The Magellanic stream

Mathewson, D. S.; Cleary, M. N.; Murray, J. D.

doi:10.1086/152875

Cited by 330 publications

(285 citation statements)

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“…For example, there is clear evidence for stripping of the LMC and SMC, which are the only Milky Way satellites more massive than 10 8 M . However, the stripped gas that comprises the Magellanic Stream and Leading Arm (Mathewson, Cleary & Murray 1974), may result from tidal effects (e.g. Lin & Lynden-Bell 1977;Besla et al 2010Besla et al , 2012Guglielmo, Lewis & Bland-Hawthorn 2014) versus ram-pressure or viscous stripping (e.g.…”

Section: Reproducing the Critical Mass Scale For Satellite Quenchingmentioning

confidence: 99%

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Fillingham

Cooper

Pace

et al. 2016

Mon. Not. R. Astron. Soc.

119

123

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Recent studies of galaxies in the local Universe, including those in the Local Group, find that the efficiency of environmental (or satellite) quenching increases dramatically at satellite stellar masses below ∼ 10 8 M . This suggest a physical scale where quenching transitions from a slow "starvation" mode to a rapid "stripping" mode at low masses. We investigate the plausibility of this scenario using observed HI surface density profiles for a sample of 66 nearby galaxies as inputs to analytic calculations of ram-pressure and turbulent viscous stripping. Across a broad range of host properties, we find that stripping becomes increasingly effective at M * 10 8−9 M , reproducing the critical mass scale observed. However, for canonical values of the circumgalactic medium density (n halo < 10 −3.5 cm −3 ), we find that stripping is not fully effective; infalling satellites are, on average, stripped of only 40 − 60% of their cold gas reservoir, which is insufficient to match observations. By including a host halo gas distribution that is clumpy and therefore contains regions of higher density, we are able to reproduce the observed HI gas fractions (and thus the high quenched fraction and short quenching timescale) of Local Group satellites, suggesting that a host halo with clumpy gas may be crucial for quenching low-mass systems in Local Group-like (and more massive) host halos.

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Section: Reproducing the Critical Mass Scale For Satellite Quenchingmentioning

confidence: 99%

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Fillingham

Cooper

Pace

et al. 2016

Mon. Not. R. Astron. Soc.

119

123

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“…The only neutral high-velocity structure in the Galactic CGM that clearly reaches beyond 30 kpc distance is the MS, a massive stream (10 8 − 10 9 M ⊙ ) of neutral and ionized gas that originates from the interaction of the two Magellanic Clouds as they approach the Milky Way (Dieter 1971;Wannier & Wrixon 1972;Mathewson et al 1974;D'Onghia & Fox 2016). Our recent studies of the MS based on UV data from FUSE, HST/STIS and HST/COS (Fox et al 2010Richter et al 2013) indicate that the MS contains more gas than the Small and Large Magellanic Clouds, feeding the Milky Way over the next 0.5 − 1.0 Gyr with large amounts of mostly metal-poor gas.…”

Section: Introductionmentioning

confidence: 99%

An HST/COS legacy survey of high-velocity ultraviolet absorption in the Milky Way’s circumgalactic medium and the Local Group

