Title  Dust in gravitationally lensed Lyman Break Galaxies
Pi     M. Sawicki
Time   94.2 hrs

   1. Name of program and authors
   
   Title:  Dust in gravitationally lensed Lyman Break Galaxies.
   Author: Marcin Sawicki, marcin.sawicki@nrc.ca


   2. One short paragraph with science goal(s)

   Star-formation rates and other properties of z~3 Lyman Break
   Galaxies (LBGs) remain only poorly constrained because of the
   presence of starlight-absorbing interstellar dust which can only be
   properly understood by combining rest-far-IR data with rest-frame
   optical and UV observations.  Normal LBGs are expected to be too
   faint at sub-mm wavelengths to yield anything but integrated fluxes
   even with ALMA.  Therefore, to gain understanding of the spatial
   distribution of dust and star formation in LBGs, we propose to
   observe three gravitationally lensed LBGs, whose fluxes are
   magnified by factors of 10-30. These observations, to be carried
   out at 450 and 900 um, will provide information about the spatial
   distribution of dust in LBGs that will be directly comparable to
   rest-frame UV and optical HST observations of these objects.  These
   observations will allow us to study each of these gravitational
   arcs with ~25-100 spatial resolution elements having a S/N=10 per
   spatial resolution element.


   3. Number of sources:  3
			     
   4. Coordinates: 

      4.1. Rough RA and DEC 
	   
                        RA(2000)    Dec(2000)   
	MS1512-cB58    15:14:22.2   +36:36:24 
        Cl1053-arc     10:53:47.2   +57:35:10
        A2218-arc      16:35:49.3   +66:13:07



      4.2. Moving target: no

      4.3. Time critical: no


   5. Spatial scales:

      5.1. Angular resolution (arcsec):  0.1

      5.2. Range of spatial scales/FOV (arcsec):
	   individual point sources - one per field

      5.3. Single dish total power data: no 

      5.4. ACA: no

      5.5. Subarrays: no


   6. Frequencies:

      6.1. Receiver band: Bands 7 and 9 

      6.2. Lines and Frequencies (GHz): 
	   continuum 

      6.3. Spectral resolution (km/s):
	   N/A

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

   7. Continuum flux density:

      7.1. Typical value (Jy): 

		   Total flux density per object
			        1-4 mJy  at 900um  
			       10-40 mJy at 450um

      7.2. Required continuum rms (Jy or K):	   0.004 mJy in Band 7
						   0.04 mJy in Band 9

      7.3. Dynamic range within image:  7


   8. Line intensity:

      8.1. Typical value (K or Jy):  N/A

      8.2. Required rms per channel (K or Jy):  N/A

      8.3. Spectral dynamic range:   N/A


   9. Polarization:  no 

      9.1. Required Stokes  N/A

      9.2. Total polarized flux density (Jy)  N/A

      9.3. Required polarization rms and/or dynamic range N/A

      9.4. Polarization fidelity  N/A


   10. Integration time for each observing mode/receiver setting (hr):
		   Band 7 continuum:  3x20.3 hr   
		   Band 9 continuum:  3x11.1 hr		   

   11. Total integration time for program (hr):	94.2  hrs

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


Review Chris Carilli: OK, integration times checked
--------------------------------------------------
Review v2.0:
 
1.2.5 Dust in gravitationally lensed Lyman Break Galaxies (Sawicki)

Not revised since DRSP 1.1. No further comment, no need for ACA or
ACA/12m array cross-correlation.