2020/11/05 by Adriana Durbala, Rose A. Finn, Mary Crone Odekon +4 · 1 citation
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Interacting galaxy #Lenticular galaxy #Luminous infrared galaxy #Photometry (optics) #Sky #Space Technology and Applications #Star formation #Stellar population #astro-ph.GA
paper · pdf · doi:10.3847/1538-3881/abc018
18 pages, 10 figures, 3 tables; original version submitted to the Astronomical Journal. For final version please refer to the published version. ALFALFA data page: http://egg.astro.cornell.edu/alfalfa/data/index.php
arxiv created 2020/11/05 · openalex created_date 2020/11/09 · openalex publication_date 2020/11/18 · arxiv updated 2020/11/25 · openalex updated_date 2026/08/06
Abstract We present a H i optical catalog of ∼30,000 galaxies based on the 100% complete Arecibo Legacy Fast Arecibo L -band Feed Array (ALFALFA) survey combined with data from the Sloan Digital Sky Survey (SDSS). Our goal is to facilitate the public use of the completed ALFALFA catalog by providing carefully determined matches to SDSS counterparts, including matches for ∼10,000 galaxies that do not have SDSS spectra. These identifications can provide a basis for further crossmatching with other surveys using SDSS photometric IDs as a reference point. We derive absolute magnitudes and stellar masses for each galaxy using optical colors combined with an internal reddening correction designed for small- and intermediate-mass galaxies with active star formation. We also provide measures of stellar masses and star formation rates based on infrared and/or ultraviolet photometry for galaxies that are detected by the Wide-field Infrared Survey Explorer and/or the Galaxy Evolution Explorer. Finally, we compare the galaxy population in the ALFALFA-SDSS sample with the populations in several other publicly available galaxy catalogs and confirm that ALFALFA galaxies typically have lower masses and bluer colors.