Richter

Nuza

Fox

et al. 2017

A&A

111

131

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Context. The Milky Way is surrounded by large amounts of diffuse gaseous matter that connects the stellar body of our Galaxy with its large-scale Local Group (LG) environment. Aims. To characterize the absorption properties of this circumgalactic medium (CGM) and its relation to the LG we present the so-far largest survey of metal absorption in Galactic high-velocity clouds (HVCs) using archival ultraviolet (UV) spectra of extragalactic background sources. The UV data are obtained with the Cosmic Origins Spectrograph (COS) onboard the Hubble Space Telescope (HST) and are supplemented by 21 cm radio observations of neutral hydrogen. Methods. Along 270 sightlines we measure metal absorption in the lines of Si ii, Si iii, C ii, and C iv and associated H i 21 cm emission in HVCs in the velocity range |vLSR| = 100 − 500 km s −1 . With this unprecedented large HVC sample we were able to improve the statistics on HVC covering fractions, ionization conditions, small-scale structure, CGM mass, and inflow rate. For the first time, we determine robustly the angular two point correlation function of the high-velocity absorbers, systematically analyze antipodal sightlines on the celestial sphere, and compare the HVC absorption characteristics with that of Damped Lyman α absorbers (DLAs) and constrained cosmological simulations of the LG (CLUES project). Results. The overall sky-covering fraction of high-velocity absorption is 77 ± 6 percent for the most sensitive ion in our survey, Si iii, and for column densities log N (Si iii) ≥ 12.1. This value is ∼ 4 − 5 times higher than the covering fraction of 21 cm neutral hydrogen emission at log N (H i) ≥ 18.7 along the same lines of sight, demonstrating that the Milky Way's CGM is multi-phase and predominantly ionized. The measured equivalent-width ratios of Si ii, Si iii, C ii, and C iv are inhomogeneously distributed on large and small angular scales, suggesting a complex spatial distribution of multi-phase gas that surrounds the neutral 21 cm HVCs. We estimate that the total mass and accretion rate of the neutral and ionized CGM traced by HVCs is MHVC ≥ 3.0×10 9 M⊙ and dMHVC/dt ≥ 6.1M⊙ yr −1 , where the Magellanic Stream (MS) contributes with more than 90 percent to this mass/mass-flow. If seen from an external vantage point, the Milky Way disk plus CGM would appear as a DLA that would exhibit for most viewing angles an extraordinary large velocity spread of ∆v ≈ 400 − 800 km s −1 , a result of the complex kinematics of the Milky Way CGM that is dominated by the presence of the MS. We detect a velocity dipole of high-velocity absorption at low/high galactic latitudes that we associate with LG gas that streams to the LG barycenter. This scenario is supported by the gas kinematics predicted from the LG simulations. Conclusions. Our study confirms previous results, indicating that the Milky Way CGM contains sufficient gaseous material to feed the Milky Way disk over the next Gyr at a rate of a few solar masses per year, if the CGM gas can actually reach the MW disk. We dem...

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“…Stanimirovic et al 2000;Kemper et al 2010;Bolatto et al 2011;Matsuura, Woods & Owen 2013). Indeed various gaseous features were created by the interactions of the MCs with each other and with the Milky Way (MW) such as the Magellanic Bridge (MB; Hindman, Kerr & McGee 1963), a common envelope of H I spanning ∼13 kpc in which both the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC) are embedded; the Magellanic Stream, a pure gaseous stream trailing the MCs as they orbit the MW (Mathewson, Cleary & Murray 1974;Nidever et al 2010) connecting both of the MCs with the MW, and the Leading Arm, a mass of high-velocity clouds leading the MCs (Putman 2000).…”

Section: Introductionmentioning

confidence: 99%

The MAGellanic Inter-Cloud (MAGIC) project – II. Slicing up the Bridge

Noël¹,

Conn²,

Read³

et al. 2015

Mon. Not. R. Astron. Soc.

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The origin of the gas in between the Magellanic Clouds (MCs), known as the Magellanic Bridge, has always been the subject of controversy. To shed light into this, we present the results from the MAGellanic Inter-Cloud II (MAGIC II) project aimed at probing the stellar populations in 10 large fields located perpendicular to the main ridge-line of H I in the Inter-Cloud region. We secured these observations of the stellar populations in between the MCs using the WFI (Wide Field Imager) camera on the 2.2 m telescope in La Silla. Using colour-magnitude diagrams, we trace stellar populations across the Inter-Cloud region. In good agreement with MAGIC I, we find significant intermediate-age stars in the Inter-Cloud region as well as young stars of a similar age to the last pericentre passage in between the MCs (∼200 Myr ago). We show here that the young, intermediate-age and old stars have distinct spatial distributions. The young stars correlate well with the H I gas suggesting that they were either recently stripped from the Small Magellanic Cloud (SMC) or formed in situ. The bulk of intermediate-age stars are located mainly in the Bridge region where the H I column density is higher, but they are more spread out than the young stars. They have very similar properties to stars located ∼2 kpc from the SMC centre, suggesting that they were tidally stripped from this region. Finally, the old stars extend to some 8 kpc from the SMC supporting the idea that all galaxies have a large extended metal-poor stellar halo.

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The Magellanic stream

Cited by 330 publications

References 0 publications

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

An HST/COS legacy survey of high-velocity ultraviolet absorption in the Milky Way’s circumgalactic medium and the Local Group

The MAGellanic Inter-Cloud (MAGIC) project – II. Slicing up the Bridge

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