The Relation between Galaxy ISM and Circumgalactic O vi Gas Kinematics Derived from Observations and ΛCDM Simulations

Kacprzak, Glenn G.; Vliet, Jacob R. Vander; Nielsen, Nikole M.; Muzahid, Sowgat; Pointon, Stephanie K.; Churchill, Christopher W.; Ceverino, Daniel; Arraki, Kenz S.; Klypin, Anatoly; Charlton, Jane C.; Lewis, James

doi:10.3847/1538-4357/aaf1a6

Cited by 37 publications

(57 citation statements)

References 117 publications

(166 reference statements)

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“…In order to study the distribution of CGM metallicities, we use the "Multiphase Galaxy Halos" Survey, which is comprised of our Hubble Space Telescope (HST) program (PID 13398) (Kacprzak et al 2015a(Kacprzak et al , 2019Muzahid et al 2015Muzahid et al , 2016Nielsen et al 2017;Ng et al 2019) as well as data taken from literature (Yuan et al 2002;Danforth et al 2010;Meiring et al 2011;Churchill et al 2012;Shull et al 2012;Tilton et al 2012;Fox et al 2013;Tilton & Shull 2013;Mathes et al 2014). All 29 quasars fields have HST imaging and UV spectra from the COS instrument on the HST.…”

Section: Observationsmentioning

confidence: 99%

“…The Keck Echelle Spectrograph and Imager (ESI; Sheinis et al 2002) was used to obtain spectra of 27 galaxies. The method of reduction used is presented in Kacprzak et al (2019). The slits used in the observations were 20″ by 1″, and the data were binned by two, which resulted in pixel sizes of 0 27-0 34 in the spatial direction and a spectral resolution of 22 km s −1 .…”

Section: Galaxy Spectramentioning

confidence: 99%

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Relationship between the Metallicity of the Circumgalactic Medium and Galaxy Orientation

Pointon

Kacprzak

Nielsen

et al. 2019

ApJ

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We investigate the geometric distribution of gas metallicities in the circumgalactic medium (CGM) around 47, z<0.7 galaxies from the "Multiphase Galaxy Halos" Survey. Using a combination of quasar spectra from Hubble Space Telescope (HST)/COS and from Keck/HIRES or Very Large Telescope/UVES, we measure column densities of, or determine limits on, CGM absorption lines. We then use a Markov Chain Monte Carlo approach with Cloudy to estimate the metallicity of cool (T∼10 4 K) CGM gas. We also use HST images to determine hostgalaxy inclination and quasar-galaxy azimuthal angles. Our sample spans a H Icolumn density range of 13.8 cm −2 < N log H I <19.9 cm −2. We find (1) while the metallicity distribution appears bimodal, a Hartigan dip test cannot rule out a unimodal distribution (0.4σ). (2) CGM metallicities are independent of halo mass, spanning three orders of magnitude at a fixed halo mass. (3) The CGM metallicity does not depend on the galaxy azimuthal and inclination angles regardless of H Icolumn density, impact parameter, and galaxy color. (4) The ionization parameter does not depend on azimuthal angle. We suggest that the partial Lyman limit metallicity bimodality is not driven by a spatial azimuthal bimodality. Our results are consistent with simulations where the CGM is complex and outflowing, accreting, and recycled gas are well-homogenized at z<0.7. The presence of lowmetallicity gas at all orientations suggests that cold streams of accreting filaments are not necessarily aligned with the galaxy plane at low redshifts or intergalactic transfer may dominate. Finally, our results support simulations showing that strong metal absorption can mask the presence of low-metallicity gas in integrated line-of-sight CGM metallicities.

