% SMM CO Bure proposal  Spring 2004
% version: 02.march 23h FB  incl. comments by Omont.
%
%-------------------------------------------------------------------
% This is a template for IRAM Proposals (originally created by R.Lucas)
% Deadline  04 Mar 2004
% Please use always the last update of proposal.sty
% (R. Neri + C.Thum Feb 02nd, 2004)
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% ATTENTION:
%
% The following line follows the LaTeX 2.09 syntax, 
% but should be also accepted by  LaTex2e. 
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% 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). 
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% 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):
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%\documentstyle[11pt,proposal]{article}
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\documentclass[11pt]{article}
\usepackage{proposal}
\usepackage{color}
\usepackage{psfig}
\usepackage{graphicx}
\usepackage{amsmath}
\usepackage{ulem}
\def\observed{14}
\def\detected{7}
\def\proposed{22}
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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{CO identification of (sub)millimeter galaxies IV.} 

\abstract{We propose to continue our successful long-term program to
determine, via CO rotational line emission, the dynamical/molecular
gas properties of a sample of $\sim 30$ SCUBA submillimeter and MAMBO
mm galaxies. % with accurate radio positions and optical redshifts.
We have detected CO emission from half the sources observed so far,
and propose to extend our sample by another 8 objects this summer.
The preliminary results of our program already provide a huge leap in our
knowledge of the gas masses and dynamical properties of the luminous, obscured
galaxies that produce at least half of the energy emitted in the early
Universe. It enables statistically meaningful comparisons with other
populations and galaxy formation models, explores the feasibility
of millimeter-based spectroscopic redshift measurements with current
and future instrumentation, proves the reliability of radio
identifications, serves as a database for calibrating present and
future photometric redshifts, and provides a crucial test of galaxy
formation models.}
%-------------------------------------------------------------------
% 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)
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%\exgalcont
\exgalco
%\exgalother
%\galcont
%\gallines
%\galcloud
%\galcse
%\galyse
%\galchem
%\galother
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% Observing type (Plateau de Bure only) (%sign  comment in or out)
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%\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{001-92, A001}
\continue{N061,N028,M05D,MD-7}
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% Amount of time (Pico Veleta only)
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% this  proposal
\hours{160}			
% {for full completion} {already allocated}
\totalhours{670}{510}
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% Sidereal time intervals:  {start} {end} {number of intervals}
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\lsta{6h}{16h}{12}
\lstb{12h}{20h}{12}
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% Receivers (Pico Veleta only) 
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%\receiveraandb
%\receivercandd
%\receiveraandd
%\receiverbandc
%\bolometer
%\hera
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% 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} { }
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\frequencies {see attachment}{}
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% Plateau de Bure confidentiality: enter here information (such as 
% frequencies, coordinates, ...) that should be kept confidential.  
%----------------------------------------------------------------
\confidential{}
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% Pico Veleta Special requirements (such as dates ...)
%----------------------------------------------------------------
\specials{None}
%\pooledobserving
%\serviceobserving
%\remoteobserving
%\polarimeter
%----------------------------------------------------------------
% Plateau de Bure configurations: all four configuration
% will be scheduled: A, B, C and D. Use ANY in case 
% you don't care about specific array configurations.
%----------------------------------------------------------------
%\confa
%\confb
\confc
\confd
%\confany
%----------------------------------------------------------------
% Principal Investigator (including name, address, telephone, fax, email)
%----------------------------------------------------------------
%\pifirstname{Reinhard Genzel,\ }
%\pilastname{Rob Ivison}
\apifirstname{Reinhard}
\apilastname{Genzel}
\apiinstitute{Max-Planck-Institut f\"ur extraterrestrische Physik}
\apistreetandnumber{Giessenbachstr. 1}
\apizipandcity{D-85741 Garching}
\apicountry{Germany}
\apiphone{(+49)89--30000-3281}
\apifax{(+49)89--30000-3601}
\apiemail{genzel@mpe.mpg.de}
\bpifirstname{Rob}
\bpilastname{Ivison}
\bpiinstitute{Astronomy Technology Centre, Royal Observatory}
\bpistreetandnumber{Blackford Hill}
\bpizipandcity{Edinburgh EH9 3HJ}
\bpicountry{UK}
\bpiphone{}
\bpifax{}
\bpiemail{rji@roe.ac.uk}
%\piinstitute{Max-Planck-Institut f\"ur extraterrestrische Physik}
%\pistreetandnumber{Giessenbachstr. 1}
%\pizipandcity{D-85741 Garching}
%\picountry{Germany}
%\piphone{(+49)89--30000-3281}
%\pifax{(+49)89--30000-3601}
%\piemail{genzel@mpe.mpg.de}
%----------------------------------------------------------------
% 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{This program is part of the PhD thesis of Thomas Greve, to be
filed in the Fall 2004, supervised by R. Ivison. }
%----------------------------------------------------------------
% Coauthors 
% macro: \coauthor{First_Name Last_Name}{affiliation} 
% use one \coauthor{ }{ } macro for each coauthor. 
% You may add as many \coauthor{ }{ } macros as needed ...
%----------------------------------------------------------------
%
%\coauthor{co-PI: R.\ Ivison}{Edinburgh, UK}
\coauthor{F.\ Bertoldi}{MPIfR, D}
\coauthor{R.\ Neri}{IRAM, F}
\coauthor{A.\ Omont}{IAP, F}
\coauthor{P.\ Cox}{IAS, F}
\coauthor{T.\ Greve}{Edinburgh, UK}
\coauthor{S.\ Chapman}{Caltech, USA}
\coauthor{A.\ Blain}{Caltech, USA}
\coauthor{I.\ Smail}{Durham, UK}
% 
%----------------------------------------------------------------
\reducer{Neri et al.}    % For Plateau de Bure
%\observer{He}                    % 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{
SMMJ030244 & 03 02 44.56 & +00 06 32.3 &  z=2.4345 \\
SMMJ030227 & 03 02 27.73 & +00 06 53.5 &  z=2.2574 \\
SMMJ123549 & 12 35 49.44 & +62 15 36.8 &  z=2.2032 \\
SMMJ123555 & 12 35 55.14 & +62 09 01.7 &  z=1.865  \\
SMMJ123622 & 12 36 22.65 & +62 16 29.7 &  z=2.4662 \\
SMMJ123707 & 12 37 07.21 & +62 14 08.1 &  z=2.486  \\
SMMJ131232 & 13 12 32.31 & +42 39 49.5 &  z=2.3204 \\
SMMJ221733 & 22 17 33.79 & +00 14 02.1 &  z=2.5553 \\
}
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% The following command will actually produce the front page. 
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\frontpage
%
%----------------------------------------------------------------
% Technical details for Plateau de Bure
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%Source list
\techsourcelist{\small
\begin{tabular}{lrrr}
\hline
Source    & RA & DEC & LSR Velocity \\
& (J2000.0)   & (J2000.0)     & (km/s)\\
\hline
SMMJ123549 & 12 35 49.44 & +62 15 36.8 &  z=2.2031 \\ 
\hline
\end{tabular}}
%Size of largest structure in (arcseconds)
\structuresize{unresolved}
%Expected continuum flux:
\continuumflux{1--4\,mJy at 1.3mm}
%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   {12CO(3-2)} {86-113} {USB} 
\rectwo   {12CO(6-5)} {212-237} {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  {160} {180}  {1} {SSB} 
\spectwo  {160} {320}  {1} {SSB} 
\specthree{160} {460}  {1} {SSB} 
\specfour {160} {600}  {1} {SSB} 
\specfive {160} {180}  {2} {DSB} 
\specsix  {160} {320}  {2} {DSB} 
\specseven{160} {460}  {2} {DSB} 
\speceight{160} {600}  {2} {DSB} 
% Expected width of spectral line (to zero power)
\linezerowidth{$\sim 400$ km/s}
% Number of lines observed simultaneously (add sketch of frequency setup):}
\numberlines{1--2 (varies by source)}
% Line frequencies:
\linefreq{varies by source}
% Expected source size in each line:
\linesize{unresolved}
% Expected line strength:
\linestrength{0.5--6\,mJy}
%
% --- For mapping projects:
% Configuration required (D, C2):
\configuration{D}
%
% --- For detection projects:
%  Observing time required:
\observingtime{20 hours for each object}
%
% --- For snapshot or size measurements:
% Baseline range in meters:
\baselinerange{}
% Configuration list:
\configlist{C,D}
% Number of hour angles per baseline:
\hourangles{}
% Observing time per hour angle:
\hourangletime{}
%
% Phase Calibrators (2 or more):
\phasecalibrators{varies by source}
% Amplitude Calibrator:
\ampcalibrator{3C345}
% Required accuracy of bandpass calibration:
\bandpass{good}
% Plateau de Bure Special requirements:
\specials{none}
%----------------------------------------------------------------
% The following command will produce the Technical Sheet for PdB.
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\techsheet
%----------------------------------------------------------------
% here we give a source-specific, additional technical sheet,
% as an example.
%----------------------------------------------------------------
\techsourcelist{\small
\begin{tabular}{lrrr}
\hline
Source    & RA & DEC & Velocity \\
& (J2000.0)   & (J2000.0)     & (km/s)\\
\hline
SMM     &  0:00:00 & 00:00:00   & 0  \\
\hline
\end{tabular}}
\configlist{C D}
%\techsheet
\maketitle
%----------------------------------------------------------------
% Scientific justification (do not neglect this part ...)
% (max. 2 pages of text plus 2 pages of Figs., Tables and Refs.)
%----------------------------------------------------------------

