (Gawro\'nski) - AMD Athlon, 2GHz, 512Mb RAM, 100Gb hard disk, CD burner, ethernet card, 19'' screen + 3yrs insurance (loss/theft/etc.) \perso~kPLN \item computer (Lew) - AMD Athlon, 2GHz, 512Mb RAM, 100Gb hard disk, CD burner, ethernet card, 19'' screen + 3yrs insurance (loss/theft/etc.) \perso~kPLN \item computer (Kunert) - AMD Athlon, 2GHz, 512Mb RAM, 100Gb hard disk, CD burner, ethernet card, 19'' screen + 3yrs insurance (loss/theft/etc.) \perso~kPLN \item computer peripherals (Marecki) - 2 SCSI 73Gb disks + 3yrs insurance (loss/theft/etc.) \scsi~kPLN \item computer peripheral (Soberski) - CD burner 200~PLN, 512Mb RAM 500~PLN, total \sober~PLN \item portable computer (``notebook'') (available to all members of the group) + 3yrs insurance (loss/theft/etc.) \portable~kPLN \end{list} Total: \equip~PLN \smallskip \begin{flushleft} 3) {\em Other direct costs (type of expenditure, amount, and relation to project plan)} \end{flushleft} These relate to the project plan in that the project is internationally competitive research and so (1) international consultants are required for providing theoretical insights and observational strategies regarding the ways in which RLAGNs and clusters of galaxies can be used as candidate topologically lensed objects, and (2) we need to be able to present our results at international conferences and consult international experts at their home research institutes. \smallskip (1) The research environment for an internationally competitive research project requires consultations from international experts for periods of between 1 week and a few months. Three people each for one month, and four people each for a week, per year, yields a total of \consultpm{} person-months over the three-year period of the project. At a rate of \consultrate~PLN/month for international consultants in cosmology, we have Total: \consult~PLN \smallskip (2) In order to present our results at conferences and other public relations exercises, attendance at two international conferences per fractional person per year would be consistent with international standards. One conference: typical economy class flight costs ($3.5$~kPLN) $+$ 1 week's accommodation and per diem in Europe/US/Japan/Australia (2~kPLN) $+$ registration fees (1~kPLN) $\Rightarrow$ \oneconfer~kPLN. Hence, two conferences/year for a 100\% person are within the recommended spending limits. \setcounter{x}{\persontotal/100} \renewcommand\x{\arabic{x}} \setcounter{y}{\persontotal-100*(\persontotal/100)} \renewcommand\x{\arabic{x}} At a rate of \confperyear per effective person, and \x{}.\y{} effective people over 3 years, this implies: Total: \allconfer~PLN. \begin{flushleft} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \begin{tabular}{cccc} {\em Date} & \multicolumn{2}{c}{\em Grantee organization }& {\em Principal Investigator}; \\ & Kierownik: & Kwestor &dr Boudewijn Roukema \\ & Prorektor ds Nauki i Wsp\'o\l{}pracy&mgr Henryk Heldt & \\ & z Zagranic\c{a} \\ & prof dr. hab. Marek Zaidlewicz & \\ \\ \\ \\ \\ & Signature & Signature & Signature \end{tabular} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \end{flushleft} \begin{flushleft} \end{flushleft} \end{document}

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grant meeting Fri 24.01 @14:00
by Boud Roukema 24 Jan '03

24 Jan '03

Witam, people *not* on the grant proposal - please ignore this message! people *on* the grant proposal - i think most of us will be at Piwnice on Fri afternoon (24.01). Could we meet at 14:00 to discuss the proposal? i've updated it a bit since the previous version, i'll bring several copies to the meeting. You may wish to see advice from Kazik Stepień about making the application: http://www.astrouw.edu.pl/~kst/KBN.html though IMHO what's most important, apart from the overall guidelines of spending rules, is the committee of astronomers - they're the only ones who will really understand (or who *should* understand) what science we are asking funding for. It seems to me that Kazik is a bit worried about bureaucrats who want to have the price of every paper clip written on the proposal and who haven't got the faintest idea of what cosmology is about... Anyway, see you this afternoon - i need some sleep... boud

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grant proposal - first (incomplete!) draft
by boud 22 Jan '03

22 Jan '03

Witam, This is just the first draft, still quite incomplete of the grant application - sorry for being slow - we should meet and discuss the details by Friday or else very, very early next week, since it then has to be signed and sent by UMK admin to KBN... pozd boud

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(fwd) Re: MAP data release?
by Andrzej Marecki 22 Jan '03

22 Jan '03

-- forwarded message -- Newsgroups: sci.astro.research Path: mat.uni.torun.pl!news.man.torun.pl!news.man.poznan.pl!news.internetia.pl!newsfeed.gazeta.pl!newsfeed.tpinternet.pl!news.iesy.de!troll.iesy.de!news.uni-stuttgart.de!uni-erlangen.de!news-nue1.dfn.de!newsfeed.r-kom.de!newsfeed.stueberl.de!logbridge.uoregon.edu!server3.netnews.ja.net!south.jnrs.ja.net!server2.netnews.ja.net!bath.ac.uk!unknown From: ebunn(a)lfa221051.richmond.edu Subject: Re: MAP data release? Approved: sci.astro.research-request(a)slimy.greenend.org.uk (mjh) Sender: unknown(a)hercules.star.bris.ac.uk (Address not verified) Organization: A poorly-installed InterNetNews site Message-ID: <mt2.0-8392-1043086785(a)star.bris.ac.uk> X-Posting-Tool: modtool v2.0 References: <mt2.0-27782-1042888051(a)star.bris.ac.uk> Date: Mon, 20 Jan 2003 18:19:46 GMT Lines: 27 Xref: mat.uni.torun.pl sci.astro.research:2220 In article <mt2.0-27782-1042888051(a)star.bris.ac.uk>, Jim Graber <jgraber(a)mailaps.org> wrote: >I understand MAP is due to make its first major data release >this month. Last I heard, towards the very end of the month. I'm pretty sure that no exact date has been announced. >Does anyone know where and when this will be announced? Some combination of press release, papers on the astro-ph arXiv, and information at the MAP web page, http://map.gsfc.nasa.gov/index.html I expect. I'd also expect Ned Wright to mention it on his News of the Universe page, http://www.astro.ucla.edu/~wright/cosmolog.htm#News Someone (me, if no one else beats me to it) will surely post something to this group when the announcement comes. -Ted -- [E-mail me at name(a)domain.edu, as opposed to name(a)machine.domain.edu.] -- end of forwarded message -- -- ----------------------------------------------------------------------------- Andrzej Marecki | Torun Centre for Astronomy | e-mail: amr(a)astro.uni.torun.pl N. Copernicus University | WWW: http://www.astro.uni.torun.pl ul. Gagarina 11 | tel: +48 56 6113032 PL-87-100 Torun, POLAND | fax: +48 56 6113009 -----------------------------------------------------------------------------

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A healthy dose of scepticism or a humbug?
by Andrzej Marecki 09 Jan '03

09 Jan '03

Paper: astro-ph/0301137 From: Blanchard Alain <alain.blanchard(a)ast.obs-mip.fr> Date: Wed, 8 Jan 2003 17:45:24 GMT (138kb) Title: Cosmological Parameters: Fashion and Facts Authors: A. Blanchard (LAOMP, Toulouse) Abstract: [...] I would like to emphasize that some results are established beyond reasonable doubt, like the (nearly) flatness of the universe and the existence of a dark non-baryonic component of the Universe. But also that the evidence for a cosmological constant may not be as strong as needed to be considered as established beyond doubt. In this respect, I will argue that an Einstein-De Sitter universe might still be a viable option. Three global tests: 1) the evolution of the abundance of clusters with redshift 2) the baryon fraction measured in local clusters 3) apparent evolution of the baryon fraction with redshift might be consistent with a high matter density for the Universe in the range $0.6-1.$. I therefore conclude that the dominance of vacuum to the various density contributions to the Universe is presently an interesting and fascinating possibility, but it is still premature to consider it as an established scientific fact. ------- Andrzej

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None
by Andrzej Marecki 03 Jan '03

03 Jan '03

A reference if you want to know what the "right" values of those $%$&*# cosmo-parameters are. ;-) --- Paper: astro-ph/0301012 From: Lawrence M. Krauss <krauss(a)theory1.phys.cwru.edu> Date: Wed, 1 Jan 2003 17:13:44 GMT (360kb) Title: The State of the Universe: Cosmological Parameters 2002 Authors: Lawrence M. Krauss (Case Western Reserve University) --- Andrzej

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OCRA relatd paper
by Boud Roukema 19 Dec '02

19 Dec '02

Here's one paper by an OCRA colleague Richard Battye (Jodrell) + others on SZE constraints on local cosmological parameters: http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2002PhRvL..88w1301W boud

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AGN formation notes
by Boud Roukema 17 Dec '02

17 Dec '02

Hi Waldek, Sorry for taking more than a week to respond, now that you have a theme for your licencjat. Here's my first suggestion at the basic ideas and reading: http://adjani.astro.uni.torun.pl:9673/zwicky/GalaxyAGNFormation Please add to this, change it, and/or write the Polish version. If you prefer to write in \LaTex rather than on zwicky, tell me and I'll find out how you can upload files (e.g. postscript files) to zWicky - otherwise you could just send them as attachments to cosmo-torun at astro.uni.torun.pl when you want to show them to people for comments. pozdrawiam boud

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zwicky pages (so far)
by Boud Roukema 06 Nov '02

06 Nov '02

Cześć wszystkim, (1) How to write in latin-2 on emacs: (1a) With a fairly new emacs (e.g. 20.7 or later): - M-x set-language-environment latin-2 - M-x set-input-method latin-2-prefix (also C-x <ret> C-\) - then can toggle input method with: C-\ Examples: `a`e`l's'c'o`z'z'n ąęłśćóżźń to stop ' being used, use, e.g., a space: ' a -> 'a (1b) You can put the following in your ~/.emacs file (custom-set-variables ;; custom-set-variables was added by Custom -- don't edit or cut/paste it! ;; Your init file should contain only one such instance. '(case-fold-search t) '(current-language-environment "latin-2") '(default-input-method "latin-2-prefix")) (2) The zwicky pages at the moment have a verrrrrrrrrry long URL: http://adjani.astro.uni.torun.pl:9673/zwicky/ Please see Tomek (czosnek) or me to create an account. pozd boud

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Re: interesting cosmo CMB software?
by Michal Frackowiak 29 Oct '02

29 Oct '02

On Mon, 2002-10-28 at 19:42, Boud Roukema wrote: > What do people think of: > > http://arcturus.mit.edu/cosmics/ > It was the first free code for calculating density peturbations with an emphasis on CMB fluctuations. CMBFast is based on it. But it calculates perturbations in linear regime using full set (not full, but cut anyway) of Boltzmann equations - as opposed to some radical approximation by CMBFast. The inconsistency however is only about 1-2%, but required comp. power is MUCH bigger. In my oppinion there is no point in dealing with this soft - CMBFast is much faster and gives you practically the same accuracy. It also has more features e.g. grav. lensing, reionization. You would need a supercomputer to run COSMICS. And just a PC to run CMBFast. regards - michal

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phenomenological
by Boud Roukema 23 Oct '02

23 Oct '02

Hi I'm having an interesting (random) discussion with Sebastian, and pointed out some nice galaxy formation pages at the IAP: http://brunello.iap.fr/galics/GalICS/main_frames.html There's a useful word related to these: "phenomenological" Its meaning is somewhere in between "theoretical" and "observational", i.e. finding formulae which are reasonable from a theoretical point of view, but not directly justified, and which can be "fit" to observations. My guess is the constraints we have on Omega_m and Omega_Lambda could probably be described as phenomenological, since although they are very directly linked to GR, which definitely counts as theory, they're not (yet) linked into the rest of physics except by a range of "reasonable" hypotheses. The challenge is to get these solid observational and/or (preferably "and") theoretical support... pozd boud

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PROPOSALS su/web/TWiki/backup/quotas DEADLINE TUE 22 OCT 00:30
by Boud Roukema 14 Oct '02

14 Oct '02

Witam, The deadline passed and there were several useful comments, onlist and offlist - thanks everyone. Here are some updates and specific proposals. ########## PROPOSALS su/web/TWiki/backup/quotas V0.1 ################## ### deadline for comments/veto Tue 22 Oct 00:30 ### (1) superusers - There is now one staff member and one student who have been suggested and who have accepted, in principle, becoming superusers. I would be happy for both of them to be su, and think 3 people is sufficient. (Other people can become ordinary users, of course, and since there is plenty of scratch space, that's enough to develop experience in GNU/Linux, IMHO.) Anyone who wishes to know their names please contact me offlist. (2) web server - I've (tried to) install the default apache server of Deb3.0, and if noone objects, would like to put it online once the decision deadline passes. Are there any recommendations for firewalls etc, or good Deb /other linux links/hints for this? (3) (T)Wiki server for * cosmic topology page - complete references to all published articles (last time I counted, there were only 36 authors during the 20th century + 1 in the last year of the 19th century) * standard ruler page * meta-page for other cosmology stuff * galaxy/AGN formation/evolution pages If there are no objections, I'd like to try installing this quickly, since I think it's a key piece of software for working together efficiently. (4) backup strategy? Initial backup strategy: - daily hard disk backups (incremental) of /home - weekly hard disk backup (full) of /home + backup of same on to CDROM(s) (max 3 CDROMs since 2GB partition) (5) initial quotas: - 200MB per user on /home - 2GB per user on a /scratch disk (6) - mail server? For the moment seems safer *not* to run adjani as a mail server, and there's no obvious need anyway. So I propose to *not* run a mail server, at least for the moment. Any comments (or veto, if for a fundamental reason of what we are here for) on (1)-(6) welcome by the deadline. ##################################################################### ########## PROPOSAL for machine installation V0.02 ################## ### deadline passed ### > - Deb 3.0r0 or RedHat ? > I would like to install Debian 3.0r0, with the 2.4.18bf kernel > flavour. This includes software like SnapPea which is useful for ... There was one strong recommendation in favour of Deb 3.0r0 :) from Michał Frąckowiak. > - superusers - I think that Andrzej M and I should be superusers, but For security reasons, it's probably better to discuss this more offlist in terms of individual names. There was one objection to having a student or two as su, but the same person agreed that if it's someone we know and trust, who knows GNU/linux, it could be OK. Another opinion was in favour of having a student or two as su. See above for a specific proposal. > - name of machine (silk, sahni, liddle, peebles, novikov, levin?) Andrzej pointed out that the "dead astronomer" tradition is really just for the solaris machines. Michał F had a bunch of suggestions which show that we have different personal tastes ;), and was not enthusiastic for using the name of a dead (or live) cosmologist. But since this is a question of taste anyway, I finally chose "Adjani" after Isabelle Adjani :). > - partition suggestions (there are 2 disks each of 60Gb) Geniu and Michał H made several useful comments - thanks. > My idea of 650MB /home is that CDROM backups should be relatively easy. However, given that disks are so big today, should we create much more backed up home space? E.g. using hard disk backups on a daily basis + tape backups once a week? Or daily hard disk + up to 3 CDROMs once a week (I don't think I would have more patience than copying 3 CDROMS, even that would be pretty boring, done every week)? 3 CDROM => approx 2GB => 200MB for 10 users. Probably plenty for the next 12 months. See proposal above. In any case, the only decision required immediately is how big the partitions should be. And of course, there could be parts of a scratch disk which are linked with ln -s from the real /home in order to look like home disks so that users know/expect that they are backed up. ######################################################################

