Massive Warm/Hot Galaxy Coronae. II. Isentropic Model

Faerman, Yakov; Sternberg, A.; McKee, Christopher F.

doi:10.3847/1538-4357/ab7ffc

Cited by 68 publications

(61 citation statements)

References 122 publications

(151 reference statements)

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“…Fukugita & Peebles 2006) and has been confirmed by numerous observations (e.g. Anderson & Bregman 2011;Bogdán et al 2017;Li et al 2017;Faerman, Sternberg & McKee 2020) Our description of this gas phase is physically motivated as a stratified medium in hydrostatic equilibrium with the dark matter halo and is consistent with the current evidence from observations, which are, however, still limited and mostly reliable only for the inner parts of the haloes. We can see from Fig.…”

Section: Influence Of the Hot Gassupporting

confidence: 86%

Most of the cool CGM of star-forming galaxies is not produced by supernova feedback

Afruni

Fraternali

Pezzulli

2020

Monthly Notices of the Royal Astronomical Society

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The characterization of the large amount of gas residing in the galaxy halos, the so called circumgalactic medium (CGM), is crucial to understand galaxy evolution across cosmic time. We focus here on the the cool (T ∼ 104 K) phase of this medium around star-forming galaxies in the local universe, whose properties and dynamics are poorly understood. We developed semi-analytical parametric models to describe the cool CGM as an outflow of gas clouds from the central galaxy, as a result of supernova explosions in the disc (galactic wind). The cloud motion is driven by the galaxy gravitational pull and by the interactions with the hot (T ∼ 106 K) coronal gas. Through a bayesian analysis, we compare the predictions of our models with the data of the COS-Halos and COS-GASS surveys, which provide accurate kinematic information of the cool CGM around more than 40 low-redshift star-forming galaxies, probing distances up to the galaxy virial radii. Our findings clearly show that a supernova-driven outflow model is not suitable to describe the dynamics of the cool circumgalactic gas. Indeed, to reproduce the data, we need extreme scenarios, with initial outflow velocities and mass loading factors that would lead to unphysically high energy coupling from the supernovae to the gas and with supernova efficiencies largely exceeding unity. This strongly suggests that, since the outflows cannot reproduce most of the cool gas absorbers, the latter are likely the result of cosmological inflow in the outer galaxy halos, in analogy to what we have previously found for early-type galaxies.

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Section: Influence Of the Hot Gassupporting

confidence: 86%

Most of the cool CGM of star-forming galaxies is not produced by supernova feedback

Afruni

Fraternali

Pezzulli

2020

Monthly Notices of the Royal Astronomical Society

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“…Our densities and temperatures also show good agreement, especially in the inner halo. Our pressure profile is lower than the Faerman et al (2020) model that also includes non-thermal sources of turbulent and magnetic/cosmic ray pressure. That model assumes HSE, but Oppenheimer (2018) showed that these low-z haloes are not well described by HSE in their inner CGMs, though at 0.5R 200 the thermal pressure gradient accounts for ≥ 75 per cent of the support against gravity (their fig.…”

Section: Hot Gas Radial Profilesmentioning

confidence: 64%

The changing circumgalactic medium over the last 10 Gyr – I. Physical and dynamical properties

Huscher¹,

Oppenheimer

Lonardi³

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the physical and dynamical states of two sets of EAGLE zoom simulations of galaxy haloes, one at high redshift (z = 2 − 3) and the other at low redshift (z = 0), with masses of ≈1012 M⊙. Our focus is how the circumgalactic medium (CGM) of these L* star-forming galaxies change over the last 10 Gyr. We find that the high-z CGM is almost equally divided between the “cool” (T < 105 K) and “hot” (T ≥ 105 K) phases, while at low-z the hot CGM phase contains 5 × more mass than the cool phase. The high-z hot CGM contains 60% more metals than the cool CGM, while the low-z cool CGM contains 35% more metals than the hot CGM. The metals are evenly distributed radially between the hot and cool phases throughout the high-z CGM. At high z, the CGM volume is dominated by hot outflows, but also contains cool gas mainly inflowing and cool metals mainly outflowing. At low z, the cool metals dominate the interior and the hot metals are more prevalent at larger radii. The low-z cool CGM has tangential motions consistent with rotational support out to 0.2R200, often exhibiting r ≈ 40 kpc disc-like structures. The low-z hot CGM has several times greater angular momentum than the cool CGM, and a more flattened radial density profile than the high-z hot CGM. This study verifies that, just as galaxies demonstrate significant transformations over cosmic time, the gaseous haloes surrounding them also undergo considerable changes of their own both in physical characteristics of density, temperature, and metallicity, and dynamic properties of velocity and angular momentum.

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“…13), where photoionization becomes important. The importance of photoionization for the CGM ion content was previously pointed out by Faerman et al (2020) in their isentropic model of the CGM of an L * galaxy.…”

Section: Cie(t = T 200cmentioning

confidence: 72%

The warm-hot circumgalactic medium around EAGLE-simulation galaxies and its detection prospects with X-ray and UV line absorption

Wijers

Schaye

Oppenheimer

2020

Monthly Notices of the Royal Astronomical Society

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We use the EAGLE cosmological simulation to study the distribution of baryons, and FUV (O vi), EUV (Ne viii) and X-ray (O vii, O viii, Ne ix, and Fe xvii) line absorbers, around galaxies and haloes of mass $\, \rm {M}_{\rm {200c}}= 10^{11}$–$10^{14.5} \, \rm {M}_{\odot }$ at redshift 0.1. EAGLE predicts that the circumgalactic medium (CGM) contains more metals than the interstellar medium across halo masses. The ions we study here trace the warm-hot, volume-filling phase of the CGM, but are biased towards temperatures corresponding to the collisional ionization peak for each ion, and towards high metallicities. Gas well within the virial radius is mostly collisionally ionized, but around and beyond this radius, and for O vi, photo-ionization becomes significant. When presenting observables we work with column densities, but quantify their relation with equivalent widths by analysing virtual spectra. Virial-temperature collisional ionization equilibrium ion fractions are good predictors of column density trends with halo mass, but underestimate the diversity of ions in haloes. Halo gas dominates the highest column density absorption for X-ray lines, but lower-density gas contributes to strong UV absorption lines from O vi and Ne viii. Of the O vii (O viii) absorbers detectable in an Athena X-IFU blind survey, we find that 41 (56) per cent arise from haloes with $\, \rm {M}_{\rm {200c}}= 10^{12.0 \rm {-}13.5} \, \rm {M}_{\odot }$. We predict that the X-IFU will detect O vii (O viii) in 77 (46) per cent of the sightlines passing $\, \rm {M}_{\star }= 10^{10.5 \rm {-}11.0} \, \rm {M}_{\odot }$ galaxies within $100 \, \rm {pkpc}$ (59 (82) per cent for $\, \rm {M}_{\star }> 10^{11.0} \, \rm {M}_{\odot }$). Hence, the X-IFU will probe covering fractions comparable to those detected with the Cosmic Origins Spectrograph for O vi.

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Massive Warm/Hot Galaxy Coronae. II. Isentropic Model

Cited by 68 publications

References 122 publications

Most of the cool CGM of star-forming galaxies is not produced by supernova feedback

Most of the cool CGM of star-forming galaxies is not produced by supernova feedback

The changing circumgalactic medium over the last 10 Gyr – I. Physical and dynamical properties

The warm-hot circumgalactic medium around EAGLE-simulation galaxies and its detection prospects with X-ray and UV line absorption

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