From amr w astro.uni.torun.pl  Fri Jan  3 12:10:13 2003
From: amr w astro.uni.torun.pl (Andrzej Marecki)
Date: Fri, 3 Jan 2003 12:10:13 +0100 (MET)
Subject: Brak tematu
Message-ID: <200301031110.MAA26878@galileo.astro.uni.torun.pl>

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 w 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
 


From amr w astro.uni.torun.pl  Tue Jan 28 09:52:34 2003
From: amr w astro.uni.torun.pl (Andrzej Marecki)
Date: Tue, 28 Jan 2003 09:52:34 +0100 (MET)
Subject: 1st MAP data release
Message-ID: <200301280852.JAA01043@galileo.astro.uni.torun.pl>

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
 

From amr w astro.uni.torun.pl  Thu Jan  9 10:21:47 2003
From: amr w astro.uni.torun.pl (Andrzej Marecki)
Date: Thu, 9 Jan 2003 10:21:47 +0100 (MET)
Subject: A healthy dose of scepticism or a humbug?
Message-ID: <200301090921.KAA13991@galileo.astro.uni.torun.pl>

Paper: astro-ph/0301137
From: Blanchard Alain <alain.blanchard w 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
 

From boud w astro.uni.torun.pl  Thu Jan  9 15:21:50 2003
From: boud w astro.uni.torun.pl (Boud Roukema)
Date: Thu, 9 Jan 2003 15:21:50 +0100 (MET)
Subject: A healthy dose of scepticism or a humbug?
In-Reply-To: <200301090921.KAA13991@galileo.astro.uni.torun.pl>
Message-ID: <Pine.SOL.4.44.0301091433010.5414-100000@hevelius.astro.uni.torun.pl>

Witam,

"Healthy skepticism of humbug?"

"humbug" is definitely unfair. Alain is a cool guy and a sincere
scientist. Narlikar, Burbidge (and the late Hoyle) are (was) good
scientists, and they are (was) right to criticise the monothink
(pensée unique) and the fashion of talking about cosmology in a way
which seems simple but in fact is misleading regarding what we have
really measured.

I hope Alain has enough stamina to keep struggling for his favorite
model of  Omega_m \approx 1 as long as Narlikar, Burbidge and Hoyle
have struggled in favour of their model. But just as they brought out
the quasi-steady state model, I guess Alain will come up with the
quasi-Omega_m=1 model... ;)


I'm happy to see that on page 4, Alain has taken notice of my
repeated insistence that approximately flat is not exactly flat,
and that the present results can be approximately expressed as:

R_C = c/ [H_0 (|Omega_total - 1|)^1/2] > R_Horiz \approx 10h^-1 Gpc

or more vaguely as R_C > c/H_0 .

The footnote "a" is rather poorly written - the FLRW model is a
mathematical model. It is still true in cosmology that space is either
flat or it is not flat, the mathematics is still correct.

But saying "nearly flat" is a good habit - it's simply honest. Just as
the Earth has a nearly flat surface, the Universe seems to be nearly flat.


Still on the philosophy of science aspect, I should remind people that
it's rather inconsistent of Alain to insist on empirical measurements
when he considers empirical measurements of the global cosmological
parameters to be a low priority.


However, it remains that to ignore dissidents in astronomy is
extremely hypocritical - we all know the history of astronomy. In the
birthplace of Copernicus, we should be perfectly aware of this!



*measurements*

This is the most interesting bit, especially Fig 4 page 10. This is
where OCRA measurements from the SZ survey will be interesting.

They should hopefully give us independent estimates of the different
luminosity functions of clusters at different redshifts.

Whatever the explanation for Alain's analysis is, we're going to have
to understand it sooner or later if we want to get anything useful
from OCRA. My own guess is the non-Gaussianity of the tail of the
perturbation distribution, but until I start trying some calcuations,
I can't really say anything seriously.


BTW, I'm copying this to Alain just in case he feels like commenting.
(The .htaccess file fails so cosmo-torun became an open list de facto,
unless someone is really paranoid I suggest we keep it open.)


pozdrawiam
Boud



[fr]
Salut Alain, si tu souhaites savoir ce que fait notre petite équipe,
veuille aller sur :

http://adjani.astro.uni.torun.pl:9673/zwicky/TCfACosmology

La page sur OCRA se trouve ici, mais nous n'avons rien mis pour l'instant
sauf un lien vers quelques jolies images :

http://adjani.astro.uni.torun.pl:9673/zwicky/OneCmRA

Tu peux répondre sans ętre abonné, mais il faut confirmer au robot par
la suite.