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PROPOSAL for longer term policy on new computer V0.01
by Boud Roukema 08 Oct '02

08 Oct '02

########## PROPOSAL for longer term policy V0.01 ######### ### no deadline for the moment ### - susers - boud + amr? + a student? - web server? - home space per user - h.m. MB? With 650MB on /home, and potentially a dozen people, that's only about 50MB each. This brings up the question of... - backup strategy? - scratch space? Probably not much to say here - except the question of whether the observers can use this for radio data while waiting for us to find other cosmo uses for this disk space. What sort of policy could be reasonable? - mail server? - (T)Wiki server for * cosmic topology page - complete references to all published articles (last time I counted, there were only 36 authors during the 20th century + 1 in the last year of the 19th century) * standard ruler page * meta-page for other cosmology stuff * galaxy/AGN formation/evolution pages - sympa vs mailman? Sympa running at the moment on "astro" is fine, but I'm just wondering... - other software? CMB stuff? specific packages? N-body stuff for galaxy formation? - standard CPU rules - more than 5 min => nice 19 - quotas for accounts and/or scratch space, decision-making on acc and/or scratch space? ######################################################################

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PROPOSAL for machine installation V0.01
by Boud Roukema 08 Oct '02

08 Oct '02

########## PROPOSAL for machine installation V0.01 ################## ### deadline Thu 10/10/02 19:00 (decisions a matter of taste, IMHO) ### - Deb 3.0r0 or RedHat ? I would like to install Debian 3.0r0, with the 2.4.18bf kernel flavour. This includes software like SnapPea which is useful for cosmic topology, and also gives the users (cosmologists) maximum control and freedom to manage the software. I don't imagine we could get easy consensus on Deb vs Redhat vs Mandrake (or other) ;), but please make any comments you feel like anyway. - superusers - I think that Andrzej M and I should be superusers, but at least one or two other people than me should also be su, e.g. a student or two. This is really a more serious and longer term decision, but if anyone wants to help install, now is the time to speak up, since I'm eager to get started... :) - name of machine (silk, sahni, liddle, peebles, novikov, levin?) In the tradition of TCfA, I guess we should pick the name of a famous astronomer. So for this machine, it should be a famous cosmologist. IMHO, it would be fun to name it after a *living* cosmologist, and preferably someone who's also a cool dude ;). Since this is a question of taste, I'm not sure how we should decide, and probably if I make an authoritarian decision, it would be reasonable since it won't really affect other people that much. But suggestions welcome :). At the moment the names I've thought of include: * liddle * silk * peebles * sahni * levin * padmanabhan * novikov - partition suggestions (there are 2 disks each of 60Gb) / 185MB /boot 15MB /tmp 150MB /home 650MB /usr 3GB /usr/local 2GB /var 1GB /var/mail 1GB /home2 2GB /scratch1 10GB /scratch[2-9] 10GB -> 80Gb /scratch10 20GB My idea of 650MB /home is that CDROM backups should be relatively easy. Any good ideas for partition? ######################################################################

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PROPOSAL for a decision-making method for new computer V0.01
by Boud Roukema 08 Oct '02

08 Oct '02

Witam wszystkim, A computer has been bought for the TCfA cosmology group! :) This is a big investment and I would like to try to apply modern management methods - specifically, consensus decision-making techniques - for deciding on how to use and run it, rather than just one or two people deciding. Please comment, criticise this proposal. (If you think it's fundamentally against what we are here for, you could argue to veto the proposal itself!) Next message: concrete proposals for the machine. boud ########## PROPOSAL for a decision-making method V0.01 ################## First, a reminder on the AIM of our group: * research and education-leading-to-research in observational cosmology * Second, background reading on what consensus is and why it's effective: flow chart: http://www.consensus.net/flowchart.html word description: http://www.consensus.net/ocac2.html Third, a simplified consensus method: DEFINITION: "anyone" is defined here as undergrad students, masters/PhD students, postdocs or faculty studying or teaching at TCfA/CAMK-Toru� in cosmology related fields. (I will put a proposal for "cafe+" type meetings on http://www.astro.uni.torun.pl/sympa/cosmo-spotka/2002-10/ soon...) PROPOSALS: WHO - anyone (the proposer) can make a proposal for use of the computer, but hopefully it should be someone willing to do the work once the decision is made! HOW - the proposal is made on the most appropriate mailing list, e.g. cosmo-torun HOW - anyone can make comments, constructive criticisms, to try to improve the proposal HOW - the proposer writes successive versions of the proposal based on the comments DECISION - after discussion seems to have converged, the proposer (or other moderator) sends an email to the same list with Subject: PROPOSAL <name of proposal> DEADLINE FOR COMMENTS/VETO <deadline>, where the deadline is X days after the date of the email. X = 2 if the decision is essentially a matter of taste X = 7 if the decision is more serious X = 1 if there is some unexpected really urgent decision to be made STEPPING ASIDE - anyone who is against the proposal, but accepts that his/her criticisms have been listened to and are not important enough for a veto, can "step aside", and these criticisms are added to the proposal. This way, others are aware of the (claimed) weak points. VETO - anyone can veto the decision, but only based on the aim of our group (see AIM: above), i.e. not for trivial reasons. He/she should explain the reason for the veto. #######################################################################

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Is DE related to CDM?
by Boud Roukema 01 Oct '02

01 Oct '02

Witam What if DE (dark energy) is not something from early universe physics but instead is directly related to the properties of the CDM (cold dark matter) particles as some sort of negative pressure? Two articles on this idea: http://de.arXiv.org/abs/astro-ph/0209584 Schwartz http://de.arXiv.org/abs/hep-ph/0209322 Gondolo \& Freese (Varun Sahni et al. had some ideas earlier - last 12-18 months - on how DE and non-baryonic DM could be the same thing, but I think it was just phenomenological. Though I'm not sure.) pozd boud

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Fwd: U Chi: Microwave Background Announcement (fwd)
by boud 26 Sep '02

26 Sep '02

CMB polarization discovered? Notice how the journalist manages to convert: "it's in line with theoretical predictions." into a much stronger statement: > verifies the theoretical framework that supports modern cosmological > theory. But i guess the DASI people will need to struggle to get as much media attention as MAP... i haven't followed the debate on CMB polarization, so i don't know how seriously a detection can constrain any models. Maybe Micha� F has done some reading on this...? pozdrawiam boud > ---------- Forwarded message ---------- > Date: Thu, 19 Sep 2002 16:26:58 -0400 (EDT) > From: David Spergel <dns@... > To: all(a)astro.Princeton.EDU > Subject: Fwd: U Chi: Microwave Background Announcement (fwd) ... >**This material was sent earlier under embargo to reporters and the >embargo having expired, is now sent to press officers.** > >THE FOLLOWING RELEASE WAS RECEIVED FROM THE UNIVERSITY OF CHICAGO, >IN ILLINOIS, AND IS FORWARDED FOR YOUR INFORMATION. (FORWARDING >DOES NOT IMPLY ENDORSEMENT BY THE AMERICAN ASTRONOMICAL SOCIETY.) >Steve Maran, American Astronomical Society > >September 19, 2002 >Contact: Steve Koppes >773-702-8366 >E-mail: s-koppes(a)uchicago.edu > >Discovery supports astronomers' >paradoxical views of the universe > >The universe really is as surprising as scientists have come to >suspect it is, according to a discovery that University of Chicago >astrophysicists will announce Thursday, Sept. 19, at the COSMO-02 >conference at Adler Planetarium and Astronomy Museum. The discovery, >which astrophysicists have pursued with increasingly sensitive >instruments for more than two decades, verifies the theoretical >framework that supports modern cosmological theory. > >Using a radio telescope called the Degree Angular Scale >Interferometer (DASI) at the National Science Foundation's >Amundsen-Scott South Pole Station, the Chicago scientists measured >the minute polarization of the cosmic microwave background, the >sky-pervading afterglow of the big bang. > >Most light is unpolarized, its many individual waves jumbled >together, each wave flickering up and down in a different plane as it >speeds toward Earth. Unpolarized light becomes polarized whenever it >is reflected or scattered. This is the principle behind polarizing >sunglasses that remove the glare from the hood of a car or the >surface of a pool. In both cases the sunglasses only permit waves >that tend to flicker up and down in the same plane to pass. > >The polarization of the cosmic microwave background was produced by >the scattering of cosmic light when it last interacted with matter, >nearly 14 billion years ago. If no polarization had been found, >astrophysicists would have to reject all their interpretations of the >remarkable data they have compiled in recent years, said John >Carlstrom, the S. Chandrasekhar Distinguished Service Professor in >Astronomy & Astrophysics at the University of Chicago. > >"Instead of stating that we think we really understand the origin and >evolution of the universe with high confidence, we would be saying >that we just don't know," said Carlstrom, who will announce the >discovery. "Polarization is predicted. It's been detected and it's in >line with theoretical predictions. We're stuck with this preposterous >universe." > >It's a universe in which ordinary matter, the stuff of which humans, >stars and galaxies are made, accounts for less than five percent of >the universe's total mass and energy. The vast majority of the >universe, meanwhile, is made of a mysterious force that astronomers >call "dark energy." This vague name reflects the fact that scientists >simply do not know what it is. They only know that it acts in >opposition to gravity, accelerating the expansion of the universe. > >In addition to the dark energy theory, cosmic inflation theory >improbably proposes that the universe underwent a gigantic growth >spurt in a fraction of a second just moments after the big bang. > >"This beautiful framework of contemporary cosmology has many things >in it we don't understand, but we believe in the framework," said >Clem Pryke, Assistant Professor in Astronomy & Astrophysics at the >University of Chicago and a member of the DASI team. "This new result >was a crucial test for the framework to pass." > >Carlstrom's other collaborators on the polarization discovery were >John Kovac and Erik Leitch, University of Chicago; and Nils Halverson >and Bill Holzapfel, University of California, Berkeley. > >The discovery follows in the wake of another important DASI finding. >Last year Carlstrom's team precisely measured temperature differences >in the cosmic microwave background, further supporting for the cosmic >inflation theory. > >The polarization signal is more than 10 times fainter than the >temperature differences that DASI detected earlier. DASI's first >discovery came after it collected data for 92 days from 32 spots in >the sky. But DASI needed to watch two spots in the sky for more than >200 days to detect the polarization. > >The discovery opens a new era in cosmic microwave background >experiments, said the Chicago astrophysicists. They predict that >increasingly sensitive detections of polarization will yield many >more discoveries. "It's going to triple the amount of information >that we get from the cosmic microwave background," said Kovac, a >Ph.D. student in Physics. "It's like going from the picture on a >black-and-white TV to color." > >The polarization is a signpost from when the universe was only >400,000 years old, when matter and energy were only just beginning to >separate from one another. "What's unique about polarization is that >it directly measures the dynamics in the early universe," Carlstrom >said. > >Temperature differences revealed patterns of lumpy matter frozen in >the early universe, but by measuring polarization, astronomers can >actually see how the early universe was moving. > >In the coming years, astronomers will attempt to use the CMB >polarization to measure gravity waves, a form of radiation predicted >by general relativity that corresponds to ripples in the fabric of >space-time, said Michael Turner, the Bruce and Diana Rauner >Distinguished Service Professor in Astronomy & Astrophysics at the >University of Chicago. > >"Detection of the polarization opens a new door to exploring the >earliest moments and answering the deep questions before us," Turner >said. > ### >sk/02-79 > >------------------------------------------------------------------ >IF YOU DO NOT WISH TO CONTINUE RECEIVING PRESS RELEASES THAT ARE >FORWARDED TO THE NEWS MEDIA VIA THE AMERICAN ASTRONOMICAL SOCIETY, >PLEASE REPLY ACCORDINGLY TO ANY INCOMING PRESS RELEASE, OR WRITE >TO hrsmaran(a)eclair.gsfc.nasa.gov. Requests for referrals to experts >should be sent to the same address.

