Cool Gas in the Magellanic Stream

Matthews, Deanna; Dyson, P. L.; Müller, Erik

doi:10.1088/0004-637x/691/2/l115

Cited by 15 publications

(16 citation statements)

References 29 publications

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“…Furthermore, the central body of the Stream is bifurcated into two main strands or filaments (see Figure 2), as was first recognized by Cohen (1982) and Morras (1983 Matthews et al (2009), via 21 cm absorption studies. They detected a cool cloud with an inferred spin temperature of 70 K toward one continuum source, but failed to detect cool gas toward three other sources, indicating the cool phase has a low covering fraction.…”

Section: The Magellanic Streammentioning

confidence: 68%

The Magellanic Stream: Circumnavigating the Galaxy

D’Onghia

Fox

2016

Annu. Rev. Astron. Astrophys.

164

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The Magellanic Clouds are surrounded by an extended network of gaseous structures. Chief among these is the Magellanic Stream, an interwoven tail of filaments trailing the Clouds in their orbit around the Milky Way. When considered in tandem with its Leading Arm, the Stream stretches over 200 degrees on the sky. Thought to represent the result of tidal interactions between the Clouds and ram-pressure forces exerted by the Galactic corona, its kinematic properties reflect the dynamical history of the closest pair of dwarf galaxies to the Milky Way. The Stream is a benchmark for hydrodynamical simulations of accreting gas and cloud/corona interactions. If the Stream survives these interactions and arrives safely in the Galactic disk, its cargo of over a billion solar masses of gas has the potential to maintain or elevate the Galactic star formation rate. In this article, we review the current state of knowledge of the Stream, including its chemical composition, physical conditions, origin, and fate. We also review the dynamics of the Magellanic System, including the proper motions and orbital history of the Large and Small Magellanic Clouds, the first-passage and second-passage scenarios, and the evidence for a Magellanic Group of galaxies.Comment: 40 pages, accepted for publication in the Annual Reviews of Astronomy and Astrophysic

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Section: The Magellanic Streammentioning

confidence: 68%

The Magellanic Stream: Circumnavigating the Galaxy

D’Onghia

Fox

2016

Annu. Rev. Astron. Astrophys.

164

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“…Star formation in the MS and LA has been postu-lated but there was no success in the hunt for stars being formed in situ in early years (e.g., Recillas-Cruz 1982;Guhathakurta & Reitzel 1998). Matthews et al (2009) conducted a search for star formation in the MS regions using cold atomic gas as an indicator. Two absorption components were identified toward a background radio source, J0119−6809.…”

Section: Star Formation In the Leading Arm Regionmentioning

confidence: 99%

The distance and properties of hydrogen clouds in the Leading Arm of the Magellanic System

For

McClure-Griffiths

Westmeier

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a high-resolution study of five high-velocity clouds in the Magellanic Leading Arm region. This is a follow-up study of our widefield Parkes survey of the region in order to probe the multiphase structures of the clouds and to give an insight to their origin, evolution and distance. High-resolution data were obtained from the Australia Telescope Compact Array. By combining with single-dish data from the Galactic All-Sky Survey (GASS), we are able to probe compact and diffuse emission simultaneously. We identify resolved and unresolved clumps. Physical parameters were derived for both diffuse structure and compact clumps. The latter are cold with typical velocity linewidths of 5 km s −1 . We find a gradient in thermal halo pressure, hydrogen density and H i column density of HVC as a function of Galactic latitude. This is possibly the first observational evidence of varying distance in the Leading Arm region, with the leading part of the Leading Arm (LA II and III) probably being closer to the Galactic disc than the trailing end (LA I).

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“…We know very little about the temperature, distribution or quantity of cool H I in the halo. At present there are only two measurements of H I gas excitation, or spin, temperature in an HVC (Wakker et al 1991;Matthews et al 2009). Absorption line measurements with the SKA, with its resolution and sensitivity, will comprehensively determine the amount of condensed gas in the halo enabling direct comparisons with theoretical and numerical models (e.g.…”

Section: Accretionmentioning

confidence: 99%

“…The SKA1-SUR all-sky absorption survey will be able to directly detect this WNM component towards hundreds of sources, as shown in Figures 3 and 4. Measurements of H I absorption will extend to HVCs, where there are currently only two (Wakker et al 1991;Matthews et al 2009). Given the sky density of background sources and the column density distribution of known HVCs (Moss et al 2013), a blind all-sky survey covering all HVCs should detect cold H I components in absorption towards most known HVCs (δ < +30 • ) with narrow line components and measure their spin temperatures.…”

Section: Goals For Ska1mentioning

confidence: 99%

Galactic and Magellanic Evolution with the SKA

McClure‐Griffiths¹,

Stanimirović²,

Murray³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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As we strive to understand how galaxies evolve it is crucial that we resolve physical processes and test emerging theories in nearby systems that we can observe in great detail. Our own Galaxy, the Milky Way, and the nearby Magellanic Clouds provide unique windows into the evolution of galaxies, each with its own metallicity and star formation rate. These laboratories allow us to study with more detail than anywhere else in the Universe how galaxies acquire fresh gas to fuel their continuing star formation, how they exchange gas with the surrounding intergalactic medium, and turn warm, diffuse gas into molecular clouds and ultimately stars. The λ 21-cm line of atomic hydrogen (H I) is an excellent tracer of these physical processes. With the SKA we will finally have the combination of surface brightness sensitivity, point source sensitivity and angular resolution to transform our understanding of the evolution of gas in the Milky Way, all the way from the halo down to the formation of individual molecular clouds.Advancing Astrophysics with the Square Kilometre Array

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Cool Gas in the Magellanic Stream

Cited by 15 publications

References 29 publications

The Magellanic Stream: Circumnavigating the Galaxy

The Magellanic Stream: Circumnavigating the Galaxy

The distance and properties of hydrogen clouds in the Leading Arm of the Magellanic System

Galactic and Magellanic Evolution with the SKA

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