The Cold Gaseous Halo of NGC 891

Oosterloo, Thomas; Fraternali, Filippo; Sancisi, R.

doi:10.1086/520332

Cited by 314 publications

(554 citation statements)

References 52 publications

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“…The vertical rotational gradient estimated in Sect. 3.3 is the same as the one found by Oosterloo et al (2007) for NGC 891; inward radial motions of 10−20 km s −1 have been found by Fraternali et al (2002) in the H i halo of NGC 2403; Boomsma et al (2008) showed the presence of vertical motions for halo gas clouds in NGC 6946.…”

Section: Comparison With External Galaxiessupporting

confidence: 80%

“…We assumed a velocity dispersion of 20 km s −1 for the halo gas. This value was estimated for NGC 891 by Oosterloo et al (2007). In the Milky Way, Ford et al (2008) regions.…”

Section: Application To the Datamentioning

confidence: 87%

“…High-velocity outflows of neutral and ionized gas from the disk are observed to be correlated with star-forming regions (Kamphuis et al 1991;Fraternali et al 2004). The extra-planar neutral hydrogen has a kinematics similar to that of the disk H i (Fraternali et al 2002), but with some peculiar properties: a) it rotates more slowly (Oosterloo et al 2007); b) it shows vertical motions (Boomsma et al 2005); c) it has a global inflow (Fraternali et al 2001). Extra-planar diffused ionized gas (eDIG) is present in all galaxies with sufficiently high star-formation rates (Rossa & Dettmar 2003) and its kinematics seems to closely follow that of the neutral component (Heald et al 2006;Kamphuis et al 2007).…”

Section: Introductionmentioning

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: Comparison With External Galaxiessupporting

confidence: 80%

“…We assumed a velocity dispersion of 20 km s −1 for the halo gas. This value was estimated for NGC 891 by Oosterloo et al (2007). In the Milky Way, Ford et al (2008) regions.…”

Section: Application To the Datamentioning

confidence: 87%

Section: Introductionmentioning

confidence: 99%

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Modelling the H i halo of the Milky Way

Marasco

Fraternali

2010

A&A

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“…While simulations require many of the metals created by a galaxy are ejected from the system (see panel c of Figure 3), there is a large mass of metals detected in galaxy halos that remains bound (Tumlinson et al, 2011;Werk et al, 2014). Westmeier et al, 2007), and NGC 891 (top right; Oosterloo et al, 2007). The Milky Way observations are shown from an external point of view with the viewing angle and distance to M31 (bottom left) and NGC 891 (bottom right).…”

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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“…This material includes hot X-ray emitting gas (e.g. Tüllmann et al 2006;Li et al 2008), ionised gas (Collins & Rand 2001;Rossa & Dettmar 2003), dust (Howk & Savage 1999;Ménard et al 2010), and neutral hydrogen (Fraternali et al 2002;Oosterloo et al 2007;Heald et al 2011). The material is found to be often (but not always, in the case of the H) closely associated with star formation in the galaxy disk.…”

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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The Cold Gaseous Halo of NGC 891

Cited by 314 publications

References 52 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

HALOGAS: Extraplanar gas in NGC 3198

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