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How the Universe got its Spots [if it has them]
by Boud Roukema 02 Sep '02

02 Sep '02

Cze�� cosmo-torun list, There was one positive comment and zero negative comments on my book proposition: http://www.astro.uni.torun.pl/sympa/cosmo-torun/2002-08/msg00003.html so i'll ask for this to be ordered. :) Cze�� Karolina, Could we please order the following cosmology book for the TCfA library? http://pup.princeton.edu/titles/7324.html > How the Universe Got Its Spots: > Diary of a Finite Time in a Finite Space > Janna Levin > Cloth | 2002 | $22.95 / ?15.95 | ISBN: 0-691-09657-0 > 224 pp. | 6 x 9 | 68 line illus. Thanks boud

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another cosmology book?
by Boud Roukema 19 Aug '02

19 Aug '02

Hi everyone, Sorry if the method of deciding and ordering library books on cosmology was a little confusing - I'm still learning about how things work here, so I take any blame which is due. A bunch of books has been ordered, and most have arrived, and Karolina and I will try to make up a list of these to help guide students and anyone else interested. Anyway, I just saw that a book has come out by one of the main people in observational cosmic topology work (Janna Levin): http://pup.princeton.edu/titles/7324.html > How the Universe Got Its Spots: > Diary of a Finite Time in a Finite Space > Janna Levin > Cloth | 2002 | $22.95 / ?15.95 | ISBN: 0-691-09657-0 > 224 pp. | 6 x 9 | 68 line illus. Why I think we should buy this: * The level of difficulty is for the common reader, but I think this should be a good motivational book, and good for bringing students up to "state-of-the-art" cosmology. * Also, most of the books we have say almost nothing on the global shape of the Universe. * There also seems to be a selection effect in the cosmology books we have so far: 50% of the population is unrepresented, and since the number of introductory cosmology books we have is something like a dozen or so, having zero introductory books by women is about 3-4 sigma inconsistent with unbiased selection. Could anyone with comments please provide them within a week or so? This way, there would be a chance of having the book not too long after students start in October-ish... Cze�� Boud

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wt/sr 20/21 sierpnia 14:00 sala budynku radio
by Boud Roukema 16 Aug '02

16 Aug '02

Cze�� wszystkim, Wprowadzenie do kosmlogii do studenci od Krak�w/Z.G�ra wtorek 20 sierpnia 14:00 �roda 21 sierpnia 14:00 wyk�adowca: boud (cosmo-torun(a)astro.uni.torun.pl) studenci: praktyki(a)astri.uni.torun.pl Witam wszystko! dla ostatnia informacja: http://www.astro.uni.torun.pl/sympa/cosmo-torun/

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strony kosmologii w TCfA
by Boud Roukema 09 Aug '02

09 Aug '02

Cze�� studenci z Krakowie/Zielona G�ra, Tu s� strony pracy kosmologia w TCfA: http://www.astro.uni.torun.pl/sympa/ Sugeruj� �e studenci prac*(a)astri.uni.torun.pl mog� tworzy� lista mejla z archiwem - tu jest przyk�ad archiw: http://www.astro.uni.torun.pl/sympa/cosmo-torun/2002-08/thrd1.html z *tej* mejlem, b�dzie: http://www.astro.uni.torun.pl/sympa/cosmo-torun/2002-08/msg00001.html - dla rozmawia� o jak uczy� si� o astronomia, gdzie s� dobre sajta internecie dla jak my�le�cie jest interesuj�cy w astronomia, itd... Mo�liwe Krzysztof G (chris@astri...) mo�e pomaga� z programem "mailman" (jest jaki program "sympa"). Je�li chcescie �e robi� wyk�ad o kosmologi�, prosz� organizowajcie si� dni i czas (np w drugie p�lowie miesi�c, ale jak chce�cie). Pracuj� w pokoju #36 w budynku radio-owy. pozdrawiam boud

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studenci Krakow/ZG
by Boud Roukema 08 Aug '02

08 Aug '02

Cze�� Krzysztof, The students from Krak�w/�.G�ra will only officially start in the radio group during the second two weeks of their visit, but since once of the best ways they can learn about astronomy research - including cosmology research - includes learning how to find and analyse observational data, and this includes them talking to each other in and writing "reports" on their ideas, i asked Andrzej Strobel if it could be possible if you could give these students computer accounts right now, and from the radio group, we could help straight away by providing them a mailing list using the "sympa" robot, which would archive all of their email messages automatically in html files, like these: http://www.astro.uni.torun.pl/sympa/ In fact, one or two of the students could be the list manager(s), this can work perfectly OK even if they only have accounts on astri machines. (I think...) I would be happy to spend some time with them getting them started, but you'd need to tell me/them what disk usage is possible/reasonable. They could of course use the mailing list for discussing spectroscopy to start off with, and then radio stuff / cosmology later... It's up to them to take the initiative. Pozdrawiam Boud PS: This message will (hopefully ;) be publicly archived here: http://www.astro.uni.torun.pl/sympa/cosmo-torun/2002-08/thrd1.html

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urlop 29/07 - 02/08
by Boud Roukema 27 Jul '02

27 Jul '02

Cze�� wszystkim, B�dzi� w urlopu 29/07 - 02/08, w Hajn�wce przez �ubr�w... Na ra�e Boud

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test with 'resurrected' asterix
by Andrzej Marecki 27 Jun '02

27 Jun '02

Is this list being correctly archived now? This is not a trivial question - asterix (the machine that keeps the archives) has got a new disk & operating system. If you can read this message at: http://www.astro.uni.torun.pl/sympa/cosmo-torun/2002-06/thrd1.html - the answer is "yes, everything is OK". -- Andrzej

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(fwd) Master Optical/Radio/Xray Catalogue (final version) now available on
by Andrzej Marecki 06 Jun '02

06 Jun '02

-- forwarded message -- Newsgroups: sci.astro.research Path: mat.uni.torun.pl!news.man.torun.pl!news.man.poznan.pl!news-fra1.dfn.de!news-lei1.dfn.de!newsfeed00.sul.t-online.de!newsfeed01.sul.t-online.de!t-online.de!newspeer1-gui.server.ntli.net!ntli.net!newspeer.clara.net!news.clara.net!server3.netnews.ja.net!bath.ac.uk!unknown From: eric(a)flesch.org (Eric Flesch ) Subject: Master Optical/Radio/Xray Catalogue (final version) now available on Approved: sci.astro.research-request(a)slimy.greenend.org.uk (mjh) Sender: unknown(a)scorpius.star.bris.ac.uk (Address not verified) Organization: Orcon Internet Message-ID: <mt2.0-4318-1023269017(a)star.bris.ac.uk> X-Posting-Tool: modtool v2.0 Date: Wed, 5 Jun 2002 09:23:20 GMT Lines: 55 Xref: mat.uni.torun.pl sci.astro.research:1433 Announcing the final version of the Master Catalogue of Radio/Xray Detections overlaid onto the Optical Background. This version is earmarked for the refereed process. Changes are as follows: Optical background: The APM catalogue has recently been completed to include the southern galactic cap, and these data have been added to the optical background of the Master catalogue (which merges APM & USNO). Thanks to Mike Irwin for the final push to complete the southern fields, and to Ray Stathakis for publishing that data on the AAO website. Radio detections: The FIRST and NVSS catalogues are found to have astrometry at least as good as the APM, so field shifts for these are restricted to corrections of the APM astrometry. Thanks to Rick White in clarifying issues involved in this. Detection of double radio lobes has been much improved in this version, and over 10,000 of these are displayed. These detections are reliable in this version, compared with an admittedly cursory effort last time. Xray detections: It is necessary to shift the ROSAT HRI, RASS, PSPC and WGA fields over the optical background to find the correct astrometry. The method has been improved now to clean up recalcitrant fields. Whilst never perfect, the bulk of xray fields have been aligned with good confidence. QSOs and AGN with optical APM/USNO signatures are included even if they do not have radio/xray associations. These include the SDSS early data release and there are about 30,000 in total. QSOs from old papers from the 70's and 80's are now correctly identified using improved likelihood algorithms. There are about 200 such objects, previously identified incorrectly, which are now assigned to the correct optical object. The Master Catalogue assigns probabilities to radio/xray objects that they are QSOs, galaxies, stars, or erroneous associations. This has been refined via a decision tree algorithm, as well as the complete APM data allowing better compensation against local sky densities. The probabilities are calculated against a 670,000,000 object whole-sky background database. Get the Master Catalogue at ftp://quasars.org/quasars . There is a ReadMe there and smaller subset catalogs. There will be some site cleanup as this catalog goes to publication, so get the subset catalogs now if you want them. This version of the Master Catalogue improves selection of about 15% of the objects compared with the previous version, but the highest-probability QSO candidates are mostly unchanged. The SUMSS southern sky radio catalog is due for release any day now, and I will update the Master Catalogue with that data when it is available. Eric Flesch Wellington, New Zealand 5 June 2002 -- end of forwarded message -- -- ----------------------------------------------------------------------------- Andrzej Marecki | Torun Centre for Astronomy | e-mail: amr(a)astro.uni.torun.pl N. Copernicus University | WWW: http://www.astro.uni.torun.pl ul. Gagarina 11 | tel: +48 56 6113032 PL-87-100 Torun, POLAND | fax: +48 56 6113009 -----------------------------------------------------------------------------

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Cosmic Background Imager
by Andrzej Marecki 05 Jun '02

05 Jun '02

The team of Cosmic Background Imager (CBI) released images with a resolution as good as 6 minutes of arc which allows to resolve blobs of matter with masses of about 5-80 x 10^14 solar masses i.e. corresponding to the mass of galaxy clusters. See: http://www.astro.caltech.edu/~tjp/CBI/ -- Andrzej

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proposition for masters students 2002/2003
by Boud Roukema 23 May '02

23 May '02

---------------------------------------------------------------------- Proposition for Supervising Masters (Magister) projects at TCfA for Oct 2002 - Sep 2003 Supervisor: B. Roukema Number of students: up to 3-4 students is possible Title: Observational Constraints on Cosmological Parameters Description: There are many possible projects which could be done as a master's thesis project, in using publicly available archival data from observational surveys to constrain one or more of the local or global cosmological parameters, either those related to shape (curvature, topology) or maybe also those unrelated to shape ("dark energy"). The precise projects would be chosen in discussion with the masters students during Oct-Nov 2002. Some examples would include further development and application of the "Dark Energy" software package which has been worked on during the "Shape of the Universe" monograph course: http://www.astro.uni.torun.pl/sympa/shape-univ/ Requirements: - basic knowledge in astronomy, physics, mathematics, computing skills - desire to measure something about the shape of the Universe - willingness both to learn from and to teach others interested in observational cosmology at TCfA - willingness to learn the following practical skills: touch-typing, emacs, \LaTeX, usage of the sympa mailing lists - willingness to participate in the "Shape of the Universe" monograph course and/or Bronek Rudak's semester 9 "Kosmologia" course: http://www.ncac.torun.pl/~bronek/KOS.html - nie ma problemu je�li student magisterowy nie (jeszcze) dobrze m�wi� po angielsku ----------------------------------------------------------------------

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XXI Texas Symposium - REGISTRATION NOW OPEN! (fwd)
by boud＠astro.uni.torun.pl 21 May '02

21 May '02

Hi everyone, I'm not that eager to go to an "expensive hotel chain" meeting, but if I miss the northern summer cosmo meetings then at least I could go to one big cosmo meeting this calendar year... Cze�� Boud > ---------- Forwarded message ---------- > Date: Mon, 20 May 2002 17:44:37 +0200 (CEST) > From: XXI Texas Symposium <texaflor(a)arcetri.astro.it> > Subject: XXI Texas Symposium - REGISTRATION NOW OPEN! > Texas in Tuscany XXI Symposium on Relativistic Astrophysics Florence, Italy, December 9-13, 2002 FIRST CIRCULAR (May 2002) Introduction The XXI Texas Symposium on Relativistic Astrophysics will be organized in Florence, 9-13 December 2002, by the National Institute of Astrophysics - Arcetri Astrophysical Observatory, in collaboration with the National Institute of Nuclear Physics and other scientific Institutions (the complete list will appear in a subsequent announcement). The meeting will be held in the Palazzo dei Congressi, in the historic center of the city, and will consist of Invited Review Talks (IT) in the morning (each lasting about 40 minutes) and Joint Discussions (JD) during the afternoon. Invited Talks will review recent developments in various fields in Astrophysics, Cosmology and related issues of Physics of Gravitation and Elementary Particles. Joint Discussions will cover specific areas with a number of shorter invited talks (about 20 minutes each). In addition, participants will be able to propose poster papers covering their recent research. The goal of the meeting is to provide a general review of the status and the prospects of research for a diversified audience of astrophysicists and physicists. How to reach Florence Florence can be reached directly by airplane from several major European cities. Alternative airports with international connections are Bologna or Pisa (both about 1 hour train ride from Florence). Another alternative is Rome (the train ride from the Rome Central Station Termini to Florence can be as short as 95 minutes) or Milan (the train ride from the Milan Central Station to Florence takes almost 3 hours). Please note, however, that both in Milan and in Rome the trip from the Airport to the Central Station will take about one additional hour. Accommodation The Organizers have selected a travel agency in Florence to handle all the problems connected with accommodation. The Organizers will not be able to help in any other way with this matter. Block reservations in various hotels are being made, which will be assigned on a first-come-first-served basis until November 15, 2002. Participants who want to arrange directly their own accommodation, or to contact a different travel agency are of course free to do so; they are however advised to book their accommodation as soon as possible, given the strong touristic pressure on Florence. Booking will be firm after a deposit equal to the cost of the first night in the chosen hotel. The quoted costs include breakfast, and all applicable taxes. The deposit will be acknowledged in the final bill, to be paid by the participant directly at the hotel upon leaving. Participants who want to leave earlier than initially arranged must notify the hotel at least 24 hours in advance. Cancellations will be possible only until November 15, 2002; in these cases the deposit will be returned less a 30% handling fee. The accommodation form is now available at http://www.arcetri.astro.it/~texaflor/accommodation_first.html Registration The registration fee for the Symposium will be 300 Euros if paid by November 1 and 400 Euros thereafter. This will cover participation, coffee breaks and a personal copy of the Proceedings. The registration form is now available at http://www.arcetri.astro.it/~texaflor/registration_first.html Program The following topics will be covered by Invited Talks and (in some cases) additional Joint Discussions: - PHYSICS AROUND THE BIG BANG - THE DEVELOPMENT OF THE EARLY UNIVERSE - COSMOLOGICAL PARAMETERS - THE DAWN OF LIGHT IN THE UNIVERSE - COSMOLOGICAL BACKGROUND - DARK MATTER AND GRAVITATIONAL LENSES - LARGE SCALE STRUCTURES AND CLUSTERS OF GALAXIES - GAMMA RAY BURSTS - ACTIVE GALACTIC NUCLEI - SUPERNOVAE, REMNANTS AND COLLAPSED STARS - BLACK HOLES - GRAVITATIONAL WAVES - COSMIC-RAY AND GAMMA-RAY ASTRONOMY - NEUTRINO PHYSICS AND ASTRONOMY Invited speakers A partial list of invited speakers includes: R. Blandford, C. Cesarsky, A. Fabian, F. Halzen, A. Lasenby, B. Leibundgut, P. Madau, I. Novikov, B. Schutz, P. Steinhardt, V. Trimble, G. Veneziano, M. Vietri, S. White. The program with the complete list of speakers and convenors of the Joint Discussions will appear on the web at http://www.arcetri.astro.it/~texaflor/program.html. The Proceedings of the Symposium will include the invited reviews and the presentations at the joint discussions (no posters). Scientific Organizing Committee F. Pacini (Chair, Italy), M. Baldo Ceolin (Italy), M. Rees (UK), R. Barbieri (Italy), V. Rubin (USA), C. Cesarsky (ESO), G. Setti (Italy), A. Gimenez (ESA), J. Silk (UK), G. Hasinger (Germany), M. Tavani (Italy), R. Kolb (USA), Y. Totsuka (Japan), R. Manchester (Australia), V. Trimble (USA), I. Novikov (Denmark), G. Veneziano (CERN), A. Olinto (USA), L. Woltjer (France) Local Organizing Committee M. Salvati (Chair), R. Bandiera, L. Falai, R. Maiolino, F. Mannucci, A. Marconi, E. Masini, N. Nagar. Further information: http://www.arcetri.astro.it/~texaflor/ e-mail: texas_florence(a)arcetri.astro.it fax ++ 39 055 220039

