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NOTE: These results have been surplanted by updated values using more recent WISE and Planck data. You can find the masks and data used for the newer measurements
here.
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Here you will find the MANGLE polygons used to mask WISE Allsky catalog data
in
DiPompeo et al. (2014)
and
DiPompeo et al. (2015).
See the papers for full details, and please cite them if you use these products.
The masks are in .ply format, and can be read into IDL using read_mangle_polygons.pro
in IDLUTILS.
Regions with moon_lev > 1: high_moon.ply
Regions with high extinction (A_g > 0.18): high_extinct.ply
Regions identified with highly clustered flagged objects (cc_flags NE 0 in W1 or W2, ext_flag NE 0, or n_b GT 2): extended_flagged.ply
Small regions around remaining objects with cc_flag NE 0, which appear to be roughly randomly distributed on the sky, but are not: individual_ccflagged.ply
The full mask containing all four of the above polygon lists, pixelized to a simple, resolution 6 scheme (scheme='6s') to speed up use: wise_mask_pix.ply
In addition, we apply two masks from the SDSS, since we use SDSS photometry to split our sample between
obscured and unobscured quasars. For more on the SDSS masks, see White et al. (2011) and
White et al. (2012), as well as the
SDSS-III Data Model.
Bad SDSS fields: badfield_mask_unphot-ugriz_pix.ply
SDSS bright stars: bright_star_mask_pix.ply