Title  Sunyaev-Zeldovich Effect of Galaxy Clusters at High Redshift
Pi     N. Sugiyama
Time   400 hrs

1. Name of program and authors
Name: Sunyaev-Zeldovich Effect of Galaxy Clusters at High Redshift
Authors: Naoshi Sugiyama, Naoki Yoshida, Tetsuo Hasegawa

2. One short paragraph with science goal(s)

Observing the fine structure of clusters of galaxies
probes 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. With 10 arc-second resolution, we can
resolve merging proto-clusters whose sizes are approximately 100kpc.
ALMA can also detect the kinematic SZE which is caused by streaming
motion of galaxy clusters. Although the expected signal is smaller
than the thermal SZE, merging clusters could imprint a peculiar dipole
pattern that can be easily identified. Multi-frequency observations
are essential.


3. Number of sources

  1' deep field; about a few high-z clusters per FOV.
  (Selected based on optical/X-ray cluster catalogue.
   Not necessary to specify a peculiar object.)

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): 1-2
  5.2. Range of spatial scales/FOV (arcsec): 60" 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): 0.01-0.1 mJy/(1" beam)
 7.2. Required continuum rms (Jy or K): 0.002 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:
 8.4. Calibration requirements: absolute      (5%)
                               repeatability (5%)
                               relative      (5%)
9. Line intensity: no

 9.1. Typical value (K or Jy):

     (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):

 9.3. Spectral dynamic range:

 9.4. Calibration requirements:

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):
    (for band 3)
    30 hours (per pointing) for the ACA-baseline_ALMA cross-correlation,
    and additional 90 hours for the stand-alone ACA

12. Total integration time for program (hr):
    500 hours (ACA-baseline_ALMA cross-correlation)
    1500 hours (ACA stand alone)

13. Comments on observing strategy :

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Review v2.0:
 
1.4.2

The requested rms level is 2 micro Jy (for both band 3 and 6,
presumably; please indicate explicitly).  The authors estimate that
integration time of 30 hours per pointing for band 3 observations with
ACA and 12-m array cross correlations, yet much shorter integration is
OK for band 3, and slightly longer integration seems to be needed for
band 6.  Please check together with the justification of the total
requested integration time.

The authors request an absolute calibration accuracy of 5 %.  I am
wondering if there is a clear reason to justify this calibration
accuracy. I understand the *relative* accuracy between band 3 and 6 is
essential for this project, but the requirement for *absolute* one is
somewhat unclear.

In the band 6 observations, we may also detect significant numbers of
SMGs toward high-z clusters of galaxies; strategy for careful removal
of them will be an issue.