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astro-ph/0205155 another step in cosmo-topology...
by Boud Roukema 13 May '02

13 May '02

Cze�� wszystkim, An interesting paper by Rocha et al., a European collaboration (including Krzyszek G�rski) on COBE analysis of equal-side-length torus models of the Universe: http://de.arXiv.org/abs/astro-ph/0205155 They use the word "asymmetric" to talk about the possibility that the side lengths might be unequal. Given the absence of any serious physical theory for the global shape of the Universe, it seems best, IMHO, to keep all options open... Pozd, Boud

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Paddy+Tirth: DE & DMatter same thing?
by Boud Roukema 09 May '02

09 May '02

Paddy and his PhD student Tirth have come up with an idea for how dark matter and dark energy could just be two components of the same thing: http://de.arXiv.org/abs/hep-th/0205055 Cool! :)

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Dimming Supernovae by Axions
by Andrzej Marecki 08 May '02

08 May '02

Yet another "non-orthodox" view on SN dimming attributed to the expansion of the Universe: http://t8web.lanl.gov/people/terning/axion.html (This is based on a paper accepted by Physical Review Letters 88 (2002), 161302.) -- Andrzej

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ASTROVIRTEL: Third Call for Proposals (fwd)
by boud 13 Apr '02

13 Apr '02

I don't think we're ready for this yet, but feel free to think about this. If anyone can think of a project, go ahead and write your thoughts to the list - be creative! And don't worry about your ideas being crazy. Starting off from a crazy idea and playing with it can often yield a good idea... Which is better than no ideas at all... > ---------- Forwarded message ---------- > Date: Fri, 12 Apr 2002 12:26:20 +0200 (MET DST) > From: AstroVirtel User <astrov at eso.org> > To: boud.roukema@... > X-SBFolder: Default > X-SBClass: OK > Subject: ASTROVIRTEL: Third Call for Proposals > > > Dear Colleague, > > The ASTROVIRTEL Project, supported by the European Commission > and managed by the ST-ECF on behalf of ESA and ESO, is aimed > at enhancing the scientific return of the ST-ECF/ESO Archive. > It offers the possibility to European Users to exploit it as > a virtual telescope, retrieving and analysing large quantities > of data with the assistance of archive operators and scientific > personnel. The first two cycles of operation of the ASTROVIRTEL > project are almost completed and some interesting results > have already been achieved and published > [see http://www.stecf.org/astrovirtel/publications.html] > > We are now announcing the Third Call for ASTROVIRTEL Proposals. > Detailed instructions for the submission of proposals can be found > at http://www.stecf.org/astrovirtel/. > > The deadline for submission is June 17th, 2002. > > ASTROVIRTEL is an initiative financed by the European Commission under > the scheme "Enhanced Access to Large Infrastructures" and therefore is > open to European scientists from EC Member and Associated States > [for a list of these states, see > http://www.stecf.org/astrovirtel/ECStates.html]. > > Do not hesitate to contact us if you need further information. The > ASTROVIRTEL email address is astrovirtel(a)eso.org . > > Best regards, > > Piero Benvenuti, Head / ST-ECF > Peter Quinn, Head / DMD > > PS: Since we merged different mailing lists, it might happen that > you receive this email twice. Our apologies. > > -- > ASTROVIRTEL > > Accessing Astronomical Archives as Virtual Telescopes > A Project supported by the European Commission > Access to Research Infrastructures > Action of the Improving Human Potential Programme > > Tel: +49 89 32006291 Fax: +49 89 32006480 > mailto:astrovirtel@eso.org URL: http://www.stecf.org/astrovirtel/

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Another confirmation of the existence of dark energy.
by Andrzej Marecki 12 Apr '02

12 Apr '02

----- Forwarded message from NewsAlert ----- NEWSALERT: Friday, March 22, 2002 @ 1504 GMT --------------------------------------------------------------------- The latest news from Astronomy Now and Spaceflight Now [...] NEW EVIDENCE: EXPANSION OF UNIVERSE IS ACCELERATING --------------------------------------------------- A team of UK and Australian astronomers has discovered new, independent evidence that the expansion of the universe is accelerating. Their findings have just appeared in the Monthly Notices of the Royal Astronomical Society. A team of 27 astronomers led by Professor George Efstathiou of the University of Cambridge has published strong evidence for the existence of dark energy using an entirely different technique. Their results show that the universe is full of dark energy, completely consistent with the earlier supernovae results. "Dark energy appears to exist and to dominate over more conventional types of matter" says Professor Efstathiou. "An explanation of the dark energy may involve String Theory, extra dimensions or even what happened before the Big Bang. At present nobody knows. The ball is now firmly in the theorists court." http://spaceflightnow.com/news/n0203/22expansion/ [...] ----- End of forwarded message from NewsAlert ----- -- Andrzej Marecki

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2 observation-linked galaxy projects (long term)
by Boud Roukema 03 Apr '02

03 Apr '02

Hi. I'm just sending this message to have it conveniently on the archive with an obvious "Subject:" header. I think I've already mentioned these two projects (or themes) which are linked to local observational facilities: (1) polarisation of radio-galaxies Ryszard Wielebi�ski of Bonn suggested that a good way to use the radio telescope here would be to observe galaxies at different frequencies, so with different amounts of Faraday rotation of polarised light, so that the polarisation could be inferred. (2) galaxy formation modelling in preparation for future infrared satellite data Ryszard Szczerba said something about NCAC being involved in an infrared satellite project (I think I got the name wrong - Ryszard, do you have a link to the web site of the project?), so if someone does some galaxy formation work in preparation for this, there would be a good chance of getting good observational constraints, and maybe even falsifying some models, and having to generate new ones, which is the exciting part of science :). Cze�� Boud Ryszard: this email will be archived on http://www.astro.uni.torun.pl/sympa/cosmo-torun/ Please reply directly to the list (unless you have something secret to say).

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OCRA - mass function of haloes
by Boud Roukema 29 Mar '02

29 Mar '02

Hi everyone, Inoue & Nagashima have a paper http://de.arXiv.org/abs/astro-ph/0110503 about the mass function of dark matter haloes, in other words, the frequency of how many objects of different masses (high or low) form at a given epoch during the collapse of matter due to gravity. I think this could be an important paper for modelling what statistical constraints on Omega_m & Omega_Lambda (or eventually w_Q) could be obtained from OCRA. Boud

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European Pdoc? (M Curie-Skl)
by Boud Roukema 21 Mar '02

21 Mar '02

Questionnaire for research institutions in Poland interested to host Marie Curie-Sk�odowska postdoctoral fellowships to be sent to ph3(a)npk.gov.pl Institution: Uniwersytet Mikolaja Kopernika Institute: Toru� Centre for Astronomy Address: ul. Gagarina, 11, PL-87-100, Toru� Homepage: http://www.astro.uni.torun.pl/sympa/ Contact person: Dr Boud Roukema Phone/fax: +48 56 611 3039/+48 56 611 3009 Email: boud(a)astro.uni.torun.pl Research field: observational cosmology Working languages: English, French, Polish Description of research topic/subject: The postdoctoral fellow would be expected to carry out original, independent research in any field of observational cosmology, and to stimulate discussion of observational cosmology among faculty and students. Fields presently being developed or likely to be developed at the Toru� Centre for Astronomy include constraints on local cosmological parameters such as the matter density parameter, the cosmological constant and the effective quintessence parameter, using public archival data; attempts to measure global parameters via topological lensing, using radio-loud AGNs, clusters and the cosmic microwave background; and galaxy formation and evolution. Candidates in other fields of observational cosmology are welcome to apply: excellence and originality of research will be the primary criteria for making a selection. >>>>>>>>>>>>>>>> cut here <<<<<<<<<<<<<<<<<<<<<<<<<<<<<<< [Comment to cosmo-torun group: This is an administrative request to see if we can get some money for a European postdoc. Andrzej M, Andrzej K and I thought it best to keep the subject open to any theme in observational cosmology. I think we have till Monday before Wydzia� Fizyka meets to discuss the proposals, so please make any comments, criticisms, complaints, suggestions quickly!]

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Wiesci Jodrell Bank
by Marcin Gawronski 11 Mar '02

11 Mar '02

Hello .. Przyjade na Wielkanoc do Polski i bede przez pewien czas w Toruniu. W zwiazku z tym chcialbym Wam opowiedziec o mojej pracy w Jodrell, ktora dotyczy ewolucji kosmologicznej AGN'ow. Chcialbym przedstawic swoje pierwsze wyniki i omowic obecne problemy w tym temacie. Udalo mi sie tez zbudowac model nieba radiowego na czestosci 30 GHz, czyli to co powinnismy widziec za pomoca OCRY. W Toruniu bede obecny przez tydzien tuz przed Swietami.. cheers MPG

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Conference Announcement (fwd)
by Boud Roukema 08 Mar '02

08 Mar '02

An important topic! ---------- Forwarded message ---------- > Date: Thu, 07 Mar 2002 19:01:49 -0500 (EST) > From: Thomas Reiprich <thr4f(a)virginia.edu> > To: "Conference, Cooling Flows": ; > Subject: Conference Announcement Dear colleague, March 5, 2002 this is the First Announcement of the Conference on ******************************************************************** * * * The Riddle of Cooling Flows in Galaxies and Clusters of Galaxies * * * * which will take place at the * * * * Omni Hotel, Charlottesville, VA, USA * * from May 31 through June 4, 2003 * * * ******************************************************************** Note that future announcements will ONLY be sent to people who pre-registered through http://www.astro.virginia.edu/coolflow/preg.php Recent observations have significantly broadened our view on cooling flows in galaxies and clusters of galaxies. The wealth of new information through observations has led to a flourishing development in theoretical modelling. The purpose of this conference is to summarize relevant observational results at all wavelengths, to compare the predictions of models and simulations to these observations, and to assess the impact of processes in cluster cores on the application of galaxy clusters as cosmological probes. All further relevant information has been posted at the conference web page ******************************************* * http://www.astro.virginia.edu/coolflow/ * ******************************************* If you are potentially interested please take a short moment to fill in the pre-registration form to ensure receiving future announcements. We apologize if you received this Announcement more than once. This Announcement was originally sent on March 5 but due to a mailing problem a very large fraction of the recipients did not receive this mail. Sincerely, Thomas Reiprich If you don't have access to the WWW you may contact Thomas Reiprich by phone: +1-434-924-4904, fax: +1-434-924-3104, or snail mail: Department of Astronomy University of Virginia PO Box 3818 530 McCormick Road Charlottesville, VA 22903-0818 USA -- You can find my address at: http://www.reiprich.net/

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cosmo TCfA mailing lists - Witamy!
by Boud Roukema 19 Feb '02

19 Feb '02

Dear Anna, Magdalena, Nazywam si� Boud Roukema. I am about to start a job at TCfA to help organise a cosmology/extragalactic research group. Sebastian just told me that you are TCfA PhD students spending some time in JBO. To help organise discussion about research projects and techniques among us, Andrzej Marecki and I have started to create some email discussion lists, which are archived on the web. If you look at the pages: http://www.astro.uni.torun.pl/sympa/ you'll see that there are several lists which might interest you. Since you are at JBO on a long time scale, probably the cosmo-torun list would be the one most useful for you right now - but, of course, you're free to subscribe to any of the lists. The list cosmo-pl would probably interest you too - for the moment there are no messages - it will evolve depending on how people want it to evolve! (I m�j po polsku nie jeszcze jest wystarczy dobry dla dobrze dyskutowa� w tej listy mejla...) So I've subscribed you both to cosmo-torun and cosmo-pl (using your astro.torun addresses - you can still send mail to the lists from a JBO address, but it requires an authentification key to avoid spam). Of course you may unsubscribe if you think there are too many uninteresting messages... A very useful function is the archive - but since research ideas may be discussed *before* they are published, there is (moderately) limited access to the http://www.astro.uni.torun.pl/sympa/cosmo-torun/ archive. If you two and Motylek could tell me or Andrzej M (on-list or off-list) the IP numbers of computer(s) at JBO you are likely to use to access the site, then we would open up access to these IP #s. (The other existing lists have unrestricted access.) Pozdrawiam Boud

