Magellanic-Cloud-Type Interstellar Dust Along Low Density Sightlines in the Galaxy

Details Magellanic-Cloud-Type Interstellar Dust Along Low Density Sightlines in the Galaxy Magellanic-Cloud-Type Interstellar Dust Along Low Density Sightlines in the Galaxy

2000-03-20

arxiv.org/abs/astro-ph/0003285v1

Astrophys.J.Suppl. 129 (2000) 147-158

Astronomy and Astrophysics

Astrophysics

12 pages, ApJS, in press (Aug 2000)

Scientific paper

10.1086/313419

We have studied the UV extinction properties along 30 Galactic sightlines using data from the International Ultraviolet Explorer (IUE) archive that have never been previously examined. These distant (d > 1 kpc) sightlines were selected to investigate the distribution and physical conditions of gas located in low density regions of the Galactic disk and halo. The average densities along these sightlines are extremely low. It is likely that they are dominated by the warm intercloud medium and have little contribution from the cold cloud medium. We find that a subsample of these sightlines has extinction curves with weak bumps and very steep far-UV extinction reminiscent of the Magellanic clouds. These sightlines all lie in the region bounded by 325 < l < 0 and -5 > b > -11. The gas along these sightlines shows forbidden velocities which may indicate that the dust has been subject to shocks. This type of low density sightline may mimic the environments found in the Magellanic Clouds. Large values of N(Ca II)/N(Na I) indicating low depletion are associated with steep far-UV extinction. A possible correlation exists between decreasing bump strength and increasing far-UV steepness for extinction curves in the Galaxy and the Magellanic Clouds.

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