Title  Gas Content and Dynamics of Elliptical Galaxies 
Pi     C. Wilson
Time   12 hrs
1. Gas Content and Dynamics of Elliptical Galaxies
   C. Wilson, K. Tatematsu, N. Nakai

2. In elliptical galaxies, the kinematics of the stars can be studied
with optical observations. Many ellipticals contain some molecular gas,
but the details of the gas content and kinematics are only known
for a few galaxies.
What are the properties of molecular gas in elliptical galaxies?
Is it organized into similar structures as spirals (i.e. GMCs, mass function,
etc.) What does molecular gas do when there isn't very much of it and
there is little or no active star formation? Is there general evidence
that the molecular gas in elliptical 
galaxies comes from mergers (major or minor)?
Peak CO 2-1 line strengths in single dish survey from Lees et al. (1991)
are in the range of 10-40 mK, so we will need good sensitivity.


3. Number of sources: 20 in initial survey, follow-up on 6 brightest
	and/or most interesting sources

4. Coordinates: 

4.1. all over the sky, avoiding galactic plane

4.2. Moving target: no

4.3. Time critical: no

4.4. Scheduling constraints: no


CO J=1-0 imaging:
----------------

5. Spatial scales:

5.1. Angular resolution (arcsec): 3"

5.2. Range of spatial scales/FOV (arcsec): 60"

5.3 Required pointing accuracy: 1"


6. Observational setup

6.1. Single dish total power data: required

     Observing modes for single dish total power: nutator or OTF

6.2. Stand-alone ACA: required

6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: 
     no

6.4. Subarrays of 12m baseline-ALMA antennas: no


7. Frequencies:

7.1. Receiver band: Band 3

7.2. Lines and Frequencies (GHz): 114 GHz

7.3. Spectral resolution (km/s): 10 km/s

7.4. Bandwidth or spectral coverage (km/s or GHz): 1000 km/s


9. Line intensity:

9.1. Typical value (K or Jy): 20-80 mK

9.2. Required rms per channel (K or Jy): 5 mK

9.3. Spectral dynamic range: 5-20

9.4. Calibration requirements: absolute      10%
                               repeatability 3%
                               relative      3%

10. Polarization:  no  

11. Integration time for each observing mode/receiver setting (hr):
		1 hours per galaxy = 20 hours


Followup in CO 2-1 and 3-2 on 6 interesting/bright galaxies:

CO J=2-1 imaging:
----------------

5. Spatial scales:

5.1. Angular resolution (arcsec): 1.2

5.2. Range of spatial scales/FOV (arcsec): 2 fields within 1' CO 1-0 map

5.3. Required pointing accuracy: 1"

6. Observational setup

6.1. Single dish total power data: required

     Observing modes for single dish total power: nutator or OTF

6.2. Stand-alone ACA: required

6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: 
     no

6.4. Subarrays of 12m baseline-ALMA antennas: no

7. Frequencies:

7.1. Receiver band: Band 6

7.2. Lines and Frequencies (GHz): 228 GHz

7.3. Spectral resolution (km/s): 10 km/s

7.4. Bandwidth or spectral coverage (km/s or GHz): 1000 km/s


9. Line intensity:

9.1. Typical value (K or Jy): 25-100 mK

9.2. Required rms per channel (K or Jy): 6 mK

9.3. Spectral dynamic range: 5-20

9.4. Calibration requirements: absolute      10%
                               repeatability 3%
                               relative      3%

10. Polarization:  no  

11. Integration time for each observing mode/receiver setting (hr):
		2 hours per field x 2 fields per galaxy = 24 hours


CO J=3-2 imaging:
----------------

5. Spatial scales:

5.1. Angular resolution (arcsec): 1.0

5.2. Range of spatial scales/FOV (arcsec): 20" 

5.3. Required pointing accuracy: 1"


6. Observational setup

6.1. Single dish total power data: no

6.2. Stand-alone ACA: no

6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: 
     no

6.4. Subarrays of 12m baseline-ALMA antennas: no


7. Frequencies:

7.1. Receiver band: Band 7

7.2. Lines and Frequencies (GHz): 342 GHz (CO 3-2)

7.3. Spectral resolution (km/s): 10 km/s

7.4. Bandwidth or spectral coverage (km/s or GHz): 1000 km/s


9. Line intensity:

9.1. Typical value (K or Jy): 25-100 mK

9.2. Required rms per channel (K or Jy): 6 mK

9.3. Spectral dynamic range: 5-20

9.4. Calibration requirements: absolute      10%
                               repeatability 3%
                               relative      3%

10. Polarization:  no  

11. Integration time for each observing mode/receiver setting (hr):
		2 hours per field x 1 field per galaxy = 12 hours



12. Total integration time for program (hr): 56 hours

13. Comments on observing strategy (e.g. line surveys, Target of
       Opportunity, Sun, ...): (optional)


--------------------------------------------------
Review v2.0:
 
Gas Content and dynamics of elliptical galaxies
Wilson et al. 

There's a relatively modest request to address an important and unique
question. It also seems to avoid being too modest to meet a time
cap. Since DRSP1 have there been developments in other areas that
allow either more precise target selection, or render some of the
power of ALMA less unique? I'm thinking of SAURON IFU optical work,
and the possibility of a SEQUOIA array working on the LMT to make an
early detection?