%----------------------------------------------------------------
%Extended Source List (sources which do not fit on cover page)
% -  place anywhere after the cover page  
% -  comment out the following 5 lines if not needed
%

\proposalhistory{Considering the fundamental importance of the dusty
  far-IR/submm population for the understanding of galaxy formation
  and evolution, recognizing the difficulties of reliable
  spectroscopic identifications of faint submillimeter (submm)
  galaxies, and realizing the strategic importance of such work for
  IRAM and for the scientific preparation of large future
  international programs such as Herschel and ALMA, in July 2002 we
  proposed to the IRAM Director CO detection observations on a new
  sample of distant submm sources with recently established
  spectroscopic redshifts.  The program was started in the late summer
  2002 semester with three targets. Our subsequent regular proposal
  M05D was accepted for the winter semester, with the option for a
  long-term status ($>4$ semester, $>30$ sources) if the program
  proves successful, and if a progress report is submitted each
  semester. Such a report was submitted each semester since, with a
  list of new targets, a total of \proposed\ so far.  Our program has
  so far been very successful in that of which \observed\ sources
  observed to date, CO was detected in \detected\ (Fig.1). For three of the
  detected sources we recently obtained high resolution
  observations for which good quality data have just been taken,
  improving the resolution of the CO maps to better than 2 arcsec
  (data in the process of being analyzed).  
  Below we give a brief update on
  the main program status.  For new PC members we repeat the science
  motivation. The results of our observations are reported in an ApJ
  Letter (Neri et al. 2003), in a conference contribution (Genzel et
  al. 2004), and in more detail in a paper in preparation by T. Greve
  as part of his PhD thesis. Given the volume of our request, we have 
  extended the length of the proposal beyond that 
  recommended, hoping that the PC will permit this exception.}

\vspace*{-1cm}
\subsection*{Background} 

At least half of the cosmic extragalactic energy density (not counting
the cosmic microwave background) emerges at far-infrared wavelengths
(Fixsen et al. 1998; Hauser et al. 1998). During the last years,
surveys with SCUBA at $\rm 850 \, \mu m$ and MAMBO at $\rm 1200 \, \mu
m$ have resolved a significant fraction of this background into a
population of faint (mJy) submm sources that may be luminous and
ultra-luminous infrared galaxies at redshifts $1<z<5$ (Smail et
al. 1997; Hughes et al. 1998; Barger et al. 1998; Bertoldi et
al. 2000; Dannerbauer et al. 2002).  This population of luminous, dusty starburst
galaxies contributes significantly to the cosmic star formation at
high redshift and may trace the epoch of bulge/elliptical
formation. While surveys at submillimeter and millimeter wavelengths
have by now identified several hundred sources, spectroscopic redshift
and CO detections had, until the summer of 2002, only been obtained
for two sources at $z \sim 3$ (Ivison et al. 2001; Frayer et al. 1998;
Genzel et al. 2003), mainly because of the faintness of their
optical/near-IR counterparts and the lack of accurate positions. 

Recently some of us have been able to substantially increase the
number of accurate source positions from deep VLA radio maps
(Ivison et al. 2002).  Optical follow-up spectroscopy at Keck for
these radio-detected submm sources was surprisingly successful,
resulting in a reliable sample of now $>90$ sources 
with optical redshifts (Chapman et al. 2003).  

Based on these results, we have observed \observed\ sources with the IRAM
Plateau de Bure interferometer since the summer of 2002, detecting CO
emission lines in \detected\ of them, confirming
in a robust way the optically determined redshifts.  Eight additional
targets are scheduled in the current winter semester. These observations have
demonstrated that the strategy adopted for our proposed long-term
program is successful.  Detecting CO line emission in ca.\ 30
 SCUBA and MAMBO sources for which both accurate
positions and optically-determined redshifts are now available, will
enable us to confirm that the (sub)mm population indeed has a mean
redshift of $z>2.5$ and contributes about half of the high-$z$ star
formation activity. It will also provide the first sample of high
redshift luminous infrared galaxies for which detailed studies of the
intrinsic source properties are possible, which eventually allows size
and mass estimates of these objects that provide a unique test of
galaxy formation models (Fig.4).

