Young SNRs, Nonradiative Shocks, and Cosmic Rays: Measuring the Expansion of SN 1006 and RCW 86

Details Young SNRs, Nonradiative Shocks, and Cosmic Rays: Measuring the Expansion of SN 1006 and RCW 86 Young SNRs, Nonradiative Shocks, and Cosmic Rays: Measuring the Expansion of SN 1006 and RCW 86

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010noao.prop..483w&link_type=abstract

NOAO Proposal ID #2010A-0483

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Scientific paper

This is a proposal to use Mosaic on the Blanco to obtain very deep H(alpha) images of two young supernova remnants (SNRs) in order to study the underlying physics at play in SNR shocks. Through comparison with images from over the past two decades, we will measure proper motions for the Balmer-dominated filaments that surround all of snten and much of rcw, the probable remnant of SN 185. Balmer filaments delineate the present position of the primary shock, and in both SNRs include some regions whose post-shock X-ray emission is synchrotron-dominated, and others where X-rays are primarily thermal. Synchrotron X-rays require a population of TeV electrons, meaning these must be sites where cosmic rays originate. For a remnant at a well- known distance, optical proper motions translate directly into the shock velocity, expected to vary significantly around the SNR rims. Comparing shock velocity with post-shock temperature, which we can determine from spectra (some in hand and some to be proposed), we will measure any energy loss across the shock, and thus assess how much energy has gone into cosmic-ray acceleration. We will also obtain broad-band images of both remnants in order to search for high proper motion stars within the shells that might indicate a possible runaway donor companion to the SN (particularly salient for snten, known to have been a Type Ia SN). We will also use these data to produce spectacular color images of each object that will be valuable for public outreach.

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