HYDROGEN EMISSION FROM THE IONIZED GASEOUS HALOS OF LOW-REDSHIFT GALAXIES
dc.contributor.author | Zhang, Huanian | |
dc.contributor.author | Zaritsky, Dennis | |
dc.contributor.author | Zhu, Guangtun | |
dc.contributor.author | Ménard, Brice | |
dc.contributor.author | Hogg, David W. | |
dc.date.accessioned | 2017-03-01T23:33:33Z | |
dc.date.available | 2017-03-01T23:33:33Z | |
dc.date.issued | 2016-12-21 | |
dc.identifier.citation | HYDROGEN EMISSION FROM THE IONIZED GASEOUS HALOS OF LOW-REDSHIFT GALAXIES 2016, 833 (2):276 The Astrophysical Journal | en |
dc.identifier.issn | 1538-4357 | |
dc.identifier.doi | 10.3847/1538-4357/833/2/276 | |
dc.identifier.uri | http://hdl.handle.net/10150/622684 | |
dc.description.abstract | Using a sample of nearly half a million galaxies, intersected by over 7 million lines of sight from the Sloan Digital Sky Survey Data Release 12, we trace H alpha + [N II] emission from a galactocentric projected radius, r(p), of 5 kpc to more than 100 kpc. The emission flux surface brightness is alpha r(p) 1.9 +/- 0.4. We obtain consistent results using only the Ha or [N II] flux. We measure a stronger signal for the bluer half of the target sample than for the redder half on small scales, r(p) < 20 kpc. We obtain a 3 sigma detection of H alpha + [N II] emission in the 50-100 kpc r(p) bin. The mean emission flux within this bin is (1.10 +/- 0.35) x 10(-20) erg cm(-2) s(-1) angstrom(-1), which corresponds to 1.87 x 10(-20) erg cm(-2) s(-1) arcsec(-2) or 0.0033 Rayleigh. This detection is 34 times fainter than a previous strict limit obtained using deep narrow-band imaging. The faintness of the signal demonstrates why it has been so difficult to trace recombination radiation out to large radii around galaxies. This signal, combined with published estimates of n(H), leads us to estimate the temperature of the gas to be 12,000 K, consistent with independent empirical estimates based on metal ion absorption lines and expectations from numerical simulations. | |
dc.description.sponsorship | NASA ADAP [NNX12AE27G]; NSF [AST-1311326]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; [NSF-1313302] | en |
dc.language.iso | en | en |
dc.publisher | IOP PUBLISHING LTD | en |
dc.relation.url | http://stacks.iop.org/0004-637X/833/i=2/a=276?key=crossref.3913864949502021f4fa9c3fd08a20c9 | en |
dc.rights | © 2016. The American Astronomical Society. All rights reserved. | en |
dc.rights.uri | http://rightsstatements.org/vocab/InC/1.0/ | |
dc.subject | galaxies: halos | en |
dc.subject | galaxies: ISM | en |
dc.subject | galaxies: kinematics and dynamics | en |
dc.subject | galaxies: structure | en |
dc.subject | intergalactic medium | en |
dc.title | HYDROGEN EMISSION FROM THE IONIZED GASEOUS HALOS OF LOW-REDSHIFT GALAXIES | en |
dc.type | Article | en |
dc.contributor.department | Univ Arizona, Steward Observ | en |
dc.contributor.department | Univ Arizona, Dept Phys | en |
dc.identifier.journal | The Astrophysical Journal | en |
dc.description.collectioninformation | This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu. | en |
dc.eprint.version | Final published version | en |
refterms.dateFOA | 2018-09-11T17:47:04Z | |
html.description.abstract | Using a sample of nearly half a million galaxies, intersected by over 7 million lines of sight from the Sloan Digital Sky Survey Data Release 12, we trace H alpha + [N II] emission from a galactocentric projected radius, r(p), of 5 kpc to more than 100 kpc. The emission flux surface brightness is alpha r(p) 1.9 +/- 0.4. We obtain consistent results using only the Ha or [N II] flux. We measure a stronger signal for the bluer half of the target sample than for the redder half on small scales, r(p) < 20 kpc. We obtain a 3 sigma detection of H alpha + [N II] emission in the 50-100 kpc r(p) bin. The mean emission flux within this bin is (1.10 +/- 0.35) x 10(-20) erg cm(-2) s(-1) angstrom(-1), which corresponds to 1.87 x 10(-20) erg cm(-2) s(-1) arcsec(-2) or 0.0033 Rayleigh. This detection is 34 times fainter than a previous strict limit obtained using deep narrow-band imaging. The faintness of the signal demonstrates why it has been so difficult to trace recombination radiation out to large radii around galaxies. This signal, combined with published estimates of n(H), leads us to estimate the temperature of the gas to be 12,000 K, consistent with independent empirical estimates based on metal ion absorption lines and expectations from numerical simulations. |