CGM<sup>2</sup> I: The Extent of the Circumgalactic Medium Traced by Neutral Hydrogen

Wilde, Matthew C.; Werk, Jessica K.; Burchett, Joseph N.; Prochaska, J. X.; Tchernyshyov, Kirill; Tripp, Todd M.; Tejos, Nicolás; Lehner, Nicolas; Bordoloi, Rongmon; O’Meara, John M.; Tumlinson, Jason

doi:10.3847/1538-4357/abea14

Cited by 47 publications

(43 citation statements)

References 109 publications

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“…with N HI ≤ 10 14 cm −2 are in the CGM, but with a fraction that increases with N HI for halo masses 10 10 M ≤ M h < 10 12 M . Wilde et al (2021) have recently suggested that R vir may underestimate the true extent of the CGM, particularly around lower mass galaxies. These authors found that, while H I absorption lines with N HI < 10 14 cm −2 are not strongly associated with massive galaxies, absorbers with N HI > 10 14 cm −2 have a high probability (i.e.…”

Section: Modelmentioning

confidence: 99%

Limits on non-canonical heating and turbulence in the intergalactic medium from the low redshift Lyman-alpha forest

Bolton,

Gaikwad,

Haehnelt

et al. 2021

Preprint

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We examine the column density distribution function (CDDF) and Doppler parameter distribution from hydrodynamical simulations and Cosmic Origins Spectrograph (COS) observations of the Lyα forest at redshift 0 ≤ z ≤ 0.2. Allowing for a factor of two uncertainty in the metagalactic H I photoionisation rate, our hydrodynamical simulations are in good agreement (1-1.5σ ) with the shape and amplitude of the observed CDDF at H I column densities 10 13.3 cm −2 ≤ N HI ≤ 10 14.5 cm −2 . However, the Doppler widths of the simulated lines remain too narrow with respect to the COS data. We argue that invoking AGN feedback does not resolve this discrepancy. We also disfavour enhanced photoheating rates as a potential solution, as this requires an unphysically hard UV background spectrum. If instead appealing to a non-canonical source of heating, an additional specific heat injection of u 6.9 eV m −1 p is required at z 2.5 for gas that has N HI 10 13.5 cm −2 by z = 0.1. Alternatively, there may be an unresolved line of sight turbulent velocity component of v turb 8.5 km s −1 (N HI /10 13.5 cm −2 ) 0.21 for the coldest gas in the diffuse IGM.

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Section: Modelmentioning

confidence: 99%

Limits on non-canonical heating and turbulence in the intergalactic medium from the low redshift Lyman-alpha forest

Bolton,

Gaikwad,

Haehnelt

et al. 2021

Preprint

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“…Using samples of absorber-galaxy pairs, the distribution of the multiphase gas around galaxies and its dependence on galaxy properties have been studied at z ࣠ 0.5 (e.g. Prochaska et al 2011Prochaska et al , 2017Stocke et al 2013;Tumlinson et al 2013;Liang & Chen 2014;Werk et al 2014;Burchett et al 2016Burchett et al , 2019Chen et al 2018;Berg et al 2019;Wilde et al 2021) and at z 2 (e.g. Rudie et al 2012Rudie et al , 2019Turner et al 2014Turner et al , 2015Fumagalli et al 2015;Bielby et al 2017b).…”

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confidence: 99%

Metal-enriched halo gas across galaxy overdensities over the last 10 billion years

