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%.IDENTIFICATION $Id: templatelarge.tex,v 1.3 2002/02/27 14:54:46 amchavan Exp$
%.LANGUAGE       TeX, LaTeX
%.ENVIRONMENT    ESOFORM
%.PURPOSE        Template application form for ESO Observing time.
%.AUTHOR         The Esoform Package is maintained by the Visiting 
%                Astronomers Section (VISAS) while the background software
%                is provided by the User Support System (USS) team.
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%                ESO PARANAL AND LA SILLA OBSERVATORIES
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%                   LARGE PROGRAMME PHASE 1 TEMPLATE
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%          PLEASE CHECK THE ESOFORM USERS' MANUAL FOR DETAILED 
%              INFORMATION AND DESCRIPTIONS OF THE MACROS. 
%     (see the file usersmanual.tex provided in the ESOFORM package) 
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%---- IMPORTANT NOTICE -------------------------------------------------
%-----------------------------------------------------------------------
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%
%            ====>>>>         ESO DEADLINE         <<<<====
%        ====>>>> October 1, 2002, AT 12:00 NOON C.E.T. <<<<====
%
%            This deadline is for proposals AND attachments 

%
%     ====>>>> TO BE SUBMITTED ONLY TO:  PROPOSAL@ESO.ORG <<<<====
% 
% By submitting this  proposal, the  Principal Investigator  takes  full
% responsibility for  the  content of  the proposal, in  particular with
% regard to  the names of CoI's  and the agreement  to act in accordance
% with the ESO policy and regulations, should observing time be granted.
% 
%-----------------------------------------------------------------------
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%
%    - LaTeX *is* sensitive towards upper and lower case letters.
%    - Everything after a `%' character is taken as comments.
%    - DO NOT CHANGE ANY OF THE MACRO NAMES (words beginning with `\')
%

\documentstyle{esoformlarge}
\def\lta{{\>\rlap{\raise2pt\hbox{$<$}}\lower3pt\hbox{$\sim$}\>}}
\def\gta{{\>\rlap{\raise2pt\hbox{$>$}}\lower3pt\hbox{$\sim$}\>}}
%
% The list of LaTeX definitions of commonly used astronomical symbols is
% already included  in the style files  esoform.sty (see Table 1  in the
% users' manual).  If  you have your  own macros or  definitions, please
% insert  them  here,    between   the \documentstyle{esoform}  and  the
% \begin{document} commands.
% 
%     PLEASE USE NEITHER YOUR OWN MACROS NOR ANY TEX/LATEX MACROS  
%       IN THE \Title, \Abstract, \PI, \CoI, and \Target MACROS.
%
% WARNING: IT IS THE RESPONSIBILITY OF THE APPLICANTS TO STAY WITHIN THE
% CURRENT BOX LIMITS AND ELIMINATE POTENTIAL OVERFILL/OVERWRITE PROBLEMS 
% 
\begin{document}

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%%%%% CONTENTS OF THE FIRST PAGE %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
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%
%---- BOX 1 ------------------------------------------------------------
%
% *** You should use this template for period 71A applications ONLY. ***
% DO NOT EDIT THE MACRO BELOW. 
\Cycle{71A}

%
% Type below, within  the curly braces {},  the title of your  observing
% programme (up to two lines).
%
% DO NOT USE ANY TEX/LATEX MACROS IN THE TITLE
% DO NOT USE ANY TEX/LATEX MACROS IN THE TITLE
% DO NOT USE ANY TEX/LATEX MACROS IN THE TITLE
\Title{The Great Observatories Origins Deep Survey:  ESO Public Observations
of the SIRTF Legacy/HST Treasury/Chandra Deep Field South}  

%
% Type below the   numeric code corresponding to the subcategory of your
% programme.  See for the complete description of the subcategories, the
% information  contained  in  the file  usersmanual.tex provided in  the
% ESOFORM package.
%
% E.g., \SubCategoryCode{B4} for a proposal linked to Galaxy Dynamics.
% 
\SubCategoryCode{A1}  

%
%---- BOX 2 ------------------------------------------------------------
%
% Type below a concise abstract of your proposal (up to 13 lines). 
%
% DO NOT USE ANY TEX/LATEX MACROS IN THE ABSTRACT
% DO NOT USE ANY TEX/LATEX MACROS IN THE ABSTRACT
% DO NOT USE ANY TEX/LATEX MACROS IN THE ABSTRACT
\Abstract{This proposal represents the continuation with VIMOS of the
ESO campaign to secure essential ground-based data for the
Great Observatories Origins Deep Survey (GOODS). Through ESO, the European
astronomy is playing a major role in this
public survey program, with raw and reduced data products to be
rapidly released to the community. GOODS combines
observations with three NASA Great Observatories ({\it HST}, {\it
SIRTF}, and {\it Chandra}), ESA's {\it XMM--Newton} and
ground--based telescopes to carry out an intensive study of galaxy
evolution and cosmology.  GOODS is designed to measure the evolution
of stellar mass content and star formation activity in galaxies from
$z\sim 5$ to $z\sim 0.5$; to map the emergence of the Hubble Sequence; 
to take a census of energetics from massive central black
holes in galaxies and study their role in galaxy evolution; and to
secure a large sample of SNe~Ia at $1.2<z<1.8$ to confirm or rule
out the accelerated cosmic expansion.  {\bf This specific program
with VIMOS will provide low-resolution spectra for redshift determination
for all $\sim 6000$ objects 
in the 160 arcmin$^2$ area of the GOODS field in the Southern hemisphere,
down to mag=25.} This public data set will allow the ESO
community to start cutting--edge research with GOODS data alone, as well as
to most efficiently plan for further follow--up studies with the VLT.}

% Please indicate below the total amount of time  (HOURS in Service Mode
% and for the   SEST, and NIGHTS  in  Visitor Mode) over all   requested
% semesters, e.g., \TotalAmountOfTime{25n} or \TotalAmountOfTime{155h}.
%
\TotalAmountOfTime{125h}

% Please  indicate  below the total  number of semesters over  which the
% observations have  to be distributed in   order to allow  a successful
% completion of your large programme, e.g., \TotalNumberOfSemesters{4}. 
%
\TotalNumberOfSemesters{3}

