<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.
% revision 9/1/94
%
% General Instructions:
%   I. Where/how/when to submit this form:
%      Send THIS file (NOT the postscript version) to
%      kpnoprop-submit@noao.edu.  The proposal and figures must be
%      submitted as separate email messages.  Figures can be submitted
%      only AFTER the proposal identification number has been returned
%      to you via email.  Proposals must be received by midnight MST
%      on 31 March for the following August-January semester, and by
%      midnight MST on 30 Sept for the following February-July semester.
% 
% Before submitting this form electronically, be sure to run it through
% LaTeX and print it out to make certain that it looks the way that
% you wish the TAC to see it.
%       
%  II. If graduate student, your advisor must send a letter citing
%      a) amount of your observing experience
%      b) your academic standing 
%      c) how does this particular proposal fit into your overall thesis plans.
%         (What other telescope time is being used in the thesis; how many
%         additional runs on what telescopes will be required to finish the
%         thesis, etc.)
%      This letter may be e-mailed (by the thesis advisor) to
%      kpno-submit@noao.edu, or sent by letter, but must be received
%      by the proposal deadline.
% III. If you are planning to bring a Visitor Instrument, you must send a 
%      separate letter or email prior to Oct 15 or April 15 to make
%      sure we fully understand what will be involved in interfacing
%      your equipment to our telescopes.
%  IV. Questions? Please send email to "kpnoprop-help" or call Judy
%      Prosser at 602-325-9279.
%
% In specifying your telescope/instrument/detector combination, please keep
% the following list in mind.  This list is revised twice a year and
% is also available in the NOAO Newsletter (March and September
% issues):
%
% Primary Instruments:
%
%4-m Telescope:
%   PF Camera + direct CCD (T2KB)
%   Echelle + (UVFast, Red Long, or Blue Long camera) + CCD (T2KB)
%   RC Spec + CCD (T2KB)
%   Cryocam (with 800 x 1200 Loral Chip) [Note 1]
%   IR Cryogenic Spectrometer (CRSP)
%   Cryogenic Optical Bench (COB)
%   IR Imager (IRIM)
%   Fourier Transform Spectrometer (FTS) [Note 2]
%   PF Camera and photographic plates [Notes 1,3,4]
% 
%WIYN 3.5-m Telescope:
%   Hydra + Bench Spectrograph + CCD (T2KC) [Note 5]
%   CCD Imager (TBD) [Note 5]
%
%2.1-m Telescope:
%   GoldCam (CCD spectrometer with dedicated 1Kx3K Loral Chip)
%   CCD Direct Camera (T1KA)
%   Cryogenic Optical Bench (COB)
%   IR Cryogenic Spectrometer (CRSP)
%   IR Imager (IRIM) [Note 1]
% 
%Coude Feed
%   Coude Spectrograph + (camera 5 or 6) + CCD (F3KB or TI5)
% 
%1.3-m
%   Simultaneous Quad Infrared Imaging Device (SQIID)
%   Cryogenic Optical Bench (COB) 
%   IR Cryogenic Spectrometer (CRSP)
%   MarkIII Optical Photometer + GaAs Coldbox [Notes 1,4,6]
% 
%0.9-m
%   CCD Direct Camera + CCD (T2KA)
%   CCD Photometer (CCDPHOT) (T5HA)
% 
%Burrell Schmidt
%   Direct or objective-prism + CCD (S2KA)
%   Direct or objective-prism + photograph plates [Note 3]
%
%Notes: 1) Reduced Availability
%       2) Service observing only
%       3) Visitors must provide their own photograph plates
%       4) Limited to programs in progress
%       5) Shared-risk operation
%       6) No long-term program
%
%DETAILED INSTRUCTIONS FOR WIYN PROPOSALS
%To apply for shared-risk observations with the new 3.5m WIYN
%Telescope, use the standard KPNO proposal form.  Specify
%either "WIYN" or "WIYN - 2hr" as the telescope and either
%"HYDRA" or "WIYN Imager" as the instrument with instrumental
%details as needed.
%
%Programs for observations from the "2 hour queue" should use
%the standard form, but keep the scientific justification to a
%half page or less.
%
%Proposals for WIYN observations MUST INCLUDE the objects
%to be observed and other observational details using
%special QUEUE OBSERVING FORM available via anonymous ftp to
%"ftp.noao.edu" (in the kpno/kpnoforms) directory, or by sending
%email to wiynprop-request@noao.edu.
% You will receive instructions for how to submit the queue form
% electronically when you submit the observing request electronically.

