Far-Ultraviolet Cooling Features of the Antlia Supernova Remnant

Abstract

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.

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

References in corpus (7)

• The SPEAR Instrument and On-Orbit Performance
• The Spectroscopy of Plasma Evolution from Astrophysical Radiation Mission
• Far-Ultraviolet & Halpha Spectroscopy of SNR0057-7226 in the SMC HII Region N66
• Simulations of Mixed Morphology Supernova Remnants With Anisotropic Thermal Conduction
• Far-UV Observations of a Thermal Interface in the Orion-Eridanus Superbubble
• SPEAR Far Ultraviolet Spectral Images of the Cygnus Loop
• Far-ultraviolet Observations of the North Ecliptic Pole with SPEAR

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