<html><head><meta name="color-scheme" content="light dark"></head><body><pre style="word-wrap: break-word; white-space: pre-wrap;">% KPNOPROP.TEX -- KPNO electronic proposal form.

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\documentstyle[kpnoprop]{article}

\begin{document}

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\title{Associated CIV Absorption and the Environments of Radio-Loud Quasars at z$&gt;$1.4}

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\begin{PI}
\name{Patrick B. Hall}			% REQUIRED
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\begin{CoI}
\name{Richard F. Green}			% REQUIRED
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\begin{abstract}
%oog

Radio-loud quasars are often found in clusters at z=0.5-0.7, and some 
quasars at higher redshift
show possible evidence for being in clusters, in the form of 
z$_{abs}$$\sim$z$_{em}$ ``associated'' CIV absorption-line systems in their spectra.  
We propose to investigate the environments of radio-loud
quasars at 1.4$&lt;$z$&lt;$2 through deep K$_s$ imaging %with IRIM 
on the 4-m in conjunction with deep R imaging on the U. of Arizona 2.3-m.
Our sample consists of 16 radio-loud quasars (RLQs) which show strong 
associated CIV absorption and 16 RLQs which have no such absorption.
Imaging this sample and three control fields will test the hypothesis 
that clusters of galaxies are responsible for associated CIV absorption
and extend our knowledge of RLQ environments to higher redshifts.
Detection of clusters around our quasars would yield a sample of high-redshift 
clusters invaluable for future study and comparison to clusters at similar redshift 
discovered by other means, and would also allow us to study the evolution of the 
cluster galaxy luminosity function, to constrain the star formation histories of 
cluster galaxies via their R-K colors at this redshift,
and to constrain cluster formation models by setting a lower limit to the 
space density of clusters in this redshift range.
 
%We propose to investigate the environments of a sample of 32 radio-loud
%quasars at z=1.4-2 through deep K$_s$ imaging with IRIM on the 4-m in 
%conjunction with deep R imaging on the Steward Observatory 2.3-m.
%Half of the quasars in our sample show strong z$_{abs}$$\sim$z$_{em}$
%%$\lambda\lambda$1548,1550 
%``associated'' CIV absorption-line systems in their spectra. 
%Imaging of those objects, a control sample of objects that do not show such 
%absorption, and three control fields will allow us 
%$\bullet$ to test the hypothesis that clusters of galaxies are responsible for associated 
%CIV absorption\\
%$\bullet$ to extend our knowledge of radio-loud quasar environments to higher redshifts,
%hopefully assembling a sample of clusters invaluable for future study and comparison
%to clusters at similar redshift eventually discovered optically, by X-ray emission, 
%or by association with radio galaxies.
%We will also use the data 
%$\bullet$ to study luminosity evolution in cluster galaxies, 
%$\bullet$ to constrain models of cluster formation by setting a lower limit to the density
%of clusters in this redshift range, 
%and 
%$\bullet$ to help constrain cluster galaxy star formation histories via their R-K colors.
 
\end{abstract}
 
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\begin{obsrun}
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\begin{obsrun}
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% In the following "essay question" sections, the delimiting pieces of
% markup (\justification, \feasibility, etc.) act as LaTeX \section*{}
% commands.  If the author wanted to have numbered subsections within
% any of these (as per this sample), LaTeX's \subsection could be used.

% Give the scientific justification for the experiment.
% This section should consist of paragraphs of text (and may include
% EPS figures) that follow the \justification line.
% Be sure to include overall significance to astronomy.

