Assessing the Nature of Extragalactic SNR Candidates

Details Assessing the Nature of Extragalactic SNR Candidates Assessing the Nature of Extragalactic SNR Candidates

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.prop...50d&link_type=abstract

NOAO Proposal ID #2000A-0050

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Scientific paper

Supernova remnants (SNRs) play an important role in driving the evolution of the interstellar medium of a galaxy. Besides the Magellanic Clouds, SNR surveys in other galaxies are limited by poor resolution and sensitivity of X-ray and radio instruments and hence can only be carried out in the optical using the [S II]/H(alpha) ratio. Of the SNR candidates identified at a distance of a few Mpc, ~50% are unresolved, ~20% are larger than 100 pc, and ~50% have only modest [S II]/H(alpha) ratios. These properties suggest that many of the candidates are either not SNRs or are unusual remnants. We request high-dispersion echelle observations of SNR candidates in M 81, M 101, and NGC 6946. These echelle observations, complemented by archival HST WFPC2 H(alpha) and continuum images, will allow us to: (1) measure the expansion velocity and use it to differentiate between bona fide SNRs and superbubbles around OB associations (SNRs have V_exp > 100 km s^-1); (2) determine size, H(alpha) luminosity, mass, and kinetic energy of the confirmed SNRs; (3) use the kinetic energy to identify ``hypernova remnants'', which have explosion energies ~ 10^53-54 erg; (4) use the observed interstellar/circumstellar environment to assess whether or not each remnant had a massive progenitor, and whether the massive progenitor was a WR star or a LBV.

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