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Section: Observationsmentioning

confidence: 99%

Section: Galaxy Spectramentioning

confidence: 99%

Relationship between the Metallicity of the Circumgalactic Medium and Galaxy Orientation

Pointon

Kacprzak

Nielsen

et al. 2019

ApJ

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“…≈50-80 km s −1 for galaxies with MUSE redshifts and ≈682 km s −1 for galaxies with only grism redshifts). As a reference point, low redshift studies (Werk et al 2016;Nielsen et al 2017;Kacprzak et al 2019) find O VI absorber-galaxy pairs, at z = 0.2, associated in velocity space within | v| 200 km s −1 .…”

Section: T H E G a L A X Y E N V I Ro N M E N T O F O Vi A B S O R B mentioning

confidence: 99%

“…Tumlinson et al 2011;Meiring et al 2013;Werk et al 2016); diffuse halo gas at the ambient halo temperature (e.g. Oppenheimer et al 2016;Werk et al 2016;Nielsen et al 2017;Oppenheimer et al 2018a;Kacprzak et al 2019); intragroup material (e.g. Stocke et al 2014Stocke et al , 2017Pointon et al 2017); or more widely spread warm-hot intergalactic medium (e.g.…”

Section: Introductionmentioning

confidence: 99%

Quasar Sightline and Galaxy Evolution (QSAGE) survey – I. The galaxy environment of O vi absorbers up to z = 1.4 around PKS 0232−04

Bielby

Stott

Cullen

et al. 2019

Monthly Notices of the Royal Astronomical Society

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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 ${\sim }50{{\ \rm per\ cent}}$ 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.

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“…At low to intermediate redshifts, metal absorbers are used as probes of CGM gas kinematics and star formation activity (Prochter et al 2006;Nielsen et al 2017;Tumlinson et al 2017). Other works further suggest a relationship between absorbers and host halo properties, such as mass (Oppenheimer et al 2016;Kacprzak et al 2019). There is also evidence of causal connection between galaxies and absorbers at very high redshifts (z > 5) with characteristics of early galaxies, such as their masses or star formation rates, showing some correlations with absorber equivalent widths or galaxy-absorber separation (Cai et al 2017;García et al 2017).…”

Section: Introductionmentioning

confidence: 86%

Evolution of neutral oxygen during the epoch of reionization and its use in estimating the neutral hydrogen fraction

Doughty

Finlator

2019

Monthly Notices of the Royal Astronomical Society

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We use synthetic sightlines drawn through snapshots of the Technicolor Dawn simulations to explore how the statistics of neutral oxygen (O i) absorbers respond to hydrogen reionization. The ionization state of the circumgalactic medium (CGM) initially roughly tracks that of the intergalactic medium, but beginning at z = 8 the CGM grows systematically more neutral owing to self-shielding. Weak absorbers trace diffuse gas that lies farther from halos, hence they are ionized first, whereas stronger systems are less sensitive to reionization. The overall O i covering fraction decreases slowly with time owing to competition between ongoing enrichment and gradual encroachment of ionization fronts into increasingly overdense gas. While the declining covering fraction is partially offset by continued formation of new halos, the ionization of the diffuse gas causes the predicted line-of-sight incidence rate of O i absorbers to decline abruptly at the overlap epoch, in qualitative agreement with observations. In comparison to the recently-observed equivalent width (EW) distribution at z ≈ 6, the simulations underproduce systems with EW ≥ 0.1Å, although they reproduce weaker systems with EW ≥ 0.05Å. By z ≈ 5, the incidence of EW < 0.1Å systems are overproduced, consistent with previous indications that the simulated ionizing background is too weak at z < 6. The summed column densities of Si ii and Si iv trace the total oxygen column, and hence the ratio of the O i and Si ii + Si iv comoving mass densities traces the progress of reionization. This probe may prove particularly useful in the regime where x H i > 10%.

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The Relation between Galaxy ISM and Circumgalactic O vi Gas Kinematics Derived from Observations and ΛCDM Simulations

Cited by 37 publications

References 117 publications

Relationship between the Metallicity of the Circumgalactic Medium and Galaxy Orientation

Relationship between the Metallicity of the Circumgalactic Medium and Galaxy Orientation

Quasar Sightline and Galaxy Evolution (QSAGE) survey – I. The galaxy environment of O vi absorbers up to z = 1.4 around PKS 0232−04

Evolution of neutral oxygen during the epoch of reionization and its use in estimating the neutral hydrogen fraction

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