Title  Composition and dynamics of giant planet stratospheres
Pi     E. Lellouch
Time   160 hrs


1. Name of program and authors
Title: Composition and dynamics of giant planet stratospheres
Authors: E. Lellouch

2. One short paragraph with science goal(s)

Abstract: ALMA can tackle a variety of problems related to giant planet 
   stratospheres: (i) composition - search for new species, in particular 
   CO in Saturn and Uranus (ii) atmospheric dynamics 
   from mapping of tracer species (including CO, HCN on Neptune, and CO,
   HCN,CS, injected from SL9 impact, on Jupiter) (iii) dynamics from 
   direct wind measurements (iv) origin of external water from HDO search.


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 for Jupiter, no otherwise

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 5, 6, 7, 8, 9

7.2. Lines and Frequencies (GHz): 

    CO: 230, 345, 460, 806 GHz
    CS: 244 GHz
    HCN: 354 GHz
    H2O: 183 and/or 325 GHz
    HC3N,CH3CN: 255 GHz
    TBD molecular searches near 250, 350, 650 GHz

7.3. Spectral resolution (km/s): 1 km/s in general. 0.05 km/s for wind measurements

7.4. Bandwidth or spectral coverage (km/s or GHz): 0.2 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       5 % 
                               repeatability  1-3% 
                               relative       1-3% 


9. Line intensity:

9.1. Typical value (K or Jy): 20 mK - 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 - 0.5 K

9.3. Spectral dynamic range:

9.4. Calibration requirements: absolute       5 % 
                               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 1 h per line, except 10 hr for HDO, and 5 h for high-resolution
studies on CO or HCN for wind measurements
In total, 2x10h (HDO) + 15 other molecular lines X 1 h + 5h = 40 h

12. Total integration time for program (hr):
About 160 hours (40 h x 4 planets)



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.