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\justification
%oog
%OVERVIEW of field: why worth doing? how will it advance knowledge? SPECIFIC!!
%then STRATEGY: how will the obs be treated to get the scientific info.
%WHAT? z=1.4-2 RLQs, 16/10 w/CIV, 16/10 w/o.
%WHY? see whether z=1-2 RLQs are in clusters like z=0.5-(1) RLQs and...
%...eventually compare w/opt/RG/Xray-selected clusters at same z;
%...study colors of such galaxies; ev sim says colors change but red field objs
%...provide constraints on quasar/cluster formation simulations
%see if aCIV RLQs are in richer/otherwise different environs (if there's no diff
%  between the 2 samples, then we have 2x as big of a sample for 1st bit)
%
%...better CIV z=1.4-2 z_assoc sample; get EW's (compare to other q's?)...foltz
%...luminosity evol. &gt;=-0.5 Kmag to K~1 (cowie etc.); -0.3 Kmag z=0.4
%   to 0.9 (aturner); -0.83,1.32 Kmag at z=1,2 (simple Tinsley'77 model)
%   BUT neg.lum.evol.+0.4 seen at faintest levels by cowie etc.
%...evrard: at z=2 12 objs r&lt;25 in 1 arcmin^2; g-r~0; K=?
%        at z=1 g-r&lt;2.5, K=? ..."easily" identifiable red cluster pop.
%...worry about unseen UV DLya/MgII absorbing galaxies, etc.; but at least
%   we know about some opt. foreground groups... dickinson doesn't.
%...some examples of possible unevolved z&gt;~1.5 gals known (Hu; Cowie 90;
%   Persson), so if they exist why not in clusters?  more likely to be
%   there since gals tend to form near density peaks 1st (Machetto 3.4)
%...where to get the quasars w/o absorption?  LBQS spect good enough? ask
%   to see Eric's spectra and any other spec. lyin' around.  look @papers too.
%...optical imaging too? for K=20.5 (K*-1) need R=25.5 to get R-K&gt;5 limit
%...r-K color of present-day E redshifted to z=2 is ...?
%...time to z=1-2?
%DETAILS:
%--MD RG clust gals are "eff. opt. invis."... R-K&gt;5.5 (BAAS?)
%--J @z=1-2 is R-U/B
%--hamilton's work, showing field E's to z=0.8
%--If you have an object with N_R/N_K &gt; 1/50 (R-K &gt; 4.25) it's easier to detect
%  in K... makes sense, limits of R~25/26 and K~21/22 being what they are today.
%--look at bershady's stuff: what galtype at what z should u look for in K vs. R
%--it is 10x more efficient at z&gt;1.1 to detect the reddest gals in K vs. I,
%  but even to z=3 it is not more efficient to detect the bluest in K vs. R/I.

The study of galaxies and clusters of galaxies at high redshift is interesting 
because when the light we see from them was emitted, the universe was billions of years
younger and galaxies and clusters may have
been very different then from the way they are today.
But even deep field galaxy surveys do not turn up many galaxies at z$&gt;$1, 
so we must resort to other methods to discover them.
Two such methods that have been successful at z$&lt;$1 are
to look for galaxies associated with metal-line absorption 
systems seen in quasar spectra (Steidel \&amp; Dickinson 1993)
and to look for galaxies associated with quasars themselves 
(Yee \&amp; Ellingson 1993; YE93).
We propose to use both of these methods to search for clusters of
galaxies around radio-loud quasars (RLQs) at z=1-2.

Intrinsically luminous (M$_{\rm B}$$&lt;$-25) RLQs are often located in clusters of 
Abell richness class 1 or greater at z=0.5-0.7 (Yee \&amp; Green 1987).  
These quasar host clusters have anomalously low velocity dispersions 
$\sigma_{\rm v}$ for their richnesses and thus form a unique sample of clusters 
which may be younger and less virialized than optically-selected clusters
(Ellingson, Yee \&amp; Green 1991, EYG91).
In addition, the environments of quasars are known to evolve:
at z$&lt;$0.5 only {\it faint} RLQs are seen in Abell richness 1 clusters (Fig~1).
EYG91 explain this evolution by postulating that galaxy interactions (more frequent 
in young, low-$\sigma_{\rm v}$ clusters) 
are largely responsible for creating and fueling radio-loud quasars, which then fade 
as the interaction rate decreases in their evolving, virializing host clusters.
However, the luminosity evolution of quasars in 
rich clusters does not extrapolate to z$&gt;$0.7 (Fig~1).
YE93 hypothesized that the cluster formation rate dropped considerably at 
z$\sim$0.7, so that in rich clusters at z$&lt;$0.7, almost all the quasars we see are 
old ones fading in luminosity on the host cluster's dynamical timescale.  
If this model is correct, luminous RLQs should still often be found in rich clusters 
at z$&gt;$0.7, but if the fraction in rich clusters decreases at some z$&gt;$0.7, 
it would indicate a peak in the cluster formation rate-- 
a valuable constraint on cluster formation models.

