%-------------------------------------------------------------------
% This is a template for IRAM Proposals (originally created by R.Lucas)
% Deadline  08 Sep 2005
% Please use always the most recent update of proposal.sty
% (R. Neri + C.Thum Jul 10th, 2005)
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% ATTENTION:
%
% The following line follows the LaTeX 2.09 syntax, 
% but should be also accepted by  LaTex2e. 
%
% You may prefer to comment it out and use the next two commands 
% instead, if you want to use the full functionalities of LaTeX2e
% (such as \includegraphics for instance). 
%
% The 11pt is ESSENTIAL in both cases to preserve readibility since 
% we may have to fax the proposals to PC members.
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% LaTeX2.09 (but should work also with LaTeX2.09):
% ---------
%\documentstyle[11pt,proposal]{article}
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% LaTex2e only:
% -------
\documentclass[11pt]{article}
\usepackage{proposal}
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\begin{document}
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% Instrument (%sign  comment in or out)
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%\plateaudebure
\picoveleta
%\blank
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% Title and abstract (replace both)
%-------------------------------------------------------------------
\title{MAMBO observations of $z \sim 6$ SDSS QSOs}

\abstract{
We propose to observe four 
$z \sim 6$ SDSS QSOs with MAMBO to search
for thermal emission from warm dust. Three of these sources were discovered 
very recently in the Sloan DS Survey (Fan et al. in prep.). This proposal is 
a continuation of our successful program to detect strong thermal emission in
the most distant QSOs known, and to 
study the evolution of the radio-to-optical 
spectral energy distributions from $z = 2$ to 6. Our goals
include: (i) studying the possible co-eval 
black hole and spheroidal galaxy formation, (ii) demonstrating the 
existence of large reservoirs of dust, and potentially molecular gas,
in the first galaxies, 
and (iii) probing the host galaxy properties 
of the most distant QSOs, into the epoch of cosmic reionization.
}

%-------------------------------------------------------------------
% Proposal Category (Plateau de Bure only) (%sign  comment in or out)
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%\onemmcat
\threemmcat
%\dualfrcat
%\timefiller
%\specialcat
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% Proposal Type (%sign  comment in or out)
%-------------------------------------------------------------------
\exgalcont
%\exgalco
%\exgalother
%\solarcont
%\solarlines
%\solarother
%\galcont
%\gallines
%\galcloud
%\galcse
%\galyse
%\galchem
%\galother
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% Observing type (Plateau de Bure only) (%sign  comment in or out)
%-------------------------------------------------------------------
%\mapping
\detection
%\sizemeasure
%\snapshot
%\mosaic
%\othertype
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% Proposal history : fill in or comment out
%
% If this proposal is a continuation or a resubmission of a previous
% IRAM proposal, please describe the history of the proposal using
% the \proposalhistory{} command at the end of this file. 
%
%-------------------------------------------------------------------
%\resubmit{}
\continue{163-04}
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% Amount of time (Pico Veleta only)
%-------------------------------------------------------------------
% this  proposal
\hours{13}			
% {for full completion} {already allocated}
\totalhours{}{}
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% Sidereal time intervals:  {start} {end} {number of intervals}
%-------------------------------------------------------------------
\lsta{7h}{17h}{1}
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% Receivers (Pico Veleta only) 
%-------------------------------------------------------------------
%\receiveraandb
%\receivercandd
%\receiveraandd
%\receiverbandc
\bolometer
%\hera
%-------------------------------------------------------------------
% Observing frequencies, CORRECTED FOR REDSHIFT 
% Pico Veleta:     \frequencies{first line}{second line}
% Plateau de Bure: \frequencies{3mm freq.}{1.3mm freq.}
% Note: the second pair of braces should be present even if unused. 
% \frequencies{115.3 231.2} { }
%-------------------------------------------------------------------
\frequencies {250}{}
%----------------------------------------------------------------
% Plateau de Bure confidentiality: enter here information (such as 
% frequencies, coordinates, ...) that should be kept confidential.  
%----------------------------------------------------------------
\confidential{None}
%----------------------------------------------------------------
% Pico Veleta Special requirements (such as dates ...)
%----------------------------------------------------------------
\specials{None}
\pooledobserving
%\serviceobserving
%\remoteobserving
%\polarimeter
%----------------------------------------------------------------
% Plateau de Bure configurations: 
% - Check ANY if no specific array configurations are needed
% - Check NEW if the extended configurations (N46,E68) are needed 
%         but consider that these configurations cannot be guaranteed
%         for the winter 2005/2006 scheduling period.
%----------------------------------------------------------------
%\confnew
%\confa
%\confb
%\confc
\confd
%\confany
%----------------------------------------------------------------
% Uncomment the \zerospacing line if a zero-spacing measurement at 
% the 30m telescope is necessary to fulfill the goals of the project.
% See also the Call for Proposals Feb 2004.
%----------------------------------------------------------------
%\zerospacing 
%----------------------------------------------------------------
% Principal Investigator (including name, address, telephone, fax, email)
%----------------------------------------------------------------
\pifirstname{Chris}
\pilastname{Carilli}
\piinstitute{NRAO}
\pistreetandnumber{PO Box O}
\pizipandcity{Socorro NM 87801}
\picountry{USA}
\piphone{1-505-835-7000}
\pifax{1-505-835-7027}
\piemail{ccarilli@nrao.edu}
%----------------------------------------------------------------
% A brief remark in case the proposed observations are part 
% of a Diploma thesis, PhD thesis, Marie-Curie fellowship, ... 
% specify here who is the fellow, who the supervisor, ... 
%----------------------------------------------------------------
%\pinote{}      
%----------------------------------------------------------------
% Coauthors 
% macro: \coauthor{First_Name Last_Name}{affiliation}{affiliation country} 
% use one \coauthor{ }{ }{ } macro for each coauthor. 
% You may add as many \coauthor{ }{ }{ } macros as needed ...
%----------------------------------------------------------------
\coauthor{F. Bertoldi}{Bonn Univ.}{Germany}
\coauthor{F. Walter}{MPIA}{Germany}
\coauthor{X. Fan}{U. Arizona}{USA}
\coauthor{K. Menten, A. Beelen}{MPIfR}{Germany}
\coauthor{P. Cox}{IRAM}{France}
\coauthor{A. Omont}{IAP}{France}
\coauthor{M. Strauss}{Princeton}{USA}
% ...
%----------------------------------------------------------------
\reducer{He}                     % For Plateau de Bure
\observer{Bertoldi, Walter, et al.}  % For Pico Veleta
%----------------------------------------------------------------
% Source list
% Please note the change: only one line for each source should be 
% given now: 
% Name   & RA      &    DEC    &   V(LSR) \\
% The epoch is given as a separate parameter.
% ADDITIONAL souces which do not fit here shall be entered in
% the new macro "\extendedsourcelist" listed at the end of this file
%----------------------------------------------------------------
\epoch{J2000.0}  % J2000 epoch coordinates preferred
\sourcelist{
0818+1722 & 08:18:27.40 & 17:22:51.8 & 6.00 \\
0927+2001 & 09:27:21.82 & 20:01:23.7 & 5.79 \\
1335+3533 & 13:35:50.81 & 35:33:15.8 & 5.93 \\
1602+4228 & 16:02:54.18 & 42:28:22.9 & 6.07 \\
}
%----------------------------------------------------------------
% The following command will actually produce the front page. 
%----------------------------------------------------------------
\frontpage
%
%----------------------------------------------------------------
% Technical details for Plateau de Bure
%----------------------------------------------------------------
%Source list
\techsourcelist{\small
\begin{tabular}{lrrr}
\hline
Source    & RA & DEC & LSR Velocity \\
& (J2000.0)   & (J2000.0)     & (km/s)\\
\hline
0221+375  &  02:27:30.813 & 37:49:32.624    & $+$0 \\
\hline
\end{tabular}}
%Size of largest structure in (arcseconds)
\structuresize{unresolved}
%Expected continuum flux:
\continuumflux{1-2 Jy}
%Expected continuum source size:
\continuumsize{unresolved}
%
% --- For pure continuum projects:
% Preferred observing frequency:
\continuumfreq{}
%Expected Line contamination at observing frequency:
\contamination{}
% Frequencies to avoid:
\avoidfreq{}
%
% --- For line projects:
% Receiver configuration: for each receiver give: line name, 
% central frequency in GHz (line appearing at IF3=390MHz) and side band.
\recone    {13CO(1-0)} {110.20137} {USB}
%\rectwo   {12CO(2-1)} {230.538}   {LSB}
% Correlator configuration: 
% for each unit give bandwidth (MHz), IF3 frequency (MHz), receiver number 
%  (1 is 3mm, 2 is 1.3mm), and Correlator mode SSB (default) or DSB
\specone  {20}  {390}  {1} {}
\spectwo  {320} {260}  {1} {}
\specthree{320} {520}  {1} {}
\specfour { 80} {400}  {1} {}
\specfive { 80} {540}  {1} {DSB}
\specsix  {320} {270}  {2} {}
\specseven{OFF} {}     {}  {}
\speceight{OFF} {}     {}  {}
% Expected width of spectral line (to zero power)
\linezerowidth{$\sim 2$ km/s}
% Number of lines observed simultaneously (add sketch of frequency setup):}
\numberlines{1}
% Line frequencies:
\linefreq{110.20137 GHz}
% Expected source size in each line:
\linesize{unresolved}
% Expected line strength:
\linestrength{$10-30 \%$ absorption}
%
% --- For mapping projects:
% Configuration required (D, C2):
\configuration{}
%
% --- For detection projects:
%  Observing time required:
\observingtime{12 hours for each object}
%
% --- For snapshot or size measurements:
% Baseline range in meters:
\baselinerange{}
% Configuration list:
\configlist{}
% Number of hour angles per baseline:
\hourangles{}
% Observing time per hour angle:
\hourangletime{}
%
% Phase Calibrators (2 or more):
\phasecalibrators{none needed}
% Amplitude Calibrator:
\ampcalibrator{planets}
% Required accuracy of bandpass calibration:
\bandpass{none}
% Plateau de Bure Special requirements:
\specials{none}
%----------------------------------------------------------------
% The following command will produce the Technical Sheet for PdB.
%----------------------------------------------------------------
%\techsheet
%----------------------------------------------------------------
% here we give a source-specific, additional technical sheet,
% as an example.
%----------------------------------------------------------------
\techsourcelist{\small
\begin{tabular}{lrrr}
\hline
Source    & RA & DEC & z \\
& (J2000.0)   & (J2000.0)     & ~ \\
\hline
0818+1722 & 08:18:27.40 & 17:22:51.8 & 6.00 \\
0927+2001 & 09:27:21.82 & 20:01:23.7 & 5.79 \\
1335+3533 & 13:35:50.81 & 35:33:15.8 & 5.93 \\
1602+4228 & 16:02:54.18 & 42:28:22.9 & 6.07 \\
\hline
\end{tabular}}
\configlist{D}
\techsheet
\maketitle
%----------------------------------------------------------------
% Scientific justification (do not neglect this part ...)
% (max. 2 pages of text plus 2 pages of Figs., Tables and Refs.)
%----------------------------------------------------------------
%\proposalhistory{Continuation of 163-04 and 187-03} 

We propose MAMBO photometry of the highest redshift QSOs known ($z
\sim 6$), selected from the Sloan Digital Sky Survey (SDSS).  The
detection of the Gunn-Peterson effect in these QSO's implies
that we are seeing these sources at the near edge of cosmic
reionization, when the first stars and massive black holes formed (Fan
et al. 2003).  The proposed observations are a continuation of
our study of the evolution of the radio-to-optical spectral energy
distributions of QSOs, one important goal of which is to address the
interesting possibility of co-eval black hole and spheroidal galaxy
formation.  Such coeval evolution is suggested by the correlation
between black hole mass and stellar bulge mass for low redshift
galaxies.  We have established a statistically significant and well
defined sample of QSOs between $z = 2$ to 6 for which we have
extensive observations at radio through optical wavelengths.

We have undertaken an extensive study of the radio through optical
SEDs, and the molecular line emission properties, of optically
selected QSOs from redshifts $z \sim 2$ to 6 (Omont et al. 2003;
Carilli et al. 2002; Beelen et al. in prep). One key aspect of these
studies is to determine the star formation, and the gas and dust
properties of the host galaxies.  This question has become paramount
since the discovery of the bulge mass -- black hole mass correlation
in nearby galaxies, a result which suggests a fundamental relationship
between black hole and spheroidal galaxy formation.  We have found
that roughly 1/3 of optically selected QSOs are also hyper-luminous
infrared galaxies ($L_{FIR} \ge 10^{13}$ L$_\odot$), corresponding to
thermal emission from warm dust. Searches for CO emission from these
sources typically result in firm detections, with implied molecular
gas masses $\ge 10^{10}$ M$_\odot$.  Such molecular gas represents the
requisit fuel for star formation, and can be used as a dynamical
tracer in a forming galaxy (Walter et al. 2004).