%
%---- BOX 3 ------------------------------------------------------------
%
% The  next  macro allows   the  description  of   the observing  run(s)
% necessary for the completion   of your program.   An observing  run is
% defined by the following sequence of parameters to be provided through
% a macro made  of nine pairs of  curly braces: ``run ID'',  ``telescope
% keyword'',   ``instrument'', ``time requested'', ``month preference'',
% ``moon      requirement'',   ``seeing  requirement'',   ``transparency
% requirement'', and ``observing mode''.
%
%
% 1. RUN ID.  
% Each   observing run  (up to  10)  required by  a   proposal should be
% identified by a different letter,  following the sequence A,B,C,...,J,
% as needed.
%
%
% 2. TELESCOPE KEYWORD. 
% Provide the keyword related to the required telescope(s), which are:
%
%               UT1   for the VLT UT1 (ANTU),
%               UT2   for the VLT UT2 (KUEYEN),
%               UT3   for the VLT UT3 (MELIPAL),
%               UT4   for the VLT UT4 (YEPUN),
%               3.6   for the ESO 3.6-m,
%               NTT   for the 3.5-m NTT,
%               2.2   for the ESO/MPI 2.2-m,
%               SEST  for the SEST.
%
%
% 3. INSTRUMENT. 
% Provide the keyword related to the required instrument, which are:
%
%               UT1:  FORS1               UT2:  UVES
%                     ISAAC                     FLAMES
%
%                                         UT4:  FORS2
%                                               NACO
%
%               3.6:  EFOSC2              2.2:  WFI    
%                     CES3.6                    FEROS
%                     TIMMI2            
%                                        
%               NTT:  SUSI2                 
%                     EMMI               SEST:  1.3Bolo               
%                     SOFI                          
%                                               
%
%               Any telescope:  Special  
%
% For visitors bringing their own Visitor Special Instrument, please use
% the   keyword ``Special''.  Remember to  fill   in the Visitor Special
% Instrument information page in Box 13.
%
%
% 4. TIME REQUESTED FOR THE FIRST SEMESTER.
% In order to allow for the automated scheduling  of proposals, you must
% provide the amount of time requested (HOURS in Service Mode and NIGHTS 
% in Visitor Mode,  except for SEST where it should always be HOURS) for 
% the first semester  of your  large programme.
% 
% FOR SERVICE-MODE PROPOSALS  AND SEST, provide at  this stage only  the
% total number of   hours requested, followed  by the  letter ``h''  for
% hours.    This should include also   the  time related  to any special
% calibrations   required  in  addition   to  the standard  calibrations
% provided  by ESO.    Any   more detailed information   about  possible
% particular scheduling   features  will be    provided during  Phase  2
% Service-Mode proposal preparation.
% 
% FOR VISITOR-MODE PROPOSALS, there is  no Phase 2 proposal preparation.
% Consequently,  you are  required  to provide already  in  Phase 1 some
% detailed information about  any particular scheduling features  needed
% for the successful completion of your programme.   You should code the
% amount of time requested (in nights) using the coding system described
% in the file usersmanual.tex provided in the ESOFORM package.
%
% E.g., 4n     (for 4 consecutive nights) is different from 
%       4n=4x1 (for 4 times 1 night with intervals in between) 
% 
%
% 5. MONTH PREFERENCE.
% Provide the first three letters of the month (e.g. jun) which would be
% your first preference  for scheduling.  Valid  months for the  current 
% period are from April (2003) to September (2003), for all instruments. 
% If you do not  have  any month  preference  simply  write ``any''.
%
% 6. MOON REQUIREMENT.
% Provide the required phase of the moon (see definitions on the Call for
% Proposals):  
%
%               d = dark time 
%               g = grey time
%               n = no restriction
%
%
% 7. SEEING REQUIREMENT.
% Provide  the maximum acceptable seeing value  in seconds of arc.  Your
% requirement must be one of the following values:
%
%               0.4   0.6   0.8   1.0   1.2   1.4
%               n = no restriction
%
%
% 8. TRANSPARENCY REQUIREMENT.
% Provide the transparency condition of  the atmosphere required  during
% your   observations.  A    programme requiring   accurate  photometric
% zeropoints may very  well need  only a subset  of the  exposures to be
% taken in  photometric  conditions, in  which case put  ``CLR''..  Your
% requirement must be one of the following values (see definitions on 
% the Call for Proposals): 
%
%               PHO = photometric, a perfect night 
%               CLR = clear sky, although with some rare clouds
%               THN = thin cirrus, inducing absorption up to 0.2 mag
%
%
% 9. OBSERVING MODE.
% Provide the required observing mode: v = visitor and s = service.
%
%
% ALTERNATIVE.
% If  the  use  of another  telescope  and/or   instrument could be   an
% acceptable alternative, then fill another line, with  the same run ID,
% following immediately the one of your prime choice and put an ``/alt''
% in the first pair of curly braces, just after the  run ID, in order to
% flag that this is only an alternative solution to the previous line.
%
%
% If   more than one   telescope  is needed for   the completion  of the
% programme,   then  fill as   many   lines   as  needed.  See   further
% explanations  in  the   file usersmanual.tex provided  in  the ESOFORM
% package.
%
% 
% E.g., \ObservingRun{A}{UT1}{FORS1}{40h}{apr}{d}{0.4}{PHO}{s}
%       \ObservingRun{A/alt}{NTT}{SUSI2}{8n=3x2+4H2}{jun}{d}{0.8}{PHO}{v}
%       \ObservingRun{B}{NTT}{SUSI2}{6n=6x1}{jul}{n}{0.6}{CLR}{v}
%
%
% NOTE FOR VIMOS USERS: Pre-imaging with VIMOS is required for subsequent 
% observation with the MXU. Pre-imaging is executed only in service mode; 
% the corresponding time must be requested as a separate run.
%
%
\ObservingRun{A}{UT3}{VIMOS}{1h}{aug}{d}{0.8}{CLR}{s} 
\ObservingRun{B}{UT3}{VIMOS}{10h}{sep}{d}{0.8}{CLR}{s} 
\ObservingRun{C}{UT3}{VIMOS}{10h}{sep}{d}{0.8}{CLR}{s} 
%
%---- BOX 4 ------------------------------------------------------------
%
% For the Principal Investigator (PI), provide below his/her initial(s),
% family name, present affiliation, the country  or organisation code of
% his/her present  institution,    and full  email   address.  For   the
% astronomers     working  for ESO   or  ESA,   the    acronyms of their
% organisations should be used instead of the  code of the country where
% they work.
% 
% Only the following country or organisation codes may be used:
%
%        B       Belgium
%        CH      Switzerland
%        D       Germany
%        DK      Denmark
%        F       France
%        I       Italy
%        NL      The Netherlands
%        S       Sweden
%        P       Portugal
%        RCH     Republic of Chile
%        UK      United Kingdom
%
%        AUS     Australia
%        USA     United States of America
%
%        ESA     European Space Agency
%        ESO     European Southern Observatory
%
%        OTHER   all other countries
%
% E.g., \PI{Initial1.}{Name1}{Paris Observatory}{F}{name@obspm.fr}  
%
% DO NOT USE ANY TEX/LATEX MACROS HERE
% DO NOT USE ANY TEX/LATEX MACROS HERE
% DO NOT USE ANY TEX/LATEX MACROS HERE
\PI{C.}{Cesarsky}{ESO}{ESO}{ccesarsk@eso.org}
%
% Provide below, for all the Co-investigators of this proposal (up to 25
% CoIs), their initials, family name,  present institution, and  country
% or organisation code of their present institution.  E.g.,
%
%       \CoI{Initial2.}{Name2}{Leiden}{NL}
%       \CoI{Initial3.}{Name3}{Geneva}{CH}   
%       \CoI{Initial4.}{Name4}{STScI}{USA}   
%       \CoI{Initial5.}{Name5}{ESO}{ESO}
%
% EACH LINE SHOULD CORRESPOND TO ONE PERSON ONLY  
%
% DO NOT USE ANY TEX/LATEX MACROS HERE
% DO NOT USE ANY TEX/LATEX MACROS HERE
% DO NOT USE ANY TEX/LATEX MACROS HERE
\CoI{J.}{Bergeron}{IAP}{F}
\CoI{S.}{Cristiani}{INAF}{I}
\CoI{L.}{da Costa}{ESO}{ESO}
\CoI{E.}{Daddi}{ESO}{ESO}
\CoI{M.}{Dickinson}{STScI}{USA}
\CoI{D.}{Elbaz}{CEA}{F}
\CoI{S.}{Ettori}{ESO}{ESO}
\CoI{R.}{Fosbury}{ST-ECF}{ESA}
\CoI{M.}{Giavalisco}{STScI}{USA}
\CoI{R.}{Hook}{ST-ECF}{ESO}
\CoI{H.}{Kuntschner}{ST-ECF}{ESO}
\CoI{B.}{Leibundgut}{ESO}{ESO}
\CoI{M.}{Nonino}{INAF}{I}
\CoI{A.}{Renzini}{ESO}{ESO}
\CoI{P.}{Rosati}{ESO}{ESO}