Some RLQs show additional evidence for being located in rich environments.
In addition to the general population of metal-line absorption line systems with 
z$_{abs}$$&lt;$z$_{em}$, there exists an excess population of CIV systems with 
z$_{abs}$ within a few thousand km s$^{-1}$ of the quasar emission redshift 
(see review by Foltz et al. 1988).
These ``associated'' absorption systems may arise in gas expelled at high velocity
from the quasars or in galaxies in clusters hosting the quasars
or very near in redshift to them.
Spectroscopic work has so far not been able to distinguish between these two hypotheses,
but deep imaging can greatly constrain the cluster hypothesis,
either by setting limits to the host cluster richnesses or 
by detecting differences between the host clusters of these objects and typical 
RLQs in central concentration, morphology, or galaxy colors in the cluster core.

Thus, to study the origin of ``associated'' absorption
and extend our knowledge of RLQ environments to z$&gt;$1, we propose to 
image the fields of 32 RLQs with z=1.4-2 %drawn 
from the unpublished `Radio-Loud Survey' of Foltz et al.
%(88 bright RLQs, 22 with strong (REW$&gt;$1.5~A) associated absorption)
and the LBQS radio database (Hooper et al. 1994).
%Each half of the sample will be comparable in terms of M$_{\rm B}$ and P$_{\rm rad}$,
We will avoid where possible objects with high-z intervening absorption to
reduce confusion about which system any detected galaxies are associated with.
%As discussed under Feasibility, 
Imaging to K$_s$=21.6 detects galaxies as faint as 1/6 of the present-day K$_*$ to z=2, 
and imaging to R=24.5 (which we will do at the SO 90'') yields valuable R-K$_s$ colors
and helps detect very blue cluster galaxies with K$_s$$&gt;$21.6.
We will be able to detect clusters of Abell richness 0 or greater to z=2 
and differences of one Abell richness class or more between the environments 
of RLQs with and without absorption simply by the excess galaxy counts in the
magnitude range expected for galaxies at the quasar redshifts.
Concentrations near the quasars of galaxies with unusual colors would be
additional evidence for clustering, but in any case a statistical comparison of the 
R-K$_s$ distributions of faint quasar- and random-field galaxies will yield the color 
distribution of the excess galaxies, which will be 
checked for consistency with expectations.

%; very red (R-K$_s$$&gt;$5) objects have been seen 
%around radio galaxies to z=1.2 and in some random fields (Dickinson 1993; Hu \&amp; 
%Ridgway 1994 \&amp; references therein); if such objects are z$&gt;$1 galaxies with old
%stellar populations, they must have formed at high redshift (z$\ge$5),
%and so might be more common in high-density cluster environments (where collapse
%tends to occur earlier) than in the field.
%
We will quantify the richnesses of the quasar environments by calculating
the spatial covariance amplitude (Longair and Seldner 1979), modified as necessary
to account for the large lookback time of our observations.
Detection of clusters around our quasars would enable us 
to study the evolution of the cluster galaxy luminosity function, since we will
probe 2 magnitudes below the present-day K$_*$ at the quasar redshifts;
to constrain the star formation histories of bright cluster galaxies, since blue
(R-K$_s$$\lesssim$2)~colors would indicate
ongoing star formation and red (R-K$_s$$\gtrsim$4.5) colors passive 
evolution after formation at high redshift 
(or possibly strong AGB light from a short recent burst of star formation);
and to constrain models of cluster formation by setting a lower limit to the space 
density of clusters over this redshift range and by providing data on cluster
morphology and member galaxy colors
to compare with simulations (Evrard \&amp; Charlot 1994) and with
similar data on any clusters at comparable redshifts eventually 
discovered optically, by X-ray emission, 
%or by association with intervening absorption line systems or radio galaxies.
by association with intervening absorption line systems, 
or by association with radio galaxies.

%longer on higher-z objs

%unpublished `Radio-Loud Survey' of Foltz et al., which contains $\sim$100 quasars 
%with 1.25$&lt;$z$_{em}$$&lt;$2.4, S(11 cm)$&gt;$100 mJy, and V$&lt;$18.5.  
%Each half of the sample will be comparable in terms of z$_{em}$, 
%absorber EW, M$_{\rm B}$, and radio properties.  

