Evidence for a Massive Warm–Hot Circumgalactic Medium around NGC 3221

Das, Sanskriti; Mathur, S.; Gupta, Anjali; Nicastro, F.; Krongold, Y.; Null, Cody

doi:10.3847/1538-4357/ab48df

Cited by 30 publications

(32 citation statements)

References 75 publications

(68 reference statements)

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“…Resolving X-ray profiles around Milky Way-like galaxies (e.g. Li & Wang 2013) as has been done for more massive spirals (Anderson, Churazov & Bregman 2016;Bogdán et al 2017;Li et al 2017;Das et al 2019) can help distinguish these contrasting models. Central X-ray emission from individual galaxies may be detectable with the Chandra X-ray telescope according to Illustris-TNG simulations (Truong et al 2020) and the eROSITA mission should be able to observe extended emission in stacks of haloes as predicted by both the EAGLE and Illustris-TNG simulations (Oppenheimer et al 2020b).…”

Section: Hot Gas Radial Profilesmentioning

confidence: 99%

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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Section: Hot Gas Radial Profilesmentioning

confidence: 99%

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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“…Only the most massive spiral galaxies, NGC 1961 (Anderson et al 2016), NGC 6753 (Bogdán et al 2017), NGC 3221 (Das et al 2019), and the CGM-MASS sample (Li et al 2017) have detectable extended X-ray emission, which O20 argued are weaker than their high-sSFR eROSITA mock stacks containing similar mass galaxies. This potential mismatch is not exclusive to EAGLE, as O20 found similar values 𝐿 𝑋 ,>10kpc in IllustrisTNG, which was also explored by Truong et al (2019) who concentrates on centralised soft X-ray emission from IllustrisTNG galaxies.…”

Section: Are Eagle Galactic X-ray Cgms Too Bright?mentioning

confidence: 96%

“…Extended X-ray emission from gaseous haloes around typical galaxies are a general prediction of cosmological hydrodynamical simulations (Toft et al 2002;Rasmussen et al 2009;Crain et al 2010Crain et al , 2013Kelly et al 2021); however, Chandra and XMM-Newton possess the sensitivity to detect emission associated with only a handful of the most massive nearby late-type galaxies (Anderson & Bregman 2011;Dai et al 2012;Bogdán et al 2013b,a;Anderson et al 2016;Bogdán et al 2017;Li et al 2017;Das et al 2019). Newer simulations, including EAGLE (Schaye et al 2015;Crain et al 2015;McAlpine et al 2016) and IllustrisTNG (Pillepich et al 2018a;Nelson et al 2018), have been tuned to fit some of the observed properties of galaxies.…”

Section: Introductionmentioning

confidence: 99%

Predictions for the X-ray circumgalactic medium of edge-on discs and spheroids

Nica,

Oppenheimer,

Crain

et al. 2021

Preprint

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We investigate how the X-ray circumgalactic medium (CGM) of present-day galaxies depends on galaxy morphology and azimuthal angle using mock observations generated from the EAGLE cosmological hydrodynamic simulation. By creating mock stacks of eROSITAobserved galaxies oriented to be edge-on, we make several observationally-testable predictions for galaxies in the stellar mass range 𝑀 ★ = 10 10.7−11.2 M . The soft X-ray CGM of disc galaxies is between 60 and 100% brighter along the semi-major axis compared to the semiminor axis, between 10-30 kpc. This azimuthal dependence is a consequence of the hot (𝑇 > 10 6 K) CGM being non-spherical: specifically it is flattened along the minor axis such that denser and more luminous gas resides in the disc plane and co-rotates with the galaxy. Outflows enrich and heat the CGM preferentially perpendicular to the disc, but we do not find an observationally-detectable signature along the semi-minor axis. Spheroidal galaxies have hotter CGMs than disc galaxies related to spheroids residing at higher halos masses, which may be measurable through hardness ratios spanning the 0.2 − 1.5 keV band. While spheroids appear to have brighter CGMs than discs for the selected fixed 𝑀 ★ bin, this owes to spheroids having higher stellar and halo masses within that 𝑀 ★ bin, and obscures the fact that both simulated populations have similar total CGM luminosities at the exact same 𝑀 ★ . Discs have brighter emission inside 20 kpc and more steeply declining profiles with radius than spheroids. We predict that the eROSITA 4-year all-sky survey should detect many of the signatures we predict here, although targeted follow-up observations of highly inclined nearby discs after the survey may be necessary to observe some of our azimuthally-dependent predictions.

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“…A popular strategy for characterizing the hot CGM gas that emits in X-ray is to fit its density profile with a β model, which is a power-law profile where the parameter β describes the power. To estimate the total mass of hot gas in a galaxy's CGM, the β model is extrapolated out to the virial radius and integrated (Anderson & Bregman 2010;Gupta et al 2012;Das et al 2019), finding ∼ 10 9−10 M of hot gas within the halo (Anderson & Bregman 2010). This method assumes that the gas maintains its hot temperature out to the virial radius and that it is only the decline in density that leads to the decrease in X-ray surface brightness below detection limits in the outskirts of galaxy halos.…”

Section: Cgm Mass Estimates From X-ray Observationsmentioning

confidence: 99%

Figuring Out Gas & Galaxies In Enzo (FOGGIE) V: The Virial Temperature Does Not Describe Gas in a Virialized Galaxy Halo

Lochhaas,

Tumlinson,

O'Shea

et al. 2021

Preprint

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The classical definition of the virial temperature of a galaxy halo excludes a fundamental contribution to the energy partition of the halo: the kinetic energy of non-thermal gas motions. Using simulations from the FOGGIE project (Figuring Out Gas & Galaxies In Enzo) that are optimized to resolve lowdensity gas, we show that the kinetic energy of non-thermal motions is roughly equal to the energy of thermal motions. The simulated FOGGIE halos have ∼ 2× lower bulk temperatures than expected from a classical virial equilibrium, owing to significant non-thermal kinetic energy that is formally excluded from the definition of T vir . We derive a modified virial temperature explicitly including non-thermal gas motions that provides a more accurate description of gas temperatures for simulated halos in virial equilibrium. Strong bursts of stellar feedback drive the simulated FOGGIE halos out of virial equilibrium, but the halo gas cannot be accurately described by the standard virial temperature even when in virial equilibrium. Compared to the standard virial temperature, the cooler modified virial temperature implies other effects on halo gas: (i) the thermal gas pressure is lower, (ii) radiative cooling is more efficient, (iii) O VI absorbing gas that traces the virial temperature may be prevalent in halos of a higher mass than expected, (iv) gas mass estimates from X-ray surface brightness profiles may be incorrect, and (v) turbulent motions make an important contribution to the energy balance of a galaxy halo.

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Evidence for a Massive Warm–Hot Circumgalactic Medium around NGC 3221

Cited by 30 publications

References 75 publications

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

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

Predictions for the X-ray circumgalactic medium of edge-on discs and spheroids

Figuring Out Gas & Galaxies In Enzo (FOGGIE) V: The Virial Temperature Does Not Describe Gas in a Virialized Galaxy Halo

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