2005/11/21 by F. D. Seward, R. M. Williams, Y. -H. Chu +4
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Cosmic Phenomena #Gamma-ray bursts and supernovae #H II region #Large Magellanic Cloud #Ridge #Spectral line #Supernova #Supernova remnant #astro-ph
paper · pdf · doi:10.1086/499767
published as Astrophys.J.640:327-334,2006 · AASTeX, 20 pages including 5 figures. Accepted for publication in The Astrophysical Journal. Figures have been reduced in resolution for space requirements; full-resolution figures may be requested by email to [email protected]
arxiv created 2005/11/21 · openalex publication_date 2006/03/13 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
A Chandra observation has defined the extent of the SNR 0454-67.2 in the LMC H II region N9. The remnant has dimension 2 3 × 3 6 and is elongated in the north-south direction. The brightest emission comes from a north-south central ridge that includes three bright patches. There is good agreement between X-ray and [O III] and [S II] morphology. The remnant is old enough so that optical data give more information about dynamics than do the X-ray data. The supernova (SN) energy release was ≥5 × 10 50 ergs, and the age is ~3 × 10 4 yr. There are several unresolved sources nearby, but none are clearly associated with the remnant. The X-ray spectrum is soft and indicates enhanced Fe abundance in the central region, consistent with a Type Ia SN origin, but a Type II origin cannot be ruled out.