Lyα Absorbers and the Coma Cluster

Yoon, Joo Heon; Putman, Mary E.

doi:10.3847/1538-4357/aa697b

Cited by 37 publications

(41 citation statements)

References 56 publications

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“…This assertion, however, runs contrary to observations of the hot intracluster medium in galaxy clusters (Mitchell et al 1976) and theoretical work which predicts a predominantly virialized gas (Voit 2005;Dekel & Birnboim 2006;Kravtsov & Borgani 2012). And, indeed, the few studies that have examined the cool CGM of galaxy clusters support a suppressed incidence of such gas both within the halo and within the halos of the cluster members (Burchett et al 2018;Yoon & Putman 2017), but see also Lopez et al (2008). These results, while still sparse, suggest a rapid decline in the cool CGM in the most massive halos.…”

Section: Introductionmentioning

confidence: 81%

Extreme Circumgalactic H i and C iii Absorption around the Most Massive, Quenched Galaxies

Smailagic

Prochaska

Burchett

et al. 2018

ApJ

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Luminous red galaxies (LRGs) are the most massive galaxies at z ∼ 0.5 and, by selection, have negligible star formation. These objects have halo masses between those of L * galaxies, whose circumgalactic media (CGM) are observed to have large masses of cold gas, and clusters of galaxies, which primarily contain hot gas. Here we report detections of strong and extended metal (C III 977) and H I lines in the CGM of two LRGs. The C III lines have equivalent widths of ∼ 1.8Å and ∼ 1.2Å, and velocity spreads of ∼ 796 km s −1 and ∼ 1245 km s −1 , exceeding all such measurements from local ∼ L * galaxies (maximal C III equivalent widths ∼ 1Å). The data demonstrate that a subset of halos hosting very massive, quenched galaxies contain significant complexes of cold gas. Possible scenarios to explain our observations include that the LRGs CGM originate from past activity (e.g., star formation or active galactic nuclei driven outflows) or from the CGM of galaxies in overlapping subhalos. We favor the latter scenario, in which the properties of the CGM are more tightly linked to the underlying dark matter halo than properties of the targeted galaxies (e.g., star formation).

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Section: Introductionmentioning

confidence: 81%

Extreme Circumgalactic H i and C iii Absorption around the Most Massive, Quenched Galaxies

Smailagic

Prochaska

Burchett

et al. 2018

ApJ

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“…Such a diffusion coefficient has a break at a rigidity of ∼ 300 GV, as a result of the transition between selfgenerated waves, with a steep spectrum, at lower rigidities, and a Kolmogorov turbulence spectrum at higher rigidities. This kind of rigidity dependence of the diffusion coefficient is exactly what is needed to explain the hardening observed in the spectra of virtually all elements in CRs (Ahn et al 2010;Adriani et al 2011;Aguilar et al 2015a,b;Yoon et al 2017) . The recent finding (Aguilar et al 2018a) that such hardening is more pronounced for secondary CRs than for primaries strongly supports the idea that it originates from a change in the particle transport regime, rather than from some peculiarity of the acceleration process.…”

Section: Discussionmentioning

confidence: 90%

Effects of re-acceleration and source grammage on secondary cosmic rays spectra

Bresci

Amato

Blasi

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The ratio between secondary and primary cosmic ray particles is the main source of information about cosmic ray propagation in the Galaxy. Primary cosmic rays are thought to be accelerated mainly in Supernova Remnant (SNR) shocks and then released in the interstellar medium (ISM). Here they produce secondary particles by occasional collisions with interstellar matter. As a result, the ratio between the fluxes of secondary and primary particles carries information about the amount of matter cosmic rays have encountered during their journey from their sources to Earth. Recent measurements by AMS-02 revealed an unexpected behaviour of two main secondaryto-primary ratios, the Boron-to-Carbon ratio and the anti-proton-to-proton ratio. In this work we discuss how such anomalies may reflect the action of two phenomena that are usually overlooked, namely the fact that some fraction of secondary particles can be produced within the acceleration region, and the non-negligible probability that secondary particles encounter an accelerator (and are reaccelerated) during propagation. Both effects must be taken into account in order to correctly extract information about CR transport from secondary-to-primary ratios.

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“…If we assume the cooler gas covering fraction is similar to that of the intracluster medium of Abell 133, we would expect it to be between that seen for the Virgo cluster (which is approximately half the mass of Abell 133) and the Coma cluster (approximately three times the mass of Abell 133). Inside the virial radius, Yoon & Putman (2017) report covering fractions for log(N H I /cm −2 ) ≥ 13.8 absorbers is 0.25 +0.24 −0.13 and 0.09 +0.13 −0.05 for Coma and Virgo, respectively.…”

Section: Nonuniform Distribution Of Warm Gasmentioning

confidence: 99%

COS Observations of the Cosmic Web: A Search for the Cooler Components of a Hot, X-Ray Identified Filament

Connor

Zahedy

Chen

et al. 2019

ApJL

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In the local universe, a large fraction of the baryon content is believed to exist as diffuse gas in filaments. While this gas is directly observable in X-ray emission around clusters of galaxies, it is primarily studied through its UV absorption. Recently, X-ray observations of large-scale filaments connecting to the cosmic web around the nearby (z = 0.05584) cluster Abell 133 were reported. One of these filaments is intersected by the sightline to quasar [VV98] J010250.2−220929, allowing for a first-ever census of cold, cool, and warm gas in a filament of the cosmic web where hot gas has been seen in X-ray emission. Here, we present UV observations with the Cosmic Origins Spectrograph and optical observations with the Magellan Echellette spectrograph of [VV98] J010250.2−220929. We find no evidence of cold, cool, or warm gas associated with the filament. In particular, we set a 2σ upper limit on Lyα absorption of log(N H I /cm −2 ) < 13.7, assuming a Doppler parameter of b = 20 km s −1 . As this sightline is ∼1100 pkpc (0.7R vir ) from the center of Abell 133, we suggest that all gas in the filament is hot at this location, or that any warm, cool, or cold components are small and clumpy. A broader census of this system -combining more UV sightlines, deeper X-ray observations, and a larger redshift catalog of cluster members -is needed to better understand the roles of filaments around clusters.Unified Astronomy Thesaurus concepts: Intergalactic medium (813); Cosmic web (330); Warm-hot intergalactic medium (1786); Intergalactic medium phases (814); Cool intergalactic medium (303); Hot intergalactic medium (751); Intracluster medium (858); Galaxy clusters (584); Ultraviolet astronomy (1786); Quasar absorption line spectroscopy (1317)

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Lyα Absorbers and the Coma Cluster

Cited by 37 publications

References 56 publications

Extreme Circumgalactic H i and C iii Absorption around the Most Massive, Quenched Galaxies

Extreme Circumgalactic H i and C iii Absorption around the Most Massive, Quenched Galaxies

Effects of re-acceleration and source grammage on secondary cosmic rays spectra

COS Observations of the Cosmic Web: A Search for the Cooler Components of a Hot, X-Ray Identified Filament

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