Where Are the Absorbers toward Q2302+029?

Bowen, David V.; Jiménez, Raúl; Jenkins, Edward B.

doi:10.1086/318351

Cited by 8 publications

(6 citation statements)

References 36 publications

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“… Pie diagram showing absorbers and galaxies in the LOS of PG 2302+029 (includes the additional objects from Bowen et al 2001). Description of figure as per Fig.…”

Section: Discussionmentioning

confidence: 99%

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The association between gas and galaxies – I. CFHT spectroscopy and pair analysis

Morris

Jannuzi

2006

Monthly Notices of the Royal Astronomical Society

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We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Lyα absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Lyα absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi‐object spectrograph on the Canada–France–Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption‐line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe. A correlation between absorbers and galaxies is detected out to separation of 1.5 Mpc. This correlation is weaker than the galaxy–galaxy correlation. There is also some evidence that the absorbing systems seen in C iv are more closely related to galaxies, although this correlation could be with column density rather than metallicity. The above results are all consistent with the absorbing gas and the galaxies coexisting in dark matter filaments and knots as predicted by current models where the column density of the absorbing gas is correlated with the underlying matter density.

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“… Pie diagram showing absorbers and galaxies in the LOS of PG 2302+029 (includes the additional objects from Bowen et al 2001). Description of figure as per Fig.…”

Section: Discussionmentioning

confidence: 99%

“…This LOS was surveyed by Bowen et al (2001), obtaining spectra for 24 objects. In this same field, we measured redshifts for 42 objects.…”

Section: Pg 2302+029mentioning

confidence: 99%

The association between gas and galaxies – I. CFHT spectroscopy and pair analysis

Morris

Jannuzi

2006

Monthly Notices of the Royal Astronomical Society

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“…The PG1148+549 Ne VIII absorbers have no resemblence to BAL outflows. Some quasars have been shown to have absorption systems due to QSO ejecta that are highly displaced in redshift from the QSO (e.g., Jannuzi et al 1996;Bowen et al 2001;Rodríguez Hidalgo et al 2011), but these also show distinctive characteristics (e.g., relatively broad and smooth absorption profiles) that do not match the PG1148+549 NeVIII systems.…”

Section: Redshift Density and Baryonic Contentmentioning

confidence: 99%

QSO ABSORPTION SYSTEMS DETECTED IN Ne VIII: HIGH-METALLICITY CLOUDS WITH A LARGE EFFECTIVE CROSS SECTION

Meiring

Tripp

Werk

et al. 2013

ApJ

123

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Using high resolution, high signal-to-noise ultraviolet spectra of the z em =0.9754 quasar PG1148+549 obtained with the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope, we study the physical conditions and abundances of Ne VIII+O VI absorption line systems at z abs =0.68381, 0.70152, 0.72478. In addition to Ne VIII and O VI, absorption lines from multiple ionization stages of oxygen (O II, O III, O IV) are detected and are well-aligned with the more highly ionized species. We show that these absorbers are multiphase systems including hot gas (T ≈ 10 5.7 K) that produces Ne VIII and O VI, and the gas metallicity of the cool phase ranges from Z = 0.3Z ⊙ to supersolar. The cool (≈ 10 4 K) phases have densities n H ≈ 10 −4 cm −3 and small sizes (< 4 kpc); these cool clouds are likely to expand and dissipate, and the Ne VIII may be within a transition layer between the cool gas and a surrounding, much hotter medium. The Ne VIII redshift density, dN /dz ∼ 7 +7 −3 , requires a large number of these clouds for every L > 0.1L * galaxy and a large effective absorption cross section ( 100 kpc), and indeed, we find a star forming ∼L ⋆ galaxy at the redshift of the z abs =0.72478 system, at an impact parameter of 217 kpc. Multiphase absorbers like these Ne VIII systems are likely to be an important reservoir of baryons and metals in the circumgalactic media of galaxies.

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“…It may (Tripp & Savage 2000;Shull et al 2003;Chen & Mulchaey 2009;Stocke et al 2014;Johnson et al 2015) or may not (Wakker & Savage 2009) be common in galaxy-group environments and/or intracluster gas (e.g. Bowen et al 2001).…”

Section: Introductionmentioning

confidence: 99%

The Cos-Halos Survey: Origins of the Highly Ionized Circumgalactic Medium of Star-Forming Galaxies

Werk

Prochaska

Cantalupo

et al. 2016

ApJ

208

256

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The total contribution of diffuse halo gas to the galaxy baryon budget strongly depends on its dominant ionization state. In this paper, we address the physical conditions in the highly-ionized circumgalactic medium (CGM) traced by O vi absorption lines observed in COS-Halos spectra. We analyze the observed ionic column densities, absorption-line widths and relative velocities, along with the ratios of N v/O vi for 39 fitted Voigt profile components of O VI. We compare these quantities with the predictions given by a wide range of ionization models. Photoionization models that include only extragalactic UV background radiation are ruled out; conservatively, the upper limits to N v/O vi and measurements of N OVI imply unphysically large path lengths 100 kpc. Furthermore, very broad O vi absorption (b > 40 km s −1 ) is a defining characteristic of the CGM of star-forming L * galaxies. We highlight two possible origins for the bulk of the observed O vi: (1) highly structured gas clouds photoionized primarily by local high-energy sources or (2) gas radiatively cooling on large scales behind a supersonic wind. Approximately 20% of circumgalactic O VI does not align with any low-ionization state gas within ±50 km s −1 and is found only in halos with M halo < 10 12 M . We suggest that this type of unmatched O VI absorption traces the hot corona itself at a characteristic temperature of 10 5.5 K. We discuss the implications of these very distinct physical origins for the dynamical state, gas cooling rates, and total baryonic content of L * gaseous halos.

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Where Are the Absorbers toward Q2302+029?

Cited by 8 publications

References 36 publications

The association between gas and galaxies – I. CFHT spectroscopy and pair analysis

The association between gas and galaxies – I. CFHT spectroscopy and pair analysis

QSO ABSORPTION SYSTEMS DETECTED IN Ne VIII: HIGH-METALLICITY CLOUDS WITH A LARGE EFFECTIVE CROSS SECTION

The Cos-Halos Survey: Origins of the Highly Ionized Circumgalactic Medium of Star-Forming Galaxies

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