Astronomy and Astrophysics – Astronomy
Scientific paper
May 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...190.4402w&link_type=abstract
American Astronomical Society, 190th AAS Meeting, #44.02; Bulletin of the American Astronomical Society, Vol. 29, p.839
Astronomy and Astrophysics
Astronomy
Scientific paper
N132D is one of two young, oxygen-rich supernova remnants in the LMC, and one of only eight known anywhere. Like their prototype, Cas A, all have filaments composed of nearly pure ejecta from core-collapse supernovae, which have not been decelerated or diluted through interactions with the ISM\@. A kinematic study of the oxygen-rich knots in N132D, using the CTIO 4m and imaging Fabry-Perot spectrograph, showed a roughly shell-like distribution, expanding at ~ 1650 \ km s(-1) , with a center of symmetry blue-shifted by ~ 500 \ km s(-1) \ with respect to the local medium (Morse, et al. 1995, AJ 109, 2104)\@. We have now used the same telescope-instrument combination for a study of N132D in the much fainter coronal [FeXIV] line, lambda 5303\@. Since [FeXIV] arises from 10(6) \ K plasma, its presence indicates material that has been recently excited by primary shocks. Not surprisingly, the [FeXIV] emission correlates well with soft X-ray maps of N132D, but our results have higher spatial resolution as well as being resolved in velocity space. The emission is distributed in two distinct regions: (1) an outer horseshoe of [FeXIV] knots coincides closely with a system of bright but cooler knots seen in Hα \ and low-velocity [OIII], at rest relative to the local medium, and (2) a small inner ring of knots which do not appear prominently in other lines, and which are blue-shifted by ~ 300 \ km s(-1) , almost the same as the center of symmetry of the fast [OIII] system. We suggest that the two regions indicate the positions of the blast wave and the reverse shock, respectively, both of which appear as limb-brightened shells at the different velocities. If this interpretation is correct, the inner [FeXIV] emission may indicate iron from the progenitor core that was mixed with other ejecta in the explosion. This work has been supported by the NSF through grant AST-9315967 and by the W.M. Keck Foundation through the Keck Northeast Astronomy Consortium.
Morse Jon A.
Stamas E. J.
Winkler Frank P.
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