\subsection*{Scientific goals} 

The scientific goals of this long-term program are to:
\begin{itemize}
\item Detect CO rotational line emission with moderate resolution
(D-configuration) interferometric observations for a significant and
representative sample of $20$ or more galaxies, increasing the prior
number of CO-confirmed redshifts by a factor of 10, at which point
statistically meaningful comparisons to other populations and galaxy
formation models can be made. 
\item This sample size will also be sufficient to determine the mean
gas and dynamical mass, and velocity width for two redshifts bins,
thus beginning to study the evolution of gas and mass properties of
the most massive star-forming (proto-elliptical) galaxies in the
history of the Universe.
\item Explore the intrinsic source properties (gas mass and physical
      properties, dynamical mass, source size, relationship to
      emission at other wavelengths) by more detailed and spatially
      resolved 1--3\,mm PdB interferometry of a sub-sample of the
      program sources. 
      As has already been shown in two cases from our
      program (SMM~J04431 and SMM~J16368), such spatially resolved
      images deliver critical information in testing current
      hierarchical galaxy formation models (Fig.4), exploring how early and
      with what mass the luminous far-IR/submm galaxies were formed.
      We may also be able to constrain the CO-luminosity function of
      bright sources at high redshifts (as Keres et al. (2003) did for
      a local sample), and thereby study its evolution, and constrain
      the total mass density of cold neutral gas in the early
      Universe.
\item survey the local environment of SMM sources for companions, and for other
      CO or continuum sources, in order to clarify the importance of merging.
\item Explore the molecular gas properties of galaxies with strong and
      weak/absent AGN.
\item Test the reliability and multiplicity of radio and optical identifications of
      (sub)mm galaxies, e.g., look for situations
      where the CO (and submm) source is related to the optical/NIR or radio
      ID -- but is actually physically distinct. 
\item create a database for calibrating present
      and future photometric redshifts, which are degenerate in
      redshift and dust temperature.
\item Explore the general feasibility of millimeter-based
      spectroscopic redshifts with current instrumentation. 
      In addition, the detection of CO will open the door for
      observations of other CO transitions and of 
      other molecular and atomic species (e.g. HCN and
      CI), which will allow to study the properties of the ISM in
      detail in a large sample of high$-z$ sources. Our
      CO survey has thereby the potential to act as a spearhead
      project for ALMA, and may well present a major legacy of IRAM.
\end{itemize}


\subsection*{Observations to date} 

By now we have observed \observed\ sources (Table 2), selected on the
basis of strong (sub)mm emission, clear radio identifications, and
the most reliable redshifts available at the time of observation. 
CO line emission
was detected towards \detected\ sources (Fig.1). Eight more objects are
scheduled to be observed in the current semester.  The reason for the
non-detection of half of our sample may either be a lower CO-to-FIR
luminosity ratio for those sources, or yet too inaccurate
redshifts. Our new H$\alpha$ Keck/LRIS redshifts may improve latter
significantly.  Our CO detections
show a wide variation in source properties. In at least one case, the
targeted object is not the CO and continuum source. 
The line profiles show a range of shapes and widths (median 600 km/s), 
and for two sources a double horn structure
characteristic of rotating disks. Some of the shapes are 
indicative of dynamically perturbed or
interacting systems. In several cases the source appears resolved,
which motivated higher resolution follow-up studies in three object
(Our Bure W03/04 program, Neri et al.).
The CO detections toward SCUBA submm sources
\begin{itemize}
\item provide an important confirmation of the optical/UV redshifts.
It is interesting that their redshift range is close to the peak of
the merging assembly history of galaxy formation. The formation of
such massive systems at $z \sim 3$ is not easy to understand in
current hierarchical models of galaxy formation (e.g., Genzel et
al. 2003). If all SMM galaxies were similar to
those we observed, their abundance would be inconsistent with current
semi-analytic models of cold dark matter galaxy formation (Fig.4).
%
\item locate the actual submm source.  In most cases, the identity was
ambiguous before our observations. In one case, the optical redshift
did not correspond to the submm/CO sources, indicating a strong
clustering of galaxies in their proximity. The multiple nature of the
submm background sources may in fact explain why we were able to
detect strong UV emission lines in these gas- and dust-rich sources.
%
\item allow to derive the dynamical masses associated with these
luminous infrared galaxies, supporting the interpretation that this
population consists of gas-rich and massive ($\sim 10^{11} M_\odot$)
interacting starburst/AGN systems, of very massive galaxies with deep
central potential wells. The median velocity FWHM of our sample is 600
km/s, indicating that these galaxies have over 12 times the mass of a
typical Lyman-break-galaxy at $z\sim 3$.
\end{itemize}

A detailed analysis was completed for the first three targets we observed (Neri et
al. 2003).  The current analysis of a larger sample will be part
of the PhD thesis of T. Greve.
% To illustrate the wealth of information
%we can gain from these observations, we refer the program committee
%also to a more detailed discussion of three sources in
%our accompanying proposal (Neri et al.).

\subsection*{Future prospects} 

Based on these initial observations, it is clear that our program is
demanding in observing time even with the superior sensitivity (a
factor 5 relative to OVRO) of the PdBI, requiring 2--3 tracks per
source for an initial detection, and more for follow-up at higher
resolution. We had anticipated that this cooperative program would
require at least 2 years for execution. With this report we restate
our request for a long-term allocation to determine the CO properties
of a sample of $\sim 30$ SCUBA submm galaxies, continuing this summer
with another 7 new objects -- plus one for which we have recently
obtained a more accurate H$\alpha$ redshift that is 1500 km/s off
the prior Ly$\alpha$ redshift, which did not produce a CO detection.
This will bring the total number of objects observed to 29, of which
we hope to detect --especially with the new H$\alpha$ redshifts-- at
least half. This approaches our set goal to observe a significant
number of sources ($>$30) in order to be able to look for any redshift
evolution in the FIR to CO luminosity, masses, 
and also to discern any differences
between objects with and without AGN.

