Statistics
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21725629m&link_type=abstract
American Astronomical Society, AAS Meeting #217, #256.29; Bulletin of the American Astronomical Society, Vol. 43, 2011
Statistics
Scientific paper
Supernovae (SNe), through their diffuse supernova remnants (SNRs), are primarily responsible for the injection of energy and heavy elements into the interstellar medium (ISM). SNe provide most of the hot gas component of the ISM, singly and through collective inputs to superbubbles (SBs). The energy and heavy elements influence future generations of star formation and profoundly affect galactic evolution. The Magellanic Clouds (MCs) contain SNRs at a wide variety of types, ages, evolutionary stages, and environments. The known, common distances and low obscuration of the MCs allows their SNRs to be studied as members of increasingly well-understood populations. Current instruments, such as the Chandra and XMM X-ray satellites and the Hubble and Spitzer Space Telescopes, have allowed high-resolution studies comparable to those for Galactic SNRs. Surveys of the MCs with the Australia Telescope Compact Array in radio, and the Magellanic Clouds Emission-Line Survey at CTIO, provide a wealth of data on these objects.
As part of a long-term multi-wavelength study of SNRs in the MCs, we have collaborated on a database of the Magellanic Cloud SNRs. This database serves to gather information, images and data on these SNRs (where possible from self-consistent datasets) for use as a general reference. In this poster we present the current state of the database, updated with new measurements from radio surveys.
We also provide our guidelines for SNR nomenclature, identification, and classification; as well as some preliminary statistics for SNR types, diameters, radio and X-ray luminosities, and other useful indicators.
The authors thank NASA's LTSA grant NNX08AM54G for support of this long-term project.
Chu Yan-Yi
Dickel John R.
Edwards Zachary
Johnson Michael D.
Lodder K.
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