Hot Extended Galaxy Halos Around Local L* Galaxies From Sunyaev-Zeldovich Measurements

Bregman, Joel N.; Hodges-Kluck, Edmund; Qu, Zhijie; Pratt, Cameron; Li, Jiang-Tao; Yun, Yansong

doi:10.48550/arxiv.2107.14281

Cited by 7 publications

(8 citation statements)

References 66 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Another observational constraint on the hot gas is the Sunyaev-Zel'dovich (S-Z) effect (Sunyaev & Zeldovich 1970). However, current observations (Planck Collaboration et al 2013;Schaan et al 2020) are limited to halos more massive than M halo ∼ 10 12.5 M , and/or exclude the central regions (Bregman et al 2021). Thus, these results are not yet able to probe the disk-halo interface of L galaxies.…”

Section: Hot Ionized Gasmentioning

confidence: 99%

The impact of cosmic rays on dynamical balance and disk-halo interaction in Lstar disk galaxies

Chan,

Keres,

Gurvich

et al. 2021

Preprint

View full text Add to dashboard Cite

Cosmic rays (CRs) are an important component in the interstellar medium (ISM), but their effect on the dynamics of the disk-halo interface (< 10 kpc from the disk) is still unclear. We study the influence of CRs on the gas above the disk with highresolution FIRE-2 cosmological simulations of late-type L galaxies at redshift z ∼ 0. We compare runs with and without CR feedback (with constant anisotropic diffusion κ ∼ 3 × 10 29 cm 2 /s and streaming). Our simulations capture the relevant disk halo interactions, including outflows, inflows, and galactic fountains. Extra-planar gas in all of the runs satisfies dynamical balance, where total pressure balances the weight of the overlying gas. While the kinetic pressure from non-uniform motion ( 1 kpc scale) dominates in the midplane, thermal and bulk pressures (or CR pressure if included) take over at large heights. We find that with CR feedback, (1) the warm (∼ 10 4 K) gas is slowly accelerated by CRs; (2) the hot (> 5 × 10 5 K) gas scale height is suppressed;(3) the warm-hot (2 × 10 4 − 5 × 10 5 K) medium becomes the most volume-filling phase in the disk-halo interface. We develop a novel conceptual model of the near-disk gas dynamics in low-redshift L galaxies: with CRs, the disk-halo interface is filled with CR-driven warm winds and hot super-bubbles that are propagating into the CGM with a small fraction falling back to the disk. Without CRs, most outflows from hot superbubbles are trapped by the existing hot halo and gravity, so typically they form galactic fountains.

show abstract

Section: Hot Ionized Gasmentioning

confidence: 99%

The impact of cosmic rays on dynamical balance and disk-halo interaction in Lstar disk galaxies

Chan,

Keres,

Gurvich

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…In these higher temperature ranges, the prominent resonance absorption lines lie in the X-ray band (0.3-0.8 keV) (Smith et al 2011). Observations of the Sunyaev-Zeldovich effect in locally brightest galaxies (Planck Collaboration et al 2013;Bregman et al 2021) imply that we should observe most missing baryons at the virial temperatures of galaxies. Thus, we expect to account for the missing baryons by extending absorption line studies to the X-ray waveband where we can probe these temperatures.…”

Section: Introductionmentioning

confidence: 77%

The Hosts of X-ray Absorption Lines Toward AGNs

Huber,

Bregman

2021

Preprint

Self Cite

View full text Add to dashboard Cite

Most baryonic matter in the universe exists in gaseous form and can be found in structures such as galactic halos and the low-density intergalactic medium. Proposed X-ray spectroscopy missions such as Athena, Arcus, and Lynx will have the capability to identify absorption lines in spectra toward bright active galactic nuclei (AGNs), which can be used as a tool to probe this missing matter. In this study, we examine the optical fields surrounding 15 primary observing targets and identify the foreground galaxies and galaxy groups that are potential hosts of absorption. We record the basic properties of the potential host and their angular and physical separation from the AGN line of sight. This process is done by marking the location of various galaxies and groups in optical images of the field surrounding the target and plotting their angular separation vs. redshift to gauge physical proximity to the background source. We identify the surrounding objects according to those which have measured redshifts and those that require them.

show abstract

“…In addition to cold gas, galaxies are surrounded by coronae of warm-hot gas. This circumgalactic medium (CGM) may contain a baryonic mass comparable to that in the stars (Werk et al 2014;Tumlinson et al 2017;Bregman et al 2021) albeit in a diffuse form distributed over a much larger volume (100s of kpc). We do not attempt to model this component as it is not detected in individual SPARC galaxies, so the model RAR would not be compatible with the observed RAR.…”

Section: The Circumgalactic Mediummentioning

confidence: 99%

The Effect of Adiabatic Compression on Dark Matter Halos and the Radial Acceleration Relation

Li,

McGaugh,

Lelli

et al. 2022

Preprint

View full text Add to dashboard Cite

We use a semi-empirical model to investigate the radial acceleration relation (RAR) in a cold dark matter (CDM) framework. Specifically, we build 80 model galaxies covering the same parameter space as the observed galaxies in the SPARC database, assigning them to dark matter halos using abundance matching and halo mass-concentration relations. We consider several abundance matching relations, finding some to be a better match to the kinematic data than others. We compute the unavoidable gravitational interactions between baryons and their dark matter halos, leading to an overall compression of the original NFW halos. Before halo compression, high-mass galaxies approximately lie on the observed RAR whereas low-mass galaxies display up-bending "hooks" at small radii due to DM cusps, making them deviate systematically from the observed relation. After halo compression, the initial NFW halos become more concentrated at small radii, making larger contributions to rotation curves. This increases the total accelerations, moving all model galaxies away from the observed relation. These systematic deviations suggest that the CDM model with abundance matching alone cannot explain the observed RAR. Further effects (e.g., feedback) would need to counteract the compression with precisely the right amount of halo expansion, even in high mass galaxies with deep potential wells where such effects are generally predicted to be negligible.

show abstract

Hot Extended Galaxy Halos Around Local L* Galaxies From Sunyaev-Zeldovich Measurements

Cited by 7 publications

References 66 publications

The impact of cosmic rays on dynamical balance and disk-halo interaction in Lstar disk galaxies

The impact of cosmic rays on dynamical balance and disk-halo interaction in Lstar disk galaxies

The Hosts of X-ray Absorption Lines Toward AGNs

The Effect of Adiabatic Compression on Dark Matter Halos and the Radial Acceleration Relation

Contact Info

Product

Resources

About