1. Name of program and authors
        Name: Sunyaev-Zel'dovich Effect of Proto-Clusters
        Authors: Naoshi Sugiyama, Naoki Yoshida, Tetsuo Hasegawa

     2. One short paragraph with science goal(s)

        Measurements of the fine scale structure of the high redshift
        clusters of galaxies probe formation history of the clusters.
        High-resolution observations of the thermal Sunyaev-Zel'dovich
        effect (SZE) can be an ideal and unique tool for this purpose.
        We can resolve merging proto-clusters whose sizes are
        approximately 100kpc with 10 arc-second resolution, which can
        be easily achieved by ALMA.


     3. Number of sources 

		3' fields for 10 clusters

     4. Coordinates:

        4.1. Rough RA and DEC 

		(uniformly distributed over the sky)

        4.2. Moving target: no

        4.3. Time critical: no


     5. Spatial scales:

        5.1. Angular resolution (arcsec): 1

        5.2. Range of spatial scales/FOV (arcsec): 180" mosaic

        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

		(220 GHz is essential to remove foreground/background)

        6.2. Lines and Frequencies (GHz): 90 and 220 GHz

        6.3. Spectral resolution (km/s): not required

        6.4. Bandwidth or spectral coverage (km/s or GHz): 8 GHz x dual pol


     7. Continuum flux density:

        7.1. Typical value (Jy): 0.1-1 mJy/(1" beam)

        7.2. Required continuum rms (Jy or K): 0.02 mJy/(1" beam)

        7.3. Dynamic range within image: 5 - 50


     8. Line intensity:

        8.1. Typical value (K or Jy):
             (take average value of set of objects)
             (optional: provide range of values for set of objects)

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

        8.3. Spectral dynamic range:


     9. Polarization:  no  (optional)

        9.1. Required Stokes

        9.2. Total polarized flux density (Jy)

        9.3. Required polarization rms and/or dynamic range

        9.4. Polarization fidelity


     10. Integration time for each observing mode/receiver setting (hr):

         10 x 5 hours for Band 3 mosaic
	10 x 25 hours for Band 6 mosaic

     11. Total integration time for program (hr):

         300 hours

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

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

Review Pierre Cox: It seems to me that these programmes could be
merged in one programme since part of the information in 1.4.2 will be
available in 1.4.1.  What is the rationale behind the number of
clusters? Time estimates are correct.

Review Chris Carilli: I think they need 14x14 pointings at 220 GHz
separated by HWHM. That gives about 1.3 hrs/pointing and sensitivity
of 0.012mJy. and this does not include overlap, so the sensivity in
the map will be about factor 2 better.  They state a required value of
0.02 mJy, so I think they could get away with factor 2 or more less
time.  On the other hand, I think they should do factor 4 or so larger
area to do this right, so let it stand as 'representative'