Uploaded image for project: 'Data Management'
  1. Data Management
  2. DM-23071

Update default aperture correction configuration in hsc to select bright stars

    Details

    • Type: Story
    • Status: Done
    • Resolution: Done
    • Fix Version/s: None
    • Component/s: obs_subaru
    • Labels:
      None
    • Templates:
    • Story Points:
      4
    • Team:
      Data Release Production

      Description

      Inspired by some anomalous behavior in simulated DESC DC2 imaging, I started an
      investigation of the difference between psf magnitudes and
      CircularAperture_12_0 magnitudes (used for calibration) on calexp s.
      This comparison is particularly important because the aperture correction maps
      that are applied to all fluxes in both calexp source catalogs and coadd
      catalogs are derived from this relationship. It turns out that there is
      significant curvature in the psf - aper relationship. These plots use all the
      stars used for the psf modeling across all 103 ccds in a visit, the same stars
      that were used to compute the aperture correction map:

      All of these plots are for some sample i-band images, but the problem is seen
      across a wide range of bands and images, see
      https://lsstc.slack.com/archives/C2JPXB4HG/p1576703633032000 and following.

      Also notable is that the scatter is reduced if you do not apply the aperture
      corrections to the psf fluxes, though an overall offset appears (as is expected
      if you don't compute any aperture correction):

      The shape of the curvature is consistent with that expected from a sky offset.
      This is further demonstrated by comparing the psf - aper bias for different
      aperture sizes:

      Further investigation has shown that the bias is indeed caused by offsets in
      the sky, and in fact are tracked by the LocalBackground estimation:

      That is, when delta-mag (psf - aper) is negative, the local background is
      negative as well (for faint stars where the background matters).

      The basic problem is that we have (known) issues with the background in the
      calexp images which we correct in the coaddition stage. However, these issues
      create problems in both the photometric calibration and the aperture correction
      computation which confuses the background problem (which is an additive
      problem) with the zeropoints and aperture corrections (which are multiplicative
      corrections).

      A pragmatic solution proposed by Robert Lupton is to do what was originally intended:
      only use bright stars when computing the aperture correction map.

      I ran processCcd on a single i-band exposure where the aperture correction
      was computed only with stars that were used for the psf modeling and had psf
      s/n > 250. This of course does not fix the curvature, but leads to much
      reduced scatter at the bright end between calibration and psf magnitudes:

      ||

      Finally, I ran all of VVDS i-band from RC2 through singleFrameDriver with
      the new configuration, and ran validate_drp (without jointcal) for both the
      RC2 "vanilla" processing from w_2019_46 and from the new aperbright
      processing. The PA1 metric reduced from 23.6 mmag to 19.5 mmag, or a
      difference in quadrature of approximately 13 mmag, which is quite a difference.

        Attachments

          Issue Links

            Activity

              People

              • Assignee:
                erykoff Eli Rykoff
                Reporter:
                erykoff Eli Rykoff
                Reviewers:
                Jim Bosch
                Watchers:
                Eli Rykoff, James Chiang, Jim Bosch, John Swinbank
              • Votes:
                0 Vote for this issue
                Watchers:
                4 Start watching this issue

                Dates

                • Created:
                  Updated:
                  Resolved:

                  Summary Panel