The Magellanic Stream and Debris Clouds

For, Bi-Qing; Staveley‐Smith, L.; Matthews, Deanna; McClure-Griffiths, N. M.

doi:10.1088/0004-637x/792/1/43

Cited by 41 publications

(29 citation statements)

References 56 publications

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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

1,034

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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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

1,034

229

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“…Likewise the MS and LA are likely significantly altered by this ambient medium. The stream exhibits strong Hα emission (Bland-Hawthorn et al 2007;Weiner & Williams 1996) and high velocity clouds (HVCs) kinematically associated with the whole complex consistently feature headtail structures well aligned with the orbital movement of the Magellanic Complex at large For et al 2014). Precise proper motion (PM) measurements of MC stars in the past decade have substantially improved our knowledge of the LMC's PM vector (Kallivayalil et al 2006;Piatek et al 2008) and enhanced our understanding of the LMC's orientation and internal rotation and the dynamical relationship between the MCs (Kallivayalil et al 2006;van der Marel & Kallivayalil 2014).…”

Section: Introductionmentioning

confidence: 99%

Ram Pressure Stripping of the Large Magellanic Cloud’s Disk as a Probe of the Milky Way’s Circumgalactic Medium

Salem

Besla

Bryan

et al. 2015

ApJ

156

228

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Recent observations have constrained the orbit and structure of the Large Magellanic Cloud (LMC), implying a well-constrained pericentric passage about the Milky Way (MW) ∼ 50 Myr ago. In this scenario, the LMC's gaseous disk has recently experienced stripping, suggesting the current extent of its HI disk directly probes the medium in which it is moving. From the observed stellar and HI distributions of the system we find evidence of a truncated gas profile along the windward "leading edge' of the LMC disk, despite a far more extended stellar component. We explore the implications of this ram pressure stripping signature, using both analytic prescriptions and full 3-dimensional hydrodynamic simulations of the LMC. Our simulations subject the system to a headwind whose velocity components correspond directly to the recent orbital history of the LMC. We vary the density of this headwind, using a variety of sampled parameters for a β-profile for a theoretical MW circumgalactic medium (CGM), comparing the resulting HI morphology directly to observations of the LMC HI and stellar components. This model can match the radial extent of the LMC's leading (windward) edge only in scenarios where the MW CGM density at pericentric passage is n p (R = 48.2 ± 5 kpc) = 1.1−.45 × 10 −4 cm −3 . The implied pericentric density proves insensitive to both the broader CGM structure and temperature profile, thus providing a model-independent constraint on the local gas density. This result imposes an important constraint on the density profile of the MW's CGM, and thus the total baryon content of the MW. From our work, assuming a β-profile valid to ∼ r vir , we infer a total diffuse CGM mass M (300 kpc) = 2.6 ± 1.4 × 10 10 M ⊙ or approximately 15% of a 10 12 M ⊙ MW's baryonic mass budget.

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“…The second mechanism is more commonly observed in small groups, where relative velocities between galaxies are low (see e.g. Koribalski & López-Sánchez 2009;For, Staveley-Smith & McClure-Griffiths 2013;For et al 2014). These mechanisms can result in a galaxy losing its hot halo and quenching of the star formation process.…”

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confidence: 99%

WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351

For

Staveley‐Smith

Westmeier

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present an H i study of the galaxy group LGG 351 using Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY) early science data observed with the Australian Square Kilometre Array Pathfinder (ASKAP). LGG 351 resides behind the M 83 group at a velocity range (cz) of ∼3500–4800 km s−1 within the rich Hydra-Centaurus overdensity region. We detect 40 sources with the discovery of a tidally interacting galaxy pair and two new H i sources that are not presented in previous optical catalogues. 23 out of 40 sources have new redshifts derived from the new H i data. This study is the largest WALLABY sub-sample to date and also allows us to further validate the performance of ASKAP and the data reduction pipeline askapsoft. Extended H i emission is seen in six galaxies indicating interaction within the group, although no H i debris is found. We also detect H i in a known ultra-faint dwarf galaxy (dw 1328−29), which demonstrates that it is not a satellite of the M 83 group as previously thought. In conjunction with multiwavelength data, we find that our galaxies follow the atomic gas fraction and baryonic Tully–Fisher scaling relations derived from the GALEX Arecibo SDSS Survey. In addition, majority of our galaxies fall within the star formation main sequence indicating inefficiency of gas removal processes in this loose galaxy group.

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The Magellanic Stream and Debris Clouds

Cited by 41 publications

References 56 publications

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

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

Ram Pressure Stripping of the Large Magellanic Cloud’s Disk as a Probe of the Milky Way’s Circumgalactic Medium

WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351

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