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Re: favoured topology of Universe candidates
by Boud Roukema 14 Feb '02

14 Feb '02

Hi again Ken & Ali, On Thu, 14 Feb 2002 Kengrimes123(a)aol.com wrote: > Thanks for that. We were rather shamefully going for the following 'quick > fix.' What do you think: The problem is that a spherical or hyperbolic, small universe would be just as exciting as a flat, small universe. The former might be more difficult to imagine, and there's more chance that Cornish et al would make errors or miss the real signal or take longer to find the result for a spherical or hyperbolic small universe than for a small, flat universe, but to me that's a secondary issue. (Using the circles principle in the most general way, the infinities of possibilities are not a problem for detection, however paradoxical that might seem!) Nevertheless, if what you really want to say is that a flat, small universe is in some ways "nicer" or "simpler" than a spherical or hyperbolic, small universe, then that is valid (and certainly defendable), but should probably be worded a bit more carefully. It would not really be that much more "hidden" from the measurement point of view, it would be more hidden simply because it's more complicated. I think the following is correct, clear and probably close to what you want to say: Replace: > 'So the universe may indeed be finite and bounded, and yet too vast to yield > to us the secret of its shape. Alternatively, the universe may possess > spherical or hyperbolic curvature, and so hide its secret shape among > limitless possibilities. Such thoughts are met with quiet stoicism by the > new wave of cosmologists: "The universe is however it is," Roukema > acknowledges, "Not how I would like it to be." by % 'So the universe may indeed be finite, bounded and flat, % and yet too vast to yield % to us the secret of its shape. Alternatively, the universe may be % small but possess % spherical or hyperbolic curvature, and so hide its secret shape among % limitless possibilities difficult for ordinary mortals to imagine % and challenging for professional % cosmologists to extract from the MAP data. Such thoughts ... And then the 2nd paragraph is fine unchanged: > But there remains the tantalising third possibility - that the universe is > relatively small, and possesses flat curvature. In that case, within a few > months of reading this article, we might well know whether Homer's donut is > truly the shape of things to come.' Cheers Boud

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Re: favoured topology of Universe candidates
by Boud Roukema 14 Feb '02

14 Feb '02

Hi again Ken & Ali, On Thu, 14 Feb 2002 Kengrimes123(a)aol.com wrote: > Thanks once again for the prompt feedback, which we would like to say was a > model in how to suggest quick and concrete improvements (if only more > contributors could do that!) We have gone for the simple expedient of > incorporating all of them. Great! Well, I've stoically ;-) learnt that careful, precise criticism tends to yield better results than general rants! > Please find below our proposed ending (featuring once more your good self - > and if you don't like the phrase 'quiet stoicism' we can go for 'cheerful > resignation' instead). We'd be very grateful if you could check this quickly, > as I think it probably repeats the 'howler' you picked out in your Point 5: > ' ... "If the universe is relatively large compared to its age,' > Levin observes, "I.e if it is significantly bigger than about 15 > billion light years across, then light from our ghost images will > not have time to reach us before the death of this planet." OK. > So the universe may indeed be finite and bounded, and yet too vast to yield > to us the secret of its shape. OK. > Alternatively, the universe may possess > hyperbolic curvature, and so hide its secret shape among limitless > possibilities. Hmm. Even though there are limitless possibilities for both the spherical and hyperbolic cases, as far as analysis of MAP data is concerned, the difference between them and the flat cases is "just" a question of calculation techniques and computer speeds. ("just" means a lot of hard work...) As you said in your article, Cornish et al. will calculate the easier cases first, simply because they're easier. The "limitless" or difficult classification of hyperbolic spaces just means it's much harder to analyse the data - the matched circles principle of Cornish, Spergel & Starkman is still perfectly valid. Just a reminder: the smallest "size" of the Universe could be: i) smaller than the horizon size (distance to last scattering surface) ii) about the same as the horizon (still maybe detectable) iii) much bigger than the horizon iv) infinite (There are in fact several "sizes" of the Universe which could be defined, the smallest one is the smallest distance between two images of the same object.) the curvature of the Universe can be: a) "slightly" spherical (like the Earth is "slightly" spherical) b) flat c) "slightly" hyperbolic There *is* some link between the two, [ a) => maximum size of Universe; b) => minimum size of Universe] but I think it's too subtle to include in your article, certainly too subtle for a conclusion. I think probably the closest correct thing to what you want to say is to compare the three possibilities: i) + ii) (put together) iii) iv) ---------------------------------------------------------------------- So here's my suggestion, to replace: > Alternatively, the universe may possess > hyperbolic curvature, and so hide its secret shape among limitless > possibilities. by % Alternatively, the universe may really be infinite and unbounded, % leaving us without the merest hope of being able to distinguish % between the two cases. ---------------------------------------------------------------------- > Such thoughts are met with quiet stoicism by the new wave of > cosmologists: "The universe is however it is," Roukema acknowledges, > "Not how I would like it to be." "quiet stoicism" and your quote are fine. :-) ---------------------------------------------------------------------- > But there remains the tantalising third possibility - that the universe is > neither vast nor hyperbolic. In that case, within a few months of reading To match the above correction: % neither vast nor infinite. In that case, within a few months of reading ---------------------------------------------------------------------- > this article, we might well know whether Homer's donut is truly the shape of > things to come.' Cheers Boud

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MAP time scale, courtesy Ken & Ali
by Boud Roukema 14 Feb '02

14 Feb '02

Dear friends, For copyright reasons I probably shouldn't post Ken & Ali's full article here, but here are a couple of paragraphs which are pretty important: > But how can we spot these circles? From 1989-93, NASA's Cosmic > Background Explorer (COBE) mapped the microwave sky, and found that > it's not a perfect 3 Kelvin everywhere - there are slight fluctuations > in its temperature. Cornish, along with his collaborators David > Spergel of Princeton University and Glenn Starkman of Case Western > Reserve University in Cleveland, Ohio, thinks that searching for > patterns in these fluctuations may be the key to finding out the > universe's shape. > > The team hopes to trace out different temperature patterns along > circles, and then find the same pattern along another circle elsewhere > in the sky. Patterns of temperature around one circle should be > identical to another, says Cornish. The precise pattern of circles > will indicate the fundamental polyhedron's shape. > > COBE's achievement in making the first map of the microwave sky was > impressive. But the map wasn't quite detailed enough for > pattern-spotting. NASA's Microwave Anisotropy Probe (MAP), launched > last year, will map the microwave sky in unprecedented detail, > providing the data that Cornish, Spergel and Starkman need for their !!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!! !!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!! > search. MAP will complete its first complete scan in March and then we > can begin our analysis, says Spergel. We hope to have the results by > the end of the year. !!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!! !!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!! Of course, it's quite possible that they'll make too many simplifying assumptions or that the integrated Sachs-Wolfe effect (between us and the last scattering surface) or "foregrounds" will cause too much confusion and lead to a false exclusion (more likely than a false detection), so Planck might still have a chance. But Archeops data would clearly be the best competitor for MAP: 25% of the sky is not that far off from 67% of the sky... Cze�� Boud

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Re: favoured topology of Universe candidates
by Boud Roukema 14 Feb '02

14 Feb '02

Hi Ken & Ali, On Wed, 13 Feb 2002 Kengrimes123(a)aol.com wrote: > Please find attached as requested our latest draft of the article, which we > will be forwarding to our editor this Friday. Great! > We fear you may be somewhat disappointed with the finished product, since, as > you can see, we have not managed to cover the 'psychological crutch' aspect > of the 4th dimension. Although we found this discussion most interesting, we > simply found it impossible to fit into a popular account with a strict word > limit which had to cover so much other material. Our apologies. On the contrary, my general opinion of your article is that you've done a good job of making a simple as possible introduction to the subject and of covering the variety of research done in Europe/North America, given a non-expert background and a finite ;-) amount of time to learn the subject. (Including the several Brazilians and one Japanese researcher would have been fair, but would have required more time and reading and would have been difficult within the word limit.) I think there are several small changes that can be made in order to be correct about the "psychological crutch" aspect, which I've listed below as (1). These would only add a dozen or so words. Since I'm convinced that you've made an effort to try to understand the question - but probably without (yet) succeeding (it might happen sometime when you're in the shower or on summer holidays and daydreaming or whatever - and you'll suddenly say, of course!), I certainly won't hold it against you if you prefer not to make these changes. After all, only you two are signing it, not me! But I think it would be both in readers' and researchers' interests if if you did consider my suggested changes... There are also a few other corrections I've suggested. > We would, of course, still be most interested in any comments you might like > to offer (especially if we've made any howlers!) In the meantime, we would > like to take the opportunity to thank you for the time, interest and support > you have given us on this project. The most fun part of science is understanding the Universe, and helping others to understand the same things. Your help in transmitting this to others is definitely worth it. It's been a pleasure to work together. :-) All the best Boud ---------------------------------------------------------------------- (1) The "psychological crutch" aspect of the 4th dimension. (2) What are "photons"? (3) topological images of galaxies, not stars (4) Recent constraints show Universe flat like continents are flat (5) Infinitely many spherical spaces ---------------------------------------------------------------------- > This hard-to-visualise fourth dimension is particularly intriguing to > cosmologists because, if it exists, then the universe might be curved > within it. An immediate critique of this idea is that, to the best of (1) I would put: ... % cosmologists because it could be used to help imagine how the universe % might be closed. An immediate critique of this idea is that, % to the best of ---------------------------------------------------------------------- > joined to each other simultaneously [EXAMPLE AT ABOVE URL, PAGE 2]. If > this `cube' were the entire space of our three-dimensional universe, > then the bending operation, possible only in a fourth dimension, would (1) I would put: ... % then the bending operation, which can be imagined by using % a fourth dimension, would ---------------------------------------------------------------------- > began. The same would be true for our closed, curved, > higher-dimensional universe. Like an Asteroids-type starship, any (1) I would put: % began. The same would be true for our closed % universe. Like an Asteroids-type starship, any or % began. The same would be true for our closed % universe thought of inside a higher-dimensional artificial universe. Like an % Asteroids-type starship, any ---------------------------------------------------------------------- > The term any object includes, of course, photons. (2) I think that there are probably 10-100 times more people who have some notion of both "light" and "particles" but haven't the foggiest about "photons", so why not help enlighten them: % The term any object includes, of course, photons (particles of light). ---------------------------------------------------------------------- > In a closed, curved universe, (1) I would put: % In a closed universe (which could sort of be thought of as curved) ---------------------------------------------------------------------- > light itself would describe a curved path, eventually (1) I would put: % light itself could sort of be thought of describing a curved path, % eventually ---------------------------------------------------------------------- > The implications for contemporary cosmology are truly staggering. When > we look up at the night sky, it is possible that what we are seeing is > not a single, vast or infinite number of stars, but the same finite > set of stars repeated throughout the sky, like torchlights in a hall (3) You probably know that you're making an error here, with the goal of simplicity. We are certain that the size of the Universe is much bigger than our Galaxy - none of the stars we see with the naked eye are repeated, topological images of one another. (Unfortunately!) What solutions are possible to try to be correct without sacrificing understandability to the ordinary reader? Replacing "stars" by "astrophysical objects" would be correct but sound heavy and academic. In French you could use the word "astre" which is short and snappy and means an arbitrary object in the sky. But you're not writing in French. ;-) How about: % The implications for contemporary cosmology are truly staggering. When % we look up at distant galaxies in the night sky, % it is possible that what we are seeing is % not a single, vast or infinite number of galaxies, but the same finite % set of galaxies repeated throughout the sky, like torchlights in a hall ---------------------------------------------------------------------- > observations suggest that the universe is flat. (4) More accurate would be: % observations suggest that the universe is pretty close to flat, like % any continent on the Earth is pretty close to flat. ---------------------------------------------------------------------- > The number of contenders for shapes which could tile a flat or > spherical universe is limited, but a hyperbolic universe offers (5) A "howler", at least from the mathematical point of view! ;-) The number of shapes (in 3D) for both the spherical and hyperbolic cases is infinite [in mathematical jargon, these are both countable infinities, i.e. the same type of infinity as that of the ordinary counting numbers: 1,2,3,4,5, ...]. I made the *error* (published, I think) of repeating the claim by someone else (who I won't name) who said that the number of hyperbolic spaces is a bigger sort of infinity than the infinity of the spherical spaces. From Jeff Weeks' explanation, I accepted that this is wrong. It is true (as far as I understand) that the hyperbolic spaces are not yet completely classified by mathematicians, and their families are certainly more complicated in certain ways, while the spherical spaces are completely classified and form relatively simple families. But both numbers of spaces are infinite. I suggest: % The number of contenders for shapes which could tile a flat % universe is limited, but a spherical or hyperbolic universe would offer ----------------------------------------------------------------------

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Re: favoured topology of Universe candidates
by Boud Roukema 11 Feb '02