\documentstyle[kpnoprop]{article}

\begin{document}

% Please don't remove these two lines:
%\proposalid{IDENT}	% Office use only
%\received{DATE}	% Office use only

% Give a descriptive title for the proposal in the \title command.
%
%    \title{TEXT}
%
% Note that a title can be quite long; LaTeX will break the title into
% separate lines automatically.  If you wish to indicate line breaks
% yourself, do so with a `\\' command at the appropriate point in
% the title text.
%oog

\title{The Environments of Radio-Loud Quasars at 1$&lt;$z$&lt;$1.4}

% Investigator's (PI and CoI) information blocks.

% Please give the investigator's name, institution and address, as
% well as an email address.  (The email address of the account used
% to send in the form will be used if you don't fill this in.)  Also
% give a phone number, and a number for a fax machine if you have
% access to one.  You must also indicate whether the investigator is
% a graduate student by putting a Y or an N inside the \gradstudent{}
% curly braces.
%
% Each member of the observing team is identified with several bits of
% information.
%
%    \name{OBSERVER NAME}
%    \affil{AFFILIATION}
%    \address{POSTAL ADDRESS}
%    \emailaddress{EMAIL ADDRESS}
%    \phone{TELEPHONE NUMBER}
%    \fax{FAX NUMBER}
%    \gradstudent{Y or N}
%
% Please note that the fax number does not print on the form at this
% time; this is intentional.  We can get your fax number from the
% electronic file if we really have to.
%
% DO NOT remove the \begin{PI} and \end{PI} or the \begin{CoI} and
% \end{CoI} lines.

\begin{PI}
\name{Patrick B. Hall}			% REQUIRED
\affil{Steward Observatory}		% REQUIRED
\address{933 N. Cherry Ave., Tucson AZ 85721}		% REQUIRED
\emailaddress{pathall@as.arizona.edu}		% May be left blank
\phone{(602) 621-6535}		% REQUIRED
\fax{}			% May be left blank
\gradstudent{Y}		% REQUIRED
\end{PI}

\begin{CoI}
\name{Richard F. Green}			% REQUIRED
\affil{KPNO/NOAO}		% REQUIRED
\address{950 N. Cherry Ave., Tucson AZ 85726}		% REQUIRED
\emailaddress{green@noao.edu}		% May be left blank
\phone{(602) 327-5511}		% REQUIRED
\fax{}			% May be left blank
\gradstudent{N}		% REQUIRED
\end{CoI}

\begin{CoI}
\name{}			% REQUIRED
\affil{}		% REQUIRED
\address{}		% REQUIRED
\emailaddress{}		% May be left blank
\phone{}		% REQUIRED
\fax{}			% May be left blank
\gradstudent{}		% REQUIRED
\end{CoI}

\begin{CoI}
\name{}			% REQUIRED
\affil{}		% REQUIRED
\address{}		% REQUIRED
\emailaddress{}		% May be left blank
\phone{}		% REQUIRED
\fax{}			% May be left blank
\gradstudent{}		% REQUIRED
\end{CoI}

% You can supply more CoI blocks, but only the first three will be
% displayed on the form.  

% Give an abstract of the scientific justification.  Please write
% the abstract between the \begin{abstract} and \end{abstract} lines.
% Limit yourself to approximately 175 words.

