| Author(s) and Co-Author(s) with Affiliation: Sayak Dutta(Inter-University Centre for Astronomy & Astrophysics, Post Bag 04, Pune, 411007, India), Sowgat Muzahid(Inter-University Centre for Astronomy & Astrophysics, Post Bag 04, Pune, 411007, India), Joop Schaye(Leiden Observatory, Niels Bohrweg 02, NL-2333 CA Leiden, the Netherlands), Sean Johnson(Department of Astronomy, University of Michigan, 1085 S. University Ave, Ann Arbor, MI 48109, USA), Nicolas F Bouche(Centre de Recherche Astrophysique de Lyon (CRAL), UMR5574, Univ Lyon1, Ens de Lyon, CNRS, 69230 Saint-Genis-Laval, France), Ramona Augustin(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), Sebastiano Cantalupo(Department of Physics, University of Milan Bicocca, Piazza della Scienza 3, I-20126 Milano, Italy), Hsiao Wen Chen(Department of Astronomy and Astrophysics, The University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USA), Martin Wendt(Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, Germany) |
| Abstract: We investigate cool H I gas traced by Lyman series absorption around 256, galaxies at z ≈ 0.48 (~9) using 15 background quasars (median impact parameter, D = 140 pkpc), as part of the MUSE Quasar-fields Blind Emitters Survey (MUSEQuBES). We find that the H I column density profile around isolated star-forming galaxies spanning ≈ 3 dex in stellar mass is well described by a power law with slope ~ −3 when expressed as a function of normalized impact parameter D/Rvir . The H I covering fraction (k) within the virial radius for log10 (N (H I)/cm−2 ) = 14 is significantly lower in high-mass passive galaxies than in isolated star-forming galaxies. The κ-profile of isolated star-forming galaxies suggests a characteristic size of the H I-rich CGM of ~ 1.5Rvir across the stellar mass range. The mean H I mass in the outer CGM (0.3–1 Rvir ) increases with stellar mass, ranging from ≈ 10^5 to 10^6 M_sun . The b-parameters of the strongest H I components correlate and anticorrelate with specific star-formation rate (sSFR) and mass, respectively, with > 2 sigma significance. Broad Lya absorbers (BLAs) with b > 60 km s−1 are predominantly associated with high-mass galaxies, likely tracing the warm-hot phase of the CGM. The velocity centroids of H I components indicate that absorbers at D < Rvir are largely consistent with being gravitationally bound to their galaxies, independent of stellar mass. Finally, leveraging ~ 3000 galaxies from the wide-field Magellan follow-up of six MUSEQuBES fields, we find that non-isolated galaxies exhibit an H I-rich environment extending roughly three times farther than in isolated counterparts. |
