2008/04/21 by Nicholas M. Ball, Robert J. Brunner, Adam D. Myers +4 · 7 citations
Environmental Science · Mathematics · Physics and Astronomy · #Advanced Statistical Methods and Models #Astronomy #Astrophysics #Galaxies: Formation, Evolution, Phenomena #Galaxy #Mathematics #Photometric redshift #Photometry (optics) #Physics #Probability distribution #Quasar #Redshift #Remote Sensing in Agriculture #Sky #Stars #Statistics #astro-ph
paper · pdf · doi:10.1086/589646
Accepted to ApJ, 10 pages, 12 figures, uses emulateapj.cls
arxiv created 2008/04/21 · openalex publication_date 2008/08/07 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We apply machine learning in the form of a nearest neighbor instance-based algorithm (NN) to generate full photometric redshift probability density functions (PDFs) for objects in the Fifth Data Release of the Sloan Digital Sky Survey (SDSS DR5). We use a conceptually simple but novel application of NN to generate the PDFs, perturbing the object colors by their measurement error and using the resulting instances of nearest neighbor distributions to generate numerous individual redshifts. When the redshifts are compared to existing SDSS spectroscopic data, we find that the mean value of each PDF has a dispersion between the photometric and spectroscopic redshift consistent with other machine learning techniques, being σ = 0.0207 ± 0.0001 for main sample galaxies to r < 17.77 mag, σ = 0.0243 ± 0.0002 for luminous red galaxies to r ≲ 19.2 mag, and σ = 0.343 ± 0.005 for quasars to i < 20.3 mag. The PDFs allow the selection of subsets with improved statistics. For quasars, the improvement is dramatic: for those with a single peak in their probability distribution, the dispersion is reduced from 0.343 to σ = 0.117 ± 0.010, and the photometric redshift is within 0.3 of the spectroscopic redshift for 99.3% ± 0.1% of the objects. Thus, for this optical quasar sample, we can virtually eliminate "catastrophic" photometric redshift estimates. In addition to the SDSS sample, we incorporate ultraviolet photometry from the Third Data Release of the Galaxy Evolution Explorer All-Sky Imaging Survey ( GALEX AIS GR3) to create PDFs for objects seen in both surveys. For quasars, the increased coverage of the observed-frame UV of the SED results in significant improvement over the full SDSS sample, with σ = 0.234 ± 0.010. We demonstrate that this improvement is genuine and not an artifact of the SDSS- GALEX matching process.