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%                    STANDARD FORMAT FOR SCIENCE CASES
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%
% Should you have any questions please contact either 
% Alvio Renzini (arenzini@eso.org) or
% Bruno Leibundgut (bleibundgut@eso.org)
%
% Documentation on the planned instrumentation for the VLT can be
% obtained from ESO (ask your friendly coordinator or one of the above).
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%!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!
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%    Look for a group of exclamation marks ('!!!!') for places to be 
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% SCIENCE CASES documents should inclide the following:
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% 1) A Scientific Rationale, up to two TEX pages.
%    The discussion should also address the possible impact of current research 
%    before the VLT will start operating.
%
%    The above is needed for ...
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% 2) A Description of the proposed observations. Including an estimate of
%    the total observing time required to achieve the scientific goal.
%    Possible La Silla observations that may be needed to prepare for the VLT
%    observations could also me mentioned and quantified.
%
%    The above is needed for ....
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% 3) List the technical requirements to accomplish the scientific goal.
%    (e.g., pointing, tracking, image quality, troughput, etc.).
%    Identify and quantitatively discuss the critical performances of the VLT
%    and the instruments that are required to achieve the science goal.
%
% 4) A list of calibration requirements.
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% 5) Identify the limits of first generation instruments for the specific
%    science case, all the way from simple items (e.g., the filter list)
%    to the whole instrumentation plan ... (No more than half a page).
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% 6) No target list required at this stage.
%
% 7) Deadline: April 30, 1996, please indicate by January 20 your
%              intent to supply a test case
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\fbox{\bf Scientific Rationale:} \par
\scriptsize
\parbox[t]{480pt}{
Up to two pages.\par\noindent
The possible impact of current
research before the VLT will start operating should also be addressed. VLT
Science Cases will have to evolve so as to remain competitive in their field of
research. The above is needed to scientifically justify the requirements
below.}
\normalsize \par
\vspace{4pt}
 #1 }
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{\bf Proposed Observations:}\par\noindent
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Describe the proposed observations. Indicate the instrument
and instrument modes, filters, gratings, etc. Include an estimate of
the total observing time required to achieve the scientific goal.
Possible La Silla observations that may be needed to prepare for the VLT
observations could also me mentioned and quantified.
The above is needed to provide facts to orient ESO policy (e.g.
the OPC) about the expected needs for small, medium, and large projects. }
\normalsize
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{\bf Technical Description of the Observations:}\par\noindent
\scriptsize
\hspace*{6pt} \parbox{480pt}{
List the technical requirements to accomplish the scientific goal.
(e.g., pointing, tracking, image quality, troughput, etc.). Identify
and quantitatively discuss the critical performances of the VLT, its
instruments, and its operations that are required to achieve the
science goal. }
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{\bf Calibration Needs:}\par\noindent
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Describe the required calibrations (type, accuracy, etc.) to achieve the 
science goal. }
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{\bf Limitation of Instrumentation and Program Extensions:}\par\noindent
\scriptsize
\hspace*{8pt} \parbox{480pt}{
Identify the limits of first generation instruments for the specific
science case, all the way from simple items (e.g., missing filters) to
the whole instrumentation plan. If appropriate, discuss to which extent
the planned VLT instrumentation will be competitive to that of other
8m class telescopes. }
\normalsize
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\Large
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\vspace*{15mm}
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%     Indicate a title for your proposal
%     !!!!
\casetitle{High redshift radio galaxies: a) their stellar content and
surrounding  clusters
}
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%     Give name and address below
%     !!!!
\name{G Miley, S di Serego Alighieri
}
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%     Enter your address on the next line (end lines with \\)
%     !!!!
\address{c/- ST-ECF\\
Karl Schwarzschild Str 2\\
D-85748 Garching bei M\"unchen
}
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%     Please indicate your phone number and e-mail address
%     Phone-Nr.:
%     !!!!
\phone{+49 89 320 06 235
}
%     e-mail:
%     !!!!
\email{miley@strw.leidenuniv.nl, sperello@arcetri.astro.it
}
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%     Please indicate any collaborators and their institutions (no
%     addresses) for this project on the next lines (end lines with \\)
%     !!!!
\collaborators{
rottgeri@strw.leidenuniv.nl (Huub R\"ottgering, Leiden)\\
{\bf miley@strw.leidenuniv.nl (George Miley. Leiden)}\\
{\bf sperello@arcetri.astro.it (Sperello di Serego Alighieri, Arcetri)}\\
C.Tadhunter@sheffield.ac.uk (Clive Tadhunter, Sheffield)\\
rfosbury@eso.org (Bob Fosbury, ST-ECF, coordinator)\\
cimatti@arcetri.astro.it (Andrea Cimatti, Florence)\\
amoorwoo@eso.org (Alan Moorwood, ESO)\\
pquinn@eso.org (Peter Quinn, ESO)\\
nb. lead author(s) for this sub-proposal in {\bf bf type}
}
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%     performance group coordinator
%     !!!!
\coordinator{R A E Fosbury
}
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\item No target list required
\item Documentation on the available VLT instruments can be obtained
from the ESO coordinator
\item Please attach figures to the form and send an electronic version 
to the ESO coordinator
\item Deadline: 30. April 1996, please indicate in written form by
20. January that you are planning to provide a test case.
\item For information please contact either Alvio Renzini
(arenzini@eso.org) or Bruno Leibundgut (bleibundgut@eso.org)
\end{list}
\normalsize
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%     Scientific Rational (not more than two pages)
%     !!!!
\rationale{This proposal intends to address two main problems: the
stellar populations at early cosmological epoch, and the relationship
between environment and activity, and its evolution. Both of these
questions can be addressed by studying the clusters of galaxies around
high redshift radio galaxies (HzRG) and radio quasars (RQ). 