% DO NOT remove the \begin{abstract} and \end{abstract} lines.

\begin{abstract}

%oog

We propose to investigate the environments of radio-loud quasars (RLQs) at 
1$&lt;$z$&lt;$1.4 through deep K$_s$ imaging on the 4-m in conjunction with 
deep {\it r} and {\it i} imaging on the Steward Observatory 2.3-m,
as part of a project to investigate the environments and 
environment-evolution connection of RLQs 
over the redshift range 0.6$&lt;$z$&lt;$2 and to study the nature of 
%z$_{abs}$$\sim$z$_{em}$ 
``associated'' CIV absorption.
%
This 1$&lt;$z$&lt;$1.4 sample consists of 36 RLQs well-matched in M$_{abs}$, 
P$_{rad}$, and radio spectral slope to our samples at 0.6$&lt;$z$&lt;$1 
and 1.4$&lt;$z$&lt;$2.0, allowing us to disentangle correlations of quasar 
environment with such properties from evolution of the environments
with redshift.
%
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 and i-K colors at these
redshifts, and to constrain cluster formation models by setting a lower limit 
to the space density of clusters in this redshift range.
 
\end{abstract}

% Indicate whether this proposal is part of your PhD thesis work by
% putting a Y or an N inside the \thesis{} curly braces.  If this is
% thesis work (a "Y" answer), you must have a separate letter sent;
% please see instructions above.

\thesis{Y}

% Indicate whether you are requesting long-term status by putting
% a Y or an N inside the \longterm{} curly braces.  If you do want
% long-term status (a "Y" answer), please tell us the number of nights,
% number of semesters, and what telescopes by filling in \longtermdetails{}.
% Please be brief; \longtermdetails is limited to one line.

\longterm{N}
\longtermdetails{}

% List the details of the observing runs being requested, for
% UP TO THREE runs.  The parameters for each run are segregated
% between \begin{obsrun} and \end{obsrun} lines.  Please be sure
% that the information is isolated properly for each run.
%
%   \telescope{}	For example, \telescope{4m}
%   \instrument{}	For example, \instrument{PFCCD + T2KB}
%   \numnights{}	For example, \numnights{3}
%   \numdays{}		For example, \numdays{}
%   \lunarphase{}	For example, \lunarphase{4}
%   \optimaldates{}	For example, \optimaldates{Sept--Nov}
%   \acceptabledates{}	For example, \acceptabledates{Sept -- mid-Dec}
%
% Please select telescope and instrument identifiers from the list
% at the top of the form.
% Instrument combinations may be specified with "+".
% PLEASE ALSO IDENTIFY FILTERS YOU MAY NEED; for example;
% "Direct CCD Cam + T1KA + UBVRI + Halpha (50A)"
%
% \numnights and/or \numdays should give the number of nights of the run
% (or for 4m FTS use, e.g., the number of days).  \lunarphase should
% specify the maximum number of nights from new moon for this run.
%
% \optimaldates should contain the range of OPTIMAL dates (should be
% 2-month window).
%
% \acceptabledates should give the range of ACCEPTABLE dates (i.e., you
% would not accept time outside those limits).
%
% If you are applying for time on WIYN, specify either "WIYN" or
% "WIYN 2hr". YOU WILL ALSO NEED TO SUBMIT A SEPARATE "QUEUE OBSERVING
% FORM", available by sending e-mail to "wiynprop-request@noao.edu" or
% via anonymous ftp to "ftp.noao.edu", cd kpno/kpnoforms.
% You will receive instructions for how to submit the queue form
% electronically when you submit the observing request electronically.

% DO NOT remove the \begin{obsrun} and \end{obsrun} blocks.

%oog

\begin{obsrun}
\telescope{4m}
\instrument{IRIM (COB acceptable); K$_s$ filter}
\numnights{3}
\numdays{}
\lunarphase{14}
\optimaldates{Mar-Apr}
\acceptabledates{Feb-May}
\end{obsrun}

\begin{obsrun}
\telescope{}
\instrument{}
\numnights{}
\numdays{}
\lunarphase{}
\optimaldates{}
\acceptabledates{}
\end{obsrun}

\begin{obsrun}
\telescope{}
\instrument{}
\numnights{}
\numdays{}
\lunarphase{}
\optimaldates{}
\acceptabledates{}
\end{obsrun}

% You may NOT supply more obsrun blocks.  Three is the limit.

