THE GAS–GALAXY CONNECTION AT<i>z</i><sub>abs</sub>= 0.35: O VI AND H I ABSORPTION TOWARD J 0943+0531

Thom, Christopher; Werk, Jessica K.; Tumlinson, Jason; Prochaska, J. Xavier; Meiring, Joseph D.; Tripp, Todd M.; Sembach, Kenneth R.

doi:10.1088/0004-637x/736/1/1

Cited by 50 publications

(55 citation statements)

References 85 publications

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“…Early results from these programs can be found in Thom et al (2011), Tumlinson et al (2011a, and Tumlinson et al (2011b). The names and basic properties of these absorbers are presented in Table 1.…”

Section: Program Summary and Observationsmentioning

confidence: 99%

THE FIRST OBSERVATIONS OF LOW-REDSHIFT DAMPED Lyα SYSTEMS WITH THE COSMIC ORIGINS SPECTROGRAPH: CHEMICAL ABUNDANCES AND AFFILIATED GALAXIES

Battisti

Meiring

Tripp

et al. 2011

ApJ

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We present Cosmic Origins Spectrograph (COS) measurements of metal abundances in eight 0.083 < z abs < 0.321 damped Lyα (DLA) and sub-DLA absorption systems serendipitously discovered in the COS-Halos survey. We find that these systems show a large range in metallicities, with −1.10 < [Z/H] < 0.31, similar to the spread found at higher redshifts. These low-redshift systems on average have subsolar metallicities, but do show a rise in metallicity over cosmic time when compared to higher-redshift systems. We find that the average sub-DLA metallicity is higher than the average DLA metallicity at all redshifts. Nitrogen is underabundant with respect to α-group elements in all but perhaps one of the absorbers. In some cases, [N/α] is significantly below the lowest nitrogen measurements in nearby galaxies. Systems for which depletion patterns can be studied show little, if any, depletion, which is characteristic of Milky Way halo-type gas. We also identify affiliated galaxies for three of the sub-DLAs using spectra obtained from a Keck/Low Resolution Imaging Spectrometer (LRIS). None of these sub-DLAs arise in the stellar disks of luminous galaxies; instead, these absorbers may exist in galaxy halos at impact parameters ranging from 38 to 92 kpc. Multiple galaxies are present near two of the sub-DLAs, and galaxy interactions may play a role in the dispersal of the gas. Many of these low-redshift absorbers exhibit simple kinematics, but one sub-DLA has a complicated mix of at least 13 components spread over 150 km s −1 . We find three galaxies near this sub-DLA, which also suggests that galaxy interactions roil the gas. This study reinforces the view that DLAs have a variety of origins, and low-redshift studies are crucial for understanding absorber-galaxy connections.

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Section: Program Summary and Observationsmentioning

confidence: 99%

THE FIRST OBSERVATIONS OF LOW-REDSHIFT DAMPED Lyα SYSTEMS WITH THE COSMIC ORIGINS SPECTROGRAPH: CHEMICAL ABUNDANCES AND AFFILIATED GALAXIES

Battisti

Meiring

Tripp

et al. 2011

ApJ

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“…However, even when a hot isotropic atmosphere is present around a galaxy, some residual cold accretion can exist, in particular for massive halos at high redshifts (e.g. Thom et al 2011;Ribaudo et al 2011). The recent works of Nelson et al 2013, based on a new generation of hydrodynamic codes, call into question this bimodal accretion scenario.…”

Section: Introductionmentioning

confidence: 99%

“…Observations (e.g. Thom et al 2011;Ribaudo et al 2011;Crighton et al 2013) and simulations (e.g. Fumagalli et al 2011) indicate that the two accretion modes are associated with different metallicity contents.…”

Section: Introductionmentioning

confidence: 99%

Metal enrichment in a semi-analytical model, fundamental scaling relations, and the case of Milky Way galaxies

