TY - JOUR
T1 - Modelling gas around galaxy pairs and groups using the Q0107 quasar triplet
AU - Beckett, Alexander
AU - Morris, Simon L.
AU - Fumagalli, Michele
AU - Tejos, Nicolas
AU - Jannuzi, Buell
AU - Cantalupo, Sebastiano
N1 - Funding Information:
This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5–26555. We also make use of observations collected at the European Southern Observatory under ESO programmes 086.A-0970, 087.A-0857 and 094.A-0131; at the W.M. Keck Observatory under programme A290D; and at the Gemini Observatory under programme GS-2008B-Q-50.
Funding Information:
AB acknowledges the support of a UK Science and Technology Facilities Council (STFC) PhD studentship through grant ST/S505365/1. SLM acknowledges the support of STFC grant ST/T000244/1.
Funding Information:
First, we thank the anonymous referee for their insightful comments that have improved the quality of this paper. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5–26555. We also make use of observations collected at the European Southern Observatory under ESO programmes 086.A-0970, 087.A-0857 and 094.A-0131; at the W.M. Keck Observatory under programme A290D; and at the Gemini Observatory under programme GS-2008B-Q-50. We thank Matteo Fossati for providing the MARZ templates used for estimating redshifts and their uncertainties. We also thank Jill Bechtold for leading the effort to obtain the Keck/DEIMOS data. We thank the contributors to SCIPY6, MATPLOTLIB7, ASTROPY8, and the PYTHON programming language, the free and open-source community and the NASA Astrophysics Data system9 for software and services. This work also made use of the DiRAC system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility10 AB acknowledges the support of a UK Science and Technology Facilities Council (STFC) PhD studentship through grant ST/S505365/1. SLM acknowledges the support of STFC grant ST/T000244/1. SC gratefully acknowledges support from Swiss National Science Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement No 864361. MF also acknowledges funding from the ERC under the Horizon 2020 programme (grant agreement No 757535). This work has been supported by Fondazione Cariplo, grant No 2018–2329.
Funding Information:
SC gratefully acknowledges support from Swiss National Science Foundation grants PP00P2_163824 and PP00P2_190092, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement No 864361. MF also acknowledges funding from the ERC under the Horizon 2020 programme (grant agreement No 757535). This work has been supported by Fondazione Cariplo, grant No 2018–2329.
Publisher Copyright:
© 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.
PY - 2023/5/1
Y1 - 2023/5/1
N2 - We examine to what extent disc and outflow models can reproduce observations of H I gas within a few virial radii of galaxies in pairs and groups. Using highly sensitive HST/COS and FOS spectra of the Q0107 quasar triplet covering Ly α for z≾1, as well as a deep galaxy redshift survey including VIMOS, DEIMOS, GMOS, and MUSE data, we test simple disc and outflow models against the H I absorption along three lines-of-sight (separated by 200–500 kpc) through nine galaxy groups in this field. These can be compared with our previous results in which these models can often be fit to the absorption around isolated galaxies. Our models can reproduce ≈ 75 per cent of the 28 identified absorption components within 500 km s−1 of a group galaxy, so most of the H I around groups is consistent with a superposition of the CGM of the individual galaxies. Gas stripped in interactions between galaxies may be a plausible explanation for some of the remaining absorption, but neither the galaxy images nor the galaxy and absorber kinematics provide clear evidence of such stripped material, and these unexplained absorbers do not preferentially occur around close pairs of galaxies. We find H I column densities typically higher than at similar impact parameters around isolated galaxies (≈ 2.5σ), as well as more frequent detections of O VI than around isolated galaxies (30 per cent of sightlines to 7 per cent).
AB - We examine to what extent disc and outflow models can reproduce observations of H I gas within a few virial radii of galaxies in pairs and groups. Using highly sensitive HST/COS and FOS spectra of the Q0107 quasar triplet covering Ly α for z≾1, as well as a deep galaxy redshift survey including VIMOS, DEIMOS, GMOS, and MUSE data, we test simple disc and outflow models against the H I absorption along three lines-of-sight (separated by 200–500 kpc) through nine galaxy groups in this field. These can be compared with our previous results in which these models can often be fit to the absorption around isolated galaxies. Our models can reproduce ≈ 75 per cent of the 28 identified absorption components within 500 km s−1 of a group galaxy, so most of the H I around groups is consistent with a superposition of the CGM of the individual galaxies. Gas stripped in interactions between galaxies may be a plausible explanation for some of the remaining absorption, but neither the galaxy images nor the galaxy and absorber kinematics provide clear evidence of such stripped material, and these unexplained absorbers do not preferentially occur around close pairs of galaxies. We find H I column densities typically higher than at similar impact parameters around isolated galaxies (≈ 2.5σ), as well as more frequent detections of O VI than around isolated galaxies (30 per cent of sightlines to 7 per cent).
KW - absorption lines
KW - evolution - intergalactic medium-quasars
KW - galaxies
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U2 - 10.1093/mnras/stad596
DO - 10.1093/mnras/stad596
M3 - Article
AN - SCOPUS:85161215120
SN - 0035-8711
VL - 521
SP - 1113
EP - 1143
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -