A deep<i>XMM–Newton</i>study of the hot gaseous halo around NGC 1961

Anderson, Michael E.; Churazov, E.; Bregman, Joel N.

doi:10.1093/mnras/stv2314

Cited by 101 publications

(129 citation statements)

References 105 publications

(132 reference statements)

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“…These two components, however, are often not explicitly separated and could mix with each other. In general, the outer halo has low metallicity and density, so faint in soft X-ray, but could dominate the total hot gas mass in a galactic halo (e.g., Crain et al 2013;Anderson et al 2016 ) could the CGM be gravitationally heated to an X-ray-emitting temperature above the peak of the radiative cooling curve (e.g., Keres et al 2009;van de Voort et al 2016). Therefore, the extended hot gas in the outer halo is only expected to be detected in the most massive spiral galaxies.…”

Section: The Lack Of High-quality X-ray Observations Of Massive Spiramentioning

confidence: 99%

The Circum-Galactic Medium of Massive Spirals. I. An Overview and a Case Study of NGC 5908

Bregman

Wang

et al. 2016

ApJ

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The Circum-Galactic Medium of MASsive Spirals is a project studying the overall content, physical and chemical properties, and spatial distributions of the multi-phase circumgalactic medium around a small sample of the most massive ( * ´ M M 2 10 11 , > -v 300 km s rot 1) isolated spiral galaxies in the local universe. We introduce the sample and present a detailed case study of the XMM-Newton observation of the hot gas halo of NGC5908. After data calibration, point source removal, and background analysis, we find that the diffuse soft X-ray emission of NGC5908 is significantly more extended than the stellar light in the vertical direction. The 0.5-1.25 keV radial intensity profile tracing hot gas emission can be detected above the background out to about ¢ 2 , or 30 kpc from the nucleus. The unresolved soft X-ray emission can be characterized using a β-model with a slope of b » 0.68. The unresolved 0.5-2 keV luminosity within ¢ 1 is´-6.8 10 erg s 39 1 , but young stellar sources may contribute significantly to it. Assuming a metallicity of 0.2solar, an upper limit (without subtracting the very uncertain young stellar contribution) to the mass of hot gas within this radius is´ M 2.3 10 9 . The cooling radius is » r 25 kpc cool or » r 0.06 200 , within which the hot gas could cool radiatively in less than 10 Gyr, and the cooling of hot gas could significantly contribute to replenishing the gas consumed in star formation. The hot gas accounts for »1.9% of the baryons detected within the cooling radius. By comparing NGC5908 to other galaxies, we find that its X-ray luminosity per stellar mass is consistent with lower-mass non-starburst field spiral galaxies. However, a large scatter in hot gas soft X-ray emissivity is indicated for spiral galaxies with * ´ M M 2 10 11 .

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Section: The Lack Of High-quality X-ray Observations Of Massive Spiramentioning

confidence: 99%

The Circum-Galactic Medium of Massive Spirals. I. An Overview and a Case Study of NGC 5908

Bregman

Wang

et al. 2016

ApJ

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“…In all simulations the parameters of the coronal medium were chosen assuming the typical properties of the Milky Way at large distances from the galactic disc (50-150 kpc, following the observed impact parameters of the COS-Halos survey). The coronal temperature was set to 2 × 10 6 K, roughly the coronal temperature of the Milky Way (Fukugita & Peebles 2006;Miller & Bregman 2015), while the coronal metallicity was set to 0.1 Z , according to the value estimated for those galaxies in which the hot halo was actually observed in X-rays (Bogdán et al 2013;Hodges-Kluck & Bregman 2013;Anderson, Churazov & Bregman 2016). For the Milky Way the value is not well constrained, but studies through both Far Ultraviolet absorption spectra and emission lines of Ovii and Oviii returned values between 0.1 and 0.3 Z (Sembach et al 2003;Miller & Bregman 2015).…”

Section: Hydrodynamical Simulationsmentioning

confidence: 99%

“…Once extrapolated to the virial radius, the mass of these coronae is comparable with the mass of the baryonic discs of these galaxies (∼ 10 11 M ), accounting for ∼ 10 − 50% of their associated 'missing baryons' (e.g. Dai et al 2012;Bogdán et al 2013;Anderson, Churazov & Bregman 2016). By combining observations of Ovi absorbers around star-forming galaxies (from the COS-Halos survey, see below) together with the Ovii and Oviii absorption associated with our Galaxy in a single model of corona, Faerman, Sternberg & McKee (2017) found that the typical coronal gas mass of a Milky-Way-like galaxy is ∼ 1.35 × 10 11 M .…”

