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Observations of the interstellar medium in the Magellanic Bridge | | N. Lehner
; K.R. Sembach
; P.L. Dufton
; W.R.J. Rolleston
; F.P. Keenan
; | | Date: |
31 Dec 2000 | | Subject: | astro-ph | | Affiliation: | 1,2), K.R. Sembach , P.L. Dufton , W.R.J. Rolleston and F.P. Keenan ( The Queen’s University of Belfast, The Johns Hopkins University | | Abstract: | We present ultraviolet and optical spectra of DI 1388, a young star in the Magellanic Bridge, a region of gas between the Small and Large Magellanic Clouds. The data have signal-to-noise ratios of 20 to 45 and a spectral resolution of 6.5 km/s. Interstellar absorption by the Magellanic Bridge at v_LSR = 200 km/s is visible in the lines of C I, C II,C II*, C IV, N I, O I, Al II, Si II, Si III, Si IV, S II, Ca II, Fe II, and Ni II. The relative gas-phase abundances of C II, N I, O I, Al II, Si II, Fe II, and Ni II with respect to S II are similar to those found in Galactic halo clouds, despite a significantly lower metallicity in the Magellanic Bridge. The higher ionization species in the cloud have a column density ratio N(C IV)/N(Si IV) about 1.9, similar to that inferred for collisionally ionized Galactic cloud interfaces at temperatures 10^5 K.We identify sub-structure in the stronger interstellar lines, with a broad component (FWHM = 20 km/s) at 179 km/s and a sharp component (FWHM = 11 km/s) at 198 km/s. The abundance analysis for these clouds indicates that the feature at 198 km/s consists of a low electron density, mainly neutral gas that may be associated with an interface responsible for the highly ionized gas. The 179 km/s cloud consists of warmer, lower density gas that is partially ionized. | | Source: | arXiv, astro-ph/0101548 | | Services: | Forum | Review | PDF | Favorites | |
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