C IV absorbers tracing cool gas in dense galaxy group/cluster environments

Manuwal, Aditya; Narayanan, A.; Muzahid, Sowgat; Charlton, Jane C.; Khaire, Vikram; Chand, Hum

doi:10.1093/mnras/stz195

Cited by 18 publications

(13 citation statements)

References 110 publications

(136 reference statements)

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“…11, and the remaining at 1 Mpc. The presence of several galaxies within narrow projected positions and radial velocities indicates that the lines of sight are probing different regions of a galaxy overdensity such as a group or a cluster, with the absorption possibly arising in the CGM or the intragroup/cluster medium, consistent with what has been found for optically thick gas (Muzahid et al 2017;Manuwal et al 2019;Pradeep et al 2019;Chen et al 2020).…”

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

confidence: 78%

Pair lines of sight observations of multiphase gas bearing O vi in a galaxy environment

Anshul

Narayanan

Muzahid

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Using HST/COS spectra of the twin quasar lines of sight Q 0107 − 025A & Q 0107 − 025B, we report on the physical properties, chemical abundances and transverse sizes of a multiphase medium in a galaxy field at z = 0.399. The angular separation between the quasars corresponds to a physical separation of 520 kpc at the absorber redshift. The absorber towards Q 0107 − 025B is a partial Lyman limit system with $\log N({{\rm H~}{\rm \small I}})/{\rm cm^{-2}}\approx 16.8$. The H i column density in the absorber along the other sightline is ≈2 orders of magnitude lower. The O vi along both sightlines have comparable column densities and broad b-values (b > 30 km s−1) whereas the low ionization lines are considerably narrower. The low ionization gas is inconsistent with the O vi when modelled assuming photoionization from the same phase. In both lines-of-sight, O vi and the broad H i coinciding, are best explained through collisional ionization in a cooling plasma with solar metallicity. Ionization models infer 1/10-th solar metallicity for the pLLS and solar metallicity for the lower column density absorber along the other sightline. Within ± 250 km s−1 and 2 Mpc of projected distance from the sightlines 12 galaxies are identified, of which 5 are within 500 kpc. The twin sightlines are at normalized impact parameters of ρ ∼ 1.1Rvir, and ρ ∼ 0.8Rvir from a M* ∼ 1010.7 M⊙, L ∼ 0.07L*, and SFR <0.1 M⊙ yr−1 galaxy, potentially probing its CGM. The next closest in normalized separation are a dwarf galaxy with M* ∼ 108.7 M⊙, and SFR ∼0.06 M⊙ yr−1, and an intermediate mass galaxy with M* ∼ 1010.0 M⊙, and SFR ∼3 M⊙ yr−1. Along both sightlines, O vi could be either tracing narrow transition temperature zones at the interface of low ionization gas and the hot halo of nearest galaxy, or a more spread-out warm component that could be gas bound to the circumgalactic halo or the intragroup medium. The latter scenarios leads to a warm gas mass limit of M ≳ 4.5 × 109 M⊙.

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

confidence: 78%

Pair lines of sight observations of multiphase gas bearing O vi in a galaxy environment

Anshul

Narayanan

Muzahid

et al. 2021

Monthly Notices of the Royal Astronomical Society

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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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“…Similar examples of H I absorbers tracing cooler intracluster gas were also presented by Burchett et al (2018), which they interpreted as gas infall from the cosmic web. On the other hand, Manuwal et al (2019) interpreted the presence of cool supersolar metallicity gas in the outskirts of Virgo cluster as possibly interstellar gas displaced from galaxies through outflows or tidal interactions.…”

Section: Introductionmentioning

confidence: 99%

Detection of metal-rich, cool-warm gas in the outskirts of galaxy clusters

Pradeep

Narayanan

Muzahid

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present an ultraviolet quasar absorption line analysis of metal lines associated with three strong intervening H I absorbers (with N(H I) > 10 16.5 cm −2 ) detected in the outskirts of Sunyaev-Zel'dovich (SZ) effect-selected galaxy clusters (z cl ∼ 0.4 − 0.5), within clustocentric impact parameters of ρ cl ∼ (1.6 − 4.7)r 500 . Discovered in a recent set of targeted far-UV HST/COS spectroscopic observations, these absorbers have the highest H I column densities ever observed in the outskirts of galaxy clusters, and are also rich in metal absorption lines. Photoionization models yield single phase solutions for the three absorbers with gas densities of n H ∼ 10 −3 − 10 −4 cm −3 and metallicities of [X/H] > -1.0 (from one-tenth solar to near-solar). The widths of detected absorption lines suggest gas temperatures of T ∼ 10 4 K. The inferred densities (temperatures) are significantly higher (lower) compared to the X-ray emitting intracluster medium in cluster cores. The absorbers are tracing a cool phase of the intracluster gas in the cluster outskirts, either associated with gas stripped from cluster galaxies via outflows, tidal streams or ram-pressure forces, or denser regions within the intracluster medium that were uniformly chemically enriched from an earlier epoch of enhanced supernova and AGN feedback.

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C IV absorbers tracing cool gas in dense galaxy group/cluster environments

Cited by 18 publications

References 110 publications

Pair lines of sight observations of multiphase gas bearing O vi in a galaxy environment

Pair lines of sight observations of multiphase gas bearing O vi in a galaxy environment

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

Detection of metal-rich, cool-warm gas in the outskirts of galaxy clusters

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