%\CoI{}{}{}{}

%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%% THE THREE PAGES OF THE SCIENTIFIC DESCRIPTION %%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
%---- BOX 5 ------------------------------------------------------------
%
% This is  the place where  the proposed  programme is  to be described.
% This description is  restricted to TWO pages and  is composed  of four
% different sections.
%
% A) Scientific rationale:    scientific  background  of the    project,
% pertinent  references;  previous work  plus  justification for present
% proposal.
%
% B) Immediate objective of  the proposal: state  what is actually going
% to be observed and what  shall be extracted  from the observations, so
% that the feasibility becomes clear.
%
% C) Justification for the  use of  the  selected telescope (e.g.,  VLT,
% NTT, etc...)  with respect to other available alternatives.
% 
% D)  Justification for    the  observing  mode requested   (Visitor  or
% Service).
%
% Use the simplified abbreviations for references as in A&A. 
%
%            THIS DESCRIPTION IS RESTRICTED TO THREE PAGES 
%
%   THE RELATIVE LENGTHS OF EACH OF THESE FOUR SECTIONS ARE VARIABLE,
%              BUT THEIR SUM IS RESTRICTED TO THREE PAGES
%
\ScientificRationale{ The first part of this section replicates the
basic information on the GOODS project, as from the GOODS Large
Programme proposal submitted for P70, approved by OPC, and and
currently being carried out. Updates, whre needed, are in {\it
italic}.  The P70 proposal had illustrated the integrated strategy for
a complete, low-resolution spectroscopic follow-up first with FORS2
(in P70) and then with VIMOS (in P71 and following periods). VIMOS is
now being offered, and the current proposal describes the GOODS
strategy with this instrument. {\bf Quotation from P70 proposal begins
here}.

\underbar{\bf GOODS in Context:} 
The Great Observatories Origins Deep Survey (GOODS) is a public,
multi--facility project that aims to answer some of the most profound
questions in cosmology: How did galaxies form and assemble their stellar mass?
When was the morphological differentiation of galaxies established and how did
the Hubble Sequence form?  How did AGN form and evolve, and what role do they
play in galaxy evolution?  How much do galaxies and AGN contribute to the
extragalactic background light?  Is the expansion of the universe dominated by
a cosmological constant?

A project of this scope requires large and coordinated efforts from many
facilities, pushed to their limits, to collect a database of sufficient
quality and size for the task at hand. It also requires that the data be
readily available to the worldwide community for independent analysis,
verification, and follow--up. To accomplish this, NASA proposed a new concept
for large--scale investigations: the Legacy/Treasury programs.  These are
defined as (1) large, coherent science investigations, not reproducible by any
reasonable number or combination of smaller General Observer programs; (2)
programs whose archived scientific data are of general and lasting importance
to the broad community; and (3) programs for which all raw and 
pipeline--processed data {\bf must enter the public domain immediately},
enabling timely and effective opportunities for follow--on observations and
archival research.

Among the approved Legacy/Treasury projects, GOODS
(http://www.stsci.edu/science/goods) is a deep, high latitude survey to study
cosmology and galaxy evolution.  The program targets two carefully selected
fields, the Hubble Deep Field North (HDF--N) and the Chandra Deep Field South
(CDF--S), with the three NASA Great Observatories ({\it HST}, {\it SIRTF} and
{\it Chandra}), ESA's {\it XMM--Newton}, and a wide variety of ground--based
facilities (see Table~1). The area common to all the observing programs is
320~arcmin$^2$, equally divided between the N and S fields. For an overview 
of GOODS, see Dickinson et al. (astro-ph/0204213) and Renzini et al. 
(astro-ph/0204214).

European collaboration was established in all major components of GOODS
since its inception, including the {\it SIRTF} Legacy Program 
(P.I.\ M.\ Dickinson; 647 hours of observing time), and the 
{\it HST} Treasury Program (P.I.\ M.\ Giavalisco; 398 orbits).
Given the public nature of the survey and the importance of wide community 
involvement, European participation at large was also stimulated through an
Open Letter, emphasizing the importance of coverage from the observatories 
at La Silla and Paranal for Legacy programs with substantial involvement 
from the ESO community 
(http://http.hq.eso.org/observing/misc/20000824.sirtf.html). 

Ground--based observations are an integral part of GOODS.  The Legacy 
project was allocated multi--year blocks of NOAO time for deep optical 
and infrared imaging, including critical $U$--band imaging, 
which cannot be done with ACS.  ESO allocated 298h of near--IR imaging
of the CDF--S with ISAAC in P68-70-72, and 40h of optical imaging with WFI to
reach deeper flux limits compared to the EIS data on the same field (see 
Table 1).  With this proposal, we seek to secure one of the most important 
parts of the whole project, namely spectroscopic observations for redshift 
identification in the CDF--S.

\medskip
\underbar{\bf Science with GOODS:} 
Each segment of the GOODS project aims at major scientific goals. 
Here we review some of these, with emphasis on the data from the CDF--S.

\medskip

$\bullet$ {\it SIRTF}/IRAC data from $3.6$ to $8.0\mu$m will sample the
rest--frame near--IR light (e.g., $K$--band at $z \sim 3$) of $\sim L^\ast$
galaxies out to $z \sim 5$, providing the best measure of stellar mass
to reconstruct the mass assembly history of galaxies from $z\sim 5$ to 
$z\sim 0.5$. {\it SIRTF} CDF--S observations are planned for 
Aug 2003 -- Feb 2004.

$\bullet$ 24$\mu$m {\it SIRTF}/MIPS data will detect dust--obscured star
forming galaxies and AGN with a $6^{\prime\prime}$ FWHM beam, locating them to
$\sim 1^{\prime\prime}$ accuracy and enabling the identification of
optical/near-IR/X-ray/radio counterparts.  ISOCAM 15~$\mu$m surveys studied
obscured star formation at $z \sim 1$; GOODS 24~$\mu$m data will extend this
work to $z \approx 2.5$ by probing the rest--frame 7.7~$\mu$m PAH emission
from relatively ``ordinary'' starburst galaxies.