%Our redshift range of 1.4-2.0 is
%the range in which models of the evolution of the upper envelope of 
%the quasar luminosity function begin to overpredict the space densities 
%of bright RLQs (Yee \&amp; Ellingson 1993); knowledge of quasar environments
%in this redshift range will help determine why this is so. 
%opt&amp;JH colors later, if we see anything; also maybe narrowband

\medskip
\noindent{\bf REFERENCES}

\leftline{Coleman, Wu, and Weedman 1980, ApJS 43, 393}
\leftline{Cowie \&amp; Songaila 1993, in `Sky Surveys: Protostars to Protogalaxies', ed. B.T. Soifer, p.193}
\leftline{Ellingson, Yee, \&amp; Green 1991, ApJ 378, 476 (EYG91)}
\leftline{Evrard \&amp; Charlot 1994, ApJL 424, L13}
\leftline{Foltz, Chaffee, Weymann, and Anderson 1988, in `Quasar Absorption Lines:
Probing the Universe', p. 53}
\leftline{Hooper, Impey, Hewett, Francis, and Foltz 1994, in preparation}
\leftline{Longair, M. S., \&amp; Seldner, M. 1979, MNRAS, 189, 433}
\leftline{Mobasher, Sharples, and Ellis 1993, MNRAS 263, 560}
\leftline{Osmer, Green, Hall, Porter, and Warren 1994, in preparation}
\leftline{Steidel \&amp; Dickinson 1993, in `The Environment and Evolution of Galaxies', ed.  Thronson \&amp; Shull}
\leftline{Tyson 1988, AJ 96, 1}
\leftline{Yee \&amp; Green 1984, ApJ 280, 79}
\leftline{Yee \&amp; Green 1987, ApJ 319, 28}
\leftline{Yee \&amp; Ellingson 1993, ApJ 411, 43 (YE93)}

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\noindent{
{\bf Figure 1:} (Yee \&amp; Ellingson 1993)
Absolute nuclear magnitude vs. redshift for samples of RLQs and radio galaxies.
Solid dots denote objects in clusters of Abell richness 1 or more, open dots
objects in poorer environments, and solid lines show sample limits.
The upper dotted line shows the expected upper envelope of these samples
due to ``normal'' quasar evolution, whereas the dashed line follows the upper envelope
for objects in rich environments.  AGN in rich clusters evolve 5-6 times
more quickly than those in poor ones, possibly due to physical
changes in the cluster environments.  The evolution does not extrapolate to
z$&gt;$0.7; there are no quasars as bright as predicted.
}

% Assess the technical and scientific feasibility of the experiment.
% This section should consist of paragraphs of text only (no figures)
% that follow the \feasibility line.
%
% List objects, coordinates, and magnitudes (or surface brightness,
% if appropriate), desired S/N, wavelength coverage and resolution.
% Justify the number of nights requested as well as the specific
% telescope(s), instruments, and lunar phase. If you've requested
% long-term status, explain why this is necessary for successful
% completion of the science.

\feasibility
%oog

%INSTRUMENT: --IRIM 4m has 0.6"/pix --&gt; 150" on a side
%--(nov-jan) COB 4m has 0.3"/pix; COB 2.1m has 0.5"/pix but 4x less scope area, 
%        but 2x &gt; QE at K (and 3 at J)... 4(2.7) hrs to K=22(J=?)
%
%Some of our target galaxies may be extended, but one hour of integration
%will still allow detection down to K$_s$=20.8 in a r=2.4'' aperture.
%COB has about twice the QE of IRIM at K and half the linear pixel size, 
%so the time necessary for a detection of the same SNR and aperture on the sky
%will be half that required with IRIM.
%
%NOAO Newsletter \#34 states that IRIM can reach K=22 in 2 hours on the 4-m,
%agreeing with calculations using parameters from the preliminary IRIM manual.
%assuming a 3$\sigma$ detection; the 5$\sigma$ limit in 2 hours is K$_s$=21.6.
%K$_s$=18.8(19.5) at z=1.5(2), and 1 hour with IRIM on the 4-m will reach our target

