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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)
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% 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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% 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.
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%    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.
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%    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.
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% 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.
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% 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
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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. }
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%     Indicate a title for your proposal
%     !!!!
\casetitle{High redshift radio galaxies: e) Absorption studies of Ly$\alpha$
and 
C~IV as probes of the circumnuclear gas --- particularly the cold component
}
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%     Give name and address below
%     !!!!
\name{H R\"ottgering
}
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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{rottgeri@strw.leidenuniv.nl
}
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%     Please indicate any collaborators and their institutions (no
%     addresses) for this project on the next lines (end lines with \\)
%     !!!!
\collaborators{
{\bf rottgeri@strw.leidenuniv.nl (Huub R\"ottgering, Leiden)}\\
miley@strw.leidenuniv.nl (George Miley. Leiden)\\
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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\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{The Ly $\alpha$ emission of distant radio galaxies is spectacular. 
It
can be as luminous as {\bf $10^{44}$} erg s$^{-1}$ and can extend up to 150 kpc
($ \sim 10''$ at $z=2.5$), suggesting a direct link between the formation of
the
galaxy and the emission line gas. The typical FWHM of Ly$\alpha$ is 1500 km/s,
much lower than that of quasars. Important results from detailed studies of the
emission line gas and and its environment include:

\begin{itemize} 
\item 
Spatially-extended Ly $\alpha$ absorption features indicating the
frequent presence of ($>30$~kpc) regions of dense neutral gas.
(see  R\"ottgering et al. 1995).  Note that
studies of the quasar absorption lines do not yield any spatial
information since the quasars are unresolved.

\item 
The discovery of large (150~kpc) rotating structures with low
velocity dispersion (250~km/s FWHM), indicating dynamical masses of
$10^{12} M_\odot $  (van Ojik 1995; Van Ojik et al. 1995).  The
existence of such a large rotating structure at such early epoch has
important implications for scenarios of galaxy evolution.
\end{itemize} 

With 4-m class telescopes the study of the absorption and emission lines gas
can
only be carried out on galaxies with the  brighter Ly $\alpha$ lines. The VLT
will offer the exciting possibility of detailed studies of faint Ly $\alpha$ 
emission as well as emission from  redshifted He and Carbon lines such as C~IV
1549 and 1909 and He~1640. Such detailed  studies include deep spectroscopy at
a
resolution of a few \AA\/  and deep narrow band imaging and should address: 

\begin{enumerate} 
\item Search for absorption features against Ly $\alpha$ emission 
from clouds with a column density at least an order less 
than has  presently been observed. 

\item  Search for absorption features against CIV emission. 

\item Determine the total extent of the presently known rotating
halos. It is well possible that these halos extend over sizes of
300--400~kpc, and thereby be the first example of Zeldovich pancakes.

\item Determine how ubiquitous such rotating halos are. 

\item Observe the faint metal-lines from the 
rotating halos. 

\end{enumerate} 

These observations will constrain physical parameters, such as
metalicity, velocity structure, density and masses of the various
components of the absorption and emission line gas.  These results
provide unique information relevant to the formation and evolution of
radio galaxies and clusters, to relationships between galaxy and
quasar activity and to physical conditions in the early Universe.\\

{\bf References}

R{\"o}ttgering~H.,  Hunstead~R.,  Miley~G.~K.,  van Ojik~R.,    Wieringa~M.~H.,
1995,{ MNRAS}, { 277}, 389

van Ojik~R.,  1995, { Ph.D. thesis}, University of Leiden

van Ojik~R.,  R{\"o}ttgering~H.,  Carilli~C.,  Miley~G.,    Bremer~M.,  1995a,
{ A radio galaxy at $z=3.6$ in a giant rotating Lyman $\alpha$ halo},
A\&A: in press
}
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%     Describe your observations in some technical detail
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\observations{
The spectroscopic observations are rather analogous to quasar absorption line 
measurements where the Ly$\alpha$ emission is used in place of a non-thermal
continuum. Resolution up to a few tens of km/s are required with good spatial
resolution.

In addition, high resolution optical imaging with a set of narrow-band filters
is required.
 }
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%     Describe your observations in some technical detail (filters,
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%     !!!!
\techniques{Moderate to high spectral resolution spatially resolved
spectroscopy (eg, UVES).

CONICA with narrow filters.

3D spectroscopy with spectral resolution of at least several thousand.

}
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\calibration{
}
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%     Limitation of the current instrumentation of the VLT and
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\limitations{
Need for a 3D spectrometer.
}
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