Far-Ultraviolet Cooling Features of the Antlia Supernova Remnant

Details Far-Ultraviolet Cooling Features of the Antlia Supernova Remnant Far-Ultraviolet Cooling Features of the Antlia Supernova Remnant

2007-10-08

arxiv.org/abs/0710.1531v2

Astronomy and Astrophysics

Astrophysics

9 pages, 4 figures, will be published in ApJ December 1, 2007, v670n2 issue. see http://astro.snu.ac.kr/~jhshinn/ms.pdf

Scientific paper

10.1086/522219

We present far-ultraviolet observations of the Antlia supernova remnant obtained with Far-ultraviolet IMaging Spectrograph (FIMS, also called SPEAR). The strongest lines observed are C IV 1548,1551 and C III 977. The C IV emission of this mixed-morphology supernova remnant shows a clumpy distribution, and the line intensity is nearly constant with radius. The C III 977 line, though too weak to be mapped over the whole remnant, is shown to vary radially. The line intensity peaks at about half the radius, and drops at the edge of the remnant. Both the clumpy distribution of C IV and the rise in the C IV to C III ratio towards the edge suggest that central emission is from evaporating cloudlets rather than thermal conduction in a more uniform, dense medium.

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