Using multi-object spectrographs at the Keck and Gemini telescopes our
program to determine optical redshift for both millimeter (MAMBO) and
submillimeter (SCUBA) selected galaxies continues now targeting mainly
MAMBO sources. A very recent Keck LRIS observation run has yielded a
number of additional excellent targets for PdBI observations, and
additional NIRSPEC/Keck (3 nights) and OHS/Subaru (3 nights)
runs in early April may add to this set. Some of the newest
sources, if they show more reliably redshift estimates, we might
request to substitute for the sources in our current list.  The new
near-IR spectra showing H$\alpha$ (Fig.2), which should more accurately trace
the redshift of the ISM in the galaxy as it arises from a greater fraction
of the gas, being less prone to emission in highly-excited,
fast-moving outflows offset from the redshift of the neutral ISM.

%By now, we have only
%exploited half of the rich pickings in the 8mJy survey. the recent keck
%LRIS run concentrated on Lockman, with NIRSPEC confirmation of optical
%redshifts.

%The current number of sources with secure redshifts is
%close to 30 (Chapman et al.  2003).


\subsection*{Observing strategy}

For the coming summer semester we propose to observe $\sim 8$ objects
for which optical redshifts were obtained with an accuracy of $\Delta
z<0.005$ (see attached source list).  We concentrate on detecting the
3\,mm CO line emission, but will use the 1\,mm receivers to try
determine accurate continuum positions and fluxes, to estimate source
sizes and to observe an additional CO tracer.

%, though the 1\,mm receivers are critical also
%to determine accurate continuum positions and fluxes, to observe an
%additional CO tracer, and to estimate source sizes and identify those
%sources which will be most suitable for higher-resolution follow-up.

%The observed 850$\mu $m flux densities range from 6 to 12\,mJy,
%resulting in expected 1.2\,mm continuum flux densities of $\sim
%1-4\,{\rm mJy}$ (for the apparenty typical $850\,{\rm \mu m}$/1.2\,mm
%flux density ratio of 3--4).

Assuming parameters from Version 3.7-00 of the Bure manual and our
previous experience, with 5 antennas and summer conditions
we expect that a single transit (giving eight
hours on-source) will yield $1\sigma$ sensitivities of 0.8\,mJy per
$\sim 100\,{\rm km\,s^{-1}}$ channel at 3\,mm, and 0.8\,mJy across the
1\,mm continuum bandpass (averaging both sidebands).
Requiring a $\geq 5\sigma$
detection and a cross-check of having at least two $\geq 3\sigma$
detections in independent datasets, we will need 2--3 tracks per
source, or a total of 16--24 tracks for eight sources.
We request on average 2.5 tracks per source, and thus
{\bf a total of 20 tracks}.

To correct for the likely
systematic blueshift of UV line features relative to CO emission, we
will tune the 3\,mm receivers slightly redward of the measured UV
redshifts, except in cases where we have spectroscopic redshifts for
nebular lines such as Lyman~$\alpha$.  For the redshift uncertainty
of $\Delta z = 0.005$, any source at $z \geq 1$ should then have the
CO line peak fall within $\rm 0.5 \times 580 \, MHz = 290 \,MHz$ of
the 3\,mm band center.  
%In the event that no line emission is seen in
%a single track from a predicted strong source, we will consider
%re-observing the source with a different bandwidth setting, adjacent
%and red-shifted from the first one.  Allowing additional tracks for
%such retunings 

The present proposal requests observing
time mostly for the D configuration, which is well suited for
detection experiments.  We may consider observing the second or third
track in the C configuration if the source is well detected in D. Such
higher resolution data yields crucial information on the source size.  

Because of our ongoing analysis
of recent spectroscopic near-IR Keck data, we propose to
retain the possibility of exchanging targets in the source list
for better targets we might identify, and in particular
for sources from the MAMBO deep fields.  In each such case a written
request for changing the source 
will be submitted to the IRAM director. A `better' target
would be one with a clearer optical/IR identification, a stronger
(sub)mm flux, or a more accurate redshift.


