Title  Kinetic Temperature Structure in Protostars and YSOs 
Pi     J. Mangum
Time   15 hrs
1. Name: Kinetic Temperature Structure in Protostars and YSOs
    Authors: J. Mangum, A. Wootten

 2. Science goal: Measure molecular spectral line emission from the
    H2CO molecule from a representative sample of protostars and
    YSOs.  Measurements of the following transitions will provide
    accurate kinetic temperatures for sources with Tk < 75 K:

           -- 3(03)-2(02) at 218.2 GHz
           -- 3(22)-2(21) at 218.5 GHz
           -- 5(05)-4(04) at 362.7 GHz
           -- 5(24)-4(23) at 363.9 GHz

    The program is based on Mangum & Wootten (1993), which described
    the kinetic temperature probing properties of the H2CO molecule.
    This technique has remained relatively untapped due to the lack of
    sensitive instrumentation which can provide the spatial resolution
    required to map the kinetic temperature structure in the youngest
    star formation regions.

3. Number of sources: 30

4. Coordinates: 

  4.1. 10 sources in Oph      (RA=16:30, DEC=-24)
       10 sources in Perseus  (RA=03,  DEC=+30)
       10 sources distributed over sky (RA=any, DEC=any visible)

  4.2. Moving target: no

  4.3. Time critical: no


5.  Spatial scales:

  5.1. Angular resolution: 0.5"
       
  5.2. Range of spatial scales/FOV: 30"

  5.3. Single dish: yes
 
  5.4. ACA: yes

  5.5. Subarrays: no
 

6. Frequencies:

  6.1. Receiver band: Band 6, Band 7

  6.2. Line: H2CO 3(03)-2(02), 3(22)-2(21), 5(05)-4(04), 5(24)-4(23)
       Frequency: 218.2 GHz, 218.5 GHz, 362.7 GHz, 363.9 GHz

  6.3. Spectral resolution (km/s): 0.05 km/s
  
  6.4. Spectral coverage (km/s or GHz): 20 km/s    


7. Continuum flux density:

  7.1. Typical value: O.3 Jy

  7.2. Continuum peak value: 0.3 Jy

  7.3. Required continuum rms: 0.0002 K

  7.4. Dynamic range in image: 20


8. Line intensity:

  8.1. Typical value: 0.03 Jy

  8.2. Required rms per channel: 0.5 K
  
  8.3. Spectral dynamic range: 20


9. Polarization: no


10. Integration time per setting: 30 x 0.5 hrs 

11. Total integration time for program: 15 hr

**************************************************************************

Review John Richer: see 2.1.1.



--------------------------------------------------
Review v2.0:
 
init_3 = 2.1.3 

Name: Kinetic Temperature Structure in Protostars and YSOs
    Authors: J. Mangum, A. Wootten

Unchanged w.r.t. DRSP 1.1. If sensitivity is an issue 7m x 12m
correlations may be useful.