% If there are dates that you cannot use for non-astronomical reasons,
% (i.e., other than moon phase or when your object is up)
% please give the dates by filling in the curly braces in \unusabledates{}.
% Please be brief; \unusabledates is limited to one line.

\unusabledates{May 4-7th: family wedding (Hall)}

% 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.
% Note that the scientific justification should be limited to one page,
% with an additional page for figures and references.
% If you are proposing for a "WIYN 2-hr" (short) observation,
% you should limit yourself to half a page.

% In order to include an EPS plot, you should use the LaTeX "figure"
% environment.  The plot file is included with the \plotone{FILENAME}
% command; two side-by-side plot files can be included by typing
% \plottwo{FILENAME1}{FILENAME2}.  Use \caption{} to specify a caption.
%
% \begin{figure}
% \plotone{sample.eps}
% \caption{Sample figure showing important results.}
% \end{figure}
%
% You can also "customize" figure location using "plotfiddle";
% see the example in "sample.tex".
%
% If you wish to use our "reference" environment, follow
% the following example:
%\begin{references}
%\reference Armandroff \&amp; Massey 1991 AJ 102, 927.
%\reference Berkhuijsen \&amp; Humphreys 1989 A\&amp;A 214, 68.
%\reference Massey 1993 in Massive Stars: Their Lives in the Interstellar
%  Medium (Review), ed. J. P. Cassinelli and E. B. Churchwell, p. 168.
%\reference Massey, Armandroff, \&amp; Pyke 1993, in prep.
%\end{references}

\justification

%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.
%oog

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 since even deep field galaxy surveys do not turn up many galaxies at z$&gt;$1, 
we must resort to other methods to discover them.
One such methods that has been successful at z$&lt;$0.7 is to look for galaxies 
associated with quasars.
%
Intrinsically luminous (M$_{\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, quasar environments are known to evolve:
at z$&lt;$0.5 only {\it faint} RLQs are seen in richness 1 clusters (Fig~1).
EYG91 explain this evolution by postulating that galaxy interactions (more 
frequent in young, low-$\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;$0.7 (Fig~1).
Yee \&amp; Ellingson 1993 (YE93) hypothesized that the cluster formation rate 
dropped considerably at 
z$\sim$0.7, so that in rich clusters at z$&lt;$0.7, almost all the quasars we see 
are old ones fading on the host cluster's dynamical timescale.  
If this model is correct, luminous RLQs should still often be found in rich 
clusters at z$&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, mostly steep spectrum sources, show additional evidence for 
being located in rich environments, in the form of ``associated'' CIV 
absorption systems (Foltz et al. 1988).
%
These 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.
Since deep imaging can greatly constrain this cluster hypothesis while 
extending our knowledge of RLQ environments to the z=1.4-2 range, 
we have been granted 4-m time this fall 
to image in K$_s$ the fields of 32 steep-spectrum RLQs, half of which 
show strong associated CIV absorption and half of which show no such absorption.
We are also using SO telescopes to obtain deep {\it r}~and {\it i}~images of 
these objects and K$_s$ images of 0.6$&lt;$z$&lt;$1 RLQs with existing optical data.
We now propose to image in K$_s$ a sample of RLQs at 1$&lt;$z$&lt;$1.4 to 
complete our study of quasar environments from z=0.6 to 2.0.
Knowledge of the environments of RLQs in this redshift range will 
help constrain models of quasar formation, fueling, and evolution.