Amitiés
Boud




On Thu, 9 Jan 2003, Andrzej Marecki wrote:

> Paper: astro-ph/0301137
> From: Blanchard Alain <alain.blanchard at 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
>

 


From amr w astro.uni.torun.pl  Wed Jan 22 09:14:42 2003
From: amr w astro.uni.torun.pl (Andrzej Marecki)
Date: Wed, 22 Jan 2003 09:14:42 +0100 (MET)
Subject: (fwd) Re: MAP data release?
Message-ID: <200301220814.JAA10907@galileo.astro.uni.torun.pl>

-- forwarded message --
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From: ebunn w lfa221051.richmond.edu
Subject: Re: MAP data release?
Approved: sci.astro.research-request w slimy.greenend.org.uk (mjh)
Sender: unknown w hercules.star.bris.ac.uk (Address not verified)
Organization: A poorly-installed InterNetNews site
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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 w star.bris.ac.uk>,
Jim Graber <jgraber w 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 w domain.edu, as opposed to name w machine.domain.edu.]
-- end of forwarded message --

-- 
-----------------------------------------------------------------------------  
Andrzej Marecki                | 
Torun Centre for Astronomy     |   e-mail: amr w 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
-----------------------------------------------------------------------------  
 


From boud w astro.uni.torun.pl  Wed Jan 22 17:46:24 2003
From: boud w astro.uni.torun.pl (boud)
Date: Wed, 22 Jan 2003 17:46:24 +0100 (MET)
Subject: grant proposal - first (incomplete!) draft
Message-ID: <Pine.SOL.4.44.0301221741340.8496-101000@hevelius.astro.uni.torun.pl>

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

-------------- następna część ---------
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Typ: application/postscript
Rozmiar: 113124 bytes
Opis: first draft - we need to discuss this
Adres: <http://cosmo.torun.pl/pipermail/cosmo-torun/attachments/20030122/d691dd50/attachment.ps>

From boud w astro.uni.torun.pl  Fri Jan 24 02:45:14 2003
From: boud w astro.uni.torun.pl (Boud Roukema)
Date: Fri, 24 Jan 2003 02:45:14 +0100 (MET)
Subject: grant meeting Fri 24.01 @14:00 
Message-ID: <Pine.SOL.4.44.0301240232120.9373-100000@hevelius.astro.uni.torun.pl>

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




 


From boud w astro.uni.torun.pl  Fri Jan 24 12:39:54 2003
From: boud w astro.uni.torun.pl (Boud Roukema)
Date: Fri, 24 Jan 2003 12:39:54 +0100 (MET)
Subject: grant meeting Fri 24.01 @14:00 
In-Reply-To: <Pine.SOL.4.44.0301240232120.9373-100000@hevelius.astro.uni.torun.pl>
Message-ID: <Pine.SOL.4.44.0301241237190.10883-201000@hevelius.astro.uni.torun.pl>

postscript and latex attached (in case anyone wishes to write
a better version...!)

boud


On Fri, 24 Jan 2003, Boud Roukema wrote:

> 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.
-------------- następna część ---------
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Typ: application/postscript
Rozmiar: 118195 bytes
Opis: g.ps  postscript
Adres: <http://cosmo.torun.pl/pipermail/cosmo-torun/attachments/20030124/c217dfe1/attachment.ps>
-------------- następna część ---------
%% ====================================================================
%% This LaTeX file was created by AbiWord.                             
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%%%%%%%%%%%%%%%%%%%
%%% personal definitions 
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\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}
\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 33}..months  (01.2004 -- 09.2006)
\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 zlotys{\footnotesize{} Polish zloty 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}

[200-300 kz\l{} seems reasonable, will depend on breakdown below]


\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 Radio 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, %  （国立天文台） 
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 Nov/Dec 1993: Visiting fellow, D.A.E.C., Observatoire de Paris - Meudon,
% France (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}

{\noin (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) %art %%IUCAA %%Lori.Johnston w ioppublishing.co.uk This is to let you know that your article has been published in CQG volume 17 (7 October 2000), issue 19, pages 3951--3963.

