A Low Resolution Hydrogen-line Survey of the Magellanic System. II. Interpretation of Results

Hindman, J. V.; Kerr, F. J.; McGee, R. X.

doi:10.1071/ph630570

Cited by 113 publications

(87 citation statements)

References 9 publications

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“…A continuous H i gas structure between the LMC and the SMC, known as the Magellanic Bridge (MB), was first reported by Hindman et al (1963), and it is found to be at a distance of ∼50-60 kpc (e.g., Harries et al 2003). There is substantial evidence for a young stellar population in the MB, with stars as young as ∼20 Myr (Irwin et al 1985(Irwin et al , 1990Grondin et al 1992;Hambly et al 1994;Demers & Battinelli 1998) and with molecular clouds detected (Lehner 2002;Muller et al 2003;Mizuno et al 2006).…”

Section: Introductionmentioning

confidence: 99%

The Magellanic Bridge as a Damped Lyman Alpha System: Physical Properties of Cold Gas Toward PKS 0312-770

Misawa

Charlton

Kobulnicky

et al. 2009

ApJ

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We measure the physical properties of a local multicomponent absorption-line system at V ∼200 km s −1 toward the quasar PKS 0312-770 behind the Magellanic Bridge (MB) using Hubble Space Telescope Space Telescope Imaging Spectrograph (STIS) spectroscopy in conjunction with photoionization modeling. At an impact parameter of ∼10 kpc from the Small Magellanic Cloud (SMC), this sightline provides a unique opportunity to probe the chemical properties and ionization structure in a nearby absorption line system with a column density of log N H i ∼20.2, at the transition between damped Lyα (DLA) and sub-DLA systems. We find that metallicity of −1.0 < log(Z/Z ) < −0.5 and ionization parameter of −6 < log U < −5 for three low-ionization components and log U ∼ −2.6 for one high-ionization component. One component at V = 207 km s −1 shows an α-element abundance log(Si/H) ∼ −5.0, making it ∼0.2 dex more metal-rich than both SMC H ii regions and stars within the MB and the SMC. The N/Si ratio in this component is log(N/Si) = −0.3 ± 0.1, making it comparable to other N-poor dwarf galaxies and ∼0.2 dex lower than H ii regions in the SMC. Another component at V = 236 km s −1 shows a similar Si/H ratio but has log(N/Si) = −1.0 ± 0.2, indicating a nitrogen deficiency comparable to that seen in the most N-poor DLA systems. These differences imply different chemical enrichment histories between components along the same sightline. Our results suggest that if these absorbers are representative some fraction of DLA systems, then (1) DLA systems along single sightlines do not necessarily represent the global properties of the absorbing cloud, and (2) the chemical composition within a given DLA cloud may be inhomogeneous.

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Section: Introductionmentioning

confidence: 99%

The Magellanic Bridge as a Damped Lyman Alpha System: Physical Properties of Cold Gas Toward PKS 0312-770

Misawa

Charlton

Kobulnicky

et al. 2009

ApJ

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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 profile at each of these points is plotted A striking feature of Figure 13 is the regular splitting into two peaks of the H-line profiles of the Small Magellanic Cloud. A discussion of the phenomenon is given in paper II (Hindman, Kerr, and McGee 1963). …”

Section: (D) Profilesmentioning

confidence: 99%

A Low Resolution Hydrogen-line Survey of the Magellanic System. I. Observations and Digital Reduction Procedures

Hindman¹,

McGee²,

Carter³

et al. 1963

Aust. J. Phys.

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SummaryA survey of neutral hydrogen in the Clouds of Magellan has been made using a digital recording system in conjunction with a multichannel receiver and a 21 ft aerial. The system has been developed for use with the 210 ft radio telescope of the Australian National Radio Astronomy Observatory at Parkes, N.S.W.Digital recording and reduction of the data proved highly successful for the rapid handling of a large amount of data.The results obtained confirm the high gas content of the Magellanic System and also show a considerable amount of gas between the Clouds, appearing to form a bridge.

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A Low Resolution Hydrogen-line Survey of the Magellanic System. II. Interpretation of Results

Cited by 113 publications

References 9 publications

The Magellanic Bridge as a Damped Lyman Alpha System: Physical Properties of Cold Gas Toward PKS 0312-770

The Magellanic Bridge as a Damped Lyman Alpha System: Physical Properties of Cold Gas Toward PKS 0312-770

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

A Low Resolution Hydrogen-line Survey of the Magellanic System. I. Observations and Digital Reduction Procedures

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