RLQs in this intermediate-redshift sample have been carefully selected, 
primarily from the 1 Jy survey (Stickel et al.) and the LBQS (Hooper et al.), 
to evenly cover the redshift range z=1-1.4 and complement our work at other 
redshifts as much as possible.  The sample spans the range of 
M$_{\rm abs}$ and P$_{\rm rad}$ 
%M$_{\rm abs}$ (-23 to -28) and P$_{\rm rad}$ (10$^{27-29}$ W/Hz) 
covered in both the low-z and high-z samples, 
allowing us to study how environment correlates with such properties over a 
small redshift range and thus disentangle such effects from redshift evolution.
%
The sample is evenly split between flat and steep radio spectrum sources,
allowing us to track the evolution of steep-spectrum RLQ environments from 
z=0.6-2 
and to compare flat- and steep-spectrum RLQ environments over the range 
z=0.6-1.4;
at z$&lt;$0.7 YE93 find no difference in their environments, but nothing is
known at higher redshift.
%
These data will also allow the study of the environments of RLQs from a 
well-defined optically-selected quasar sample from z=0.3-1.4, since
imaging of LBQS RLQs at z$&lt;$1 is being done by us and by Hooper et al.
%
We avoid objects with known associated CIV absorption, although such 
information is not always available for objects at these redshifts, 
to avoid introducing another variable into the study in this redshift range.
%
Where possible, we have also avoided objects with high-z intervening absorption
to reduce confusion about with which system any detected galaxies are 
associated.
Finally, we have preferentially selected HST Quasar Absorption Line Key Project
targets, in order to eventually know whether low-z intervening absorption, 
and possibly associated CIV absorption, is present in the objects' spectra.

Imaging to K$_s$=21.1 detects galaxies as faint as 1/6 of the present-day 
K$_*$ to z=1.4.  
%
%We will be able to detect clusters of Abell richness 0 or greater to z=1.4
%and differences of one Abell richness class or more between the environments 
%of various subsamples of our data (flat vs. steep spectrum, etc.) simply by 
%the excess galaxy counts in the
%magnitude range expected for galaxies at the quasar redshifts.
%
To obtain color information invaluable for discriminating foreground from 
associated galaxies, we will image our fields to r=24 and i=22.5 at the SO 2.3m.
Concentrations near the quasars of galaxies with unusual colors would be
additional evidence for clustering, but in either case a statistical comparison 
of the r-K$_s$/i-K$_s$ color distribution of faint quasar- and 
control-field galaxies (from control fields we will image this fall)
will yield the color distribution of the excess 
galaxies, which will be checked for consistency with expectations.
%
%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 back to a time when clusters and 
some cluster galaxies may have been newly forming;
%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
via their r-K$_s$/i-K$_s$ colors;
%
%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 at these redshifts 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.

\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, submitted}
\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{Stickel, Meisenheimer, and Kuhr 1994, A\&amp;AS 105, 211}
\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)}

\bigskip

\bigskip

\bigskip

\bigskip

\bigskip

\bigskip

\bigskip

\bigskip

\bigskip

\bigskip

\bigskip

\bigskip

\bigskip
 
\bigskip
 
\bigskip
 
\bigskip
 
\bigskip
 
\bigskip
 
\bigskip
 
\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

%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 

%but going deeper would allow r-K,i-K colors rather than limits for more objs

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=1.4 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$_s$=19.1 at z=1.4, and 1/2 hour with IRIM on the 4-m will reach our target of 
K$_s$=21.1.  
From Coleman et al. 1980, an L$_*$ galaxy would have {\it at most}
R=22.5 at z=1.4 for our cosmology, if it had a UV upturn and $\sim$1 magnitude 
of luminosity evolution, and 1/2 hour with the 4-m/T2KB would reach our target
of R=24.5.  
Galaxy counts in K$_s$ (Cowie \&amp; Songaila 1993) and R (Tyson 1988) show 
$\sim$17 galaxies per arcmin$^2$ from K$_s$=19.1-21.1 or R=22.5-24.5.  
Thus the expected excess of galaxies might be equally detectable in R with 
3 nights dark 4-m time. 
However, we can use the SO 2.3m to get deep optical data (r=24, i=22.5)
on our fields in a feasible number of nights, whereas we could not use it to 
get IR data to K$_s$=21.1 on our fields in the same amount of time.
Obtaining both IR and optical data allows us to study the color evolution
of quasar host cluster galaxies all the way from z=0.6 to 2.