11 Feb '02

On Sat, 9 Feb 2002 Kengrimes123(a)aol.com wrote: > Could you please confirm your title and institution for the Astronomy > article? Dear Ken & Alison, Title: Dr Institution (full name): Torun Centre for Astronomy, Nicholas Copernicus University International linguistic trivium: The "n" in Torun should have a "grave accent" on top, i.e. a forward slanting accent, like the accent on top of "e" in "�t�" ('et'e, = "summer" in French). > Date: Fri, 25 Jan 2002 16:51:33 EST > From: Kengrimes123(a)aol.com > To: boud(a)astro.uni.torun.pl > Subject: Re: favoured topology of Universe candidates > > Sorry for the hiatus. We thought, 'We'll get back to Boud as soon as we've > got our heads round this.' Still trying! Did you get anywhere with this? I admit that in my case it took many years between learning about the existence of non-Euclidean geometry and developing an intuition in which I was satisfied that this was possible without needing an extra dimension. (The latter time happened to be when I attended a course on algebraic topology.) During the intervening time, I accepted that people were probably correct in their claims, but it was rather unsatisfying. My hope is that with proper explanation, the period of years could be replaced by the space of an hour or so..., or, at least, an hour or so of initial reading followed by a week of deep thought and playing with idea in one's mind... I'm sure that playing with the games on Jeff Weeks' site that I referred you to should help. Don't be embarrassed to play games - understanding is not a matter just of cold logic, it also requires intuition via the chaotic process of a neural network. Playing games is what mathematicians do most of the time. Since you're both journalists, probably the word games that Jeff has provided would sink deepest into the cores of your minds. E.g. try the games http://humber.northnet.org/weeks/TorusGames/html/WordSearch.html http://humber.northnet.org/weeks/TorusGames/html/Crossword.html with Java and auto-image-load enabled (this is probably the case by default). And try them with the "Klein bottle" setting! Try to "unlearn" what you thought you knew about physics, just have fun playing the games instead. Imagine you're really living in the WordSearch.html, like a good movie. And then, chances are a moment will occur when, all of a sudden, you'll realise that a multiply connected flat space makes perfect sense without needing an extra dimension... > Thanks, Ken & Alison. BTW, would you be able to run the final version of the draft text by me, at least the part of the text regarding our discussions? You would of course be free to ignore or follow my comments as you wish, but it would be good that I have the chance to at least make my suggestions. Cheers Boud

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succès du vol Archeops (fwd)
by Boud Roukema 11 Feb '02

11 Feb '02

> ---------- Forwarded message ---------- > Date: Fri, 08 Feb 2002 21:28:24 +0100 (MET) > From: Programme National de Cosmologie <pnc(a)iap.fr> > To: diffusion PNC <pnc(a)iap.fr> > Subject: [iso-8859-1] succ�s du vol Archeops > > --------------------------------------------------------------------------- > PNC PNC PNC http://webast.ast.obs-mip.fr/pnc/ PNC PNC PNC PNC > --------------------------------------------------------------------------- > message # 138 8 f�vrier 2002 > > 1. Succ�s du vol Archeops des 7 et 8 f�vrier 2002 > > --------------------------------------------------------------------------- > PNC PNC PNC http://webast.ast.obs-mip.fr/pnc/ PNC PNC PNC PNC > --------------------------------------------------------------------------- > > 1. Succ�s du vol Archeops des 7 et 8 f�vrier 2002 > > Apr�s un vol interrompu pr�maturement en janvier 2002 pour un > probl�me li� au ballon, la nacelle Archeops a effectu� un vol sans > faute de Kiruna (Su�de) jusqu'� Noril'sk (Sib�rie) de 19 heures au > plafond (dont 12h30 de nuit), conduit sous la responsabilit� du > CNES. Une analyse pr�liminaire des signaux montre une bonne > sensibilit� pour la mesure des anisotropies du rayonnement fossile > cosmologique a 3K. > > Cette r�ussite de l'un des programmes phare du PNC est un succ�s pour > toute notre communaut�. > > Toutes les informations sur Archeops et sur ce vol se trouvent sur > la page WEB de la collaboration : > http://www.archeops.org > This is good news for European observational cosmology - Archeops is a balloon project, mainly French, which will cover about 25% of the sky with more or less the same instruments to be used with Planck - but the observations are to be made much, much sooner... Brief translation: a flight of Archeops on 7/8 Feb 2002 went perfectly, from Kiruna (Sweden) to Noril'sk (Siberia) with 19 hours at the "roof" (12.5 h of night), organised by the CNES (French space agency). Initial analyses look good for 3K CMB fluctuation measurements. More info at the web site. Czesc Boud

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(1) proceedings (2) new lists (3) www link (4) Moriond
by Boud Roukema 05 Feb '02

05 Feb '02

Cze�� wszystkie, (1) proceedings ;) (2) A.M.: new lists please! (3) vario@...? link from home page to .../sympa/ (4) someone to go to Moriond? ---------------------------------------------------------------------- (1) The good news about proceedings for the Wed 23 Jan mini-workshop is that... you don't have to write them! But seriously, it's probably useful for those outside of Toru� to have a brief idea of what went on, so here's my version of proceedings - any one else is free to correct them! My memory and judgment are not perfect. (In fact, proof that I am capable of making errors in judgment comes from the fact that I thought people would only be comfortable with a one hour meeting - look through the archive and you'll see this. Andrzej M. suggested a full afternoon, and I thought he was wrong. Thanks to this list, his idea was adopted, and he was right and I was wrong - thanks Andrzej!) The mini-workshop went well, IMHO. Starting from the general relativity basics of what scalar fields and quintessence are (Micha� F), going through Toru�'s big observational project which could in principle lead to direct measurement of local cosmological parameters like curvature, but maybe also quintessence and the details of perturbation statistics (Sebastian) and then an introduction to curvature and topology (Rafa�), we got back to the galaxy scale with Micha� H on how magnetic fields evolve within galaxies and how this should be related to star formation, with a nice flow diagram showing all the links and some nice videos of simulations, and then observational work on topology (Andrzej M) and on the curvature parameters (me). A lot to absorb in one afternoon. We even had several non-speaking participants! So, hopefully this will start everyone thinking about what each other is interested in and how we can have useful, productive conversations with each other. Since time ran short, we only had a brief discussion on organising questions, a main result which was people just suggested I create additional mailing lists and so how their usage evolves. Hence, point (2)... ---------------------------------------------------------------------- (2) Andrzej M, could you please create the following three mailing lists on sympa, just copy all the initial properties of cosmo-torun (except for the htaccess file, these three should be with open access, so no htaccess file is needed), and I'll adjust things once you've made them and got the daemons running. Here I'll just put the names I suggest and the descriptions. (2a) name: cosmo-spotka description: This mailing list is for all sorts of discussions on meetings of various sorts related to cosmology at Toru�. This can include (1) Discussion of what sort and frequency of regular TCfA meetings to organise (weekly vs fortnightly vs monthly; presentations of own research vs "journal club" talks on cosmo news items vs creative new idea generation sessions vs introductory reviews; should we have a separate seminar from the regular Monday ones or just use the Monday ones? - probably all these questions should be left open and fluid for some time and will probably be answered in an evolving way - hence the need for a list!); (2) Other organising info on TCfA meetings themselves; (3) Offers by people, e.g. from around Poland or internationally, to give cosmo seminars - if someone wants to give a seminar, they should briefly introduce themselves here and say something like "hey, I'd like to give a talk at Toru�", this way the information flow will be more efficient than if it has to go through just one seminar organiser; (4) Requests by outsiders for a Toru� person to give a seminar at their institute can go directly to this list - this would help give everyone a chance at giving outside seminars. (5) Other meeting related discussion. (2b) name: cosmo-pl description: Debaty generalne mi�dzy kosmologi w polsce, dla organisowa� badania i spotkanie kosmologi. Mo�e by� kilka rozmawiane b�d� zacz�� tutaj i przeprowdza� si� do cosmo-spotka, lub vice-versa. Nie jest problemu. R�nica: cel cosmo-spotka jest TCfA, a cel ta lista jest ca�a grupy lub naukowcy individualny z kosmologiem w Polsce. Chyba b�d� uzywa� po polsku, je�li po polsku kosmology zagraniczn�w nie jest zbytnio �mieszny ;). Wol� kodeks litery latin-2 (iso-8859-2), nie kodeks Micro$oft. [You can correct the po polsku putting in the correct odmian przypadk�w, if you like, o.w. just put it as it is!] (2c) name: cos-rule description: This list is for organising a workshop on the claimed features in the power spectrum/correlation function of extragalactic objects on scales at or above 100h^-1Mpc. According to standard "linear theory" of the FLRW model, these features should serve as cosmological standard rulers if they real, and initial results certainly favour this. Both observational results, for and against, and theoretical explanations, are sought for this workshop. It would be hoped to organise this for the Northern Spring/Summer of 2002, at Toru�. Anyone wishing to speak or help organise is welcome to post an introductory message here and participate. ---------------------------------------------------------------------- (3) I propose that on the left bar of the www.astro. ... page we have a yellow tage with something like "Cosmology group" pointing to .../sympa/ so that people can easily find all four lists. If people agree, could someone do this? (Apparently vario@... is the webmaster.) ---------------------------------------------------------------------- (4) Moriond - The Cosmological Model Les Arcs, France (March 16-23, 2002) http://moriond.in2p3.fr/J02/ I noticed there's special funding for East Europeans to go to this, and I don't know of many EE cosmo groups who could take up the offer... Polish people under 35 can also get funding under the "European" heading (see the page). This would be a good meeting for learning standard stuff (e.g. for starting to think about what to do with OCRA...), and for starting to get to know other European cosmologists, but it's *very* expensive and no point going unless you're fully funded. (You had also better like skiing - talks are something like 9:00-12:30 and 4:30-7:30, so that most people ski in the afternoon... ) Officially the funding deadlines have passed, but if very few East Europeans have applied, the organisers might be happy to accept some late offers. Be warned that any travel requires a bit of time invested, paperwork etc., thinking about the budget, but I think most of us have some travel experience. It's also a distraction from getting work done. But might give you new ideas or help you learn things. If anyone wants to apply, it might help if you do a cc: to me which would show to the organisers that you're in contact with someone they know, but I'm in Paris for getting a visa right now so I can't sign any forms for you - and in any case, you need a "senior scientist" to sign the request for funding form. ---------------------------------------------------------------------- Pozdrawiam Boud

3 3

Updated programme!
by Andrzej Marecki 21 Jan '02

21 Jan '02

Updated programme! == Cosmo-Torun Mini-Workshop 14:00, Wed 23 Jan 2002 TCfA == Welcome to the Cosmo-Torun Mini-Workshop. This is intended to help us start to learn about each others' interests in cosmology and how we can carry out research together. Please feel free to invite anyone likely to be interested, and help them to access the page containing this document! Background reading of http links is not compulsory but would obviously help. Date: Wed 23 Jan 2002, time: 14:00-17:30 Proposed programme, including links to background reading: 14:00-14:30 (5 mins presentation, 25 mins qns, discussion) Michał Frąckowiak - A few words about quintessence 14:30-15:00 (5 mins presentation, 25 mins qns, discussion) Sebastian Soberski - A few words about OCRA 15:00-15:30 (5 mins presentation, 25 mins qns, discussion) Rafał Kosiński - A few words about cosmic topology 15:30-15:40 coffee/tea break 15:40-16:10 (20 mins presentation, 10 mins qns, discussion) Michał Hanasz - Cosmic rays and magnetic fields - are they relevant for galactic evolution? 16:10-16:40 (25 mins presentation, 5 mins qns, discussion) Andrzej Marecki "How can we use radio-loud AGNs as probes of topology?" http://de.arXiv.org/abs/astro-ph/0201092 16:40-17:00 (20 mins discussion based on points in msg00018.html) discussion of the cosmo-torun list and related mailing lists http://www.astro.uni.torun.pl/sympa/cosmo-torun/2001-12/msg00018.html 17:00-17:30 (15 mins presentation, 15 mins qns, discussion) Boud Roukema "A Cosmic Standard Ruler" http://de.arXiv.org/abs/astro-ph/0106135 --------------------- See: http://www.astro.uni.torun.pl/sympa/cosmo-torun/2002-01/thrd1.html to find out more. -- Andrzej

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spotkania cosmo-torun 21-25 stycnia?
by Boud Roukema 18 Jan '02

18 Jan '02

Cze�� wszystko, Proponuj� wizyt� w Piwnice 21-25 stycznia, i spotkania cosmo-torun. Co my�lecie? My guess is that a one-hour meeting would be enough, but Andrzej suggested a full afternoon. I would be happy either way, but it only makes sense to do what most people prefer. Could everyone (except Motylek who I presume is in JBO now) say what they would prefer in terms of (i) time length (ii) which time (iii) which topics? I suggest people just write their answers to the list or concatenate them with previous answers. Our numbers are small enough that cut/paste should be enough. (i) 1 hour meeting ? one afternoon 14h-17h30 meeting ? (ii) Mon 21 Tue 22 Wed 23 Thu 24 Fri 25 Which are impossible? preferred? (iii) My idea of an easy cut/paste way to see what people want to talk about. Please put a rating + 0 - in front of the following topics (or concatenate your rating to previous ones). The values are +1, 0, -1 respectively. The final ratings are added up and then we will know which people are most interested in. science ------- + Rafa� - cosmic topology? (Just say something about what you understand, or what your questions are, or why you think we're doing things wrongly, what you think we should do, whatever! This is not an exam: we know you have not published any research papers in the subject, so there's no embarrassment if there are gaps in your knowledge. There are certainly big gaps in my knowledge. Be creative!) + Micha� F - quintessence? Could you teach us something about quintessence, scalar fields in a way that we all understand and can relate to our work? + Sebastien - something about OCRA? What you are doing, what is planned, the time schedule. How the scientific use of the data is planned (this is in fact partly a political question, which you should probably discuss with Andrzej Kus - maybe Andrzej K could come along and let us know what the ideas for this are so that nobody gets upset by us suggesting analysis plans against the wishes of the people running the project!) 0 Andrzej M - non-topology work or topology work, as you like - Micha� H - something about your AGN work - Boud - cosmic topology; cosmic standard ruler; or galaxy formation meta-discussion --------------- + discussion of the cosmo-torun list, what do people think of creation of the other spinoff lists I've suggested (listed below) or which others may suggest, in particular, the idea of a list dedicated to each project or article? 0 development of cosmo-torun web pages - is anything needed yet? Ideas for spinoff lists: ------------- * cosmo-seminar: For organising meetings (whatever the title, "journal club", "seminar", "workshop", "conference") in Toru� and/or Warsaw and/or other Polish cities (e.g. there's a theoretical cosmo group in Krak�w). I suggest no access restrictions, since no "unpublished research ideas" are likely to be posted here. * cosmo-pl: For general discussion, organisational, scientific, whatever, among Polish cosmologists and extragalacticians. Again, no access restrictions. * topo-rlagn: [cosmic topology radio-loud AGN projects] * ocra: Sebastian Sober ? * shape-univ: I've offered to Andrzej Woszczyk and said to some students that I would be happy to teach a "monograph course" on observational constraints on the shape of the Universe (curvature + topology) during the next semester (which I believe starts 18th Feb 2002). * other Are there any existing lists? Someone told me something about a list called astronomia(a)astri.uni.torun.pl . It seems to me one list which could be useful (for publicity purposes) would be one for discussing TCfA web pages. It's not always obvious what changes are good ones, and it's a lot of pressure on the webmaster if he/she alone has to decide to accept/reject suggestions/requests. A mailing list would make the decisions more collective. Pozdrawiam, Boud Summary: These are the questions which it would be good to answer or give a rating to (respectively) in order that the meeting can be in the best interests of everybody! Just cut, paste and edit! ====================================================================== -- cut ---- cut ---- cut ---- cut ---- cut ---- cut ---- cut ---- cut -- ====================================================================== (i) 1 hour meeting ? one afternoon 14h-17h30 meeting ? (ii) Mon 21 Tue 22 Wed 23 Thu 24 Fri 25 Which are impossible? preferred? (iii) Please add + 0 - to the beginning of each line. You can add other lines for discussion if you wish! + Rafa� - cosmic topology? (Just say something about what you + Micha� F - quintessence? Could you teach us something about quintessence, + Sebastien - something about OCRA? What you are doing, what is planned, 0 Andrzej M - non-topology work or topology work, as you like - Micha� H - something about your AGN work - Boud - cosmic topology; cosmic standard ruler; or galaxy formation + discussion of the cosmo-torun list, what do people think of creation 0 development of cosmo-torun web pages - is anything needed yet? ======================================================================

