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%\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}

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\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@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}

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