Chemical compositions of four B-type  supergiants in the SMC wing

Lee, J.K.; Rolleston, W. R. J.; Dufton, P. L.; Ryans, R.

doi:10.1051/0004-6361:20041345

Cited by 52 publications

(62 citation statements)

References 20 publications

(32 reference statements)

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“…The column density of the SMC wing component was determined in the spectral fit assuming a low metallicity (reduced compared to the galactic metallicity by −0.5 dex, cf. Lee et al 2005) consistent with other findings. From a 21-cm Parkes map of the SMC field a column of neutral hydrogen of 1.06 × 10 21 cm −2 was inferred in the direction of RX J0209.6−7427 (Brüns et al 2001).…”

Section: X-ray Outburstssupporting

confidence: 92%

Discovery of an X-ray binary in the outer SMC wing

Kahabka

Hilker

2005

A&A

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Abstract. The discovery of an X-ray binary RX J0209.6−7427 in the outer wing of the SMC is reported from two archival ROSAT PSPC observations. The data show variability in the X-ray light curve with a timescale of ∼40 days that probably is related to the binary orbital period of the system. A V = 14 mag star in the X-ray error circle of the source is the likely optical counterpart. The optical spectrum of the star shows Hα emission with an equivalent width of −10.8 ± 0.2 Å. The spectral type of the star is constrained as B0-B1.5IV-Ve and consistent with that of a Be star. RX J0209.6−7427 is therefore a Be-type X-ray binary. The mean X-ray luminosity of the source is derived to be ∼1.0 × 10 38 erg s −1 (for a distance of 60 kpc), which is comparable to luminosities derived for Be-type X-ray binaries in the body of the SMC. This makes RX J0209.6−7427 the first candidate Be-type X-ray binary discovered in the outer SMC wing that directly extends into the Magellanic Bridge. This finding is consistent with the existence of a young (∼10-30 Myr) stellar population in the outer region of the SMC wing. Star formation due to an encounter of the SMC with the LMC and the Magellanic system with the Galaxy may explain this likely high-mass X-ray binary in an area far from the main body of the SMC.

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Section: X-ray Outburstssupporting

confidence: 92%

Discovery of an X-ray binary in the outer SMC wing

Kahabka

Hilker

2005

A&A

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“…This is similar to the SMC Body gas-to-dust ratio (Bot et al 2004) and indicates that the SMC Tail material has been recently stripped from the SMC Body. This agrees with the measured metallicities of stars in the SMC Tail (Lee et al 2005) and numerical simulations (Connors et al 2006). The SAGE-SMC observations show a number of point sources in the SMC Tail detected at 24, 70, & 160 μm.…”

Section: Status Of Observationssupporting

confidence: 89%

Early results from the SAGE-SMC Spitzer legacy

et al. 2008

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Abstract.Early results from the SAGE-SMC (Surveying the Agents of Galaxy Evolution in the tidally-disrupted, low-metallicity Small Magellanic Cloud) Spitzer legacy program are presented. These early results concentrate on the SAGE-SMC MIPS observations of the SMC Tail region. This region is the high H i column density portion of the Magellanic Bridge adjacent to the SMC Wing. We detect infrared dust emission and measure the gas-to-dust ratio in the SMC Tail and find it similar to that of the SMC Body. In addition, we find two embedded cluster regions that are resolved into multiple sources at all MIPS wavelengths.

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“…A revealing indication is that stars closest to Sk 191 investigated by Lee et al (2005) seem to have abundances that more closely match those of stars within the SMC proper, and the same holds for Sk 191 itself (Trundle et al 2004). Moreover, the spectrum of Sk 191 is one of the very few cases where we have a marginal detection of interstellar O I absorption at 1356Å that lines up perfectly at the correct velocity.…”

Section: The Special Cases Of Azv 456 and Sk 191mentioning

confidence: 68%

“…Dynamical simulations by Gardiner & Noguchi (1996) and Hammer et al (2015) suggest that the MB was created by a tidal interaction when the Large and Small Magellanic Clouds collided some 200−300 Myr ago. Several stars embedded in the MB midway between the SMC and LMC show abundances even lower than those in the SMC (Rolleston et al 1999 ;Lee et al 2005 ;Dufton et al 2008), and the results of Lehner et al (2001); indicate that the same holds for gas in this region.…”

Section: The Special Cases Of Azv 456 and Sk 191mentioning

confidence: 99%

Interstellar Gas-phase Element Depletions in the Small Magellanic Cloud: A Guide to Correcting for Dust in QSO Absorption Line Systems^∗

Jenkins

Wallerstein

2017

ApJ

105

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We present data on the gas phase abundances for 9 different elements in the interstellar medium of the Small Magellanic Cloud (SMC), based on the strengths of ultraviolet absorption features over relevant velocities in the spectra of 18 stars within the SMC. From this information and the total abundances defined by the element fractions in young stars in the SMC, we construct a general interpretation on how these elements condense into solid form onto dust grains. As a group, the elements Si, S, Cr, Fe, Ni, and Zn exhibit depletion sequences similar to those in the local part of our Galaxy defined by Jenkins (2009). The elements Mg and Ti deplete less rapidly in the SMC than in the Milky Way, and Mn depletes more rapidly. We speculate that these differences might be explained by the different chemical affinities to different existing grain substrates. For instance, there is evidence that the mass fractions of polycyclic aromatic hydrocarbons (PAHs) in the SMC are significantly lower than those in the Milky Way. We propose that the depletion sequences that we observed for the SMC may provide a better model for interpreting the element abundances in low metallicity Damped Lyman Alpha (DLA) and sub-DLA absorption systems that are recorded in the spectra of distant quasars and gamma ray burst afterglows.

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Chemical compositions of four B-type supergiants in the SMC wing

Cited by 52 publications

References 20 publications

Discovery of an X-ray binary in the outer SMC wing

Discovery of an X-ray binary in the outer SMC wing

Early results from the SAGE-SMC Spitzer legacy

Interstellar Gas-phase Element Depletions in the Small Magellanic Cloud: A Guide to Correcting for Dust in QSO Absorption Line Systems^∗

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Chemical compositions of four B-type supergiants in the SMC wing

Cited by 52 publications

References 20 publications

Discovery of an X-ray binary in the outer SMC wing

Discovery of an X-ray binary in the outer SMC wing

Early results from the SAGE-SMC Spitzer legacy

Interstellar Gas-phase Element Depletions in the Small Magellanic Cloud: A Guide to Correcting for Dust in QSO Absorption Line Systems∗

Contact Info

Product

Resources

About

Interstellar Gas-phase Element Depletions in the Small Magellanic Cloud: A Guide to Correcting for Dust in QSO Absorption Line Systems^∗