We assume H$_o$=75 km s$^{-1}$~Mpc$^{-1}$\ and q$_o$=${{1}\over{2}}$.
We need to reach 2 magnitudes below L$_*$ to z=2 to detect enough cluster galaxies 
to see the cluster above the background.
Using K$_*$=-25.1 (Mobasher et al. 1993), an unevolved K$_*$ galaxy would have 
K$_s$=19.5 at z=2, and 1 hour with IRIM on the 4-m will reach our target of K$_s$=21.6.
&gt;From Coleman et al. 1980, an L$_*$ galaxy would have {\it at most} R=23.5 at z=2 for our 
cosmology, if it had a UV upturn and $&gt;$1 magnitude of luminosity evolution;
1 hour with the T2KB on the 4-m would also reach our target of R=25.5.
However, K$_s$ band galaxy counts (Cowie \&amp; Songaila 1993) show 
$\sim$22 galaxies per arcmin$^2$ from K$_s$=19.5-21.5,
while R band galaxy counts (Tyson 1988) show $\sim$35
galaxies per arcmin$^2$ from R=23.5-25.5.
Thus the expected excess of galaxies is easier to pick out in K$_s$; 
identical results in R would require 6 nights dark time.
We will obtain deep K$_s$ counts with 3 hours integration on 3 control fields
with existing deep optical data (Osmer et al. 1994) to be sure
that any zeropoint or other differences between our K$_s$ filter and that used for
the published counts do not affect our background counts.

After registering dithered images, each IRIM field should cover about 2\'\ on a side,
%(0.7 Mpc at z=2), 
thus including 88$\pm$9.4 background galaxies in that magnitude range
(assuming poisson fluctuations).
Typical Abell richness 0(1) clusters have excesses above the background
of 40(65) galaxies within 2 magnitudes of L$_*$ 
within r=1.5 Mpc of their center (Longair \&amp; Seldner 1979).
Since quasar host cluster galaxies are distributed with core radii of 
$\sim$125~kpc (Yee \&amp; Green 1984) and IRIM covers 0.7 Mpc on a side at z=2,
an Abell richness 0(1) quasar host cluster should show 
20(33) excess galaxies per IRIM field in the magnitude range.
Thus detecting clusters around these quasars is quite feasible, but we are also 
interested in differences between clusters.
If we assume for feasibility calculation that RLQs with 
associated absorption are found in richness 1 clusters, and those
without are found in richness 0 clusters, then we must image enough fields so
that the difference between the two average excesses (13 galaxies)
is several sigma above the background.  
This requires 16(10) fields for a 5(4) sigma detection.  
Imaging 16 fields will also allow leeway for a significant ($\geq$3$\sigma$)\ detection 
even if faint K$_s$ 
galaxy counts show $&gt;$$\sqrt{\rm N}$ fluctuations from field to field 
or if quasar host clusters have larger core radii at higher redshift.
Since we will spend 1 hour on each target 
%(slightly less for the lowest redshift and slightly more for the highest)
and have 32 quasars and 3 control fields in our sample, we request 4 nights of bright 
4-meter time to complete our program, allowing for 25\% overhead time.
COB would be suitable for this project if IRIM is unavailable, since 
its deeper images of a slightly smaller field would produce similar results.

%1.3*sqrt(N) yee
%...how many "bkgd" gals in field to K=21/22?
%        ...consider mag range 19.5-21.5; approx. 79750/deg^2, or 22.15/arcmin^2
%        IRIM covers 150"/side, or 120" after offset trimming: 88.6+-9.4/field
%        Abell 0/1 cluster is 40/65 gals is 4/6.7 sig xcess BUT that's within 1.5 Mpc.
%        If we cover the central r=~60" of the cluster, that's central r=~0.4 Mpc, 
%	 and combination of reduction due to smaller area and increase due to radial 
%	 concentration yields 1/2 of the Abell excess in our fields:
%        excess gals/field: 20/33; 2.1/3.5 sig
%if the excess signal is e gals/field and bkgd sig is s gals/field, to get an overall 
%N sig detn, need to reduce bkgd sig to (e/N), meaning must coadd (N^2)*(s/e)^2 fields.
%	A0: 20 gals/field; 3sig, bkdgsig=6.6, 2 fields; 4sig, bkgdsig=5, 4 fields;
%	 5sig, bkgdsig=4, 6 fields
%	A1: 33 gals/field; 5 sig, bkdsig=6.5, 2 fields.
%A0 vs. A1: A0 field has 108.6+-10.4 gals/field
%           A1 field has 13 galaxies in excess; 1.25sig
%3sig, bkgdsig=4.3, 6 fields; 4sig, bkgdsig=3.25, 10 fields; 5sig, bkgdsig=2.6, 16 fields
%...could do calc for reg. abell, w/0.35 of counts w/in irim field... should be doable
%...ok if regA0 has 14 excess, and regA1 23, diff.excess is 9 in bkgd of 102.6+-10.1
%...3sig, bkgdsig=3, 11 fields; 4sig, bkgdsig=2.25, 20 fields; 5sig, bkgdsig=2, 32 fields
%...16 fields gives 3.6sig for reg. abell clusts
%...and 4sig if the field-to-field flucts are 1.3*poisson, a la YG84
%
%However, COB's 0.3'' pixel scale is better for resolving objects very 
%close to the quasar sightline, which are more likely to be responsible for the 
%associated absorption.  COB's 1.25' FOV still covers a useful 0.6 Mpc 
%projected distance at z=1.5-2, and we could still obtain enough control
%field data in 3 hours to be able to compare our K$_s$ calibration to that of the
%published deep counts.
%Thus, either IRIM, COB, or ideally some combination thereof
%would be acceptable for our project.  
%Observations we make with COB will help characterize its performance 
%in detecting objects at very faint flux levels.