Dutta

Fumagalli

Fossati

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a study of metal-enriched halo gas traced by Mg ii and C iv absorption at z < 2 in the MUSE Analysis of Gas around Galaxies survey and the Quasar Sightline and Galaxy Evolution survey. Using these large and complete galaxy surveys in quasar fields, we study the dependence of the metal distribution on galaxy properties and overdensities, out to physical projected separations of 750 kpc. We find that the cool, low-ionization gas is significantly affected by the environment across the full redshift range probed, with ≈2 − 3 times more prevalent and stronger Mg ii absorption in higher overdensity group environments and in regions with greater overall stellar mass and star formation rates. Complementary to these results, we have further investigated the more highly ionized gas as traced by C iv absorption, and found that it is likely to be more extended than the Mg ii gas, with ≈2 times higher covering fraction at a given distance. We find that the strength and covering fraction of C iv absorption show less significant dependence on galaxy properties and environment than the Mg ii absorption, but more massive and star-forming galaxies nevertheless also show ≈2 times higher incidence of C iv absorption. The incidence of Mg ii and C iv absorption within the virial radius shows a tentative increase with redshift, being higher by a factor of ≈1.5 and ≈4, respectively, at z > 1. It is clear from our results that environmental processes have a significant impact on the distribution of metals around galaxies and need to be fully accounted for when analyzing correlations between gaseous haloes and galaxy properties.

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“…The one-to-one association of absorption features with log N HI < 14 with galaxies is more ambiguous (Chen et al 2005). Statistical studies show associations of galaxies and weaker absorbers to 1 Mpc or more (Morris et al 1993;Tripp et al 1998;Tejos et al 2014), consistent with the positions of galaxies within the large scale structure of the cosmic web (Prochaska et al 2011b;Burchett et al 2020;Wilde et al 2021).…”

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confidence: 82%

Identifying Circumgalactic Medium Absorption in QSO Spectra: A Bayesian Approach

Scott,

Shoemaker,

Hamill

2021

Preprint

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We present a study of candidate galaxy-absorber pairs for 43 low redshift QSO sightlines (0.06 < z < 0.85) observed with the Hubble Space Telescope/Cosmic Origins Spectrograph that lie within the footprint of the Sloan Digital Sky Survey with a statistical approach to match absorbers with galaxies near the QSO lines of sight using only the SDSS Data Release 12 photometric data for the galaxies, including estimates of their redshifts. Our Bayesian methods combine the SDSS photometric information with measured properties of the circumgalactic medium to find the most probable galaxy match, if any, for each absorber in the line of sight QSO spectrum. We find ∼630 candidate galaxyabsorber pairs using two different statistics. The methods are able to reproduce pairs reported in the targeted spectroscopic studies upon which we base the statistics at a rate of 72%. The properties of the galaxies comprising the candidate pairs have median redshift, luminosity, and stellar mass, all estimated from the photometric data, z = 0.13, L = 0.1L * , and log(M * /M ) = 9.7. The median impact parameter of the candidate pairs is ∼430 kpc, or ∼ 3.5 times the galaxy virial radius. The results are broadly consistent with the high Lyα covering fraction out to this radius found in previous studies. This method of matching absorbers and galaxies can be used to prioritize targets for spectroscopic studies, and we present specific examples of promising systems for such follow-up. INTRODUCTION

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CGM² I: The Extent of the Circumgalactic Medium Traced by Neutral Hydrogen

Cited by 47 publications

References 109 publications

Limits on non-canonical heating and turbulence in the intergalactic medium from the low redshift Lyman-alpha forest

Limits on non-canonical heating and turbulence in the intergalactic medium from the low redshift Lyman-alpha forest

Metal-enriched halo gas across galaxy overdensities over the last 10 billion years

Identifying Circumgalactic Medium Absorption in QSO Spectra: A Bayesian Approach

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CGM2 I: The Extent of the Circumgalactic Medium Traced by Neutral Hydrogen

Cited by 47 publications

References 109 publications

Limits on non-canonical heating and turbulence in the intergalactic medium from the low redshift Lyman-alpha forest

Limits on non-canonical heating and turbulence in the intergalactic medium from the low redshift Lyman-alpha forest

Metal-enriched halo gas across galaxy overdensities over the last 10 billion years

Identifying Circumgalactic Medium Absorption in QSO Spectra: A Bayesian Approach

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CGM² I: The Extent of the Circumgalactic Medium Traced by Neutral Hydrogen