$\bullet$ {\it HST}/ACS {\it is now imaging} the GOODS field in the
F435W ($B$), F606W ($V$), F775W ($i$), and F850LP ($z$) bands with
``near--HDF'' sensitivity.  The observations (see Fig.\ 2) are phased
in 5 epochs (with the CDF--S in the period Aug 2002 -- Feb 2003) to
allow detection of type~Ia supernovae at $1.2<z<1.8$ to test the
transition from decelerated to accelerated expansion predicted in
``dark energy'' cosmological models.  Deep, high--resolution imaging
will trace the emergence of the Hubble Sequence, gather a census of
Lyman break galaxies (LBGs) out to $z \approx 6.5$ (i.e.\ approaching
the reionization epoch), and provide a rich resource for studying the
cosmic mass distribution via weak gravitational lensing. {\it At the
time of submitting this proposal complete data for the first three
epochs have been successfully completed, and the reduced data for the
first epoch have been publicly released.}

$\bullet$ Deep $JHK_s$ imaging with ISAAC over the GOODS/CDF--S bridges
the wavelength gap between ACS and {\it SIRTF}, providing optical
rest--frame photometry for high redshift galaxies.  Data for about 1/3
of the field have already been taken in P68 and have been made immediately
publicly available from the ESO/GOODS URL (www.eso.org/science/goods).
The preliminary (V0.5) version of the coadded and reduced frames have
{\it been released in March 2002}. These include $JK_s$ data for part of the 
field from another program (PI E.\ Giallongo), whose PI kindly waived his
proprietary rights.  
%{\it The delivery of V1.0 is planned for the end of
%July 2002, and will include mosaiced images and source catalogs.}

\medskip

Besides the above data taken explicitly for the GOODS project, other
complementary data on the two GOODS fields are publicly available or
are now being collected.  These include:

\medskip

$\bullet$ The deepest {\it Chandra} (1--2 Msec) and {\it XMM--Newton}
(225--500 ksec) X--ray observations.  Using these X-ray data, the sample 
of SIRTF 24~$\mu$m-selected sources will be ``sorted'' among starburst 
galaxies and AGN, enabling a census of energetic output from both types 
of objects, and a determination of the relative abundance of type 2 
(obscured) vs.\ type 1 (unobscured) AGN at the ``quasar epoch'' 
($z \sim 2$--3).

$\bullet$ Far-UV (135-180 nm) and Near-UV (180-300 nm) imaging of the
GOODS fields will be secured by GALEX, to be launched by NASA in {\it February
2003}.

$\bullet$ Radio observations, including data from the VLA and new CDF--S
observations from the ATCA.

$\bullet$ The {\it SIRTF}/SWIRE Legacy Project.  While shallower than 
GOODS, it includes a much larger (7.2~deg$^2$) field around the
CDF--S, with ESO supporting optical imaging from WFI (PI A.\ Franceschini).

$\bullet$ The COMBO-17 project, having imaged a $30^\prime\times30^\prime$
region around CDF--S through 17 broad and intermediate-band filters, 
will observe this area with {\it HST}/ACS through F606W and F850LP
as a Large Program ({\it GEMS}, PIs K. Meisenheimer \& H.-W. Rix).   


%The PI  has decided to refrain 
%from submitting a FORS2 spectroscopic proposal for
%P70, declaring that the data proposed here for the GOODS project will 
%satisfy their immediate needs. 

\medskip

From this list it is clear that GOODS offers an absolutely unique combination
of area, depth, angular resolution and wavelength coverage for studying the
distant universe. GOODS is arguably the most ambitious, complete and coherent
attempt to understand fundamental cosmology and galaxy formation and evolution
for many years to come. The GOODS data base will set the ground for a variety
of follow--up programs from future facilities such as NGST and ALMA.

Clearly, imaging alone is not sufficient to reach GOODS scientific
goals.  Spectroscopy is essential to get reliable redshifts, which provide 
the time coordinate needed to delineate the evolution of galaxy masses, 
morphologies, and star formation.  It will also calibrate the photometric 
redshifts that can be derived from the 13--band imaging data at 
0.36--8$\mu$m.   Spectroscopy will measure physical diagnostics for
galaxies in the GOODS field (e.g., emission line strengths and ratios 
to trace star formation, AGN activity, ionization, and chemical abundance; 
absorption lines and break amplitudes that reflect stellar population ages).
Precise redshifts are also indispensable to properly plan for future 
follow--up at higher dispersion, e.g., to study galaxy kinematics or 
detailed spectral line properties.

Among southern hemisphere observatories, ESO has unparalleled spectroscopic
multiplex.  It is therefore proposed that ESO will lead the southern campaign
with an effort proportional to the unique capabilities of its VLT.  In the
same spirit as the multiwavelength GOODS imaging programs, we aim to 
collect and disseminate a public data resource of low resolution spectra
for {\it all} the objects in the GOODS/CDF--S field which can feasibly be
observed.  As demonstrated below, this can be achieved with a rather modest
investment of VLT time.  Given the size of the GOODS/CDF--S field, the
field of view of the VLT multiobject spectrographs, and the number of feasible
targets, we argue that this campaign is most efficiently done as a single
project, as opposed to a set of several smaller projects each selecting
targets according to different criteria. For a project of the scientific
importance of GOODS, we argue that {\bf completeness} and {\bf uniformity} of
the low--resolution spectroscopic database is mandatory.

The ESO/GOODS spectroscopic program is a complete,
magnitude--limited survey, observing all galaxies for which VLT
optical spectroscopy is likely to yield useful data ({\it
i.e. redshifts}). The program will make full use of the VLT instrument
capabilities (FORS2 and VIMOS), matching targets to instrument and
disperser combinations in order to maximize the effectiveness of the
observations.  The magnitude limits and selection bandpasses depend to
some degree on the instrumental setup being used. {\it The aim is to
reach mag = 25 with adequate S/N, with this limiting magnitude being
in the $B$ band for objects observed with the VIMOS LR-Blue grism, in
the $V$ band for those observed in the LR-Red grism, and in the $z$
band for the objects being now observed with FORS2.}  This is not only
a practical limit, however, but is also well matched to the scientific
aims of the GOODS program.  The ACS $i$-band imaging will sample
rest--frame optical ($B$--band) light out to $z = 1.2$, where $i_{AB}
= 25$ reaches 1.5 to 2 magnitudes past $L^\ast_B$.  This is also the
practical limit for high--quality, quantitative morphological
measurements from the ACS images (cf.\ Abraham et al.\ 1996).
Similarly, $i_{AB} = 25$ is $\sim 1$~mag fainter than the measured
$L^\ast_{UV}$ for $z = 3$ LBGs, and 0.5~mag fainter than that at $z =
4$ (Steidel et al.\ 1999).  These are the limits to which GOODS/{\it
SIRTF} IRAC data will robustly measure rest--frame near--IR light, and
hence constrain the stellar mass.  The proposed ESO spectroscopy will
therefore target galaxies to luminosities where the {\it HST} and {\it
SIRTF} data will be most valuable.

Certainly, low-resolution spectroscopy alone will not answer all the
scientific questions that will arise by studying the GOODS database.
Spectroscopy at higher resolution than that proposed here will be necessary to
derive dynamical masses for high redshift galaxies (from rotation curves of
spirals and velocity dispersion of spheroids), chemical compositions of
passively evolving and star-forming galaxies, detailed stellar population
indices, etc.  However, such projects are sufficiently diverse and 
self--contained that they may be carried out more effectively with 
dedicated follow--up programs.  As a public survey, GOODS will concentrate on
low--resolution spectroscopy for the purpose of redshift identification.
These data, together with the multiwavelength imaging from ground--
and space--based observatories, will then promote both archival research
and dedicated programs of follow--up observations.   ESO will make every 
effort to promote effective coordination among those teams from the community 
that aim to submit such proposals, and hence a more efficient use of the 
VLT.

{\bf End of quote from P70 proposal}.


}
\ImmediateObjective{

Two spectrographs are needed to carry out the GOODS observing program,
namely 1) VIMOS, the workhorse instrument due to its uniquely large 
multiplexing power, which will be used every time that extreme red sensitivity 
is not key to the success of the observations; and 2) the newly refurbished 
FORS2, when its unique sensitivity at red wavelengths is required. 
While the observing time has already been allocated on FORS2 in P70, and the
observations are under way (data can already be retrived from

www.eso.org/science/goods/products.html\#spectroscopy, see also Fig. 3),
here we provide a description of the 
overall observing program with both instruments, as currently envisaged.

To the limits of VIMOS spectroscopic capability 
(say, $V_{\rm AB}=25$), there are $\sim 6000$ objects over the 160 arcmin$^2$ 
of the GOODS field, or $\sim 37$ arcmin$^{-2}$. This is $\sim 10\times$ higher 
than the surface density of VIMOS slits ($\sim 800/224=3.6$ arcmin$^{-2}$). 
Hence, more than 10 masks per pointing are necessary to ensure virtual
completeness in the spectroscopic survey.
Moreover, the VIMOS field of view ($16'\times 18'$, with a cross gap of $2'$ 
between the quadrants) is such that only 50\% of it can overlap with the 
$10'\times 16'$ GOODS field. So, up to 400 objects at a time could be 
observed.  We calculate that $\sim 24$ VIMOS {\it masks, 6 for each of
4 pointings} are necessary to ensure 
$\sim 90\%$ completeness in the spectroscopic coverage of $\sim 6000$ targets 
in the GOODS field, with the extra bonus of longer--than--average integration
times on sources located in 45\% of the field (Renzini et al.\ 2002, 
astro-ph/0204214).  With an average integration time of 4h per pointing, 
and $\sim 30\%$ overhead, this makes a total of 125h, or $\sim 13$ nights.  
%The whole VIMOS survey  is just above the minimum size
%for a Large Program, while rendering CDF--S unique in terms of
%combination of depth and spectroscopic redshift completeness.

As mentioned above, there are three possible instrument/disperser combinations
to carry out the GOODS low-resolution spectroscopic survey: VIMOS/LR-Blue, 
VIMOS/LR-Red, and FORS2, and in order to maximize the efficiency of the survey
a strategy is needed to identify the setup of choice for each target. 
Figure 1 shows the total instrument+telescope throughput 
for these three options, and Table 2
summarizes the situation. It shows that $\sim 60\%$ of the objects are best
observed with VIMOS/LR-Red, $\sim 30\%$ with VIMOS/LR-Blue, and $\sim 10\%$ 
with FORS2. 
The P70 GOODS proposal was focused 
on the FORS2 observations dedicated to objects best observed with this 
instrument, i.e. those with $(R-I)_{\rm AB}>1$ and $I_{\rm AB}<25$. In 
practice, for the observations being carried out in P70 it was decided to use
the superior GOODS/ACS data already publicly available, hence the actual 
selection 
has been $(i-z)_{\rm AB}>0.6$ and $z_{\rm AB}<24.5$ with $\sim 450$ galaxies
fulfilling this criterion. Also for the GOODS/VIMOS
spectroscopic observations the targets will be selected from the GOODS/ACS 
catalogs.

For the observation with VIMOS a simple color criterion would not ensure
the best target-to-setup assignement, and a more refined, two step strategy 
will be applied. Step 1: On the basis of photometric redshifts (from
GOODS publicly available $UBVizJHK$ data) the $\lambda$-range in which
the key spectral features are expected will be identified, and following
Table 2 $\sim 2/3$ of the objects will be observed first with VIMOS red and 
$\sim 1/3$
with VIMOS blue, primarily in P71+P72. Step 2: Objects 
which fail to yield redshifts in P70-72 will be re-observed in P74 
with the complementary grism. No observations are planned for P73. It is also 
planned to reach down 
to $B<25$ for objects observed with the blue grism and to $V<25$  for those 
with the red grism.
}
\TelescopeJustification{Spectroscopy of so many objects down to the stated
limiting magnitudes requires VLT+VIMOS.}
\ModeJustification{Service mode is preferable, given that the S/N of faint
object spectra will critically depend on the seeing. However, visitor mode
will also be acceptable.}

%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%% THE TWO PAGES OF THE ATTACHMENTS %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
% Up  to TWO pages of  attachments made of encapsulated PostScript files
% (e.g., figures),  to be submitted   as PostScript files  only, can  be
% added, using   the following commands.    These PostScript  files  (no
% color, black-and-white only) will be submitted separately by email, as
% soon  as the PI  has received back the proposal  ID [e.g.  69.B-1234].
% If the  attachments  do  not  reach ESO   within 12  hours   after the
% successful  submission   of the  Latex   file,  the  proposal will  be
% processed and refereed by the OPC without attachments.  See the users'
% manual for a complete   description of the submission of  attachments.
%
% COLOR POSTSCRIPT ATTACHMENTS ARE NOT SUPPORTED: WILL BE PRINTED IN B&W
%
% E.g.:
%
%  \MakePicture{galaxy.ps}{Fig.1 - Galaxy NGC 9999}{width=15cm,
%                                                 height=8.0cm,angle=90}
%  \MakeCaption{Fig.1  This is a very brief caption.}
%
\MakeCaption{
\begin{center}
{\bf Table 1: GOODS Observations and Complementary Data Sets.}


\renewcommand{\arraystretch}{1.4}
\setlength\tabcolsep{5pt}
\begin{tabular}{lll}
\hline\noalign{\smallskip}
Wavelength & Facility & Sensitivity (S/N=5) \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}

0.36$\mu$m      & KPNO+CTIO 4m          & AB = 27.3  ($U$) \\
0.4-0.9$\mu$m   & {\it HST}/ACS         & AB = 27.9, 28.2, 27.5, 27.4$^{\mathrm a}$ ($BViz$)\\
1.2-2.2$\mu$m   & VLT, KPNO 4m          & AB = 25.2, 24.7, 24.4 ($JHK_s$) \\
3.6-8.0$\mu$m   & {\it SIRTF}/IRAC      & AB = 24.5, 24.5, 23.8, 23.7 
                                          (0.6--1.2 $\mu$Jy)$^{\mathrm b}$ \\
24$\mu$m        & {\it SIRTF}/MIPS      & 20-80 $\mu$Jy$^{\mathrm c}$ \\

\noalign{\smallskip}
\hline\noalign{\smallskip}
Type & Facility & Notes \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}

Spectroscopy    & VLT, Gemini, Keck     &  Various PIs; GOODS programs \& collabs. \\
X-ray           & {\it Chandra}, {\it XMM}  &  Public {\it Chandra} data and {\it XMM} GTO progs.\\
70, 160$\mu$m   & {\it SIRTF}/MIPS      &  {\it SIRTF} GTO program;  SWIRE Legacy program \\
Sub-mm          & SCUBA, SEST           &  Various PI programs \\
Radio           & VLA, ATCA             &  Various PIs; CDF--S observs.\ in progress \\

\noalign{\smallskip}
\hline

\end{tabular}
\end{center}
\smallskip\noindent
\hskip 2 truecm $^{\mathrm a}$ For 0.5 arcsec diameter aperture \par\noindent
\hskip 2 truecm
$^{\mathrm b}$ For ``handbook'' IRAC PSF;  3.6 and 4.5$\mu$m performance 
may be better \par\noindent
\hskip 2 truecm
$^{\mathrm c}$ Uncertain sensitivity; depends on instrument performance and 
source confusion
}
%\vspace*{-1.0 truecm}
\noindent

\MakeCaption{\begin{center}
{\vspace*{-1.0 truecm}\bf Table 2: Most Effective Instrument Setups vs Redshift}

\renewcommand{\arraystretch}{1.4}
\setlength\tabcolsep{5pt}
\begin{tabular}{lrll}
\hline\noalign{\smallskip}
Redshift & Fraction  & Key Features & Instrument/grism \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}

$z < 0.5$&24\% &[OII], H$\beta$, [OIII], (H$\alpha$), CaII H\&K & VIMOS blue \\
$0.5 < z < 1.3$  &  56\% & [OII], H$\beta$, CaII H\&K   & VIMOS red/FORS2 \\
$1.3 < z < 2.3$  &  12\% & [OII], CaII H\&K; CIV, AlII & 
                                           FORS2/FORS1-UV(?)$^{\mathrm a}$\\
$ 2.3 < z < 3.5$ &  6\%  & Ly$\alpha$, SiII, CII, CIV, OI, SiIV & VIMOS blue \\
$z > 3.5$        &  1\%  & Ly$\alpha$, SiII, CII, CIV, OI, SiIV& VIMOS red/FORS2\\
\hline
\end{tabular}
\end{center}
This table shows for the various redshift intervals the fraction of galaxies
in a $R=25$ limited sample (from photometric redshifts), the features most 
useful for 
redshift determination, and the most appropriate instrument/grism combination
for detecting such features.

$^{\mathrm a}$ In this range the lack of a near-IR spectrograph and of a 
UV-optimized spectrograph will limit somewhat 
the capability of measuring the redshift of intrinsically red and blue 
galaxies, respectively.


}
\vspace{-1cm}

\MakePicture{grismsbw.ps}{Fig.\ 1 - The VIMOS and FORS2 
throughput for the grisms adopded for the GOODS survey.}
{height=6.0cm,angle=0}
\MakePicture{vimcarpet.eps}{Fig.\ 2 - The VIMOS field of View and its
4-pointing imprint over the GOODS field.}
{width=12.0cm,angle=0}
\MakeCaption{{\it Left:} The geometry of the VIMOS field of view, for either 
imaging or multiobject spectroscopy. {\it Right:} The CDFS/GOODS
$10'\times 16'$ field, in the same scale as the VIMOS FoV. The VIMOS 4-pointing
imprinting on the GOODS field is rendered with
different shadings. Dark areas: areas common to all 4 VIMOS basic
pointings (A set of subfields). Shaded areas: areas common to 2 VIMOS
pointings (B set of subfields). Lightly shaded areas: areas covered by
only one VIMOS pointing (C set of subfields). Subfields A
will be covered by all the 24 planned masks, subfields B by 12 masks,
and subfields C by 6 masks only. Correspondingly, spectra will be
obtained for $\sim 100\%$ of targets down to mag$\sim 25$ in area A,
for $\sim 85\%$ in area B, and for $\lta 60\%$ in area C. The actual 
efficiency may be somewhat reduced in area B when using the blue grism, 
as for each pointing there will relatively few objects to observe, i.e.
$\sim 3$ times the maximum number of slits.} 
\MakePicture{fors2spec.ps}{Fig.\ 3  - A sample of GOODS/FORS2 spectra.}
{height=6.0cm,angle=0}
\MakeCaption{These spectra have been obtained during the October 2002 run
of the GOODS program with FORS2, and have been retrived from the ESO public
archive. The sky-subtracted spectra shown here come
from only one of the two FORS2 CCDs.}
%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%% THE PAGE OF BOXES 6, 7, AND 8 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
%---- BOX 6 ------------------------------------------------------------
%
% Indicate  below  the  experience  of the  applicants  with telescopes,
% instrumentation,  and data reduction.
%
\Experience{Many of the proposers have extensive experience with deep
multiobject spectroscopy of faint targets
with the VLT and other facilities, and are well versed in the reduction
of these sorts of data.  Moreover, many have lead or contributed to major
surveys with rapid public data releases, such as the HDF and EIS programs.}

%
%---- BOX 7 ------------------------------------------------------------
%
% Indicate  below the  strategy  for data  reduction  and  analysis with
% description of the available resources to the observing team, such as:
% computing capabilities, research assistants, etc...
%

\Resources{ESO shall take responsibility for the whole data taking,
reduction, and prompt dissemination world--wide, both in the spirit of
Legacy/Treasury Programs and as a firm commitment to its own
community. The list of targets, maps, etc. will be posted on the
ESO/GOODS web well in advance of the observations.  The immediate
public release of the raw data will be made using the standard
resources of the ESO archive.  For the processing and prompt
dissemination of the spectroscopic data, a dedicated team is being
established including -- besides the proposers -- a suitable number of
scientists from the ESO community.  This opportunity will also be
widely advertised through the web and The Messenger, and it is ESO
commitment to achieve the widest possible involvement of the community
in the data production process. Data products will include reduced,
coadded, calibrated and extracted spectra.  The Team will be committed
to exploit VIMOS/FORS pipeline tools, experiencing an in-house
scientific validation of such tools and provide feedback to the
pipeline producers.  Besides working as an early testbed for
pipelines, the GOODS project is already offering to the AVO project
data to start built ``bottom-up'' Virtual Observatory tools using top
quality data in wide demand.  Funding will be requested from the EC
for Fellowships associated with the exploitation of GOODS data.}


%
%---- BOX 8 ------------------------------------------------------------
%
% Take advantage of  this box to provide  any special remark  (up to ten
% lines).
% In  case of coordinate observations with XMM, please specify here both
% the ESO period (P69, P70, or P71) and  the  preferred  month  for  the
% observations. 
%
\SpecialRemarks{Two other major European programs are underway on the
CDF-S field and are submitting VIMOS proposals: the follow-up of XMM X-ray 
sources and optically selected AGNs (PI J. Bergeron) and the VIMOS follow-up
of the COMBO17/GEMS 
project (PI M. Barden). To avoid overlap with GOODS, the PIs of these
two projects have decided to refrain from submitting a proposal for
VIMOS low-resolution spectroscopy, and will concentrate on
intermediate- and high-resolution spectroscopy, expecting sufficient
low-resolution data will be made publicly available from GOODS. GOODS
is a community-service project, and it is very important that the
community is widely involved. ESO resources will be used to attract
young scientists to ESO to participate in the preparation of the
observations and data reduction efforts. Information for and from the
community is organized through the Web, as well as through focused ESO
workshops, the first one on ``The Mass of Galaxies at Low and High
Redshift,'' was held in the fall of 2001. A second such workshop is
now planned for 2003 on ``Multiwavelength Mapping of Galaxy Formation
\& Evolution''.

