Galactic fountains and the rotation of disc-galaxy coronae

Marinacci, Federico; Fraternali, Filippo; Nipoti, Carlo; Binney, James; Ciotti, Luca; Londrillo, P.

doi:10.1111/j.1365-2966.2011.18810.x

Cited by 108 publications

(187 citation statements)

References 38 publications

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“…These include a galactic fountain of cool gas that spins up hot gas (Marinacci et al 2011), a hot galactic fountain of superbubble ejecta that produces an exponential disk before cooling, or infall from the cosmic web with some preferential direction. Our measurements cannot, by themselves, distinguish between these models (which may not be mutually exclusive), but they are an important kinematic constraint for future halo and galaxy formation models.…”

Section: Discussionmentioning

confidence: 99%

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The Rotation of the Hot Gas Around the Milky Way

Hodges-Kluck

Miller

Bregman

2016

ApJ

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The hot gaseous halos of galaxies likely contain a large amount of mass and are an integral part of galaxy formation and evolution. The Milky Way has a2 10 6 K halo that is detected in emission and by absorption in the O VII resonance line against bright background active galactic nuclei (AGNs), and for which the best current model is an extended spherical distribution. Using XMM-Newton Reflection Grating Spectrometer data, we measure the Doppler shifts of the O VII absorption-line centroids toward an ensemble of AGNs. These Doppler shifts constrain the dynamics of the hot halo, ruling out a stationary halo at about s 3 and a co-rotating halo at s 2 , and leading to a best-fit rotational velocity of =  f v 183 41 km s −1 for an extended halo model. These results suggest that the hot gas rotates and that it contains an amount of angular momentum comparable to that in the stellar disk. We examined the possibility of a model with a kinematically distinct disk and spherical halo. To be consistent with the emission-line X-ray data, the disk must contribute less than 10% of the column density, implying that the Doppler shifts probe motion in the extended hot halo.

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Section: Discussionmentioning

confidence: 99%

“…Also, if the material is fresh infall from the cosmic web then it likely accretes along filaments, which lead to a preferential orbital angular momentum axis. Finally, gas ejected from the disk (either cold or hot) could spin up the halo (Marinacci et al 2011), although perhaps not to the velocity that we infer.…”

Section: Halo and Disk Modelsmentioning

confidence: 99%

The Rotation of the Hot Gas Around the Milky Way

Hodges-Kluck

Miller

Bregman

2016

ApJ

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“…For example, Marinacci et al (2011) and Marasco et al (2012) have suggested gas driven into the hot coronae by recent star formation in the disk may cause the halo gas to cool. This cool gas can then accrete onto the galaxy.…”

Section: The Formation Of Disksmentioning

confidence: 99%

Clues to the formation of the Milky Way’s thick disk

Haywood

Matteo

Snaith

et al. 2015

A&A

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We analyze the chemical properties of a set of solar vicinity stars, and show that the small dispersion in abundances of α-elements at all ages provides evidence that the star formation history (SFH) has been uniform throughout the thick disk. In the context of longtimescale infall models, we suggest that this result points either to a limited dependence of the gas accretion on the Galactic radius in the inner disk (R < 10 kpc) or to a decoupling of the accretion history and SFH due to other processes governing the interstellar medium in the early disk, suggesting that infall cannot be a determining parameter of the chemical evolution at these epochs. We argue that these results and other recent observational constraints -namely the lack of radial metallicity gradient and the non-evolving scale length of the thick disk -are better explained if the early disk is viewed as a pre-assembled gaseous system, with most of the gas settled before significant star formation took place -formally the equivalent of a closed-box model. In either case, these results point to a weak or non-existent inside-out formation history in the thick disk or in the first 3-5 Gyr of the formation of the Galaxy. We argue, however, that the growing importance of an external disk whose chemical properties are distinct from those of the inner disk would give the impression of an inside-out growth process when seen through snapshots at different epochs. The progressive, continuous process usually invoked may not have actually existed in the Milky Way.

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“…Fraternali & Binney 2006) show that there must be additional mechanisms governing the kinematics of extraplanar gas, because these simple models obtain lags that are too shallow compared with observations. A possibility is the interaction between the uplifted gas and a corona of slowly rotating hot gas, which would explain the magnitude of the observed lags (Marinacci et al 2011). Other explanations for the properties of extraplanar gas involve, for example, thermal instabilities in the corona (Kaufmann et al 2006; but see Binney et al 2009), pressure gradients, or the effect of the magnetic field (Benjamin 2002).…”

Section: Introductionmentioning

confidence: 99%

HALOGAS: Extraplanar gas in NGC 3198

Gentile

Józsa

Serra

et al. 2013

A&A

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We present the analysis of new, deep H observations of the spiral galaxy NGC 3198 as part of the Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) survey, with the main aim of investigating the presence, amount, morphology, and kinematics of extraplanar gas. We present models of the H observations of NGC 3198. The model that matches best the observed data cube features a thick disk with a scale height of ∼3 kpc and an H mass of about 15% of the total H mass; this thick disk also has a decrease in rotation velocity as a function of height (lag) of 7-15 km s −1 kpc −1 (though with large uncertainties). This extraplanar gas is detected for the first time in NGC 3198. Radially, this gas appears to extend slightly beyond the actively star-forming body of the galaxy (as traced by the Hα emission), but it is not more radially extended than the outer, fainter parts of the stellar disk. Compared to previous studies, thanks to the improved sensitivity we trace the rotation curve out to larger radii. We model the rotation curve in the framework of modified Newtonian dynamics (MOND) and confirm that, with the allowed distance range we assumed, fit quality is modest in this galaxy, but the new outer parts are explained in a satisfactory way.

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Galactic fountains and the rotation of disc-galaxy coronae

Cited by 108 publications

References 38 publications

The Rotation of the Hot Gas Around the Milky Way

The Rotation of the Hot Gas Around the Milky Way

Clues to the formation of the Milky Way’s thick disk

HALOGAS: Extraplanar gas in NGC 3198

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