Title Search for broad lines in the tropospheres of the giant planets 
Pi     E. Lellouch
Time   16 hrs


1. Name of program and authors
Title: Search for broad lines in the tropospheres of the giant planets
Authors: E. Lellouch

2. One short paragraph with science goal(s)

Abstract: A few molecular lines are expected to be formed in 
   giant planet tropospheres (at 0.1-1 bar), and as such, to be 
   broad (several GHz). Observing them would provide new information 
   on the composition of giant planet tropospheres. Species will include CO, PH3,
   and HCl. In addition, continuum measurements at a variety of wavelengths can 
   elucidate belt-zone structure and temperature at different altitudes. Such studies
   are already performed in the cm range and need to be extended to the mm/submm.
   Seasonal variability will be investigated by repeating the observations 6 times over
   several years.

3. Number of sources : 4
   
   Jupiter, Saturn, Uranus, Neptune


4. Coordinates:

4.1. Rough RA and DEC 

     variable

4.2. Moving target: yes

4.3. Time critical: yes (seasonal variability will be investigated)

4.4. Scheduling constraints: (optional)
	

5. Spatial scales:

5.1. Angular resolution (arcsec): 0.2" (Neptune) to 2" (Jupiter)

5.2. Range of spatial scales/FOV (arcsec): 2" (Neptune) to 50" (Jupiter)

     (optional: indicate whether single-field, small mosaic,
     wide-field mosaic...)

5.3. Required pointing accuracy: 0.2"


6. Observational setup

6.1. Single dish total power data: required (Jupiter/Saturn)

     Observing modes for single dish total power:  wobbler switch

     (e.g., nutator switch; frequency switch; position switch;
     on-the-fly mapping; and combinations of the above)

6.2. Stand-alone ACA: no

6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: 
     required (Jupiter/Saturn)

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


7. Frequencies:

7.1. Receiver band: Band 6, 7, 9

7.2. Lines and Frequencies (GHz): 

    CO: 230, 345 GHz
    PH3: 267 
    HCl: 626 GHz

7.3. Spectral resolution (km/s): 20 km/s 

7.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz


8. Continuum flux density:

8.1. Typical value (Jy): Jupiter: 160 K, Saturn: 110 K, Uranus and Neptune: 80 K

     (take average value of set of objects)
     (optional: provide range of fluxes for set of objects)

8.2. Required continuum rms (Jy or K): 0.1 K

8.3. Dynamic range within image:

     (from 7.1 and 7.2, but also indicate whether, e.g., weak objects
     next to bright objects)

8.4. Calibration requirements: absolute       1-3% 
                               repeatability  1-3% 
                               relative       1-3% 


9. Line intensity:

9.1. Typical value (K or Jy): 3 K - 20 K

     (take average value of set of objects)
     (optional: provide range of values for set of objects)

9.2. Required rms per channel (K or Jy): 0.03 K

9.3. Spectral dynamic range:

9.4. Calibration requirements: absolute       1-3% 
                               repeatability  1-3% 
                               relative       1-3% 


10. Polarization: no 

10.1. Required Stokes parameters:

10.2. Total polarized flux density (Jy):

10.3. Required polarization rms and/or dynamic range:

10.4. Polarization fidelity:

10.5. Required calibration accuracy:


11. Integration time for each observing mode/receiver setting (hr):
Typically 10 min per line.


12. Total integration time for program (hr):
About 16 hours (10 min x 4 lines x 4 planets x 6 repetitions)



13. Comments on observing strategy : (optional)

    (e.g. line surveys, Target of Opportunity, Sun, ...):
--------------------------------------------------
Review v2.0:
 
Review 4.1.1-4.1.8

The only question I have with regards to these projects is the use of
ACA cross-correlated with ALMA-12m. Several projects list this option
as 'required' or as 'beneficial', but no arguments are given. 

- When listed as 'required' does this mean that the observations are
  mosaics, and that the ACA is needed to provide the intermediate
  scales? If so, are the cross-correlations with the ALMA-12m antennas
  needed, or could simultaneous ACA-7m-only observations also suffice?

- When listed as 'beneficial' is this purely for S/N reasons or also
  for uv-coverage? The cross-correlation option is fairly demanding on
  the scheduling, and unlikely to be used unless absolutely necessary.