FUSEMeasurements of Far‐Ultraviolet Extinction. II. Magellanic Cloud Sight Lines
- 1 September 2005
- journal article
- research article
- Published by American Astronomical Society in The Astrophysical Journal
- Vol. 630 (1) , 355-367
- https://doi.org/10.1086/431922
Abstract
We present an extinction analysis of nine reddened/comparison star pairs in the Large and Small Magellanic Clouds (LMC and SMC) based on Far-Ultraviolet Spectroscopic Explorer (FUSE) FUV observations. To date, just two LMC sight lines have probed dust grain composition and size distributions in the Magellanic Clouds using spectral data for wavelengths as short as 950 Å. We supplement these two with data from four regions distinguished by their IR through UV extinction curves and grouped as LMCAvg, LMC2, SMC bar, and SMC wing. Despite the distinct characters of extinction in the Clouds and Milky Way, our results are generally analogous to those found for Galactic curves—namely, that the FUSE portions of each extinction curve are described reasonably well by Fitzpatrick & Massa curves fitted only to longer wavelength data and lack any dramatic new extinction features, and any deviations from the Cardelli, Clayton, & Mathis (CCM) formalism continue into FUV wavelengths. A maximum entropy method analysis of all of these curves suggests that LMCAvg and SMC wing sight lines, whose extinction parameters more closely resemble those for Galactic paths, require more silicon and/or carbon in dust than current abundance measurements would indicate are available. The requirements for LMC2 and SMC bar sight lines do not fully tax the available reservoirs, in part because large grains contribute less to the extinction in these directions. An intermediate product of this extinction analysis is the measurement of new H2 abundances in the Magellanic Clouds. Collectively considering Cloud sight lines that possess significant H2 column densities, E(B - V)/N(H ) ratios are reduced by significant factors relative to the Galactic mean, whereas the corresponding E(B - V)/N(H2) values more closely resemble their Galactic counterpart. These trends reflect the fact that among these sight lines f(H2) values are lower than those common in the Milky Way for paths with similar degrees of reddening.Keywords
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This publication has 43 references indexed in Scilit:
- Interstellar Dust GrainsAnnual Review of Astronomy and Astrophysics, 2003
- Dust Grain Size Distributions from MRN to MEMThe Astrophysical Journal, 2003
- Astro-2 Observations of Interstellar Dust and Gas in the Large Magellanic CloudThe Astrophysical Journal, 1996
- Evolution of macromolecular dust: Far-ultraviolet spectral dust extinction and gas absorption of stellar light as measured with the Hopkins Ultraviolet TelescopeThe Astrophysical Journal, 1994
- An IUE survey of interstellar H I LY alpha absorption. 2: InterpretationsThe Astrophysical Journal, 1994
- The relationship between infrared, optical, and ultraviolet extinctionThe Astrophysical Journal, 1989
- An average interstellar extinction curve for the Large Magellanic CloudThe Astronomical Journal, 1986
- Interstellar extinction variations in the Large Magellanic CloudThe Astrophysical Journal, 1985
- Ultraviolet interstellar absorption toward stars in the Small Magellanic Cloud. III - The structure and kinematics of the Small Magellanic CloudThe Astrophysical Journal Supplement Series, 1985
- Interstellar H2 - The population of excited rotational states and the infrared response to ultraviolet radiationThe Astrophysical Journal, 1976