%Objects with moderate or strong absorption which are
%observable for at least a few hours in the spring include
%1206+43 (z=1.40), 0919+218 (1.42), 1416+159 (1.47), 0326+277 (1.53), 1323+65 (1.62),
%1556+335 (1.64), 1343+38 (1.84), 0033+098 (1.92), 0256-005 (1.99), 1157+01 (1.99), 
%and 1456+09 (1.99).  Other objects with weaker absorption, and ones with no detected 
%absorption, will be observed as well.
%
%0119-04 (z=1.94), fall

%0919+218 %1.421, virgin!
%1343+38 %1.84; virgin! only radio stuff
%1456+09 %1.991; virgin! a very few radio papers
%
%0256-005 %1.9951, is LBQS but so prob. post-89 lit; borderline strong
%0119-04 %1.948 str za&gt;ze known
%4C 09.01 %0033+098, 1.918; 0033+098 (1.918; 1.9036 and 1.7776), steidel Mg II
%1157+01 %BAL? 1.986; 1.72, 1.91-1.98, well-studied
%1206+43 %1.40; 1.37, 1.38, 1.39... known, obviously
%1416+159 %1.472in literature;(1.472; 1.473 ,1.478)
%
%%mediaum strong...
%4C 65.15 %1323+655; 1.618; 1.52, 1.61... see Junkk. 1991 ApJS 77
%0326+277 %1.533; virgin; med. str. za&gt;ze
%
%lbqs control non-CIV fields (18)... do a ned check on 'em.  
%
%ned -- means nothing of interest found in ned; ned ck means check ned to look
%for known ALS; 
%
%1430-0046 p ned --   1.0229           25.82          -25.87           57.59
%1229-0207   ned ck   1.0448           27.11          -26.01          999.92
%1324+0039   ned --   1.0607            26.4          -25.47          321.88
%1308+0109   ned --   1.0746            26.2          -25.65          171.27
%1137+0110   ned --   1.1379           26.58          -25.64          410.41
%hintzen etal AJ 88, 709 '83
%1210+1324   ned ck    1.141           27.37          -26.26         1424.71
%1239+0028   ned --   1.2138           24.37          -26.52            1.14ny
%1145+0235   ned --   1.2174           24.22          -26.09             1.2ny
%1435-0134   ned ck     1.31           26.68          -28.14           52.25
%
%1215+1121   ned ck   1.3984           27.03          -27.64          184.43
%1239+1118   ned --   1.4872           24.63          -26.26            2.63ny
%1333+0133   ned --    1.577           24.42          -26.59             1.2ny
%1319+0039   ned --   1.6191           26.75          -26.64          245.61
%1212+1445   nedbal?  1.6556           24.71          -26.71            2.08ny
%1320+0103   ned --   1.7765           24.64          -26.66            1.83ny
%1216+1754   ned --   1.8097           26.82          -26.72          264.09
%1331-0108   nedbal?  1.8813           24.99          -27.02            2.98ny
%1148-0007   ned ck   1.9761           28.27          -27.74         2937.46
%
% Why Kitt Peak? If you have access to telescopes through your home
% institutions, explain why KPNO facilities are needed.
%
% This section should consist of paragraphs of text only (no figures)
% that follow the \whykpno line.

