On the possible environmental effect in distributing heavy elements beyond individual gaseous haloes

Johnson, Sean D.; Chen, Hsiao‐Wen; Mulchaey, John S.

doi:10.1093/mnras/stv553

Cited by 161 publications

(257 citation statements)

References 61 publications

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“…Liang & Chen (2014) have estimated this drop to be at d/Rvir ≈ 0.7 for Si II, Si III Si IV, C II and C IV. A similar drop of the C IV column densities was reported by Bordoloi et al (2014) at d/R200m ≈ 0.5, and for O VI by Johnson et al (2015) at d/Rvir ≈ 1.…”

Section: Comparison Of the Column Density Profiles In Simulations Andsupporting

confidence: 85%

“…Some studies adopt rest frame equivalent width of W0 = 0.05 − 0.1Å and log N0 = 13.5 cm −2 as detection thresholds (Liang & Chen 2014;Johnson et al 2015). We adopt these values here for comparison with the derived covering fraction of data from Liang & Chen (2014) and Johnson et al (2015) for O VI. For observations where only equivalent width measurements are available, Liang & Chen (2014) adopted the threshold Wr = 0.05Å.…”

Section: Comparing the Cgm Covering Fractionsmentioning

confidence: 99%

“…The Cosmic Origins Spectrograph (COS; Green et al 2012) on board the Hubble Space Telescope (HST) has offered a unique opportunity to systematically probe low-redshift (z ≈ 0) galactic halos in the UV regime. Commonly observed absorption lines arising in the CGM are the Lyα λ1215, Si II λ1260, Si III λ1206, C II λ1334, C IV λλ1548, 1550 (e.g., Chen 2012;Borthakur et al 2013;Liang & Chen 2014;Bordoloi et al 2014), and O VI λλ1031, 1036 (e.g., Prochaska et al 2011;Tumlinson et al 2011;Johnson et al 2015). In the intermediate redshift range, many researchers have probed the gaseous halos using optical ground-based facilities via Mg II Gauthier et al 2010;Bordoloi et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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Column density profiles of multiphase gaseous haloes

Liang

Kravtsov

Agertz

2016

Mon. Not. R. Astron. Soc.

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We analyze circumgalactic medium (CGM) in a suite of high-resolution cosmological resimulations of a Milky-Way size galaxy and show that CGM properties are quite sensitive to details of star formation-feedback loop modelling. The simulation that produces a realistic late-type galaxy, fails to reproduce existing observations of the CGM. In contrast, simulation that does not produce a realistic galaxy has the predicted CGM in better agreement with observations. This illustrates that properties of galaxies and properties of their CGM provide strong complementary constraints on the processes governing galaxy formation. Our simulations predict that column density profiles of ions are well described by an exponential function of projected distance d: N ∝ e −d/hs . Simulations thus indicate that the sharp drop in absorber detections at larger distances in observations does not correspond to a "boundary" of an ion, but reflects the underlying steep exponential column density profile. Furthermore, we find that ionization energy of ions is tightly correlated with the scale height h s : h s ∝ E 0.74 ion . At z ≈ 0, warm gas traced by low-ionization species (e.g., Mg II and C IV) has h s ≈ 0.03 − 0.07R vir , while higher ionization species (O VI and Ne VIII) have h s ≈ 0.32 − 0.45R vir . Finally, the scale heights of ions in our simulations evolve slower than the virial radius for z 2, but similarly to the halo scale radius, r s . Thus, we suggest that the column density profiles of galaxies at different redshifts should be scaled by r s rather than the halo virial radius.

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Section: Comparison Of the Column Density Profiles In Simulations Andsupporting

confidence: 85%

Section: Comparing the Cgm Covering Fractionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Column density profiles of multiphase gaseous haloes

Liang

Kravtsov

Agertz

2016

Mon. Not. R. Astron. Soc.