}

%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%% THE PAGE OF BOXES 9 AND 10 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
%---- BOX 9 ------------------------------------------------------------
%
% Provide below a careful justification of the requested lunar phase and
% of the    requested number of  nights  or  hours.   ESO  Exposure Time
% Calculators exist for all  Paranal and for  some La  Silla instruments
% and are available at the following web address:
%                 http://www.eso.org/observing/etc
% In relation to the telescope(s) and instrument(s)  to be used,  please
% indicate  what version  of the  ESO Exposure Time  Calculator you have
% used.  Do  not include any   correction for unexpected  meteorological
% conditions.
%
\WhyLunarPhase{For the deep optical spectroscopy of the faint galaxies
in the field dark time is mandatory.}

\WhyNights{The telescope time is set by two requirements: 
completeness down to the limiting magnitude, and adequate S/N.
The target sample 
consists of $\sim 6000$ galaxies down to $B$ (or $V$)=25.
The layout of the VIMOS FoV is shown in Fig. 2:  
a minimum of 4 VIMOS
pointings is necessary to ensure that all parts of the GOODS field  are
covered by at least one of 
the pointings. The chosen
pattern consist of 4 VIMOS pointings in which in turn each of the 4
outer corners of the VIMOS FoV coincides with each of the 4 GOODS
field corners. For each pointing, the central cross gaps of VIMOS separate 4
sub-fields over GOODS, for a total coverage of 112 arcmin$^2$. 
Hence,
for each pointing, 
the fraction of the VIMOS low resolution multiplex
expendable on GOODS is 112/224 (50\%,), i.e., with an {\it effective
multiplex} $0.5\times 800=400$.
These 4 pointings  imprint on the GOODS field a set of
subfields, with some being common to all 4 pointings (set A, 45\% of GOODS), 
some only to 2 pointings (set B, also 45\% of GOODS), and 2 subfields are 
covered by 
only one pointing (set C, 10\% of GOODS). This is also shown in Fig. 2.
For a set of 6 masks for each of the 4 pointings, all targets 
in A subfields can be observed at least once, and some twice, i.e. for a 
total 8h integration; we estimate that $\sim 85\%$ of 
all targets in B  subfields can be observed once, while only $\lta 60\%$
of targets in subfields C could be observed. Hence, with a total 
of $6\times 4=24$ sets of masks one can ensure $\sim 90\%$ completeness 
over the whole field. In any case, priority in slit assignement will be given 
to observe objects with $z_{\rm phot}\gta 0.5$, including LBGs, EROs, AGN
candidates, and few objects with special characteristics.

The current exposure VIMOS time calculator has been used under default 
assumptions (i.e., new moon, 1.2 airmass, $0''.8$ seeing, 
$1^{\prime\prime}$ slit, point sources) using elliptical,
Sb, and starburst galaxy templates redshifted to $z>1$. For both $B=25$
objects with the LR-Blue grism and $V=25$ objects with the LR-Red grism 
one reaches S/N$>10$ per resolution element (3-4 pixels).
The overhead is 17m per observation (from VIMOS web). To reach 4h 
integration per mask 4 OBs, 1h each, are necessary, hence the overhead is 68m
per mask. The total telescope time is therefore $24\times (240+68)$ min =
7392 min = 123h, or $\sim 13$ nights. 
For the pre-imaging, 4 exposures 15m each are necessary, or 22m including
7m overhead, for a total of 68m, i.e. $\sim 1$h.
{\bf NB: for the targets lying inside the VIMOS FoV but outside the GOODS field
the same selection criteria as for the GOODS field will be followed.
ACS COMBO17/GEMS data are publicly available,
and the  COMBO17/GEMS team will provide the astrometric catalogs for mask 
preparation.}
}

% Proposals   asking for  observations in  Service   Mode may need  more
% calibrations than   the   standard  calibrations provided    with  the
% automated  data reduction  pipelines.   Please,  uncomment one  of the
% following two macros.  In the case of special calibrations, the amount
% of time needed   to carry them out  should  be included in   the total
% amount  of time requested in Box  3 and some explanations/descriptions
% should be  provided  between the  curly braces  at    the end of   the
% corresponding macro.
%
%\StandardCalibrations
\SpecialCalibrations{Do we need special calibrations???????}

% If the  OPC   does  not allocate any  observing   time  to your  large
% programme, would you agree to see it  reviewed by the  OPC as a normal
% programme ?  Please,  uncomment in any case one  of  the following two
% macros:
%
%\ConvertLargeToNormal
%\DoNotConvertLargeToNormal

%
%---- BOX 10 -----------------------------------------------------------
% 
% Applicant's  publications related to   the  subject of this  proposals
% during  the past  two years.   Use  the  simplified  abbreviations for
% references   as in A&A.  Separate  each   reference with the following
% usual LaTex command: \smallskip\\
%
%   {
%   Name1 A., Name2 B., 2001, ApJ, 518, 567: Title of article1
%   \smallskip\\
%   Name3 A., Name4 B., 2002, A\&A, 388, 17: Title of article2
%   \smallskip\\
%   Name5 A. et al., 2002, AJ, 118, 1567: Title of article3
%   }
%
\Publications{
Cristiani, S., Appenzeller, I., Arnouts, S., et al.\ 2000,
A\&A, 359, 489:
``The first VLT FORS1 spectra of Lyman-break candidates in the HDF-S
and AXAF Deep Field.''

\smallskip
Daddi, E., Cimatti, A., \& Renzini, A., 2000,
A\&A, 362, L45:~~
``EROs and the formation epoch of field ellipticals.''
\smallskip

Elbaz, D., Cesarsky, C., Fadda, D, et al.\ 1999,
A\&A, 351, L37:
``Source counts from the 15~$\mu$m ISOCAM Deep Surveys.''
\smallskip

Ferguson, H.C., Dickinson, M., Williams, R., 2000, ARA\&A, 38, 667:
``The Hubble Deep Fields.''

Genzel, R., \& Casarsky, C.\ J., 2000,
ARA\&A, 38, 761:
``Extragalactic Results from the Infrared Space Observatory.''
\smallskip

Giacconi, R., Rosati, P., Tozzi, P., et al.\ 2001,
ApJ, 551, 624:
``First Results from the X-ray and Optical Survey of the
Chandra Deep Field South.''
\smallskip

Giavalisco, M., \& Dickinson, M., 2001, ApJ, 550, 177:
``Clustering Segregation with UV Luminosity in Lyman-Break
Galaxies at $z \sim 3$ and its Implication.''

\smallskip
Hook, R. N., Pasquali, A., Pirzkal, N.,
 Walsh, J. R., Fosbury, R. A. E., et al. 2001, BAAS, 197, 1219:
``Spectrophotometry with the ACS Wide Field Camera.''

\smallskip
Papovich, C., Dickinson, M., \& Ferguson, H.\ C., 2001, 
ApJ, 559, 620:
``The Stellar Populations and Evolution of Lyman Break Galaxies.''

\smallskip
Tozzi, P., Rosati, P., Nonino, M., Bergeron, J., et al.\ 2001,
ApJ, 562, 42:
``New Results from the X-ray and Optical Survey of the Chandra Deep Field
South: The 300ks Exposure.''

\smallskip
Leibundgut, B. 2001, ARA\&A, 39, 67: ``Cosmological Implications from 
Observations of Type Ia Supernovae''

\smallskip
Daddi, E., Cimatti, A., Broadhurst, T., Renzini, A., et al. 2002, A\&A, 384, 
L1: ``The K20 Survey II. The different spacial clustering of $z\sim 1$ old 
and dusty star-forming EROs.''