%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%


\newpage

\begin{minipage}{15cm}
%\includegraphics[width=14.cm,clip]{SMMsurveyspectra.eps}
\includegraphics[width=14.cm,clip]{smm.eps}
\end{minipage}

\vspace{.5cm}
\noindent{\small \textbf{Figure 1.}
CO(3-2) and (4-3) spectra of the
7 submm galaxies which were detected in CO line emission, from a
total of 14 surveyed to date. The spectrum of SMM J02399-0136 (from
Genzel et al. 2003) is shown for comparison. The redshifts determined
from the CO emission are given for each source.}

\vspace{.5cm}

\begin{minipage}{15cm}
\includegraphics[bb=33 182 568 530,width=15.cm,clip]{smail.ps}
\end{minipage}

\vspace{.5cm}
\noindent{\small \textbf{Figure 2.}
Examples of near-infrared spectra of four of the
    submm galaxies taken with NIRSPEC on Keck.
%: MAMBO.22 (ul), HDF.172 (ur), MAMBO.46 (ll), HDF.76 (lr).  
% and cover the wavelength region which should contain the
%    H$\alpha$ line at the UV-derived redshift of the galaxies.  All four
%    galaxies are well detected in
    H$\alpha$ provides significantly more
    reliable estimates of the probable redshifts for the CO
    emission. These spectra also provide estimates of the star
    formation rates in these galaxies and the likely contribution from
    AGN to their emission (from the ratio of H$\alpha$/[NII]). The lower
    trace in each panel is the raw spectrum, the upper trace has been
    smoothed to the instrumental resolution.  The vertical dotted
    lines show the wavelengths of the H$\alpha$ and [NII] emission lines
    at the best-fit redshift and the shaded region denotes sections of
    the spectra which are badly effected by atmospheric absorption or
    emission.
}

\vspace{1.cm}

\begin{minipage}{9cm}
  \includegraphics[width=8.5cm,clip]{lfir_lco3.ps}
\end{minipage}
\begin{minipage}{8cm}
\noindent{\small \textbf{Figure 3.}
CO luminosity vs.~far-IR luminosity for three samples
of local (U)LIRGs (Sanders et al.~1991; Solomon et al.~1997; Yao et al.~2003)
and for a sample of high-redshift (sub)millimetre selected galaxies (Neri
et al.~2003; Greve et al.~in prep.). The CO luminosities for the ULIRGs
are all based on the CO$\,J=1-0$ line, whereas for the sub-mm galaxies the
line luminosities are derived from the $3-2$ (black symbols) and $4-3$
(red symbols) transitions. The far-IR luminosities were derived from IRAS
60/100$\mu$m fluxes which had been measured for all the ULIRGs, and in the
case of the sub-mm galaxies were estimated using the FIR-radio correlation
(Condon et al.~1992). For the submm galaxies the CO(1-0) luminosity 
was derived by assuming
constant brightness temperature. (from Greve et al. in prep.).
}
\end{minipage}

\begin{minipage}{9cm}
  \includegraphics[width=8.5cm,clip]{mtest.ps}
\end{minipage}
\begin{minipage}{8cm}
\noindent{\small \textbf{Figure 4.} Comoving number density of
galaxies with baryonic massess $> 10^{11} M_\odot$ as a function of
redshift. 
% Triangle and open squares show densities of massive stellar
% systems at $z=0$ (Cole et al. 2001) and $z\sim 1$ (Drory et al. 2003);
The large rectangle shows the density of massive (sub)mm galaxies at $z=2-3$,
the arrow a likely factor 30 correction for burst lifetimes. Solid curves show the
predictions of semi-analytic modelling --
% by Kauffmann et al. (1999) and Baugh et al. (2003) -- 
the two models use different values of $\Omega_b$. The models
strongly underestimate the observed number density of massive 
systems at high redshift. (Adapted from Genzel et al. 2004) }
\end{minipage}