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“…Kacprzak et al (2015) found that the equivalent width decreases as the distance of the absorber from the galaxy increases for the isolated sample. Similarly, Tumlinson et al (2011) and Johnson et al (2015) found that the column density decreases as the ratio of the impact parameter and the virial radius increases. We investigate this trend in group Prochaska et al (2011), (2) galaxies by showing the equivalent width as a function of the impact parameter in Figure 3.…”

Section: Modelingmentioning

confidence: 80%

The Impact of the Group Environment on the O vi Circumgalactic Medium

Pointon

Nielsen

Kacprzak

et al. 2017

ApJ

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We present a study comparing O VI λλ1031, 1037 doublet absorption found towards group galaxy environments with that of isolated galaxies. The O VI absorption in the circumgalactic medium (CGM) of isolated galaxies has been studied previously by the "Multiphase Galaxy Halos" survey, where the kinematics and absorption properties of the CGM have been investigated. We extend these studies to group environments. We define a galaxy group to have two or more galaxies having a line-of-sight velocity difference of no more than 1000 km s −1 and located within 350 kpc (projected) of a background quasar sightline. We identified a total of six galaxy groups associated with O VI absorption W r > 0.06 Å that have a median redshift of z gal = 0.1669 and a median impact parameter of D = 134.1 kpc. An additional 12 non-absorbing groups were identified with a median redshift of z gal = 0.2690 and a median impact parameter of D = 274.0 kpc. We find the average equivalent width to be smaller for group galaxies than for isolated galaxies (3σ). However, the covering fractions are consistent with both samples. We used the pixel-velocity two-point correlation function method and find that the velocity spread of O VI in the CGM of group galaxies is significantly narrower than that of isolated galaxies (10σ). We suggest that the warm/hot CGM does not exist as a superposition of halos, instead, the virial temperature of the halo is hot enough for O VI to be further ionised. The remaining O VI likely exists at the interface between hot, diffuse gas and cooler regions of the CGM.

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“…This phenomenon suggests a deeper, underlying causal relationship between group galaxies and the larger dark matter halos in which they reside. While the question naturally arises whether environmental effects manifest in the CGM, research on the matter (Tejos et al 2012;Yoon & Putman 2013;Johnson et al 2014Johnson et al , 2015Wakker et al 2015;Finn et al 2016) is in its infancy.…”

Section: Introductionmentioning

confidence: 99%

A DEEP SEARCH FOR FAINT GALAXIES ASSOCIATED WITH VERY LOW REDSHIFT C iv ABSORBERS. III. THE MASS- AND ENVIRONMENT-DEPENDENT CIRCUMGALACTIC MEDIUM

Burchett

Tripp

Bordoloi

et al. 2016

ApJ

108

170

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Using Hubble Space Telescope Cosmic Origins Spectrograph observations of 89 QSO sightlines through the Sloan Digital Sky Survey footprint, we study the relationships between C iv absorption systems and the properties of nearby galaxies as well as large-scale environment. To maintain sensitivity to very faint galaxies, we restrict our sample to 0.0015 < z < 0.015, which defines a complete galaxy survey to L 0.01 L * or stellar mass M * 10 8 M . We report two principal findings. First, for galaxies with impact parameter ρ < 1 r vir , C iv detection strongly depends on the luminosity/stellar mass of the nearby galaxy. C iv is preferentially associated with galaxies with M * > 10 9.5 M ; lower mass galaxies rarely exhibit significant C iv absorption (covering fraction f C = 9 +12 −6 % for 11 galaxies with M * < 10 9.5 M ). Second, C iv detection within the M * > 10 9.5 M population depends on environment. Using a fixed-aperture environmental density metric for galaxies with ρ < 160 kpc at z < 0.055, we find that 57 +12 −13 % (8/14) of galaxies in low-density regions (regions with fewer than seven L > 0.15 L * galaxies within 1.5 Mpc) have affiliated C iv absorption; however, none (0/7) of the galaxies in denser regions show C iv. Similarly, the C iv detection rate is lower for galaxies residing in groups with dark-matter halo masses of M halo > 10 12.5 M . In contrast to C iv, H i is pervasive in the CGM without regard to mass or environment. These results indicate that C iv absorbers with log N (C iv) 13.5 cm −2 trace the halos of M * > 10 9.5 M galaxies but also reflect larger scale environmental conditions.

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On the possible environmental effect in distributing heavy elements beyond individual gaseous haloes

Cited by 161 publications

References 61 publications

Column density profiles of multiphase gaseous haloes

Column density profiles of multiphase gaseous haloes

The Impact of the Group Environment on the O vi Circumgalactic Medium

A DEEP SEARCH FOR FAINT GALAXIES ASSOCIATED WITH VERY LOW REDSHIFT C iv ABSORBERS. III. THE MASS- AND ENVIRONMENT-DEPENDENT CIRCUMGALACTIC MEDIUM

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