High-Velocity Clouds in the Galactic All Sky Survey. I. Catalog

Moss, V. A.; McClure-Griffiths, N. M.; Murphy, Tara; Pisano, D. J.; Kummerfeld, Jonathan K.; Curran, James

doi:10.1088/0067-0049/209/1/12

Cited by 22 publications

(49 citation statements)

References 39 publications

(55 reference statements)

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“…In reality, these clouds may be destroyed via hydrodynamical instabilities as they fall back onto the disc (Heitsch & Putman 2009), a process that is likely not fully captured in our models. Regardless, these clouds could be interpreted as high velocity clouds (HVC), which are observed in the Milky Way halo (Blitz et al 1999;Wakker 2004;Moss et al 2013Moss et al , 2017. The origin of the HVCs is still an open question (Lockman et al 2019), and although the most distant ones are likely from cosmic origin (see e.g., Richter 2012), there are plenty of clouds observed within few tens of kpc (see Wakker et al 2008), compatible with our runaways model.…”

Section: Comparisons To Observationssupporting

confidence: 67%

How runaway stars boost galactic outflows

Andersson

Agertz

2020

Monthly Notices of the Royal Astronomical Society

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Roughly ten per cent of OB stars are kicked out of their natal clusters before ending their life as supernovae. These so called runaway stars can travel hundreds of parsecs into the low-density interstellar medium, where momentum and energy from stellar feedback is efficiently deposited. In this work we explore how this mechanism affects large scale properties of the galaxy, such as outflows. To do so we use a new model which treats OB stars and their associated feedback processes on a star-by-star basis. With this model we compare two hydrodynamical simulations of Milky Way-like galaxies, one where we include runaways, and one where we ignore them. Including runaway stars leads to twice as many supernovae explosions in regions with gas densities ranging from 10 −5 cm −3 to 10 −3 cm −3 . This results in more efficient heating of the inter-arm regions, and drives strong galactic winds with mass loading factors boosted by up to one order of magnitude. These outflows produce a more massive and extended multi-phase circumgalactic medium, as well as a population of dense clouds in the halo. Conversely, since less energy and momentum is released in the dense star forming regions, the cold phase of the interstellar medium is less disturbed by feedback effects.

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Section: Comparisons To Observationssupporting

confidence: 67%

How runaway stars boost galactic outflows

Andersson

Agertz

2020

Monthly Notices of the Royal Astronomical Society

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“…M12), and the latter's H I disk and HVCs fill a sizeable fraction of the spatial and spectral search volume (e.g. Peek et al 2011;Moss et al 2013): an overlap in V LSR between Galactic H I clouds and dSph stars is therefore unlikely to imply a physical association between them. An investigation of the H I content of dSphs in these confused fields requires deep, wide-field H I mapping, and even then associating H I features with stellar systems at the same location is not straightforward (e.g.…”

Section: Discussionmentioning

confidence: 99%

The Dearth of Neutral Hydrogen in Galactic Dwarf Spheroidal Galaxies

Spekkens¹,

Urbancic²,

Mason³

et al. 2014

ApJ

153

173

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We present new upper limits on the neutral hydrogen (H I) content within the stellar half-light ellipses of 15 Galactic dwarf spheroidal galaxies (dSphs), derived from pointed observations with the Green Bank Telescope (GBT) as well as Arecibo L-band Fast ALFA (ALFALFA) survey and Galactic All-Sky Survey (GASS) data. All of the limits M lim HI are more stringent than previously reported values, and those from the GBT improve upon contraints in the literature by a median factor of 23.−5 , irrespective of location in the Galactic halo. Comparing these relative H I contents to those of the Local Group and nearby neighbor dwarfs compiled by McConnachie, we find that the Galactic dSphs are extremely gas-poor. Our H I upper limits therefore provide the clearest picture yet of the environmental dependence of the H I content in Local Volume dwarfs. If ram pressure stripping explains the dearth of H I in these systems, then orbits in a relatively massive Milky Way are favored for the outer halo dSph Leo I, while Leo II and Canes Venatici I have had a pericentric passage in the past. For Draco and Ursa Minor, the interstellar medium mass that should accumulate through stellar mass loss in between pericentric passages exceeds M lim HI by a factor of ∼ 30. In Ursa Minor, this implies that either this material is not in the atomic phase, or that another mechanism clears the recycled gas on shorter timescales.

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“…In the past it has been used to study the MW halo (Ford et al 2008;Winkel et al 2011;Ben Bekhti et al 2012;Venzmer et al 2012;Hernandez et al 2013;Moss et al 2013;For et al 2014;Röhser et al 2014;Hammer et al 2015;Lenz et al 2016;Kerp et al 2016b) and the disk-halo interaction (Ford et al 2010;McClureGriffiths et al 2010;Lenz et al 2015;Röhser et al 2016a). Likewise the MW disk material itself can be explored in much greater detail than previously feasible (e.g., Haud 2013; , also revealing spectacular Galactic super-shells (McClure-Griffiths et al 2006;Moss et al 2012).…”

Section: Introductionmentioning

confidence: 99%

HI4PI: a full-sky H i survey based on EBHIS and GASS

Bekhti

Flöer

Keller

et al. 2016

A&A

Self Cite

943

229

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Context. Measurement of the Galactic neutral atomic hydrogen (H i) column density, N H i , and brightness temperatures, T B , is of high scientific value for a broad range of astrophysical disciplines. In the past two decades, one of the most-used legacy H i datasets has been the Leiden/Argentine/Bonn Survey (LAB). Aims. We release the H i 4π survey (HI4PI), an all-sky database of Galactic H i, which supersedes the LAB survey. Methods. The HI4PI survey is based on data from the recently completed first coverage of the Effelsberg-Bonn H i Survey (EBHIS) and from the third revision of the Galactic All-Sky Survey (GASS). EBHIS and GASS share similar angular resolution and match well in sensitivity. Combined, they are ideally suited to be a successor to LAB. Results. The new HI4PI survey outperforms the LAB in angular resolution (ϑ FWHM = 16 .2) and sensitivity (σ rms = 43 mK). Moreover, it has full spatial sampling and thus overcomes a major drawback of LAB, which severely undersamples the sky. We publish all-sky column density maps of the neutral atomic hydrogen in the Milky Way, along with full spectroscopic data, in several map projections including HEALPix.

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High-Velocity Clouds in the Galactic All Sky Survey. I. Catalog

Cited by 22 publications

References 39 publications

How runaway stars boost galactic outflows

How runaway stars boost galactic outflows

The Dearth of Neutral Hydrogen in Galactic Dwarf Spheroidal Galaxies

HI4PI: a full-sky H i survey based on EBHIS and GASS

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