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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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%    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.
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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.
%
%    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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 #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: b) gas kinematics and jet/cloud 
interactions
}
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%     Give name and address below
%     !!!!
\name{C N Tadhunter
}
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%     Enter your address on the next line (end lines with \\)
%     !!!!
\address{c/o 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{C.Tadhunter@sheffield.ac.uk
}
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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)\\
{\bf 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{
One of the major motivations for studying high redshift radio galaxies is to
use
them to probe galaxy formation and evolution in the early universe. The
discovery of galaxy-scale extended emission line regions (EELR) with blue
continuum colours around  many high-z radio galaxies in the mid-1980's led to
speculation that the EELR sample galaxies in the process of formation. However,
a period of retrenchment followed when it was realised that the EELR are
closely
aligned with the radio structures and much of the extended UV continuum can be
explained in terms of scattered AGN light and nebular continuum.

Some uncertainty remains about the origin of the aligned emission line
structures. Although it has been suggested that the alignments are due to {\it
illumination} of the gaseous haloes of the host galaxies by the radiation cones
of quasars hidden in the cores of the galaxies, HST images of the idividual
high-z radio galaxies show jet-like structures along the radio axis which too
highly collimated to be consistent with the relatively broad radiation cones
predicted by the unified schemes. Furthermore, the large emission line widths
(500 $< $ FWHM $<$ 2000 km/s) and radial velocity amplitudes (500 $< \Delta V <
$ 1500 km/s) are generally inconsistent with illumination of the  ambient
medium
in the galaxy haloes. Thus, it appears more likely that the aligned structures
are the result of pre-existing clouds in the galaxies being swept up,
accelarated
and ionized by shocks driven through the galaxies by the radio jets.

By themselves, the bright, aligned structures are not a useful diagnostic of
conditions in the haloes of the galaxies, since most of their observed
properties are a consequence of jet/cloud interactions. However, in order for
the closely aligned emission line structures to be such a common feature of the
high-z radio galaxies, there must be a plentiful supply of relatively dense
clouds available  to interact with the jets along the radio axes. There are two
possibilities for the origin of these clouds:
\begin{enumerate}
\item Generalised large-scale haloes of clouds which show no preferential
alignment with the radio axis. These haloes could have an intrinsic filamentary
structure in which case the apparent strength of the alignment effect would
depend on their relative orientations.
\item Extended haloes of clouds which are elongated and 
closely aligned with radio axes in a causal manner (eg, West 1994).
\end{enumerate}
If the first of these possibilities proves correct, then the extended haloes
will be illuminated by the broad radiation cones of the hidden quasars, and it
will be possible to detect the haloes as low surface brightness emission line
regions outside the main aligned structures. This opens up the exciting
possibility of using the low surface brightness EELR to investigate the
kinematics and physical conditions in the large-scale haloes, and thereby test
models for the formation of massive galaxies in the early universe.

On the other hand, if we fail to detect the extended low-surface brightness
emission line regions, and the gaseous haloes are really intrinsically aligned
along the radio axes, then this will have profound implications for our
understanding of the origins of the radio activity and jet collimation. 
}
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\observations{We propose to search for the low-surface brightness haloes of
high-z radio galaxies using spectroscopic and imaging observations of a
carefully selected sample of closely aligned sources. The material in the
haloes
has not been shocked or swept up by the radio jets, and we expect a much lower
surface brightness for the haloes than in the main aligned structures.
Therefore
we require the light gathering power of an 8m telescope to be certain to detect
the haloes. We will place the slit of FORS
perpendicular to the radio axes to pass through both the known aligned emission
line structures and the parts of the putative quasar radiation cones which are
well away from the radio axis. The halo gas will be readily distinguished
because we expect it to display much smaller linewidths and a higher ionization
state than the material directly interacting with the radio jets. In cases
where
we detect the extended low surface brightness emission line regions we plan to
map the extended haloes in depth. 

We are particularly interested in determining the kinematics of the gas in the
extended haloes, since this will provide the best diagnostic of the origin(s)
of
the haloes. If the gaseous haloes are remnants of the formation of the host
galaxies through the  collapse of a single primaeval clouds, then we expect
there to be little sign of rotation on a large scale, since the angular
momentum
in the stellar haloes of the product --- massive early-type galaxies --- is
low.
However, if the galaxies form through dissipational mergers of galaxies, we
expect considerable velocity gradients in the haloes, as is already observed in
some nearby radio galaxies (Tadhunter et al. 1988).

As a secondary goal we will search for signs of cone-like structures in the
extended haloes, as expected in the case of illumination by quasars hidden in
the cores of the galaxies. This will provide a further test of the unified
schemes for the powerful, high redshift objects.

In this project we are encouraged by the recent detection of an extended
Ly$\alpha$ halo around a high redshift radio galaxy by van Ojik et al.
}
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%     Describe your observations in some technical detail (filters,
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\techniques{
\begin{enumerate}
\item FORS spectroscopy
\item FORS and CONICA imaging (with tailor-made narrow-band filters)  
\end{enumerate}
}
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\calibration{tbd
}
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%     Limitation of the current instrumentation of the VLT and
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\limitations{
}
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