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Re: favoured topology of Universe candidates
by Boud Roukema 13 Jan '02

13 Jan '02

Hi, just an explanation for the discussion with the media people. I think it's useful to cross-post this (1) so that in case the journalists publish wrong or misleading statements, there are at least some colleagues who know what my version of the story was; (2) it's probably useful for everyone since it's a discussion at a very pedagogical level, and should help to make it clear to everyone that I'm not a "believer" in any of the hypotheses I work on. If there's a lot of this, I would prefer to spin this off into a completely open list, e.g. cosmo-torun-media , so that anyone interested could read it. Cze�� Boud

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Re: favoured topology of Universe candidates
by Boud Roukema 13 Jan '02

13 Jan '02

Dear Ken & Alison, Glad you're getting back to me for feedback. This is definitely a good way to check we understand each other. :-) > Date: Sat, 12 Jan 2002 14:28:52 EST > Subject: Re: favoured topology of Universe candidates > To: boud(a)astro.uni.torun.pl > Dear Boud, > > Many thanks for your prompt reply. We have read through your e-mail and BASI > review, and would like to check that we have understood correctly (not being > experts in this field). > > We understand that you are researching possible shapes of the universe which > are finite, unbounded, and multiply connected (such as a hypersphere, > 3-torus, 3-Klein Bottle or other 4D polyhedra). This would imply that we are OK, two comments. (a) science Correct, except that I'm also researching possible *infinite*, unbounded, and multiply connected models. A finite model would be more aesthetically pleasing, but it is best to do observational work with as few prior hypotheses as possible. The Universe is how ever it is, not how I would like it to be. (b) pedagogical, terminology The "shapes" such as the hypersphere, the 3-torus, the 3-Klein Bottle are *not* "4D polyhedra". Technically, they are called "3-manifolds", but since that is rather scary to non-specialists (including many astronomers!), a more friendly term would be "3-spaces" or "3-dimensional spaces" - which can be thought of with the *help* of a 4th dimension - or which can be thought of as 3D polyhedra where certain faces are identified in some way. It is *very* important to explain that when a 4th dimension is used to help think about a 3-space, this is purely a psychological tool, a mental crutch for human beings having difficulties thinking in a multiply connected and/or curved 3-space, simply because we are biased from our childhood experiences and school education to think in terms of Euclidean, simply connected 3-space. It might sound like gestalt psychotherapy ;-) to say this, but as far as a mathematician or physicist is concerned, a 3-dimensional space exists in and of itself, it has no need for the existence of extra dimensions to be itself, even if an extra dimension or too helps it (or beings living inside it!) to understand what it is. In "brane theory", it is true that 4th & 5th dimensions are thought of as true physical dimensions, but the field of observational studies of the topology of the Universe is separate from brane theory. But then again, the 4-dimensional or 5-dimensional models could again be thought of in spaces with an extra "psychological" dimension of no physical meaning, i.e. 5D or 6D spaces, again with the extra dimension just as a thinking aid. So I think the issue of a dimension as a thinking aid with no physical meaning cannot be avoided. I would recommend that in your article you explain something of this issue - the fact that as far as most observational cosmologists interested in either curvature and/or topology are concerned, a 4th dimension is a useful psychological tool for thinking, but is used without any physical meaning. If we go one dimension down, to make things easier, I can refer to Figure 1 of my BASI article http://uk.arXiv.org/abs/astro-ph/0010185 . Here I discuss a 2-space, the "2-torus". There are three different ways (i)-(iii) of thinking about the same space. It's a good exercise to try switching between the three ways and checking that you can understand them as the same thing. In (i) (lower figure), I use ordinary 3-space to help the reader imagine what the 2-space is. In (ii) and (iii), the reader does not need to think at all in 3-space. 2-space is enough, even though it may seem a little weird. Going back up a dimension, it is possible to imagine various 3-spaces, either like (i) within a 4-space or like (ii) and (iii) just within ordinary 3-space, but a little weird. > seeing repeated copies of a small universe (rather than a single very large > or infinite one). Your research centres around studying the sky to identify > repeated patterns of objects (celestial bodies and/or temperature signatures > in the microwave sky) to infer a size and shape for this "tiled" universe. Correct. For more clarity, you might want to put "...studying the sky in three dimensions to identify..." BTW, when you say "tiled" Universe, you're referring to mode (iii) of thinking. > Presumably, in order to decide in which directions, and at which distances, > to look for these repetitions, you must be working from a hypothesis about > the possible shape. For example, according to John Gribbin's New Scientist > article from that date, in 1997 you seemed to be looking for quasar patterns > to support a "twisted torus" or "3-Klein bottle" hypothesis. Nope. I'm a skeptical observer who works the other way around! There is no serious theory for the extension of general relativity which would give a theory of global geometry, and even if there was, the best bet would still be to make observations with as few preconceived ideas as possible. The standard Big Bang model, by the way, is a preconceived idea which I and my colleagues *do* assume, since it (and the theory of general relativity) is (are) extremely well established observationally. Rather than working from a specific hypothesis about the shape, my general approach is on finding the best ways of using existing (or near future) observational data catalogues. It happens that during some of these projects, serendipitous candidate topologies have turned up. I think all of (1), (2) and (3) that I gave you in the previous message are best described as serendipitous, though (2) comes from a (slightly) more systematic approach than (1) and (3). The candidate from my John Gribbin article was found using a very systematic approach, but at the moment it is just sitting in my "list-of-things-to-do". Although it was found systematically, I would probably class its "subjective probability" as 5%. But my subjective probabilities are... subjective. The only serious way to check candidates is by further observational work. BTW, the implicit 3-Klein-bottle-like model was what the observations gave, not what I was looking for. I would have preferred to find a 3-torus than a 3-Klein-bottle-like model! > Your e-mail suggests that your current research focuses on the use of galaxy > clusters and microwave patterns to identify a "model class: 2-torus". Are we Hmmm. I don't know if the following is too subtle for a general audience. See how you like it. I would prefer to say: ---- My current research focuses on the use of galaxy clusters and microwave patterns in which serendipitously discovered 2-torus models offer good prospects of observational tests. Later on, if more complicated models are offered as candidates, the experience in testing 2-torus models will be important for testing the more complicated models. After all, if it is not possible to observationally test a 2-torus model, which is relatively simple, how could we possibly hope to test a more complicated model? Candidate (3) is even less ambitious: it involves just one generator, or path between two images of (hypothetically) the same object. ---- [plus a modification of the term "2-torus" as per the comment below] > right in assuming that this refers to an actual universe in the shape of a > (non-twisted?) 4D 3-torus, which is modelled as a 3D 2-torus? OK, I used an abbreviation without explaining it, sorry! Firstly, as I explained above, the 3-torus is really 3D, and the 2-torus is really 2D, even if an extra dimension is used as a psychological crutch. The model I've called "2-torus" for my observational work on the real Universe (as opposed to pedagogical explanations with one dimension subtracted) is really the 3-torus, but one side length is considered bigger than the horizon diameter, so big that observations made that far away would require the light to have been emitted before the Universe was born. If you called it a "3-torus with one very long side" or a "3-torus with one presumably infinite side length" that would be correct, would probably help avoid confusing readers, and would avoid experts in the field getting confused about what I'm doing. > We would also be interested in your views on other possible tessellated > polyhedra models. In particular, we are interested in any topologies which Well, again, I would prefer to say "other possible 3-spaces" or "other possible, multiply connected 3-spaces, which can be thought of as tesselated polyhedra models". > may be consistent with the recently emerging field of braneworlds. For > example, Michael R. Feltz's website - http://www.cyburban.com/~mrf/ - > identifies brane theory with the Riemannian hypersphere topology. Well, I quite like the idea of non-experts writing web pages (if I hadn't been job-hunting for the past few years I probably would have made more effort to interact with non-specialists, and maybe sometime in the future I will be able to...), but I'm afraid there is some confusion in Michael Feltz's page: : The discussion here attempts to answer this question as it relates to : the often hypothesized, but little explored, "finite but unbounded" : universe. The formal name for this model in topology and cosmology is : a "closed cosmic hypersphere". There are many finite but unbounded models other than the hypersphere, e.g. the 3-torus. : Otherwise the days of an expanding universe are numbered because this : high density model will expand only to certain maximum size and then : contract into a "big crunch" ("big bang" in reverse) at some future : date at least tens of billions of years from today. Correct. And the geometry of *this* model is a 3-sphere, also known as a hypersphere. : The alternate model explored in this series of essays is the long : suspected and often hypothesized "closed cosmic hypersphere" which : incorporates a fourth spatial dimension. The hypersphere provides one of the three possible curvatures, plus the assumption of trivial topology. Calling it the "closed cosmic hypersphere" is OK. But it does *not* incorporate a fourth spatial dimension. A fourth, psychological, dimension is just one possible way to think about it. And it is not an "alternate" model. It is the model which (for reasonable values of the local cosmological parameters, which show that the Universe is "approximately" flat, like any continent on the Earth is "approximately" flat) will expand to a maximum size and then contract into a "big crunch". Back to your question! My views on other possible "tesselated polyhedra" models (and now you know they're physically only 3D, not 4D), are that I'm totally open to any of these multiply connected models, whether for a flat Universe (where the angles of a triangle add up to 180�, and this includes the "3-torus with a very long side" models - this is a flat model!), for a spherical Universe ("hypersphere", where the angles of a triangle add up to more than 180�) or for a "saddle-shape" Universe ("hyperbolic", where than angles of a triangle add up to *less* than 180�). Of course, in either the spherical or the saddle-shape cases, the observable part of the Universe would be approximately flat, again like any continent on the Earth is approximately flat. > Given that the readers of Astronomy are mainly non-scientists, we would be > very grateful if you could provide as simple an explanation as possible. I know very little about brane-theory, but I think it is still much too theoretical to have any serious links with observational work. I think the best link you could make between observational cosmic topology work and brane theory could be something like the following: ---- Scientists trying to measure the 3-dimensional shape of space (with a type of non-expanding map of the Universe called "comoving" - although in reality the Universe is expanding, in this special map, the Universe can be thought of as static) sometimes use a psychological 4th dimension to explain or think about different possibilities for the shape of space, e.g. a 3-space which seems to be tesselated by many copies of the Universe. Other, more theoretical scientists, working on "brane theory", think that 4th and 5th dimensions might have real physical meaning (of course, there's also time, making a 6-dimensional world). However, the scientists trying to measure the 3-dimensional shape of space (also called the topology and curvature of space) prefer a more conservative, purely empirical approach and would like to measure the shape of 3-space without any preconceived notions, apart from the standard Big Bang model. They hope to detect any of many possible shapes of 3-space, whether it's the 3-torus with one very long side or any other. ---- For more on brane theory, you might want to ask Nathalie.Deruelle(a)obspm.fr, who gave a very nice explanation during a workshop in Paris last year, but unfortunately I was too tired and stressed to really listen properly :-(, though she did seem to give a good explanation. She's definitely an expert in brane theory, and is very supportive of work in cosmic topology. And she's probably one of the best people around who can make an intelligent comment on whether there's any link between the two. > Many thanks once again for your help, My pleasure :-) - feel free to keep passing draft texts to me for comment and/or other questions. Boud boud(a)astro.uni.torun.pl Torun Centre for Astrophysics, University of Nicolas Copernicus, Torun http://www.astro.uni.torun.pl/ (affiliation by the time the article is published!)

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An AGN HR diagram? astro-ph/0201089
by Boud Roukema 11 Jan '02

11 Jan '02

A key to understanding AGN? Proceedings by Peter Barthel from Gr�ningen: "An AGN Hertzsprung-Russell Diagram" http://de.arXiv.org/abs/astro-ph/0201089 Motylek, Andrzej, Micha�, any thoughts?

