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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.
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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
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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. }
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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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\par
\vspace*{15mm}
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%     Indicate a title for your proposal
%     !!!!
\casetitle{High redshift radio galaxies: d) UV nebular diagnostics of the 
extended gas
}
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%     Give name and address below
%     !!!!
\name{R A E Fosbury
}
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%     Enter your address on the next line (end lines with \\)
%     !!!!
\address{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{rfosbury@eso.org
}
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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)\\
miley@strw.leidenuniv.nl (George Miley. Leiden)\\
sperello@arcetri.astro.it (Sperello di Serego Alighieri, Arcetri)\\
C.Tadhunter@sheffield.ac.uk (Clive Tadhunter, Sheffield)\\
{\bf 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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%     The following line should contain the name of the ESO science
%     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{Emission line plasma diagnostic techniques have been applied
successfully to low redshift extended emission line regions (EELR, eg, Robinson
et al. 1987) and, given a good quantitative understanding of the ionization
mechanism, are capable of yielding information about the chemical composition
of
the gas and its dust content (Villar-Martin et al. 1996). These analyses have
been carried out in the optical spectrum where there are suitable forbidden
lines of common species. The rest-frame ultraviolet, while rich in strong
resonance lines, is less suitable for abundance analyses but gives powerful
clues to the geometrical configuration of ionized clouds and illuminating
sources.

The low z EELR show a remarkably uniform chemical composition around solar
values (Robinson et al. 1987) which suggests a common origin for the extended
gaseous haloes of powerful radio sources. It is important to carry out similar
observations of the HzRG since their haloes may consist of relatively
unprocessed material. Very extended Lyman-$\alpha$ haloes are known (van Ojik
et al. ) at redshifts around 3. Althought the inner regions of these EELR
appear disturbed by the radio jets, the outer part are quiescent.

This is the abstract of a submitted paper on UV diagnostics by Villar-Martin,
Binette \& Fosbury - just to give a flavour of the topic.

In the powerful, high redshift radio galaxies, it is believed that the dominant
source of ionization for the interstellar gas is the hard radiation field
associated with the active nucleus. The photon sources is generally external to
the clouds being ionized and so the geometrical perspective from which the gas
is observed and the presence and distribution of dust must be properly
accounted for in the diagnostic process. In this paper, we examine the
formation of the three strong lines: CIV$\lambda$1549, Ly$\alpha$\ and
CIII]$\lambda$1909 which are often observed in these sources. We find that the
observed trends, in particular the high CIV$\lambda$1549/Ly$\alpha$ ratio, are
often better explained by geometrical (viewing angle) effects than by the
presence of large quantities of dust either within or outside the excited
clouds. We show that neutral condensations along the line-of-sight, by
refelecting photons near the wavelength of Ly$\alpha$, can increase the
observed CIV/Ly$\alpha$ ratio. The existence of HI absorption clouds
(i.e., mirrors) external to the emission region lead also to the prediction of
large, diffuse haloes of what appears to be narrow Ly$\alpha$\ emission.
}
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%     Technical requirements
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%     Describe your observations in some technical detail
%     !!!!
\observations{
This proposal will probably be combined with HzRG-e on Lyman alpha
spectroscopy.
}
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%     Which instruments are needed?
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%     Describe your observations in some technical detail (filters,
%     gratings, throughput, stability, etc.)
%     !!!!
\techniques{
}
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%     Done with page 4
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\newpage
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%     Describe your required calibration to achieve the science goal 
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\calibration{
}
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%     Limitation of the current instrumentation of the VLT and
%     possible extensions of the observing program
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%     Describe limitations of the current ESO instrumentation program 
%     and possible extensions of the observational project
%     !!!!
\limitations{
}
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