After registering dithered images, each IRIM field should cover about 2\'\ on 
a side, thus including 68$\pm$8.3 background galaxies from K$_s$=19.1-21.1 
(assuming poisson fluctuations).
Typical Abell richness 0(1) clusters have excesses above the background
of 40(65) galaxies within 2 magnitudes of L$_*$ 
within r=1.5 Mpc of their center (Longair \&amp; Seldner 1979).
Since quasar host cluster galaxies are distributed with core radii of 
$\sim$125~kpc (Yee \&amp; Green 1984) and IRIM covers 0.7 Mpc on a side at z=1.4,
an Abell richness 0(1) quasar host cluster should show 
20(33) excess galaxies per IRIM field in the magnitude range we will cover.
Thus detecting clusters around these quasars is feasible, but we are also 
interested in differences between clusters around quasars with different
M$_{abs}$, spectral slope, etc.
If we assume for a feasibility calculation that steep-spectrum RLQs are found 
in richness 1 clusters and flat-spectrum RLQs in richness 0 clusters, then we 
must image enough fields so that the difference between the two average 
excesses (13 galaxies) is several sigma above the background.  
%
%13 gals is 5sig detn if sig=2.6, which occurs if sqrt(n)=8.3/2.6 n=10
%13 gals is 4sig detn if sig=3.25, which occurs if sqrt(n)=8.3/3.25 n=7
%
Imaging 18 fields of each quasar type will yield a 6$\sigma$ detection in this
case and will allow leeway for a significant 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 1/2 hour on each target and have 36 quasars in our sample, 
we request 3 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.

%This fall we will obtain control field data at K$_s$ to ensure that any 
%zeropoint or other differences between our K$_s$ filter and that used for the 
%published counts do not affect the background counts we will use for the 
%z$&gt;$1 quasars.

% 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=1.4, 
which is essential for this part of the thesis.
Most of the thesis can and is being done on SO telescopes; we are using them to
study z$&lt;$1 quasars in the near-IR and to do deep {\it r} and {\it i}
imaging of our z=1-2 quasar fields.
%
The current proposal is self-contained and will require no more than 3
clear nights of 4-m bright time.
If our December 1994 run for the z=1.4-2 sample is affected by weather
enough that an adequate size sample is not observed, 
we would ask for an appropriate number of nights with COB next fall 
to complete observations of a useful number of objects.
Beyond that possibility, no further KPNO time will be requested for this thesis.

% 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

\relatedwork{3.5 nights upcoming to Hall \&amp; Green on 4-m with IRIM in 12/94 for 
observations of z=1.4-2 Radio-Loud Quasar fields as part of Hall's thesis.}

3 nights to Osmer, Green, Hall, Porter, Warren on KPNO 4-m + Hydra in May 
93 for deep multi-color survey; publications in preparation.
 
7 nights to Green, Griffiths, Sarajedini on 4m in Jan and Oct 94 for multislit
spectra of HST MDS galaxies; first results in ApJ Letters.
 
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.
  
12 nights to Green, Jannuzi, Bahcall et al. on KPNO 4m + RCSP in 4/93, 1/94, 
2/94 for multi-object spectra of galaxies in quasar absorber fields; data 
fully reduced and being analyzed.

2.5 nights on KPNO 2.1-m and 6 nights on Burrell Schmidt to Jannuzi, Green,
and collaborators for imaging of galaxy fields on quasar absorber sightlines.

6 nights to Boroson \&amp; Green on KPNO 4-m + RCSP in 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; paper in preparation 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.
%
% Similarly, the completed "WIYN queue" form should be submitted
% to kpnoprop-submit@noao.edu in an analogous manner as figures.
%
% 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.
</pre></body></html>