Accretion of gas on to nearby spiral galaxies

Fraternali, Filippo; Binney, James

doi:10.1111/j.1365-2966.2008.13071.x

Cited by 223 publications

(294 citation statements)

References 66 publications

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“…The typical orbits of this "accreting Galactic fountain" differ from those of a fountain without accretion for the presence of inward radial motions (Fig. 6 in Fraternali & Binney 2008), which indeed were observed in the H i halo of NGC 2403 (Fraternali et al 2001). In Sect.…”

Section: Discussionmentioning

confidence: 99%

“…Fraternali & Binney (2006) successfully reproduced the vertical gaseous distribution of NGC 891 and NGC 2403 by modelling the halo as a continuous flow of non-interacting Galactic fountain clouds moving ballistically in the galactic potential (see also Collins et al 2002;Heald et al 2007). However, they were forced to include interactions of these clouds with the environment in order to reproduce the vertical rotational lag (Fraternali & Binney 2008): in this scenario the fountain clouds accrete gas from an ambient medium with a low angular momentum with respect to the galactic disk. This process slows down the rotation of the Galactic fountain clouds and produces gas accretion towards the disk.…”

Section: Discussionmentioning

confidence: 99%

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Modelling the H i halo of the Milky Way

Marasco

Fraternali

2010

A&A

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Aims. We studied the global distribution and kinematics of the extra-planar neutral gas in the Milky Way.Methods. We built 3D models for a series of Galactic H i layers, projected them for an inside view, and compared them with the Leiden-Argentina-Bonn 21-cm observations. Results. We show that the Milky Way disk is surrounded by an extended halo of neutral gas with a vertical scale-height of 1.6 +0.6 −0.4 kpc and an H i mass of 3.2 +1.0 −0.9 × 10 8 M , which is ∼5−10% of the total Galactic H i. This H i halo rotates more slowly than the disk with a vertical velocity gradient of −15 ± 4 km s −1 kpc −1 . We found evidence for a global infall motion in the halo, both vertical (20 +5 −7 km s −1 ) and radial (30 +7 −5 km s −1 ). Conclusions.The Milky Way H i extra-planar layer shows properties similar to the halos of external galaxies, which is compatible with it being predominantly produced by supernova explosions in the disk. It is most likely composed of distinct gas complexes with masses of ∼10 4−5 M , of which the intermediate velocity clouds are the local manifestations. The classical high-velocity clouds appear to be a separate population.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Modelling the H i halo of the Milky Way

Marasco

Fraternali

2010

A&A

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“…The dominant mode of accretion at the star forming component of a galaxy remains to be determined. The interplay between enriched outflowing gas with gas coming in may be key in this process (Fraternali & Binney, 2008;Putman et al, 2012;Marinacci et al, 2010;Voit et al, 2015).…”

Section: Expected Modes Of Accretionmentioning

confidence: 99%

An Introduction to Gas Accretion onto Galaxies

Putman¹

2017

Gas Accretion Onto Galaxies

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Evidence for gas accretion onto galaxies can be found throughout the universe. In this chapter, I summarize the direct and indirect signatures of this process and discuss the primary sources. The evidence for gas accretion includes the star formation rates and metallicities of galaxies, the evolution of the cold gas content of the universe with time, numerous indirect indicators for individual galaxies, and a few direct detections of inflow. The primary sources of gas accretion are the intergalactic medium, satellite gas and feedback material. There is support for each of these sources from observations and simulations, but the methods with which the fuel ultimately settles in to form stars remain murky.

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“…Since their kinematics appear incompatible with a pure "fountain model" (Shapiro & Field , the occurrence of such gaseous halos has been connected to the accretion of gas from the ambient intergalactic medium onto the disk. Fraternali & Binney 2008 conclude that a contribution of low-angular momentum gas in addition to fountain material is needed to explain the kinematics of gaseous halos. In an accretion scenario, such low angular momentum material might comes from outer warped disks, formed by accretion, which supply gas to the inner disk in the process of their (slow) decomposition.…”

Section: Observational Evidence For Infall Of Matter In Warped Galaxiesmentioning

confidence: 99%

Warps and Accretion

Józsa¹

2010

Proc. IAU

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Abstract. Warps are a basic feature of disk galaxies. Usually they occur at radii where the optical disk fades and become most pronounced in the outermost gaseous disks.As such, warps present a massive reservoir to replenish star forming material in the inner, star forming disks. Furthermore, some possible excitation mechanisms for warps connect their formation to the accretion of extragalctic material. Interactions or mergers with gas-rich companions or the direct accretion of the ambient intergalactic medium might lead to the formation of warps, at the same time supplementing fuel to maintain star formation in galactic disks.Employing a number of H i studies of warped galaxies, including ultra-deep observations of the prototype warped galaxies NGC 5907 and NGC 4013, I discuss whether the observed kinematics may show evidence for a connection of warps and accretion from the ambient medium.

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Accretion of gas on to nearby spiral galaxies

Cited by 223 publications

References 66 publications

Modelling the H i halo of the Milky Way

Modelling the H i halo of the Milky Way

An Introduction to Gas Accretion onto Galaxies

Warps and Accretion

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