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


   5. Spatial scales:

      5.1. Angular resolution (arcsec): 3

      5.2. Range of spatial scales/FOV (arcsec): 1' 

      5.3. Single dish total power data: yes

      5.4. ACA: yes

      5.5. Subarrays: no


   6. Frequencies:

      6.1. Receiver band: Band 3

      6.2. Lines and Frequencies (GHz): 114 GHz

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

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


   7. Continuum flux density:

      7.1. Typical value (Jy):
           (take average value of set of objects)
           (optional: indicate range of fluxes within set of objects)

      7.2. Required continuum rms (Jy or K):

      7.3. Dynamic range within image:
           (from 7.1 and 7.2, but also indicate whether e.g. weak objects
            next to bright objects)


   8. Line intensity:

      8.1. Typical value (K or Jy): 20-80 mK
           (take average value of set of objects)
           (optional: indicate range of fluxes within set of objects)

      8.2. Required rms per channel (K or Jy): 4 mK

      8.3. Spectral dynamic range: 5-20


   9. Polarization:  no  

   10. 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:

   5. Spatial scales:

      5.1. Angular resolution (arcsec): 0.5

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

      5.3. Single dish total power data: yes

      5.4. ACA: yes

      5.5. Subarrays: no


   6. Frequencies:

      6.1. Receiver band: Band 6

      6.2. Lines and Frequencies (GHz): 228 GHz

      6.3. Spectral resolution (km/s): 3 km/s

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


   7. Continuum flux density:

      7.1. Typical value (Jy):
           (take average value of set of objects)
           (optional: indicate range of fluxes within set of objects)

      7.2. Required continuum rms (Jy or K):

      7.3. Dynamic range within image:
           (from 7.1 and 7.2, but also indicate whether e.g. weak objects
            next to bright objects)


   8. Line intensity:

      8.1. Typical value (K or Jy): 25-100 mK
           (take average value of set of objects)
           (optional: indicate range of fluxes within set of objects)

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

      8.3. Spectral dynamic range: 5-20


   9. Polarization:  no  

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



   5. Spatial scales:

      5.1. Angular resolution (arcsec): 0.5

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

      5.3. Single dish total power data: no

      5.4. ACA: no

      5.5. Subarrays: no


   6. Frequencies:

      6.1. Receiver band: Band 7

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

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

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


   7. Continuum flux density:

      7.1. Typical value (Jy):
           (take average value of set of objects)
           (optional: indicate range of fluxes within set of objects)

      7.2. Required continuum rms (Jy or K):

      7.3. Dynamic range within image:
           (from 7.1 and 7.2, but also indicate whether e.g. weak objects
            next to bright objects)


   8. Line intensity:

      8.1. Typical value (K or Jy): 25-100 mK
           (take average value of set of objects)
           (optional: indicate range of fluxes within set of objects)

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

      8.3. Spectral dynamic range: 5-20


   9. Polarization:  no  

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



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

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

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Review Chris Carilli: OK.