Stackphot Initial Release

I have finished up some major work on the IPP stack extended source photometry analysis, and I am placing a small example on an rsync server for people to investigate.

The data can be found at: rsync://pikake.ifa.hawaii.edu/md04.stackphot

Download it with a command like:

rsync -auv rsync://pikake.ifa.hawaii.edu/md04.stackphot/ md04.stackphot/

There are two sets of files in this directory:

  • MD04.skycell.079.stk.* : these are the inputs to the stackphot analysis
  • MD04.skycell.079.stkphot.* : these are the outputs from the stackphot analysis.

The analysis was performed using the griz images from the current 'refstack' for MD04. Those stacks do not include some of the recent fixes related to the covariance matrix calculation. That point may affect the depth to which psphot did the analysis.

There are 4 sets of output files, one for each of the input filter images (0 = i, 1 = g, 2 = r, 3 = z). The *.im.fits is the psf-matched image, *.wt.fits is the equivalent variance, *.mk.fits is the equivalent mask, *.cmf is the set of FITS tables with detection information. In the cmf files, there are 4 data units. The primary data unit is the header with metadata about the input image (not very complete or accurate I'm afraid -- we are fixing this up). The next (EXTNAME = SkyChip?.psf) is the PSF table. This uses a new format 'PS1_SV1' which includes fields for the radial profile information (see below), along with the cmf fields familiar from the PS1_V2 version. (Note that we will continue to use PS1_V2 for all photometry analysis except stackphot and diff -- for diff we will be using the PS1_DV1 format which I've mentioned before). The next data unit (EXTNAME = SkyChip?.xsrc) is the extended source table, with the elliptical profile data and the petrosians -- note that these are only provided for 'extended' sources. The final data unit (EXTNAME = SkyChip?.deteff) is the detection efficiency table.

Note that we are intending to change the EXTNAMEs to all upper case (perhaps before next week).

Over the next few days, I'll be running more of these MD04 skycells. We also will create a new set of stacks using all of the images to date (or a 'best seeing' subset).


Here is a summary of the stackphot analysis:

In the stack photometry analysis, we start with a set of skycell images (normally stacks, but they could be warps as well). In the case of stacks, the input stack data has both convolved (PSF-matched) and unconvolved images. For the stackphot analysis, like in the stack analysis, we define a target PSF and smooth the input images to generate a set of PSF-matched images that have the desired target PSF. We can optionally use the convolved stacks or the unconvolved stacks as the input to this PSF-matching step.

We then use the unconvolved images for the detection process. We perform the detection process on the individual images. We also generate a chi square image from all inputs and run the detection analysis on that image as well.

The detected sources in each of the input images are merged together into a set of common objects. For images where a source is not detected, we generate one from the common object at the location -- in the end all positions for which a source is detected on any image is then treated as a source. For all sources, we force a common position (average of the actual detections).

We then use the convolved images (PSF-matched to the target PSF) to perform the analysis. In addition to the standard psf photometry, we now generate additional measurements: for all sources, we measure aperture fluxes for a series of radial apertures, along with the errors and the 'fill factor' (the number of pixels used for a given radius divided by the area at that radius in pixels -- this is useful to judge the amount of masking and quality of the aperture).

For extended sources, we also measure the elliptical contour at the 0.25 Peak flux level. We use this contour to generate a re-normalized radial profile, following the elliptical contour. In order to generate a clean radial profile, we measure the profile separately for each of 30 angular bins and compare 180-degree opposite bins -- the shallower of the opposite profiles wins out. This enforces 180 degree rotational symmetry and approximates the SDSS deblender. Also note that the analysis of a single source is performed with the other sources subtracted (using the best fit psf or simple galaxy model), so the resulting analysis is essentially isolated to a single source.

We then use the radial profiles to measure Petrosian quantities (Petrosian radius, magnitude, R50, R90 values as defined by SDSS). We also report the surface brightness and enclosed flux at specific major axis radii for the elliptical contours. (Again -- these are only reported for the extended sources).

I have made comparisons to the SDSS analysis using SDSS images and find that the results agree well (I'll put together a report over the next few days).

For both the circular and elliptical apertures, we are currently using the radii defined by SDSS. The inner and outer radii in pixels are listed below:

@RADIAL.ANNULAR.BINS.LOWER           F32     0.00 0.56 1.69 2.59 4.41 7.51 11.58 18.58 28.55 45.50  70.51 110.53 172.49 269.52 420.51
@RADIAL.ANNULAR.BINS.UPPER           F32     0.56 1.69 2.59 4.41 7.51 11.58 18.58 28.55 45.50 70.51 110.53 172.49 269.52 420.51 652.50

Some points and caveats:

  • unlike SDSS, we are currently using the Petrosian flux measured on a given image to determine R50 and R90 for that image (SDSS uses the r-band)
  • the average object positions are used to measure the radial, not r-band specifically like SDSS
  • we do not currently resample and recenter the source pixels to place the center at a pixel center (as photo does). this should only be an important effect in the inner ~2 pixels if the image is nearly undersampled (which we clearly are not).
  • the zero points are not being carried into the stack correctly, so the photometry is NOT currently calibrated. The data in the sample is from MD04, which overlaps SDSS, so it should be easy to calibrate from SDSS.
  • the astrometric calibration is being applied to the output 'cmf' tables, but the WCS seems to be broken in the header
  • there is a bit of work still needed to integrate the analysis into the IPP automatically.
  • non-linear model fits are still not being included in the analysis