2 1

favoured topology of Universe candidates
by Boud Roukema 09 Jan '02

09 Jan '02

Dear Ken & Alison, I would be pleased for my scientific work to be featured in the article. :) I don't know how much you would like me to write and how much you would like to rewrite yourselves. But I think it's in the interests of non-scientists' right to "eavesdrop on science" for me to give you more detail, including published references, than you are likely to want to publish. If you wade through the articles and come out feeling dizzy, please feel free to ask more questions and I'll try to help clarify things. Even so, I'm not convinced that my initial response explains enough for the lay reader, but it's already rather long as it stands, so have a read through and tell me where you want to go from here. * General reading: I would strongly recommend that you read my BASI review http://uk.arXiv.org/abs/astro-ph/0010185 which should be quite accessible to science journalists and give you my version of how the different approaches relate to one another. * Affiliation: By the time your article is published, my affiliation will be Torun Centre for Astrophysics, University of Nicolas Copernicus, Torun ---------------------------------------------------------------------- > 1) Which (if any) of the current candidates for the topology of the universe > do you favour, and why? 1a) which candidates do "I favour" ? 1b) why? ---------------------------------------------------------------------- 1a) which candidates do "I favour" ? Well, the verb "to favour" is really about my personal pyschological reactions, which only weakly correlate to scientific reality! But I can tell you the three candidates, in chronological order, for which I think observational predictions should be tested, as well as the intuitive, subjective probabilities which I've tried to assign to their being correct - since you asked! If that's what you mean by "favour", fine. (1) "three cluster identity": Coma cluster/RX J1347.5-1145/CL09104+4109 model class: 2-torus comoving size of Universe: about 1 h^{-1}Gpc (Hubble constant = 100h km/s/Mpc) subjective probability: 10% references: - Serendipitous discovery in discussion of clusters seen in X-rays http://uk.arXiv.org/abs/astro-ph/9706166 Roukema & Edge - optical analysis from archival data http://uk.arXiv.org/abs/astro-ph/9903038 Roukema & Bajtlik - COBE cosmic microwave background (CMB) analysis (assumes cosmological constant=0) http://uk.arXiv.org/abs/astro-ph/9910272 Roukema (2) "COBE counterexample" model class: 2-torus comoving size of Universe: about 2 h^{-1} Gigaparsec or greater subjective probability: 20% references: - COBE cosmic microwave background (CMB) analysis http://uk.arXiv.org/abs/astro-ph/0007140 Roukema (3) "radio galaxy pair": identity of radio-loud active galaxies 3C186/4C+36.21 model class: only one generator hypothesised comoving size of Universe: about 1 h^{-1} Gigaparsec subjective probability: 10% references: http://uk.arXiv.org/abs/astro-ph/0111052 Roukema, Marecki, Bajtlik, Spencer ---------------------------------------------------------------------- 1b) why? Probably my true answer for (1)-(3) is: because they haven't been falsified yet. (A technical note: (1) was falsified in astro-ph/9910272 under the assumption of zero cosmological constant, which was still a reasonable assumption at the time the work was done, in 1998, but it is now clearly a bad assumption, so (1) is again a valid candidate.) As for the values of my subjective probabilities, well, they're subjective. I did happen to notice after writing them down that: P(subjective)= 10% size of Universe in h^{-1}Gpc but this is not a true description of my personal psychological state, since I would not give a 100% probability to a model 10h^{-1}Gpc in size! ---------------------------------------------------------------------- > 2) What research methods are you (and others sharing your view) following, > and what progress is being made? (1) "three cluster identity". This candidate makes predictions that it should be possible to point a telescope at certain angular positions in the sky and detect clusters at certain distances (redshifts). If a cluster is found at the correct position and redshift, the hypothesis would be strengthened. If it were definite that no cluster existed at the predicted position and redshift, the hypothesis would be falsified. With my colleagues Jean-Michel Alimi, Jean-Pierre Luminet, Dominique Proust, (LUTH & GPI, Observatoire de Paris-Meudon), Stanislaw Bajtlik (Nicolas Copernicus Astronomical Centre, Warsaw) and Etienne Pointecouteau (Tohoku University, Japan), various requests for observing time on optical telescopes have been made. We had some service time allotted in 2001 on the Anglo-Australian Telescope, in principle, but the schedule did not allow observations to be made. We will continue this programme of optical telescope tests. (Note: members of the group differ on the subjective probabilities they assign to the candidate being the right one!) (2) "COBE counterexample" Although this is the candidate I'm probably the most interested in, it's also the hardest to test, because the larger scale implies that multiple images ("topological lensed images") of ordinary astrophysical objects exist at high redshifts, meaning long lookback times into the past history of the Universe, so that not only is it most difficult to observe the high redshift images (because they are faint!), it's also likely that the objects didn't exist yet at that early epoch. The MAP and Planck satellites will probably provide the best tests of this hypothesis, though making a correct analysis with as few as possible theoretical assumptions is likely to be fiendishly difficult. As far as I know (but science history is not my field!), Geoffrey Marcy and Paul Butler missed the detections of exoplanets in their own data in the early 1990's because they had accepted the theorists' "reasonable" assumption that massive planets (Jupiters) could not exist in short period orbits. Such "reasonable" assumptions for detecting cosmic topology might also lead to a discovery remaining hidden for many years... (3) "radio galaxy pair": Although the morphologies (shapes) of these two radio galaxy jets are strikingly similar, the redshift (equivalently, cosmological epoch when the light was emitted) of only one of them is known. Radio galaxy jets expand at very high speeds, from 1% to over 100% (in apparent speed) of the speed of light. So, the hypothesis can only be valid if the redshift - and the cosmological time of emission of the light making the image - of 4C+36.21 is just slightly higher - cosmological time slightly earlier - than for 3C186. The prediction for the redshift of 4C+36.21 is 1.0630 < z < 1.0635. A redshift measurement will either strengthen the hypothesis, or falsify it. My colleague Andrzej Marecki (Torun Centre for Astrophysics, University of Nicolas Copernicus, Torun) has time on the William Herschel Telescope in the Canary Islands for a spectroscopic measurement of this redshift, so we hope to have an answer in the coming year! ---------------------------------------------------------------------- > From: Kengrimes123(a)aol.com > Date: Mon, 07 Jan 2002 13:18:13 -0500 (EST) > Subject: Astronomy magazine article. > To: boud(a)iucaa.ernet.in > Dear Dr Roukema > We are two science journalists currently writing an article for Astronomy > magazine (a US title with a circulation of approximately 300,000 readers). > The subject of the article is hyperspace and the topology of the universe, > and we wonder if you would be interested in being featured in the article. > > The issues we are concerned with are: > > 1) Which (if any) of the current candidates for the topology of the universe > do you favour, and why? > 2) What research methods are you (and others sharing your view) following, > and what progress is being made? > > We can be contacted at this return e-mail address (kengrimes123(a)aol.com). > Should you prefer to speak via telephone, please let us know what would be a > suitable time to call you. Email is fine. > Many thanks for you attention, > > Ken Grimes & Alison Boyle. Glad to be of help, Boud Roukema boud(a)astro.uni.torun.pl Torun Centre for Astrophysics, University of Nicolas Copernicus, Torun http://www.astro.uni.torun.pl/ (affiliation by the time the article is published!)

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Do Type Ia Supernovae prove Lambda > 0 ?
by Andrzej Marecki 04 Jan '02

04 Jan '02

Paper: astro-ph/0201034 From: M.Rowan-Robinson <m.rrobinson(a)ic.ac.uk> Date: Thu, 3 Jan 2002 16:29:08 GMT (64kb) Title: Do Type Ia Supernovae prove Lambda > 0 ? Authors: Michael Rowan-Robinson Comments: 10 pages, 10 figures. Accepted for publication by MNRAS -- Andrzej

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Re: cosmo-torun
by Andrzej Marecki 20 Dec '01

20 Dec '01

Boud wrote: > PS: Anyone on the list should feel free to invite others who would > find the list useful. People can unsubscribe themselves later if they > find there's too much mail coming through. By the way: this is what I always wanted to know (but was afraid to ask before :-) if "cosmo-torun" is somehow arbitrarily limited to .torun.pl domain and serves Toruń people only or it actually means: "cosmo-torun-warszawa-paris-etc-if-you-only-want-to-join-and-share-ideas" To be more specific: how about inviting the cosmologists from CAMK, Warszawa (Staszek, Ewa, etc.). Maybe you could just take the opportunity of sitting next to them and talk to them. You know them better than I do so I leave this issue entirely to your discretion. What I particularly have in mind (if we decide to join the forces, of course) is to organise such "one-afternoon-workshops" in the future together with Warsaw people. (To this end sometimes they would come to Piwnice, sometimes we would go to CAMK, or sometimes we could meet half(?)-way, at CAMK-Toruń.) Pozdrawiam Andrzej

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introductions
by Boud Roukema 19 Dec '01

19 Dec '01

Cze�� koledzy, By now you've had a short scientific introduction from Micha� F., and I think you know, or if not, you will know after this sentence, that Andrzej Marecki and I are working on an RLAGN project for developing principles of techniques of detecting the global shape of the Universe, according to the standard, hot big bang, Friedmann-Lema�tre model. E.g. for a beginner's review see http://de.arXiv.org/abs/astro-ph/0010185 Would the others be able to introduce yourselves? You can, of course, find out who has subscribed using list commands (see HELP below), but so far, the others and what seem to me to be their cosmological/extragalactic interests are (in arbitrary order): Sebastian - interested in OCRA (one cm array project) Rafa� - interested in cosmic topology (as a sideline) Marcin/Motylek - interested in FRI/FRII evolution Micha� Hanasz - magnetic fields in low z (<< 1) AGN, but moving to high z (2-3) AGNi ?? I'll be back in Toru� in a few weeks time, and it would be nice to have a face-to-face meeting, but in the meantime, could everyone just say a few lines about their interests (correcting my above summary!), and feel free to make meta-suggestions (about the list or about how to organise discussions or work, whatever) as well as direct discussion of science. Pozdrawiam, Boud

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First "workshop" (was: Re: introductions)
by Andrzej Marecki 18 Dec '01

18 Dec '01

Witam wszystkich! Boud wrote: > I'll be back in Toruń in a few weeks time, and it would be nice to have a face-to-face meeting, To jest bardzo dobry pomysł, Boud! (It's a very good idea, Boud :-) Let it be our - very informal yet very serious in terms of scientific background - 1st "workshop". I can give a talk about what I've done recently. I'm sure, you, Boud, might be a key speaker with an "invited" talk. ;-) I, also, can be an "acting" LOC. Pozdrowienia, Andrzej

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cosmo-torun
by Boud Roukema 18 Dec '01

18 Dec '01

CC: cosmo-torun Hi Bronek, Andrzej M. and I have started up a web-supported, threaded, mailing list for people interested in cosmology research in Toru�: http://www.astro.uni.torun.pl/sympa/cosmo-torun/ Please feel welcome to subscribe! Instructions on how to do this are on the site. In spite of your not officially being a cosmologist, you have a reputation of knowing the basics pretty well... Cze�� Boud PS: Anyone on the list should feel free to invite others who would find the list useful. People can unsubscribe themselves later if they find there's too much mail coming through.

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Michal: quintessence
by Boud Roukema 17 Dec '01

17 Dec '01

Cześć, Michał Frąckowiak has been playing around with some ideas on quintessence. He suggested to me some ideas and asked if I could test these on the data that Staszek, Gary and I have already analysed. Well, creativity generally requires that you generate 100 ideas and try to throw away 99. If you end up throwing away 100, well, you have to go on to the next 100... Or you can modify the ideas and gradually come up with something unexpected. In fact, there's often something interesting enough to be worth talking about. So, let's see. ----- Michał, I'm not sure I understand your calculation. You express w as a Taylor series of (a-1), but normally this only makes sense if (a-1) is much smaller than 1. [ a is the expansion factor: coordinates can be chosen in which the Universe is static, and all the expansion is represented by a single function of cosmological time: a(t). By convention, a(t)=1 now. The Big Bang is simply the extrapolation a(t) -> 0 as t -> 0^+ , i.e. arbitrary separations between any coordinates get multiplied by nearly zero as t -> 0 from above. So outside of the Sun, a-1 is a negative number between 0 and -1. ] You wrote: > w(a)= w^(0) (a-1)^0 + w^(1) (a-1)^1 + w^(2) (a-1)^2 + ... > What is interesting, it seems absolutely sufficient to consider only the 2 > first terms in w !!! (up to z=500). Then the evolution reads: w(a)= w^(0) + w^(1) (a-1) (equation (*)) Well, a = 1/(1+z), so a-1 = -z/(1+z), so at, say, z=2, a-1 = -2/3. Are you interested in redshifts where z=0.01 or where z=2? The SNeIa data are mostly at about z=0.4-0.8, and the quasar data at about z=0.5 to z=2.4 (roughly). This makes the (a-1)^i terms decrease (in magnitude) very slowly. I can only see a rapid convergence if you already know something about w^(1), w^(2), ..., that they go very quickly to zero. Do you have in mind a quintessence model where these derivatives go to zero very fast? Or have I misunderstood? In any case, it is certainly possible for me to test equation (*) on the data, though at the moment it seems to me more likely that we would get reasonable error bars by estimating w(z=0.8) and w(z=1.4) and w(z=1.9) independently. From those three points with error bars, it would of course be easy (apart from error propagation ;-) ) to calculate w^(0) and w^(1) under the assumption that other terms can be neglected. If we could simply obtain significantly different values in the three redshift bands, this would be a big enough result, though of course it would be useful to have some theoretical comments of what that might mean. Pozdrawiam Boud

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Re: new thread: mhonarc options
by Boud Roukema 13 Dec '01

13 Dec '01

The above are just test messages. Don't take the values of Omega_m there too seriously ;-). I wonder if http links get automatically converted, e.g. my article with Staszek and Gary independently showing that Om_m is close to 0.3 and that Omega_total is close to 1 (in the sense that the Universe is about as flat as a 1 radian radius surface area of the Earth: if the Earth is nearly flat, then yes, the Universe is nearly flat): http://de.arXiv.org/abs/astro-ph/0106135

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new thread: mhonarc options
by Boud Roukema 13 Dec '01

13 Dec '01

Does reply using netscape work?

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new thread: mhonarc options
by Boud Roukema 12 Dec '01

12 Dec '01

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4th message
by Boud Roukema 12 Dec '01

12 Dec '01

now with archive.pl running as a !daemon!

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