UV Emission Line Study of the Elemental Abundances in the Supernova Remnant Puppis A

Details UV Emission Line Study of the Elemental Abundances in the Supernova Remnant Puppis A UV Emission Line Study of the Elemental Abundances in the Supernova Remnant Puppis A

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1807f&link_type=abstract

IUE Proposal ID #NFGRF

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The southern hemisphere nebula known as Puppis A is a suspected young supernova remnant (SNR). Optically the remnant consists of short bright filamentary arcs and knots whose spectra indicate high nitrogen and oxygen enrichment, velocity dispersions of 150-200 km s^1, and radial velocities of several hundred km s^-1. X-ray observations via Einstein Observatory so suggest heavy element overabundance with the ratios of O/Fe and Ne/Fe 3 to 5 times cosmic values. These data point to a relatively young SNR probably from a Type II event which may be similar to an older CAS A. Puppis A offers an excellent target for studying the UV emission lines from Type II remnants. While other chemical rich and likely Type II SNRs e.g. CAS A, N132D, G292 + 1.8 and the remnant in NGC 4449 have very faint emission filaments or are too highly reddened, Puppis A's filaments are relatively bright with low foreground extinction [E(B-V) 4 0.21. Because many strong and higher ionization emission lines fall in the ultraviolet spectral region (e.g. C II, C III, C IV, O III, Si III, Si IV), obtaining UV spectra of Puppis A's filaments is highly desirable. We propose, therefore, to obtain low dispersion long and short wavelength spectra of three of Puppis A's brightest optical filaments. Our objectives are: 1) to measure relative line intensities, 2) estimate shock velocities and densities using shock model analysis, and 3) investigate the elemental abundances and variations in the chemically peculiar remnant.

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