\whykpno
%oog

The Steward Observatory NICMOS3 array cannot be used on the MMT; otherwise it 
could be used for this project.  The SO NICMOS3 array on the SO 90'' and the 
older NICMOS2 on the MMT both reach only K=20 in 1 hour integration.
Thus no SO facility is able to probe 2 magnitudes below K$_*$ at z=2, which is 
essential for this part of the thesis.
Most of the thesis can and is being done on SO telescopes,
which we are using to study quasar host clusters in the near-IR to z=1.
%and have proposed CTIO 1.5-m time for a similar study of southern quasars.
We plan to propose 3 nights of KPNO 4-m time with IRIM in the spring
to study the environments of a %well-defined 
sample of z=1-1.4 RLQs from the LBQS,
thereby extending this proposal's sample down in redshift to 
connect with the work being done at the SO 90'' and 61''.
However, the current proposal is self-contained and will require no more than 4 
clear nights of 4-m bright time; the spring project would merely be a useful extension.
%
The only other part of the thesis where KPNO time might conceivably be requested 
in the future is for 1.3m time to study low redshift objects where IRIM or SQIID's 
fields of view, and SQIID's simultaneous JHK capability, would prove useful.
 
%For the part of the thesis proposed in this project, we anticipate that 4 
%nights of 4-m time will be sufficient.  If the weather is good, this should 
%be the only proposal we will need to submit for the project.  
%If we lose some time to weather, we would ask for 2, 3, or 4 nights next fall,
%as appropriate, to complete observations of a useful number of objects.

% How effectively have you used NOAO telescope time in the past?
% List your allocation of telescope time at KPNO and CTIO during the
% past 2 years, together with the current status of the data (cite
% publications where appropriate).  Mark any allocations of time
% related to the current proposal with a \relatedwork{} command.

\thepast

10 nights to Osmer, Green, Hall, Porter, Warren on KPNO 4-m + Hydra in May \&amp; Sept
92 \&amp; May 93 for deep multi-color survey; publication in preparation; first results
presented at AAS 1/93.%}
 
3 nights to Green, Griffiths, Sarajedini on 4m in 1/94 for multislit
spectra of HST MDS galaxies.%}
 
9 nights to Green, Griffiths, Sarajedini on KPNO 4-m in 93 and 94 for
deep IR imaging of HST MDS galaxies with SQIID and IRIM.
 
4 nights to Yanny, York, Green et al. on KPNO 4-m + Fabry-Perot in Jan 93 for
[O II] detection in distant clusters; snow, wind, ice, fog.%}
 
12 nights to Green, Jannuzi, Bahcall et al. on KPNO 4m + RCSP in 1/93, 4/93, 1/94, 2/94
for multi-object spectra of galaxies in quasar absorber fields; data fully reduced and
being analyzed.
 
3 nights to Lauroesch, York \&amp; Green on KPNO 4-m + Echelle in 6/92 for
long-focus spectra of quasar absorption-line systems; Laureosch thesis nearing
completion.%}

9 nights to Boroson \&amp; Green on KPNO 4-m + RCSP in Sept 92, Mar 93, \&amp; Oct 93
for spectra of quasar emission-line profiles; 1992 data published.%}

6 nights to Boroson \&amp; Green on KPNO 2.1-m + Goldcam in Jul 93, for EUVE 
sources; data reduction in progress with Berkeley collaborators.

\end{document}

% Send proposal files to kpnoprop-submit@noao.edu.  The proposal and
% any figures MUST be submitted as separate email messages (1 file per
% message, please).  You will receive a short confirmation of receipt
% of each file.  The message that is sent back after this proposal file
% is submitted will explain how to identify the figures.
%
% Figures cannot be submitted until AFTER the proposal identification
% number has been returned to you via email; this will normally happen
% practically instantaneously.  Figures should also be submitted to
% kpnoprop-submit@noao.edu; they must be Encapsulated PostScript files
% (1 per message, please).  If you submit figures without supplying
% the proper identifying information (per the email explanation), the
% figures stand a reasonable chance of being lost, aggravation on your
% part (and probably KPNO staff) will ensue, and the overall flux of
% bad kharma in the universe will be increased.
%
% Please be careful in following the instructions.  We will do our best
% to handle all the submissions properly.  Please remember that you
% will be interacting mostly with a computer that has very limited
% expertise regarding KPNO proposals.  Thanks for your patience as
% we try out this new method of managing observing proposals at Kitt
% Peak National Observatory.

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