<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.

\title{The Evolution of Faint Quasars at High Redshift}

% 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 S. Osmer}			% REQUIRED
\affil{Astronomy Dept.}		% REQUIRED
\address{174 W. 18th Ave., Columbus, OH 43210-1106}		% REQUIRED
\emailaddress{posmer@payne.mps.ohio-state.edu}		% May be left blank
\phone{614 292 2022}		% REQUIRED
\fax{614 292 2928}			% May be left blank
\gradstudent{N}		% REQUIRED
\end{PI}

\begin{CoI}
\name{Patrick B. Hall}			% REQUIRED
\affil{Steward Observatory, University of Arizona}		% REQUIRED
\address{Tucson, AZ}		% REQUIRED
\emailaddress{pathall@as.arizona.edu}		% May be left blank
\phone{602 621 6535}		% REQUIRED
\fax{}			% May be left blank
\gradstudent{Y}		% REQUIRED
\end{CoI}

\begin{CoI}
\name{Richard F. Green}			% REQUIRED
\affil{NOAO}		% REQUIRED
\address{Tucson, AZ}		% REQUIRED
\emailaddress{green@noao.edu}		% May be left blank
\phone{602 325 9299}		% 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}

% 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}

We propose spectroscopic observations of high-redshift ($3 &lt; z &lt; 5$)
quasar candidates and faint quasar/AGN candidates with expected
$z &lt; 2.3$ selected from a deep, multicolor survey with the 4-m.
The new data will be critical to determining the nature of
the decline in space density of quasars at $z &gt; 3.3$ at 
less extreme luminosities than originally studied and for
distinguishing between luminosity and density evolution
for $z &lt; 2.3$.  We will also advance our knowledge of
the evolution of the environments
of quasars at $z &gt; 1$.

\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{N}

% 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.

\begin{obsrun}
\telescope{4-m}
\instrument{Cryocam + Loral Chip + Grism 770 + Long-slit and Multislit Modes}
\numnights{4}
\numdays{}
\lunarphase{7}
\optimaldates{Apr-May}
\acceptabledates{Mar-Jul}
\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{April 26-30, May 4-7}

% 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

We have carried out a deep multicolor survey for quasars in 0.83 sq deg 
of sky at high 
galactic latitude with a 2048 x 2048 CCD and the KPNO 4-m telescope.  It
consists of
photometrically calibrated images in six filters covering the 
wavelength range 0.34 to 0.86 
$\mu$ and reaching to B = 23.8 (5 $\sigma$ limit in a single exposure).  
The 125 CCD 
images represent a unique data set in terms of area, spectral coverage, 
and deep limiting 
magnitude.  The images have been analyzed with FOCAS, and a catalog
of 21,375 stellar objects containing positions, magnitudes in each
filter, and error estimates has been compiled.
Spectroscopic identifications have been made with Hydra for 180 candidates.
We found 41 quasars with $0.6 &lt; z &lt; 4.3$ and 41 
emission-line galaxies with 
$0.05 &lt; z &lt; 0.8$, along with a variety of rare or unusual stars.  

The main goals of the survey are 
to study the luminosity function of high-redshift quasars at 
fainter magnitudes than have 
been previously attained and of quasars/AGNs near redshift 2.  
The high-z quasars are 
critical to understanding how the apparent decline in 
space density at $z &gt; 3.5$ (Warren, Hewett, and Osmer (WHO) 1994, 
Schmidt, Schneider and Gunn (SSG) 1991) depends on luminosity.
If there are quasars that have been dimmed by dust associated
with intervening absorbers, they might begin to appear at fainter
magnitudes.  Indeed, we have significantly
more faint candidates than predicted
by WHO and SSG.   
Similarly, at redshifts about 2, pushing to low-luminosity 
quasars and to
AGNs is essential to understanding the issues of luminosity 
and density evolution.  While 
the current luminosity function data for quasars is 
often parameterized by luminosity 
evolution models, the questions of long-lived vs. short-lived
quasars and dramatic number density evolution at a given
luminosity are very much alive.  Answers depend on determining
the luminosity function at $z \approx 2$ down to sufficiently
faint magnitudes to distinguish between the competing hypotheses. 
Having reached the limit of Hydra and determined the initial 
properties of our survey, we are 
now in a position to observe samples of fainter candidates 
that will enable an attack on such questions. 
Specifically, we propose to:

\begin{itemize}

\item Complete the spectroscopic followup of the high-redshift
($2.3 &lt; z &lt; 5$) candidates with $R &lt; 22$.  No other published survey
probes to such a faint limit.  As mentioned above,
our preliminary results indicate
a larger number of such quasars than predicted by
the results of WHO and SSG; however, this is only speculation
in the absence of spectroscopic confirmation.

\item  Obtain spectra of a representative sample of faint, UVX 
candidates to yield a significant estimate of the luminosity
function for $z &lt; 2.3$ down to B = 23.1, fainter than has been
done to date.

\item Use the multislit capability of Cryocam to study the galaxies
in the vicinity of the UVX selected quasars.  Ellingson, Yee, and Green
(1991) and Yee and Ellingson (1993) have shown how the environment of
quasars and quasars themselves evolve dramatically at lower redshifts.
We are in a position to 1) investigate
the environments of optically selected quasars at redshifts beyond 1;
and 2) investigate the physical association of galaxies and absorbers
at intermediate redshifts, the sizes of absorption cross sections,
and the connection between absorbers and peaks in the galaxy
redshift distribution.

\item Confirm the spectroscopic identifications of objects from the
Hydra survey whose nature or redshift is uncertain owing to the
low S/N ratio of the data.  This will provide the needed and solid
basis to anchor our results.

\end{itemize}

\begin{references}
\reference Ellingson, E., Green, R. G., Yee, \&amp; H. K. C. 1991, ApJ,
378, 476

\reference Schmidt, M., Schneider, D. P., \&amp; Gunn, J. E. 1991,
in the Space Distribution of Quasars, ed. D. Crampton (San
Franciso: ASP), 109

\reference Warren, S. J., Hewett, P. C., \&amp; Osmer, P. S. 1994,
ApJ, 421, 412

\reference Yee, H. K. C., and Ellingson, E. 1993, ApJ, 411, 43

\end{references}
 


% 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

Our objects for this semester
are in fields at $14^H, 0\deg$ and $17^H, +50\deg$.  They
are too faint to reach with Hydra and require the
best faint object spectroscopic capability of
the 4-m, Cryocam, which has twice the sensitivity
of the R-C Spectrograph.  If Cryocam is not available, we
can make use of R-C Spec by increasing exposure times.
In priority order, we plan to observe:

10 faint ($20 &lt; R &lt; 22$) $z &gt; 3$ quasar candidates that still
need spectroscopic identification.  Allowing 1 hour per
object, we need 1.2 nights.

A sample of 10-15 UVX candidates to determine the
luminosity function of quasars with $z &lt; 2.3$ down to B = 23.1.
We will also observe galaxies in the vicinity of these candidates
in the same exposures; the galaxies will be selected from the
imaging data.  This will require 1.8 - 2.8 nights at 1.5 hours  
per field.

4 objects from our Hydra observations with
tentative broad lines of unknown redshift, a half-dozen
objects that could
be quasars with weak lines, and at least one very late-type star
(M6 or later) that need further spectroscopic observation to
confirm their nature.  These will be observed in the remaining
time of the four nights.

We also have brighter objects from the survey that we can observe
in less than ideal weather conditions.

% 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

The Perkins 1.8-m telescope at Lowell Observatory is too small
to carry out observations of the faint quasars proposed here.

% 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

KPNO 4-m + Hydra: Oct. 92, 3 nights; May 93, 3 nights.  These were
successful runs and provide the basis for the present proposal.
The data have been reduced and analyzed.  Hall presented a first
paper on the results for his candidacy exam.  We are now preparing
the first articles on the survey for the ApJ.

Related publications by P.I. based on KPNO and
CTIO data are Warren, Hewett, and Osmer 1994,
ApJ, 421, 412; and Osmer, Porter, and Green, 1994, ApJ (in press). 

\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.

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