\medskip
\noindent
{\bf Table 1.}  Proposed targets. \\[2pt]
%\centerline
\noindent
{\begin{tabular}{lcccccccccc}
\hline
\multicolumn{1}{l}{Source} &
\multicolumn{1}{c}{$S_{1.4}\ \pm$} & 
\multicolumn{1}{c}{$S_{850}\ \pm$} & 
\multicolumn{1}{c}{$z$} & 
\multicolumn{1}{c}{tracer} & 
\multicolumn{1}{c}{Line} &
\multicolumn{1}{c}{$\nu_{\rm obs}$} \\
\multicolumn{1}{l}{(1)} & 
\multicolumn{1}{c}{(2)} & 
\multicolumn{1}{c}{(3)} & 
\multicolumn{1}{c}{(4)} & 
\multicolumn{1}{c}{(5)} & 
\multicolumn{1}{c}{(6)} & 
\multicolumn{1}{c}{(7)}  \\
\hline\hline
SMMJ030244.56+000632.3 (6)        &  51.0$\pm$ 9.5& 5.2$\pm$ 1.1 &  2.4345 & H$\alpha$ & 3-2& 100.68\\ % #6   Ha
SMMJ030227.73+000653.5 (15)       & 217.1$\pm$ 9.7& 4.4$\pm$ 1.3 &  2.2574 & H$\alpha$ & 3-2& 106.16\\ % #15  Ha
SMMJ123549.44+621536.8 (HDF.76)   &  74.6$\pm$ 9.5& 8.3$\pm$ 2.5 &  2.2032 & H$\alpha$ & 3-2& 107.95\\ % HDF.76  Ha
SMMJ123555.14+620901.7 (HDF.85)   & 212  $\pm$ 14 & 6.0$\pm$ 1.8 &  1.865  & Ly$\alpha$& 3-2&  80.47\\ % HDF.85 LyA, (weak SiII,CII)
SMMJ123622.65+621629.7 (HDF.143)  &  70.9$\pm$ 8.7& 7.7$\pm$ 1.3 &  2.4662 & H$\alpha$ & 3-2&  99.76\\ % HDF.143 Ha
SMMJ123707.21+621408.1 (HDF.242)  &  45  $\pm$ 7.9& 4.7$\pm$ 1.5 &  2.486  & Ly$\alpha$& 3-2&  99.20\\ % HDF.242 LyA
SMMJ131232.31+423949.5 (SA13.570) &  94.8$\pm$ 3.3& 4.7$\pm$ 1.1 &  2.3204 & H$\alpha$ & 3-2& 104.14\\ % SA13.570 Ha, prev. obs. at 2.32
SMMJ221733.79+001402.1 (22.139)   &  44.5$\pm$ 13.& 7.4$\pm$ 1.0 &  2.5553 & H$\alpha$ & 3-2&  97.26\\ % 22.139 Ha
%   3-2: 345795.9899  2-1: 230538.0000
\hline
\end{tabular}} \\[4pt]
\noindent
Columns: 
%(3) redshift, known to $\Delta z = \pm 0.005$ but represented here to $\Delta z = \pm 0.1$; 
(5) tracer of optical redshift;
(6-9) CO transitions  and frequencies to be observed at the PdBI.
%\vspace*{1.5cm}

\newpage
%\bigskip

\noindent
{\bf Table 2.}  Status of the CO observations towards (sub)mm galaxies.\\[-2pt]
\begin{small}
\begin{verbatim}
---------------------------------------------------------------------------------------------
name             Pr   det CO  S/N pk  wid I_CO     --offset-- z     S850 alias & comments
                                  mJy kms Jy*km/s  "  "  km/s        mJy
1                2     3  4   5   6   7   8   9    10 11   12 13     14  15 
------------------------------------------------------------------------------------------S02
J044307.3+021023 MD-7  +  3-2         350 1.4 0.2  -1 -1   17 2.509 7.2  3as extended
J094303.7+470015 MB-7  +  4-3         420 1.1 0.1  -4 -1 -207 3.346 10.5 H6,wrong opt ID  
J163650.4+405735 MA-7  +  3-2         840 2.3 0.2         115 2.3853 8.2 N2850.4          
                 M-14  +  7-6             1.1 0.2         -85 2.383
------------------------------------------------------------------------------------------W02
J105155.5+572313 MB5d  -  4-3                                (3.70) 4.5  LE850.18
J105230.7+572210 MC5d  -  3-2                                 2.6   11.0 LE850.6  
J105238.3+572436 MD5d  -  3-2                                 3.0   10.9 LE850.2  
J163631.5+405547 ME5d  -  3-2                                 2.28   6.3 N2850.13 
J163639.0+405636 MF5d  -  3-2                                 2.04   9.0 N2850.7  
J163658.2+410523 MH5d  +  3-2 7.8 1.8 700 1.3       0  0 -300 2.45  10.7 N2850.2  ERO      
------------------------------------------------------------------------------------------S03
J123600.2+621047 NI28  -  3-2                                 1.999      
J131201.1+424208 NC28  +  4-3 9.1 2.2 500 1.1       1  1 -400 3.408  6.2 extended
J131232.3+423950 ND28  -  3-2                                 2.32   5.9 latest Ha z: 2.3257
J163706.5+405314 NJ28  +  3-2 3.7 1.2 brd           0  0 +400 2.378  12  MAMBO Elais(46) 
J221736.0+001554 NG28  +  3-2 4.1 .94 500 0.5       2  4 -400 3.097  6.3 (135) 
------------------------------------------------------------------------------------------W03
J123553.2+621337                                              2.098  8.8 (82) 
J123555.1+620901                                              1.875  6.0 (85) 
J123600.1+620253                                              2.710  6.9 (92) 
J123606.8+621021                                              2.330 11.6 (105)
J123621.2+621708                                              1.988  7.8 (140)
J163627.9+405811                                              3.180  6.3 (e.43)
J163655.7+405910                                              2.607  2.8 (m.20)
J221737.3+001025                                              2.639  6.1 (851)
---------------------------------------------------------------------------------------------
(1) SMM object name, i.e. coordinate
(2) IRAM target name
(3) + detected, - not detected
(4) CO transition
(5) signal to noise of line peak intensity
(6) peak line flux
(7) line FWHM, in km/s
(8)-(9) integrated line flux and uncertainty, sigma
(10)-(12) offset in position and velocity from optical target
(13) redshift of CO line, or optical z 
(14) 350 GHz continuum flux density
(15) SMM source alt. name, comments
\end{verbatim}
\end{small}


