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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
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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
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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
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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
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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
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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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\Large
\framebox[510pt]{\bf \centerline{Form for VLT Science Test Cases}}
\par
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% Indicate a title for your proposal
% !!!!
\casetitle{High redshift radio galaxies: c) Imaging- and spectro-polarimetry
to identify and separate the scattered component
}
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% Give name and address below
% !!!!
\name{A Cimatti
}
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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{cimatti@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)\\
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)\\
{\bf 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 aim of polarimetry is to separate and investigate the nature of
the different radiation components contributing to the rest-frame total UV and
optical flux, and to provide important by-products like deep total flux images
and spectra in case of imaging-polarimetry and spectropolarimetry respectively.
Polarimetry is also an important tool for testing the of the unified model of
radio-loud AGN by searching for quasar features in the polarized spectra.
However, the faintness of HzRGs places strong limits to the range of the
feasibile observations with the 4m-class telescopes, and makes the VLT the
necessary instrument to perform detailed studies. The main issues that can be
investigated are summarized as follows :
{\bf Polarized radiation.\/ } The polarization of the {\it continuum} will be
investigated both with deep, broad-band, multi-color imaging-polarimetry and
spatially resolved spectropolarimetry, providing spatial distributions and
spectral information on the polarized radiation. The polarization properties of
the {\it emission lines} will be studied with high s/n spectropolarimetry. If
HzRGs are misdirected quasars, broad permitted lines are expected in the
polarized spectra (for example MgII$\lambda$2800). Higher spectral resolution
will be used for the brightest objects in order to analyse in detail the
structure of the scattered broad lines. The polarization of the narrow
forbidden
lines is equally important because it can provide constraints on the spatial
extension of the obscuring torus: the low ionization lines (eg,
[OII]$\lambda$3727) are supposed to be emitted isotropically outside the torus
(and so are unpolarized), but the highest ionization lines like [NeIV] and
[NeV]
might be partially obscured, and then show some detectable polarization.
Furthermore, for the first time, the VLT will allow us to perform imaging
polarimetry (and spectropolarimetry ?) in the near-IR ($JHK$ bands) and to
understand whether the rest-frame optical continuum is dominated by unpolarized
starlight, as is now only supposed. In summary, the combination of deep
imaging-polarimetry and spatially resolved spectropolarimetry of HzRGs (both
possible only with 8--10m-class telescopes), will provide a complete set of
information which will allow us to test the generality of the unified model, to
have geometrical constraints on the obscuring torus and to study in detail the
contribution of the polarized radiation to the alignment effect in a broad,
rest-frame
spectral range $\sim$0.1--1.0 $\mu m$. The important key for a successful
program
is the observation of a significant sample of HzRGs ($>$10 objects). It is also
highly advisable the observation of a sample of low redshift RGs ($z
\sim$0.1--0.3) in the bluest spectral region accessible from the ground in
order
to compare the properties of the polarized radiation at low and high redshifts.
Finally, a sample of high redshift radio-loud quasars with radio steep spectra
(ie, matched to those of HzRGs) should be observed in order to find and
investigate `transition' objects oriented at intermediate lines of sight
between
`radio galaxies' and `radio quasars' (expected in the unified model).
{\bf Unpolarized radiation and stellar populations.\/ } The nature and the
fractional contribution of the unpolarized UV-optical light is still poorly
known. The sum of the 4 images or spectra obtained at 4 position angles for
polarimetry provide very deep images of spectra of the total flux. The deep
images will allow us to investigate the colours and the structure of the
faintest
components, while the deep spectra will be used to search for signatures of
stellar radiation. In particular, absorption lines of O and B stars (starburst)
will be searched for in the rest-frame $<$2000~\AA (typically accessible in
HzRGs
with z$>$2), while the 4000~\AA~ break, the CaII H\&K and CN absorptions will
be
studied in the HzRGs with z around 1. In addition, the spectropolarimetric data
will provide further clues. In fact, the comparison of the EW of the broad
component in the total flux and polarized spectra is related to the fractional
contribution of the unpolarized radiation to the total flux. The observation of
the redhsifted (in the far red or near-IR) H$\beta$ emission line will also
allow the estimate of the nebular contribution to the UV continuum. Finally,
the
detailed study of $P(\lambda)$ across the 4000~\AA~ break will provide a
completely independent measure of the dilution due to the old stellar
population
unpolarized radiation.