Cousin

Buat

Boissier

et al. 2016

A&A

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Context. Gas flows play a fundamental role in galaxy formation and evolution, providing the fuel for the star formation process. These mechanisms leave an imprint in the amount of heavy elements that enrich the interstellar medium. Thus, the analysis of this metallicity signature provides additional constraint on the galaxy formation scenario. Aims. We aim to discriminate between four different galaxy formation models based on two accretion scenarios and two different star formation recipes. We address the impact of a bimodal accretion scenario and a strongly regulated star formation recipe on the metal enrichment process of galaxies. Methods. We present a new extension of the eGalICS model, which allows us to track the metal enrichment process in both stellar populations and in the gas phase. Based on stellar metallicity bins from 0 to 2.5 Z , our new chemodynamical model is applicable for situations ranging from metal-free primordial accretion to very enriched interstellar gas contents. We use this new tool to predict the metallicity evolution of both the stellar populations and gas phase. We compare these predictions with recent observational measurements. We also address the evolution of the gas metallicity with the star formation rate (SFR). We then focus on a subsample of Milky Way-like galaxies. We compare both the cosmic stellar mass assembly and the metal enrichment process of such galaxies with observations and detailed chemical evolution models. Results. Our models, based on a strong star formation regulation, allow us to reproduce well the stellar mass to gas-phase metallicity relation observed in the local Universe. The shape of our average stellar mass to stellar metallicity relations is in good agreement with observations. However, we observe a systematic shift towards high masses. Our M −Z g −SFR relation is in good agreement with recent measurements: our best model predicts a clear dependence with the SFR. Both SFR and metal enrichment histories of our Milky Way-like galaxies are consistent with observational measurements and detailed chemical evolution models. We finally show that Milky Way progenitors start their evolution below the observed main sequence and progressively reach this observed relation at z 0.

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“…The mass of this halo is comparable to the gas mass of the galaxy itself (i.e., the ISM; Thom et al 2011;Tumlinson et al 2011;Werk et al 2013) and hence plays an important role in the evolution of galaxies. Models of the CGM indicate that gas can flow in and out of this reservoir, which in turn controls the star formation rate of the galaxy and the metallicity of stars formed from this gas (Oppenheimer & Davé 2008;Lilly et al 2013;Kacprzak et al 2016).…”

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confidence: 99%

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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THE GAS–GALAXY CONNECTION ATz_abs= 0.35: O VI AND H I ABSORPTION TOWARD J 0943+0531

Cited by 50 publications

References 85 publications

THE FIRST OBSERVATIONS OF LOW-REDSHIFT DAMPED Lyα SYSTEMS WITH THE COSMIC ORIGINS SPECTROGRAPH: CHEMICAL ABUNDANCES AND AFFILIATED GALAXIES

THE FIRST OBSERVATIONS OF LOW-REDSHIFT DAMPED Lyα SYSTEMS WITH THE COSMIC ORIGINS SPECTROGRAPH: CHEMICAL ABUNDANCES AND AFFILIATED GALAXIES

Metal enrichment in a semi-analytical model, fundamental scaling relations, and the case of Milky Way galaxies

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

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THE GAS–GALAXY CONNECTION ATzabs= 0.35: O VI AND H I ABSORPTION TOWARD J 0943+0531

Cited by 50 publications

References 85 publications

THE FIRST OBSERVATIONS OF LOW-REDSHIFT DAMPED Lyα SYSTEMS WITH THE COSMIC ORIGINS SPECTROGRAPH: CHEMICAL ABUNDANCES AND AFFILIATED GALAXIES

THE FIRST OBSERVATIONS OF LOW-REDSHIFT DAMPED Lyα SYSTEMS WITH THE COSMIC ORIGINS SPECTROGRAPH: CHEMICAL ABUNDANCES AND AFFILIATED GALAXIES

Metal enrichment in a semi-analytical model, fundamental scaling relations, and the case of Milky Way galaxies

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

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Product

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THE GAS–GALAXY CONNECTION ATz_abs= 0.35: O VI AND H I ABSORPTION TOWARD J 0943+0531