Section: Introductionmentioning

confidence: 98%

The survival of gas clouds in the circumgalactic medium of Milky Way-like galaxies

Armillotta

Fraternali

Werk

et al. 2017

Monthly Notices of the Royal Astronomical Society

157

135

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Observational evidence shows that low-redshift galaxies are surrounded by extended haloes of multiphase gas, the so-called 'circumgalactic medium' (CGM). To study the survival of relatively cool gas (T < 10 5 K) in the CGM, we performed a set of hydrodynamical simulations of cold (T = 10 4 K) neutral gas clouds travelling through a hot (T = 2 × 10 6 K) and low-density (n = 10 −4 cm −3 ) coronal medium, typical of Milky Way-like galaxies at large galactocentric distances (∼ 50 − 150 kpc). We explored the effects of different initial values of relative velocity and radius of the clouds. Our simulations were performed on a two-dimensional grid with constant mesh size (2 pc) and they include radiative cooling, photoionization heating and thermal conduction. We found that for large clouds (radii larger than 250 pc) the cool gas survives for very long time (larger than 250 Myr): despite that they are partially destroyed and fragmented into smaller cloudlets during their trajectory, the total mass of cool gas decreases at very low rates. We found that thermal conduction plays a significant role: its effect is to hinder formation of hydrodynamical instabilities at the cloud-corona interface, keeping the cloud compact and therefore more difficult to destroy. The distribution of column densities extracted from our simulations are compatible with those observed for low-temperature ions (e.g. Siii and Siiii) and for high-temperature ions (Ovi) once we take into account that Ovi covers much more extended regions than the cool gas and, therefore, it is more likely to be detected along a generic line of sight.

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“…To date, haloes of hot gas have been observed around some massive spiral galaxies. In the giant spirals NGC 1961, UGC 12591 and NGC 266, X-ray emission has been detected at more than 50 kpc from the center, indicating the presence of extended structures of hot gas (Dai et al 2012;Bogdán et al 2013;Anderson, Churazov & Bregman 2016). The mass of these coronae is comparable with the disc baryonic mass ( 10 11 M ), accounting for 10 − 50% of the missing baryons associated to those galaxies.…”

Section: Introductionmentioning

confidence: 95%

Efficiency of gas cooling and accretion at the disc–corona interface

Armillotta

Fraternali

Marinacci

2016

Mon. Not. R. Astron. Soc.

126

133

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In star-forming galaxies, stellar feedback can have a dual effect on the circumgalactic medium both suppressing and stimulating gas accretion. The trigger of gas accretion can be caused by disc material ejected into the halo in the form of fountain clouds and by its interaction with the surrounding hot corona. Indeed, at the disc-corona interface, the mixing between the cold/metal-rich disc gas (T 10 4 K) and the hot coronal gas (T 10 6 K) can dramatically reduce the cooling time of a portion of the corona and produce its condensation and accretion. We studied the interaction between fountain clouds and corona in different galactic environments through parsec-scale hydrodynamical simulations, including the presence of thermal conduction, a key mechanism that influences gas condensation. Our simulations showed that the coronal gas condensation strongly depends on the galactic environment, in particular it is less efficient for increasing virial temperature/mass of the haloes where galaxies reside and it is fully ineffective for objects with virial masses larger than 10 13 M . This result implies that the coronal gas cools down quickly in haloes with low-intermediate virial mass (M vir 3 × 10 12 M ) but the ability to cool the corona decreases going from late-type to earlytype disc galaxies, potentially leading to the switching off of accretion and the quenching of star formation in massive systems.

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A deepXMM–Newtonstudy of the hot gaseous halo around NGC 1961

Cited by 101 publications

References 105 publications

The Circum-Galactic Medium of Massive Spirals. I. An Overview and a Case Study of NGC 5908

The Circum-Galactic Medium of Massive Spirals. I. An Overview and a Case Study of NGC 5908

The survival of gas clouds in the circumgalactic medium of Milky Way-like galaxies

Efficiency of gas cooling and accretion at the disc–corona interface

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