\item \pub \underline{Roukema, B.F.}, 2000c;;The Topology of the Universe;;Bulletin of the Astronomical Society of India;;28;;483 
%art  %%BASI
\ (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) %art %%IUCAA

\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) %art %%DARC/LUTH, IUCAA

\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
velocites 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 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 precise as possible. Just as the supernova type Ia
method was just one among many methods for measuring local cosmological
parameters, 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 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}



\begin{center}
\begin{tabular}{clcr}
No.  &
Name and description of task & Expected completion date (mm/yy)& 
Expected cost (z\l{})  \\
1 & purchase computer items & 12/2004 & 25 kPLN \\
Total & & & 25 kPLN 
\end{tabular}

\end{center}

\begin{flushleft}
\textbf{G. PROPOSED BUDGET}
\end{flushleft}

\begin{flushleft}
\begin{spacing}{1.24}

\end{spacing}
\end{flushleft}

\begin{center}
\begin{spacing}{1.24}



\begin{tabular}{lccc|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 &
42.167  & 42.167 & 31.622 & 115.956 PLN \\
{\footnotesize{}2/} Equipment      & 25k &  & &  25.000 PLN\\
{\footnotesize{}3/} Other direct costs &&&&\\
international cosmology consultants & 
20k &20k &20k &  60.000 PLN  \\
conferences, public relations & 
20k &20k &20k &  60.000 PLN  \\
Subtotal: & 107.167 & 82.167& 71.622  & 260.956 PLN \\
&&&&\\
{\bf 2} Indirect costs (admin costs to UMK - 25% 1st yrs; 30% 2nd, 3rd yrs)
&&&&\\
& 26.791 & 24.650  & 21.487 & 72.928 PLN \\
\hline
{\bf 3} Total costs (1+2) &&&& 333.884 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 33} person-months}
\end{flushleft}

Based on KBN guidelines, 100\% of 11500PLN/annum for the principal 
investigator if dr., 
75\% for other investigators if dr., 
50\% of 11500PLN/annum for other investigators if mgr.
Hence:

\begin{list}{(\roman{enumi})}{\usecounter{enumi}}
\item dr Boudewijn Roukema 11500PLN *2.75 = 31.625 PLN
\end{list}

\begin{flushleft}
{\em Staff {\bf 165} person-months}
\end{flushleft}

\begin{list}{(\roman{enumi})}{\usecounter{enumi}}
\addtocounter{enumi}{1}
\item dr Andrzej Marecki 7667PLN *2.75 = 21.083 PLN
\item mgr Magda Kunert 5750PLN *2.75 = 15.812 PLN
\item mgr Sebastian Soberski 5750PLN *2.75 = 15.812 PLN
\item mgr Marcin Gawro\'nski 5750PLN *2.75 = 15.812 PLN
\item (future mgr) Bartosz Lew 5750PLN *2.75 = 15.812 PLN (on condition
that mgr degree is awarded)
\end{list}

Total: 115.956 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).

Purchases are planned for 2004.

* 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) 1kPLN

* colour laserwriter/scanner/copier?   + 3yrs insurance (loss/theft/etc.)
7kPLN?

* portable computer (``notebook'')?  + 3yrs insurance (loss/theft/etc.)
10kPLN?

* non-portable computer - AMD Athlon?  + 3yrs insurance (loss/theft/etc.)
7kPLN 

Total:  25kPLN

(One year's spending up to (1+0.67 +4*0.5 = 3.67) *  13700 = 50 kPLN 
is within the limit of our group; so we are being extremely conservative
here.)


\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 and observational data on 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.


5 kPLN/month for international consultants in cosmology:

60 kPLN = 12 person-months

5 kPLN/month for presentation of our results at international
conferences, consultations with international experts in their
institutes

60 kPLN = 12 person-months



\begin{flushleft}

\end{flushleft}
\begin{flushleft}

\end{flushleft}

\begin{flushleft}
\begin{tabular}{ccc}
 {\em  Date} & {\em  Grantee organization	}&
  {\em Principal Investigator}; \\
 & Kierownik: &  dr Boudewijn Roukema \\
 & Prorektor ds Nauki i Wsp\'o\l{}pracy &  \\
 & z Zagranic\c{a}  & \\
 & prof dr. hab. Marek Zaidlewicz & \\
 & Kwestor mgr Henryk Heldt & \\

\\
\\
\\
& 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}

From boud w astro.uni.torun.pl  Mon Jan 27 23:49:30 2003
From: boud w astro.uni.torun.pl (boud)
Date: Mon, 27 Jan 2003 23:49:30 +0100 (MET)
Subject: grant appln revised: deadline wtorek 28.01 poludniu! more comments?
Message-ID: <Pine.SOL.4.44.0301272336420.13455-101000@hevelius.astro.uni.torun.pl>

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\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, %  （国立天文台）
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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From amr w astro.uni.torun.pl  Tue Jan 28 09:33:53 2003
From: amr w astro.uni.torun.pl (Andrzej Marecki)
Date: Tue, 28 Jan 2003 09:33:53 +0100 (MET)
Subject: RL/RQ quasar dichotomy
Message-ID: <200301280833.JAA00923@galileo.astro.uni.torun.pl>

Paper: astro-ph/0301526
From: Cirasuolo Michele <ciras w 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