The Ultraviolet Detection of Diffuse Gas in Galaxy Groups

Stocke, John T.; Keeney, Brian A.; Danforth, Charles W.; Oppenheimer, Benjamin D.; Pratt, Cameron T.; Berlind, Andreas A.; Impey, C. D.; Jannuzi, Buell T.

doi:10.3847/1538-4365/aaf73d

Cited by 18 publications

(16 citation statements)

References 78 publications

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“…This may be an indication that we are not observing a hot, volume filling IGrM; instead we are detecting cooler pockets of gas that are perhaps in pressure confinement within the IGrM. This would line up more closely with what was concluded in Stocke et al (2017); Pointon et al (2017) and Stocke et al (2019) for more massive groups. If this is indeed correct, X-ray spectroscopy of O VII and O VIII would be required to observe the hotter component of the IGrM, even for lower mass groups (10 12.8 − 10 13.7 M ).…”

Section: Discussionsupporting

confidence: 81%

“…The possibility that the O VI detections were tracing cooler clouds rather than the hot component of the IGrM was still a hypothesis and it lacked any direct observational confirmation. Other O VI studies by Pointon et al (2017) and Stocke et al (2017) compared the detections in group environments to the circumgalactic medium (CGM) of isolated galaxies. These studies found that group environments contained O VI absorption that could be modeled with broader components than isolated systems and concluded that O VI was characteristic of the boundary between cooler CGM gas and the hotter IGrM.…”

Section: Introductionmentioning

confidence: 99%

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Detection of a Multiphase Intragroup Medium: Results from the COS-IGrM Survey

McCabe,

Borthakur,

Heckman

et al. 2021

Preprint

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We present the results of the COS Intragroup Medium (COS-IGrM) Survey that used the Cosmic Origins Spectrograph on the Hubble Space Telescope to observe a sample of 18 UV bright quasars, each probing the intragroup medium (IGrM) of a galaxy group. We detect Lyα, C II, N V, Si II, Si III, and O VI in multiple sightlines. The highest ionization species detected in our data is O VI, which was detected in 8 out of 18 quasar sightlines. The wide range of ionization states observed provide evidence that the IGrM is patchy and multiphase. We find that the O VI detections generally align with radiatively cooling gas between 10 5.8 and 10 6 K. The lack of O VI detections in 10 of the 18 groups illustrates that O VI may not be the ideal tracer of the volume filling component of the IGrM. Instead, it either exists at trace levels in a hot IGrM or is generated in the boundary between the hotter IGrM and cooler gas.

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Section: Discussionsupporting

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Detection of a Multiphase Intragroup Medium: Results from the COS-IGrM Survey

McCabe,

Borthakur,

Heckman

et al. 2021

Preprint

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“…Since X-ray emission scales with the square of gas density, diffuse warm and cool phases of the IGrM are prohibitively difficult to observe directly in emission. While several groups have pioneered efforts to characterize the warm and cool IGrM/ICM with UV absorption specifically targeting group environments (Pointon et al, 2017;Nielsen et al, 2018;Stocke et al, 2019), the Virgo (Yoon et al, 2012;Manuwal et al, 2019) and Coma (Yoon & Putman, 2017) clusters, other clusters (Burchett et al, 2018;Connor et al, 2019), cluster outskirts (Muzahid et al, 2017;Pradeep et al, 2019), as well as low-mass group halos hosting ETGs (Zahedy et al, 2019), such studies are limited by the available number of background sources with existing instrument sensitivities. For this reason, simulations of groups offer a unique insight into the multiphase structure of the IGrM and the physical origins of its different components.…”

Section: The Multiphase Igrmmentioning

confidence: 99%

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

et al. 2021

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Galaxy groups are more than an intermediate scale between clusters and halos hosting individual galaxies, they are crucial laboratories capable of testing a range of astrophysics from how galaxies form and evolve to large scale structure (LSS) statistics for cosmology. Cosmological hydrodynamic simulations of groups on various scales offer an unparalleled testing ground for astrophysical theories. Widely used cosmological simulations with ∼(100 Mpc)3 volumes contain statistical samples of groups that provide important tests of galaxy evolution influenced by environmental processes. Larger volumes capable of reproducing LSS while following the redistribution of baryons by cooling and feedback are the essential tools necessary to constrain cosmological parameters. Higher resolution simulations can currently model satellite interactions, the processing of cool (T≈104−5 K) multi-phase gas, and non-thermal physics including turbulence, magnetic fields and cosmic ray transport. We review simulation results regarding the gas and stellar contents of groups, cooling flows and the relation to the central galaxy, the formation and processing of multi-phase gas, satellite interactions with the intragroup medium, and the impact of groups for cosmological parameter estimation. Cosmological simulations provide evolutionarily consistent predictions of these observationally difficult-to-define objects, and have untapped potential to accurately model their gaseous, stellar and dark matter distributions.

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“…Extended O VI distributions of this sort are seen, for example, in simulations of dwarf galaxies (Mina et al 2020). Other possible sources include dwarf galaxies with masses below 10 8 M , quiescent galaxies, galaxy groups and clusters, and the IGM (Prochaska et al 2011;Finn et al 2016;Bielby et al 2019;Burchett et al 2018;Stocke et al 2019).…”

Section: Danforth+2016 Tripp+2008mentioning

confidence: 96%

The CGM$^2$ Survey: Circumgalactic O VI from dwarf to massive star-forming galaxies

Tchernyshyov,

Werk,

Wilde

et al. 2021

Preprint

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We combine 126 new galaxy-O VI absorber pairs from the CGM 2 survey with 123 pairs drawn from the literature to examine the simultaneous dependence of the column density of O VI absorbers (N O VI ) on galaxy stellar mass, star formation rate, and impact parameter. The combined sample consists of 249 galaxy-O VI absorber pairs covering z = 0-0.6, with host galaxy stellar masses M * = 10 7.8 -10 11.2 M and galaxy-absorber impact parameters R ⊥ = 0-400 proper kiloparsecs. In this work, we focus on the variation of N O VI with galaxy mass and impact parameter among the star-forming galaxies in the sample. We find that the average N O VI within one virial radius of a star-forming galaxy is greatest for star-forming galaxies with M * = 10 9.2 -10 10 M . Star-forming galaxies with M * between 10 8 and 10 11.2 M can explain most O VI systems with column densities greater than 10 13.5 cm −2 . 60% of the O VI mass associated with a star-forming galaxy is found within one virial radius and 35% is found between one and two virial radii. In general, we find that some departure from hydrostatic equilibrium in the CGM is necessary to reproduce the observed O VI amount, galaxy mass dependence, and extent. Our measurements serve as a test set for CGM models over a broad range of host galaxy masses.

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The Ultraviolet Detection of Diffuse Gas in Galaxy Groups

Cited by 18 publications

References 78 publications

Detection of a Multiphase Intragroup Medium: Results from the COS-IGrM Survey

Detection of a Multiphase Intragroup Medium: Results from the COS-IGrM Survey

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

The CGM$^2$ Survey: Circumgalactic O VI from dwarf to massive star-forming galaxies

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