We have recently extended our cm and mm studies of optically selected
QSOs into the epoch of reionization ($z > 6$).  We find that 3 of the
14 previously known $z> 6$ QSOs are also hyper-luminous IR galaxies,
including the most distant QSO known, J1148+5251 at $z=6.42$ with
$S_{250} = 5.5$ mJy, plus J1048+4637 at $z = 6.2$ with $S_{250} = 3.0$
mJy, (Bertoldi et al. 2003a), and a new source J0840+5624 at $z =
5.85$ with $S_{250} = 3.2$ mJy that was detected in our MAMBO program last
winter and that is target now of extensive follow-up molecular 
observations.  CO line emission has been detected
from J1148+5251 (Walter et al. 2003; Bertoldi al. 2003b), with an
implied molecular gas mass of $\sim 2\times 10^{10}$ M$_\odot$.
Sensitive radio continuum imaging yields a reasonable detection of
J1148+5251 with $S_{1.4} = 55 \pm 12 \mu$Jy and J0840+4637 with
$S_{1.4} = 47 \pm 11 \mu$Jy, while J1048+4637 is marginally detected
with $S_{1.4} = 26 \pm 12 \mu$Jy (Carilli et al. 2004).  Comparison of
the radio and FIR luminosities shows that all three sources have
radio-to-FIR luminosity ratios in the range defined by star forming
galaxies via the radio-FIR correlation (Fig. 1). The implied (massive)
star formation rates are $\sim 10^3$ M$_\odot$ year$^{-1}$. Imaging of
the molecular line emission from 1148+5251 implies a dynamical mass
within 3 kpc of the galaxy center $\sim 4\times 10^{10}$ M$_\odot$,
which is comparable to the molecular gas mass (Walter et al. 2004).

This proposal is a continuation of our efforts to detect mm-emission from the
highest-z QSOs (e.g. 163-04), now including three new sources discovered last
winter in the SDSS survey (Fan et al. in prep), plus one QSO from 163-04 that
was not observed last season.  You may ask: what will 4 new sources add to the
existing sample of 14 already observed at $z \sim 6$? Again, we have detected
3 of the 14 with MAMBO. Of these three, the highest redshift QSD 1148+5251 at
$z = 6.42$, remains the brightest of the mm detections, and the only CO
detection at these extreme redshifts.  But even this one molecular line
detection has proven to be a critical pathfinder for future mm telescopes,
such as ALMA, demonstrating that large dust and molecular gas masses can exist
in the earliest galaxies, and showing the wealth of unique information that
can be obtained on the host galaxies with mm line and continuum observations
(Walter et al. 2003, Bertoldi et al. 2003b, Walter et al. 2004).  Even one
other example of the 1148-type would be instrumental in pushing mm studies of
galaxy formation into the epoch of reionization.  We are actively pursuing the
other two MAMBO QSOs to search for CO emission using the IRAM, GBT, and
Effelsberg facilities, and this current proposal is the natural extension of
the MAMBO search for dust. Given the current statistics, we hope to detect one
source in the new sample.

The study of the first generation of galaxies, during reionization ($z \ge
6$), is one of the prime motivations for all large area future
telescopes, from meter to X-ray wavelengths.  We should point out that
submm galaxies have become important targets for mm line studies of
galaxy formation, but these samples are still limited to $z < 4$.  
While admittedly extreme systems, the host galaxies of the $z
\sim 6$ SDSS QSOs remain the only existing sample for extending mm
studies of galaxy formation into cosmic reionization using current
instrumentation. 

\newpage

\centerline{\bf Time Justification}

In the past we have aimed at a 3-sigma detection limit of $\sim 1.5$ mJy,
which we like to reach for this sample as well. Following
the recommendation of the IRAM observing time estimator, we apply for 13 hours
of observing time for the 4 sources to reach an rms noise level of 0.5 mJy in
typical winter conditions, including overheads. 

\vskip 0.1in

\noindent Bertoldi etal. 2003b, A\&A letters, 406, L55

\noindent Bertoldi etal. 2003a, A\&A letters, 409, L47

\noindent Carilli et al. 2004, AJ, 128, 997

\noindent Carilli et al. 2002, AJ, 122, 1679

\noindent Fan et al. 2003, ApJ, 125, 1649

\noindent Omont et al. 2003, A\&A, 398, 857

\noindent Walter et al. 2003, Nature, 424, 406

\noindent Walter et al. 2004, ApJ, 615, L17

\noindent Yun et al. 2001, ApJ, 554, 803

\vskip 2.6in

\special{psfile=Q.Z6.ps
hoffset=-10 voffset=-280 hscale=70 vscale=70}
\vskip 55mm
{\footnotesize {\bf Fig. 1:} The radio-FIR correlation for the IRAS
2Jy galaxy sample (x) from Yun et al. (2001), and for J1148+5251,
J1048+4637, and J0840+4637  (points with error bars).  The
$q$ parameter definition is given in Yun et al. (2001), corresponding
to a log ratio of IR to radio luminosity. The solid line is the mean
value for the IRAS galaxies, and the dotted lines indicate the range
defined as star forming galaxies by Yun et al. (2001).}

%----------------------------------------------------------------
%

\end{document}
