Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 466, Issue 2, Pages 1582-1596Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw3151
Keywords
methods: statistical; surveys; galaxies: distances and redshifts
Categories
Funding
- Australian Research Council Laureate Grant [FL0992131]
- Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]
- Netherlands Organization for Scientific Research, NWO [614.001.451]
- Netherlands Organization for Scientific Research, NWO through FP7 grant from the European Research Council [279396]
- Polish National Science Center [UMO-2012/07/D/ST9/02785]
- Australian Research Council through the award of a Future Fellowship
- European Research Council [647112]
- Deutsche Forschungsgemeinschaft under Emmy Noether grant [Hi 1495/2-1]
- Deutsche Forschungsgemeinschaft [TR33]
- Australian Astronomical Observatory [A/2014B/08]
- Alexander von Humboldt Foundation
- Australian Research Council Future Fellowship [FT130101086]
- ESO VST-ATLAS survey [177.A-3011]
- National Aeronautics and Space Administration
- Australian Research Council [FT130101086] Funding Source: Australian Research Council
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We present a new training set for estimating empirical photometric redshifts of galaxies, which was created as part of the 2-degree Field Lensing Survey project. This training set is located in a similar to 700 deg(2) area of the Kilo-Degree-Survey South field and is randomly selected and nearly complete at r < 19.5. We investigate the photometric redshift performance obtained with ugriz photometry from VST-ATLAS and W1/W2 fromWISE, based on several empirical and template methods. The best redshift errors are obtained with kernel-density estimation (KDE), as are the lowest biases, which are consistent with zero within statistical noise. The 68th percentiles of the redshift scatter for magnitude-limited samples at r < (15.5, 17.5, 19.5) are (0.014, 0.017, 0.028). In this magnitude range, there are no known ambiguities in the colour-redshift map, consistent with a small rate of redshift outliers. In the fainter regime, the KDE method produces p(z) estimates per galaxy that represent unbiased and accurate redshift frequency expectations. The p(z) sum over any subsample is consistent with the true redshift frequency plus Poisson noise. Further improvements in redshift precision at r < 20 would mostly be expected from filter sets with narrower passbands to increase the sensitivity of colours to small changes in redshift.
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