\smallskip
Mainieri, V., Bergeron, J., Hasinger, G., Lehmann, I., et al.  2002, A\&A, 393,
425: ``XMM-Newton observation of the Lockman Hole. II. Spectral analysis.''

}

%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%% THE PAGE OF THE TARGET LIST %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
%---- BOX 11 -----------------------------------------------------------
%
% Provide    the  complete  list  of   targets/fields   proposed in this
% programme, i.e., run id(s) (you may use the  same target/field in more
% than one run), target/field name, RA(h min s), DEC(deg ' ''), equinox,
% magnitude, angular diameter, additional    information  (e.g. globular 
% cluster), and  reference star ID (only  for  NAOS/CONICA observations) 
% for  each  target/field.  Decimal  seconds of time  and  arc should be  
% omitted.  If  your programme is  related to  some future  targets with 
% still unknown coordinates (e.g., ToO), please respect the format:  
% {00 00 00}.  E.g.:
%
%
%\Target{A}{J0240-34}{02 40 07}{-34 34 19}{J2000}{17.5}{}{sep=6''}{}
%\Target{AB}{NGC 104}{11 20 00}{-17 40 00}{B1950}{4.08}{1 deg}{globular}{}
%\Target{B}{NGC 105}{22 55 12}{-47 50 30}{B1950}{}{}{}{S111230045821}
%
% For designation of guide stars please see ESOFORM manual
%
%           THE LIST OF TARGETS/FIELDS IS LIMITED TO ONE PAGE
% Should the  number of  targets exceed  the available space  defined by
% this page, please  provide instead the  central coordinates  of target
% fields.
% 
%DO NOT USE ANY TEX/LATEX MACROS FOR THE TARGETS
%DO NOT USE ANY TEX/LATEX MACROS FOR THE TARGETS
%DO NOT USE ANY TEX/LATEX MACROS FOR THE TARGETS
\Target{A}{CDF-S}{03 32 28}{-27 48 30}{J2000}{}{}{}{}
\Target{B}{CDF-S}{03 32 28}{-27 48 30}{J2000}{}{}{}{}
\Target{C}{CDF-S}{03 32 28}{-27 48 30}{J2000}{}{}{}{}

%
% Use TargetNotes to  include any comments that  apply to all  targets,
% e.g.:
% \TargetNotes{The planned grid pointings around the targets listed
%              above will be defined during the first observing night.}
\TargetNotes{}

%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%%%% THE PAGE OF SCHEDULING REQUIR. AND INSTRUMENT CONFIGURATIONS %%%%%
%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%
%---- BOX 12 -----------------------------------------------------------
%
% Scheduling Requirements for the first semester:
% 
% In order to allow  for the automated scheduling of all observing runs,
% please provide the following information, whenever applicable.
%

%
% 1. RUN SPLITTING, FOR A GIVEN ESO TELESCOPE (Visitor Mode only).
% Provide, if you ask for non-consecutive nights, the exact splitting of
% the observing  time  into different  sub-runs, with indication  of the
% time intervals.  The  first argument should be the  run ID, the second
% argument should express the way the run should be split into different
% sub-runs.   Check    the   ESOFORM users' manual  for    more detailed
% information.
% 
% E.g., \RunSplitting{A}{2,10s,2,20w,2,15s,4H2}. 
%
\RunSplitting{}{}

%
% 2. SPECIFIC DATE(S) FOR TIME CRITICAL OBSERVATIONS.
% Provide any date for critical time windows.  E.g.,
%
% \TimeCritical{A}{12-may-03}{14-may-03}{parallel observation with HST}.
%
\TimeCritical{}{}{}{} 

%
% 3. UNSUITABLE PERIOD(S) OF TIME.
% Provide any date windows for unsuitable periods of time.
%
% \UnsuitableTimes{A}{12-jul-03}{14-jul-03}{International Conference}
%
\UnsuitableTimes{}{}{}{}

%
% 4. LINK FOR COORDINATED OBSERVATIONS WITH ANY OTHER FACILITIES.
% Provide any  link scheduling requirements  for coordinated observation
% with  any other part of  this run (ESO  telescopes) or other runs with
% any other facilities (e.g., HST).
%
%  \Link{B}{after}{A}{10 days}
%  \Link{B}{after}{A}{any}
%  \Link{B}{simultaneous}{C}{}
%
\Link{}{}{}{}

%
% 5. SPECIAL REQUIREMENT(S).
% Provide any other special scheduling requirements.
%
%  \SpecialRequirements{A}{ There should be some coordination  
%  with AAT observations which are not yet scheduled.  Please  
%  contact PI before scheduling. }
% 
\SpecialRequirements{}{}

%
% 6. UPPER LIMIT OF PROPER MOTIONS OF MOVING TARGETS.
% Provide (if   applicable)  upper limit of  proper   motions  of moving
% target.
%
%  \MovingTargets{A}{ large proper motion, still to be estimated }
%
\MovingTargets{}{}

%
% 7. SEST. (For SEST users only):
%
% Provide below your preferred LST interval.
%
\SESTLST{}

% Provide below  the  periods when the targets   can be observed, taking
% into account the sun constraint (50 degrees).
%
\SESTperiod{}

%
%---- BOX 13 -----------------------------------------------------------
%
% INSTRUMENT CONFIGURATIONS:
%
% You must remove the `%' sign in  front of the \INSconfig{}{}{}{} macros,
% i.e.,   uncomment them,  in  order to   make  these lines take effect.
% Uncomment only the lines related to instrument configuration(s) needed
% for  the acquisition   of your planned  observations.    You will find
% detailed  information  in    the  users'  manuals   of   the available
% instruments.
% You must add the run ID in the first brackets.
%
% Do NOT specify Instrument Configuration for alternative runs.
%
%-----------------------------------------------------------------------
%---- VIMOS at the VLT-UT3 (MELIPAL) -------------------------------------
%-----------------------------------------------------------------------
%
\INSconfig{A}{VIMOS}{PRE-IMG}{R}
\INSconfig{B}{VIMOS}{MOS-grisms}{LR-Red}
\INSconfig{C}{VIMOS}{MOS-grisms}{LR-Blue}
%\INSconfig{}{VIMOS}{MOS-grisms}{LR-Interm}
%\INSconfig{}{VIMOS}{MOS-grisms}{HR-Red}
%\INSconfig{}{VIMOS}{MOS-grisms}{HR-Orange}
%\INSconfig{}{VIMOS}{MOS-grisms}{HR-Blue}

%\INSconfig{}{VIMOS}{MOS-slits-targets}{0.8" < slit width < 1.4", targets:stellar}
%\INSconfig{}{VIMOS}{MOS-slits-targets}{0.8" < slit width < 1.4", targets:extended}
%\INSconfig{}{VIMOS}{MOS-slits-targets}{slit width > 1.4", targets:stellar}
%\INSconfig{}{VIMOS}{MOS-slits-targets}{slit width > 1.4", targets:extended}
%\INSconfig{}{VIMOS}{MOS-masks}{Enter here number of mask sets (1 set = 4quadrants)}



%
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%%%%% THE END %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
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\MakeProposal
\end{document}

%
% Everything following `\end{document}' is discarded. 
%
% NOTE: Being submitted via electronic mail, this file will be processed 
% automatically by the ESO Proposal Handling and Reporting System (PHRS)
%
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