The relation between Ly<i>α</i>absorbers and local galaxy filaments

Bouma, Sietske; Richter, Philipp; Wendt, Martin

doi:10.1051/0004-6361/202039786

Cited by 12 publications

(8 citation statements)

References 54 publications

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“…A stacking approach has also recently been successfully applied to ROSAT X-ray data (Tanimura et al 2020b). Finally, by exploiting lines-of-sight to quasars that pass through the axes between known cluster pairs, possible Lyman-alpha absorption from filamentary gas has been reported (e.g., Tejos et al 2016;Pessa et al 2018;Bouma et al 2021).…”

Section: Introductionmentioning

confidence: 99%

A high-resolution view of the filament of gas between Abell 399 and Abell 401 from the Atacama Cosmology Telescope and MUSTANG-2

Hincks,

Radiconi,

Romero

et al. 2021

Preprint

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We report a significant detection of the hot intergalactic medium in the filamentary bridge connecting the galaxy clusters Abell 399 and Abell 401. This result is enabled by a low-noise, high-resolution map of the thermal Sunyaev-Zeldovich signal from the Atacama Cosmology Telescope (ACT) and Planck satellite. The ACT data provide the 1.65 resolution that allows us to clearly separate the profiles of the clusters, whose centres are separated by 37 , from the gas associated with the filament. A model that fits for only the two clusters is ruled out compared to one that includes a bridge component at > 5 σ. Using a gas temperature determined from Suzaku X-ray data, we infer a total mass of (3.3 ± 0.7) × 10 14 M associated with the filament, comprising about 8% of the entire Abell 399-Abell 401 system. We fit two phenomenological models to the filamentary structure; the favoured model has a width transverse to the axis joining the clusters of ∼1.9 Mpc. When combined with the Suzaku data, we find a gas density of (0.88 ± 0.24) × 10 −4 cm −3 , considerably lower than previously reported. We show that this can be fully explained by a geometry in which the axis joining Abell 399 and Abell 401 has a large component along the line of sight, such that the distance between the clusters is significantly greater than the 3.2 Mpc projected separation on the plane of the sky. Finally, we present initial results from higher resolution (12.7 effective) imaging of the bridge with the MUSTANG-2 receiver on the Green Bank Telescope.

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Section: Introductionmentioning

confidence: 99%

A high-resolution view of the filament of gas between Abell 399 and Abell 401 from the Atacama Cosmology Telescope and MUSTANG-2

Hincks,

Radiconi,

Romero

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…A final technique is to search for absorption lines in the spectra of quasars caused by intervening WHIM, and recent possible detections have been made with O VI , O VII , O VIII , and H I absorption (e.g. Tejos et al 2016 ;Nicastro et al 2018 ;Pessa et al 2018 ;Ne v alainen et al 2019 ;Bouma, Richter & Wendt 2021 ).…”

mentioning

confidence: 99%

A high-resolution view of the filament of gas between Abell 399 and Abell 401 from the Atacama Cosmology Telescope and MUSTANG-2

Hincks

Radiconi

Romero

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We report a significant detection of the hot intergalactic medium in the filamentary bridge connecting the galaxy clusters Abell 399 and Abell 401. This result is enabled by a low-noise, high-resolution map of the thermal Sunyaev-Zeldovich signal from the Atacama Cosmology Telescope (ACT) and Planck satellite. The ACT data provide the 1.65′ resolution that allows us to clearly separate the profiles of the clusters, whose centres are separated by 37′, from the gas associated with the filament. A model that fits for only the two clusters is ruled out compared to one that includes a bridge component at >5σ. Using a gas temperature determined from Suzaku X-ray data, we infer a total mass of (3.3 ± 0.7) × 1014 M⊙ associated with the filament, comprising about $8{{\ \rm per\ cent}}$ of the entire Abell 399–Abell 401 system. We fit two phenomenological models to the filamentary structure; the favoured model has a width transverse to the axis joining the clusters of ∼1.9 Mpc. When combined with the Suzaku data, we find a gas density of (0.88 ± 0.24) × 10−4 cm−3, considerably lower than previously reported. We show that this can be fully explained by a geometry in which the axis joining Abell 399 and Abell 401 has a large component along the line of sight, such that the distance between the clusters is significantly greater than the 3.2 Mpc projected separation on the plane of the sky. Finally, we present initial results from higher resolution (12.7″ effective) imaging of the bridge with the MUSTANG-2 receiver on the Green Bank Telescope.

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“…The presence of H I absorption beyond the virial radius is now widely accepted for a range of galaxy stellar masses (e.g. Prochaska et al 2011;Tejos et al 2012Tejos et al , 2014Wilde et al 2021;Bouma et al 2021;Borthakur 2022). In Wilde et al (2021) (Paper I) we found an empirical relation between galaxy stellar mass and the extent of the CGM as indicated by H I covering fractions.…”

Section: Introductionmentioning

confidence: 73%

CGM$^2$ $+$ CASBaH: The Mass Dependence of H~I Ly$α$-Galaxy Clustering and the Extent of the CGM

Wilde¹,

Miville-Deschênes²,

Werk³

et al. 2023

Preprint

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We combine datasets from the CGM 2 and CASBaH surveys to model a transition point, R cross , between circumgalactic and intergalactic media (CGM and IGM, respectively). In total, our data consist of 7244 galaxies at z < 0.5 with precisely measured spectroscopic redshifts, all having impact parameters of 0.01 − 20 comoving Mpc from 28 QSO sightlines with high-resolution UV spectra that cover H I Lyα. Our best-fitting model is an exclusionary two-component model that combines a 3D absorber-galaxy cross correlation function with a simple Gaussian profile at inner radii to represent the CGM. By design, this model gives rise to a determination of R cross as a function of galaxy stellar mass, which can be interpreted as the boundary between the CGM and IGM. For galaxies with 10 8 ≤ M /M ≤ 10 10.5 , we find that R cross (M ) ≈ 2 ± 0.6R vir . Additionally, we find excellent agreement between R cross (M ) and the theoretically-determined splashback radius for galaxies in this mass range. Overall, our results favor models of galaxy evolution at z < 0.5 that distribute T ≈ 10 4 K gas to distances beyond the virial radius.

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The relation between Lyαabsorbers and local galaxy filaments

Cited by 12 publications

References 54 publications

A high-resolution view of the filament of gas between Abell 399 and Abell 401 from the Atacama Cosmology Telescope and MUSTANG-2

A high-resolution view of the filament of gas between Abell 399 and Abell 401 from the Atacama Cosmology Telescope and MUSTANG-2

A high-resolution view of the filament of gas between Abell 399 and Abell 401 from the Atacama Cosmology Telescope and MUSTANG-2

CGM$^2$ $+$ CASBaH: The Mass Dependence of H~I Ly$α$-Galaxy Clustering and the Extent of the CGM

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