\medskip
\noindent
{\small \textbf{References:}
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$\bullet $ Barger et al. \ 1999, ApJ, 518, L5~~
$\bullet $ Bertoldi et al.\ 2000, A\&A, 360, 92~~
  % $\bullet $ Blain 1999, MNRAS, 309, 955~~
  % $\bullet $ Blain et al.\ 2002, Physics Reports, in press (astro-ph/0202228)~~
  % $\bullet $ Carilli, Yun, 2000, ApJ, 530, 618~~
  % $\bullet$ Chapman et al.\ 2001, ApJ, 548, L147~~
$\bullet $ Chapman et al.\ 2003, Nature, 422, 695~~
  % $\bullet $ Condon 1992, ARAA, 30, 575~~
  % $\bullet $ Cowie et al.\ 2002, AJ, 123, 2197~~
  % $\bullet $ Cox et al.\ 2002, in The Cold Universe, in press.~~
$\bullet $ Dannerbauer et al.\ 2002, ApJ, 573, 473~~
  % $\bullet $ Downes et al.\ 1999, A\&A, 347, 809~~
  % $\bullet $ Dunlop et al.\ 2002, MNRAS, submitted (astro-ph/0205480)~~
$ \bullet$ Fixsen, D.J. et \ 1998, ApJ, 508, 123~~
$\bullet $ Frayer et al.\ 1998, ApJ, 506, L7~~
  % $\bullet $ Frayer et al.\ 1999, ApJ, 514, L13~~
  % $\bullet $ Frayer et al.\ 2000, AJ, 120, 1668~~
$\bullet $ Genzel et al.\ 2003, ApJ, 584, 633~~
$\bullet $ Genzel et al.\ 2004, Venice conference~~
$\bullet $ Hauser, M.G. et al. 1998, ApJ, 508, 25~~
$\bullet $ Hughes et al.\ 1998, Nature, 394, 241~~
  % $\bullet $ Ivison et al.\ 1998, MNRAS, 298, 583~~
  % $\bullet $ Ivison et al.\ 2000, MNRAS, 315, 209~~
  % $\bullet $ Ivison et al.\ 2001, ApJ, 561, L45~~
$\bullet $ Ivison et al.\ 2002, MNRAS, 337, 1 ~~
$\bullet $ Keres et al. \ 2003, ApJ, 582, 659
  % $\bullet $ Scott et al.\ 2002, MNRAS, 331, 817~~
$\bullet $ Neri, Genzel, Ivison, Bertoldi, Blain, Chapman, Cox, Greve, Omont, Frayer 2003,
           ApJ~~597, L113
$\bullet $ Sanders et al. 1991, ApJ, 370, 158.
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$\bullet $ Webb et al.\ 2003, ApJ, 582, 6
$\bullet $ Yao et al. 2003, ApJ, 588, 771.
}

\end{document}


%\zerospacingparagraph{Fill in this paragraph to justify the need
%                    for zero-spacing data with the 30m telescope.}



********************************** Additional Info: *****************

CO    redshift coverage
      115-81    245-205  GHz
1-0  0.0-0.42 
2-1  1.0-1.84  0.00-0.12
3-2  2.0-3.27  0.41-0.68
4-3  3.0-4.69  0.88-1.24
5-4  4.0-6.11  1.35-1.81
6-5            1.82-2.37

<etc> more CO-frequencies
 28001  CO
  115271.2018   .0005 -5.0105 2     .0000  3 -28001 101 1           0
  230538.0000   .0005 -4.1197 2    3.8450  5 -28001 101 2           1
  345795.9899   .0005 -3.6118 2   11.5350  7 -28001 101 3           2
  461040.7682   .0005 -3.2657 2   23.0695  9 -28001 101 4           3
  576267.9305   .0005 -3.0118 2   38.4481 11 -28001 101 5           4
  691473.0763   .0005 -2.8193 2   57.6704 13 -28001 101 6           5
  806651.8060   .0050 -2.6716 2   80.7354 15 -28001 101 7           6
  921799.7000   .0050 -2.5590 2  107.6424 17 -28001 101 8           7
 1036912.3930   .0050 -2.4751 2  138.3904 19 -28001 101 9           8
 1151985.4520   .0110 -2.4156 2  172.9780 21 -28001 10110           9

http://spec.jpl.nasa.gov/ftp/pub/catalog/catform.html

Submm background sources with CO line measurements:
(SCUBA sources from Frayer et al. 1997,1998)

           z   850   1200  CO

SMMJ14011 2.6         ~3   2.4  OVRO      Downes, Frayer
SMMJ02399 2.8   25   7/4.0 2.5  PdB/OVRO  Tacconi, Frayer (unclear!)
HR10      1.4        4.9   1.4  PdB

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%

