TY - JOUR
T1 - Quasar Sightline and Galaxy Evolution (QSAGE) survey-I. The galaxy enVIronment of O VI absorbers up to z = 1.4 around PKS 0232-04
AU - Bielby, R. M.
AU - Stott, J. P.
AU - Cullen, F.
AU - Tripp, T. M.
AU - Burchett, J. N.
AU - Fumagalli, M.
AU - Morris, S. L.
AU - TEJOS SALGADO, NICOLÁS ANDRÉS
AU - Crain, R. A.
AU - Bower, R. G.
AU - Prochaska, J. X.
N1 - Publisher Copyright:
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
Copyright:
Copyright 2021 Elsevier B.V., All rights reserved.
PY - 2019/6/11
Y1 - 2019/6/11
N2 - We present the first results from a study of O vi absorption around galaxies at z < 1.44 using data from a near-infrared grism spectroscopic Hubble Space Telescope Large Programme, the Quasar Sightline and Galaxy Evolution (QSAGE) survey. QSAGE is the first grism galaxy survey to focus on the circumgalactic medium at z ∼1, providing a blind survey of the galaxy population. The galaxy sample is H α flux limited (f(H α) > 2 × 10-17 erg s-1 cm-2) at 0.68 < z < 1.44, corresponding to 0.2-0.8 M· yr-1. In this first of 12 fields, we combine the galaxy data with high-resolution STIS and COS spectroscopy of the background quasar to study O vi in the circumgalactic medium. At z ∼1, we find O vi absorption systems up to b ∼350 kpc (∼4Rvir) from the nearest detected galaxy. Further, we find ∼50% of 1 M· yr-1 star-forming galaxies within 2Rvir show no associated O vi absorption to a limit of at least N(O vi) = 1013.9 cm-2. That we detect O vi at such large distances from galaxies and that a significant fraction of star-forming galaxies show no detectable O vi absorption disfavours outflows from ongoing star formation as the primary medium traced by these absorbers. Instead, by combining our own low-and high-redshift data with existing samples, we find tentative evidence for many strong (N(O vi) > 1014 cm-2) O vi absorption systems to be associated with M· ∼109.5-10 M· mass galaxies (Mhalo ∼1011.5-12 M· dark matter haloes), and infer that they may be tracing predominantly collisionally ionized gas within the haloes of such galaxies.
AB - We present the first results from a study of O vi absorption around galaxies at z < 1.44 using data from a near-infrared grism spectroscopic Hubble Space Telescope Large Programme, the Quasar Sightline and Galaxy Evolution (QSAGE) survey. QSAGE is the first grism galaxy survey to focus on the circumgalactic medium at z ∼1, providing a blind survey of the galaxy population. The galaxy sample is H α flux limited (f(H α) > 2 × 10-17 erg s-1 cm-2) at 0.68 < z < 1.44, corresponding to 0.2-0.8 M· yr-1. In this first of 12 fields, we combine the galaxy data with high-resolution STIS and COS spectroscopy of the background quasar to study O vi in the circumgalactic medium. At z ∼1, we find O vi absorption systems up to b ∼350 kpc (∼4Rvir) from the nearest detected galaxy. Further, we find ∼50% of 1 M· yr-1 star-forming galaxies within 2Rvir show no associated O vi absorption to a limit of at least N(O vi) = 1013.9 cm-2. That we detect O vi at such large distances from galaxies and that a significant fraction of star-forming galaxies show no detectable O vi absorption disfavours outflows from ongoing star formation as the primary medium traced by these absorbers. Instead, by combining our own low-and high-redshift data with existing samples, we find tentative evidence for many strong (N(O vi) > 1014 cm-2) O vi absorption systems to be associated with M· ∼109.5-10 M· mass galaxies (Mhalo ∼1011.5-12 M· dark matter haloes), and infer that they may be tracing predominantly collisionally ionized gas within the haloes of such galaxies.
KW - galaxies: distances and redshifts
KW - intergalactic medium
KW - quasars: absorption lines
UR - http://www.scopus.com/inward/record.url?scp=85072544109&partnerID=8YFLogxK
U2 - 10.1093/mnras/stz774
DO - 10.1093/mnras/stz774
M3 - Article
AN - SCOPUS:85072544109
VL - 486
SP - 21
EP - 41
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 1
ER -