TY - JOUR
T1 - The CGM2Survey
T2 - Circumgalactic O vi from Dwarf to Massive Star-forming Galaxies
AU - Tchernyshyov, Kirill
AU - Werk, Jessica K.
AU - Wilde, Matthew C.
AU - Prochaska, J. Xavier
AU - Tripp, Todd M.
AU - Burchett, Joseph N.
AU - Bordoloi, Rongmon
AU - Howk, J. Christopher
AU - Lehner, Nicolas
AU - O'Meara, John M.
AU - Tejos, Nicolas
AU - Tumlinson, Jason
N1 - Funding Information:
Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. A listing of the participating institutions can be found at https://www.sdss.org/collaboration/citing-sdss/ .
Funding Information:
K.T. would like to thank Matt McQuinn and Yakov Faerman for useful discussions, Ben Oppenheimer and Zhijie Qu for providing predictions from their models, and the referee for a helpful and constructive report. This research has made use of the HSLA database, developed and maintained at STScI, Baltimore, USA. K.T., J.K.W., and M.C.W. acknowledge support from from NSF-AST 1812521. Additionally, J.K.W. and K.T. acknowledge support from the Research Corporation for Science Advancement, Cottrell Scholar grant ID No. 26842. The ongoing efforts of the Student Quasar Absorption Diagnosticians (aka Werk SQuAD) in the University of Washington Astronomy Department to vet automated measurements of thousands of galaxy redshifts and vet Voigt profile fits for thousands of absorption lines in CGM were instrumental to the science presented in this study. This work benefited from lively Zoom discussions during KITP’s “Fundamentals of Gaseous Halos” program, and thus was supported in part by the National Science Foundation under grant No. NSF PHY-1748958. 2
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/3/1
Y1 - 2022/3/1
N2 - We combine 126 new galaxy-O vi absorber pairs from the CGM2 survey with 123 pairs drawn from the literature to examine the simultaneous dependence of the column density of O vi absorbers (N O VI) on galaxy stellar mass, star-formation rate, and impact parameter. The combined sample consists of 249 galaxy-O vi absorber pairs covering z = 0-0.6, with host galaxy stellar masses M ∗ = 107.8-1011.2 M o˙ and galaxy-absorber impact parameters R ⊥ = 0-400 proper kiloparsecs. In this work, we focus on the variation of N O VI with galaxy mass and impact parameter among the star-forming galaxies in the sample. We find that the average N O VI within one virial radius of a star-forming galaxy is greatest for star-forming galaxies with M ∗ = 109.2-1010 M o˙. Star-forming galaxies with M ∗ between 108 and 1011.2 M o˙ can explain most O vi systems with column densities greater than 1013.5 cm-2. Sixty percent of the O vi mass associated with a star-forming galaxy is found within one virial radius, and 35% is found between one and two virial radii. In general, we find that some departure from hydrostatic equilibrium in the CGM is necessary to reproduce the observed O vi amount, galaxy mass dependence, and extent. Our measurements serve as a test set for CGM models over a broad range of host galaxy masses.
AB - We combine 126 new galaxy-O vi absorber pairs from the CGM2 survey with 123 pairs drawn from the literature to examine the simultaneous dependence of the column density of O vi absorbers (N O VI) on galaxy stellar mass, star-formation rate, and impact parameter. The combined sample consists of 249 galaxy-O vi absorber pairs covering z = 0-0.6, with host galaxy stellar masses M ∗ = 107.8-1011.2 M o˙ and galaxy-absorber impact parameters R ⊥ = 0-400 proper kiloparsecs. In this work, we focus on the variation of N O VI with galaxy mass and impact parameter among the star-forming galaxies in the sample. We find that the average N O VI within one virial radius of a star-forming galaxy is greatest for star-forming galaxies with M ∗ = 109.2-1010 M o˙. Star-forming galaxies with M ∗ between 108 and 1011.2 M o˙ can explain most O vi systems with column densities greater than 1013.5 cm-2. Sixty percent of the O vi mass associated with a star-forming galaxy is found within one virial radius, and 35% is found between one and two virial radii. In general, we find that some departure from hydrostatic equilibrium in the CGM is necessary to reproduce the observed O vi amount, galaxy mass dependence, and extent. Our measurements serve as a test set for CGM models over a broad range of host galaxy masses.
UR - http://www.scopus.com/inward/record.url?scp=85126596092&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ac450c
DO - 10.3847/1538-4357/ac450c
M3 - Article
AN - SCOPUS:85126596092
VL - 927
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 147
ER -