{\bf Interstellar medium and environment.\/ } Both electrons and dust particles
are present in the ISM of HzRGs. However, the it is not clear what is the
dominant population of scatterers. The answer to this question is also
important
to provide clues to the ISM state and its relative `ingredients'. In this
regard,
spectropolarimetry, possibly extended to the near-IR, is the most powerful
tool.
In fact, the shape of the polarized spectrum is the convolution of the
scattering efficiency of the particles with the incident spectrum. Also the
shape of $P(\lambda)$ and the intrinsic (undiluted) degree of polarization are
related to the nature of the scatterers. Moreover, the FWHM of the scattered
broad lines can provide a rather accurate way to estimate the temperature of
the
scatterers in case of electron scattering, and additional clues on the physical
state of the ionized gas. Also, the luminosity of the scattered broad lines,
together with the luminosity of the incident line, allow an estimate of the
column density of the scatterers. Finally, deep spectra and polarimetry around
2200~\AA~ will provide clues to the dust properties at high redshifts. We
have available a dust scattering model and a code for spectral deconvolution
working in the UV-optical range.
It is important to stress again that the proposed observations and studies are
not feasible with the 4m class telescopes at a sufficiently detailed level, and
that the VLT will be crucial to open new research frontiers in this field.\\
{\bf Principal references}
Antonucci R. 1984, {\it ApJ}, 278, 499
Cimatti A., di Serego Alighieri S., Fosbury R. A. E., Salvati M., \& Taylor D.
1993, {\it MNRAS}, 264, 421
Cimatti A., di Serego Alighieri S. 1995, {\it MNRAS}, 273, L7
Cimatti, A., Dey, A., van Breugel, W., Antonucci, R.,
Spinrad, H., 1996, {\it ApJ}, in press --- {\bf Keck observations}
di Serego Alighieri S., Fosbury R., Quinn P., Tadhunter C. 1989, {\it Nature},
341, 307
di Serego Alighieri S., Cimatti A., \& Fosbury R. 1994, {\it ApJ}, 431, 123
di Serego Alighieri S., Cimatti A., Fosbury R., Perez-Fournon I. 1996, {\it
MNRAS} submitted
Dey, A., Cimatti, A., van Breugel, W., Antonucci, R.,
Spinrad, H., 1996, {\it ApJ}, in press --- {\bf Keck observations}
Jannuzi B.T., Elston R. 1991, {\it ApJ}, 366, L69
Jannuzi B.T., Elston R., Schmidt G., Smith P., Stockman H. 1995, {\it ApJ}, in
press
Manzini A., di Serego Alighieri S. 1996, {\it A\&A}, in press
Tadhunter C.N., Fosbury R.A.E., di Serego Alighieri S. 1988, Proceedings ``BL
Lac
Objects", ed. Maraschi L., Maccacaro T., Ulrich M.H., Springer-Verlag, p. 79
Tadhunter C.N., Scarrott S.M., Draper P., Rolph C. 1992, {\it MNRAS}, 256, 53p
}
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\observations{
Principal modes of observation are imaging and spectropolarimetry in the
optical
and $JHK$ spectral regions. Since the observations are all sky limited, it is
essential to use a two-beam polarimeter as provided by FORS (but not definitely
with ISAAC). For at least the spectral work, a rotatable half-wave plate is
essential to allow the use of the same slit position throughout the
polarization observations.
}
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\techniques{
FORS, ISAAC, CONICA
}
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% Describe your required calibration to achieve the science goal
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\calibration{Precise instrumental polarization calibration (to $\sim 0.1$\%)
}
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% Limitation of the current instrumentation of the VLT and
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\limitations{Essential to have a two-beam polarimeter and a rotatable half-wave
plate (see above).
}
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