Up to now almost all information on objects in the early Universe has
been obtained from active objects, because it is easier to detect them,
and to measure their redshifts and their main physical properties. However
if one wishes to study the formation and early evolution of most
galaxies that we see in the local Universe, which are non--active, these
active galaxies have the disadvantage that their morphology and spectra
are influenced by the activity. The case of quasars is very clear, since
tha strong nuclear source overwhelmes the stellar light. Also in HzRG the
morphological and spectral signatures of activity are clear (eg,
McCarthy, 1993, ARAA, 31, 639). Although for HzRG spectropolarimetry can
help in disentangling the stellar component from the active one (di
Serego Alighieri et al., 1994, ApJ, 431, 123; see also test case c),
the measurement of the stellar SED and absorptions is inhevitably more
difficult, and one is left with the doubt that even the stellar
component can be influenced by the activity and therefore cannot give
information applicable to the majority of galaxies.

AGN (particularly the radio-loud objects) can nevertheless be 
used as signposts for galaxies more in general. We know that they occour
in clusters and groups (Yee, ... , Dickinson, 1996...): looking around
AGN we can surely find other more normal galaxies, and most of them
will be at the same redshift. We then propose to study these cluster
galaxies to obtain information on their stellar populations from the
morphology and spectra. The aim is to determine the age of the
stars (in particular of the oldest ones), its evolution with redshift
and its spread in a single cluster, in order to provide constraints on
the formation and early evolution of normal galaxies. An important
analysis tool will be the spectral synthesis codes developed to
reproduce both the general shape and the detailed features of the
spectra of stellar populations (eg, Bressan et al., 1994, ApJSS, 94,
63, and 1995, A\&A, ...).

The second main theme of this proposal is the relationship between
activity and environment. It has often been claimed that activity is
triggered by the interaction between the active galaxy and one or more
companions and even that the material necessary to fuel the
activity comes from companions . Indeed some nearby AGN have
double nuclei and companions with distorted morphology. On the other
hand it is also clear that an AGN influences the environment, eg, with
the radio plasma and with strong anisotropic ionizing radiation. We
intend to study these interactions on the most powerful AGN
and on the youngest ones, where the causes and effects can be hopefully
separated and shed light on the properties of the central power source. 
The necessary data again are images, to look for distorted
morphologies, and spectra, to study the kinematics of the cluster and of
individual members and the ionization as a function of the distance of
the companion and of its direction with respect to the axes of the AGN.

We believe that addressing this second problem we can also give
constraints on the possibility that most galaxies, also those that are
not active now, have had an active phase in the past. Clearly, if all
galaxies have been active and if the
triggering of the activity requires a strong galaxy-to-galaxy
interaction, which leaves long-lasting traces, we should see these
today. On the other hand, if most of the distorsions and peculiar
spectra which we see around AGN are a temporary effect of the activity
(like illumination and ionization) then we do not expect to see much of
it after the activity is finished. (nb. this may
require a more detailed discussion of the duration of effects: eg,
kinematical effects may last longer than ionization). 
}
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\observations{The observations necessary are of two types: first
imaging, to find the cluster members and to study their morphology,
second spectroscopy to study the SED, stellar spectral features, and
emission lines. The morphology can best be studied with the HST (eg,
Dickinson, 1996...). However the search for companions, in particular
for those useful for the study of stellar populations at the highest
redshifts, is probably best accomplished in the near IR from the ground
(some simulations to quantify this would be very useful).
The most important stellar spectral features for the old stellar population
occur between 3500 and 6000 \AA , which is moved in the near IR for
z=2-4. So we need spectroscopy in the JHK bands (ISAAC). Multiobject
spectroscopy in JHK would be a very big advantage, as well as OH suppression.
The younger OB stellar features require the optical range (FORS) for the same
redshift range.
 }
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%     Describe your observations in some technical detail (filters,
%     gratings, throughput, stability, etc.)
%     !!!!
\techniques{Single and multi-object spectroscopy with resolutions from a few
hundred to a few thousand. Requirements are to identify and measure stellar
absorption features and to measure stellar velocity dispersions.

Principal instruments will be FORS and ISAAC. }
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\calibration{tbd
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\limitations{Needs further discussion --- possibly need more objects per
multi-object field.
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