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Welcome to the DeepFields.SuperDeblending wiki!

Here we present our astronomical software suite for super-deblending photometry of deep fields.

Methodology

The idea of super-deblending is using a deep prior source catalog and multiwavelength information of each source to provide deblended photometry of these sources on large PSF images, e.g. Herschel SPIRE band images, and ground-based sub-millimeter (SMM) band images.

Photometry of prior source fitting -- galfit

At each band, what our tool needs is a prior catalog, and three fits format images. Our photometry tool (superdeblending-galfit) will produce an output plain text file containing the photometric measurement of each prior source.

Pre-selection of rior source list -- galcat

The prior catalog can vary at each band, and needs to be carefully selected. At SPIRE and SMM bands, though multiwavelength SED we predict that some sources are too faint to be detected, therefore we reduce the deep catalog to be shallower, then take the reduced catalog as our prior catalog at these bands. The tool (superdeblending-galcat) will read two input files: one deep initial catalog, and one SED fitting result file; then produce a reduced prior catalog for the photometry tool (superdeblending-galfit) at each band.

Spectral energy distribution (SED) fitting -- galsed

Since we make use of multiwavelength SED information to reduce the deep initial catalog at each band, the SED fitting becomes an important step. Our SED fitting tool (superdeblending-galsed) will read a plain text catalog (with certain text format) then produce some SED fitting result files. These SED fitting result files will be used both to derive physical properties of galaxies, and for our reducing of catalog (superdeblending-galcat) at large PSF bands.

Flow chart

Therefore, a simple flow of our super-deblending is:

• (1) having a deep initial catalog, and having multiwavelength images;
• (2) running the SED fitting with whatever available and trustable (superdeblending-galsed);
• (3) preparing the prior catalog for photometry (superdeblending-galcat);
• (4) running the photometry (superdeblending-galfit);
• (5) running the simulation (superdeblending-galsim);
• (6) checking the photometric residual image, find additional sources (superdeblending-galcat) and loop over from step (3);
• (7) moving to next band and loop over from step (2);
• (8) deriving final super-deblended photometry and catalog; producing galaxy multiwavelength cutouts/montages (superdeblending-galmon); and obtaining other scientific results and analyses;