Revealing the Explosion Geometry of Nearby GRB-SNe

Details Revealing the Explosion Geometry of Nearby GRB-SNe Revealing the Explosion Geometry of Nearby GRB-SNe

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007hst..prop11161s&link_type=abstract

HST Proposal ID #11161. Cycle 16

Computer Science

Scientific paper

The connection between gamma-ray bursts and Type Ibc supernovae is well-established in broad terms. However, our recent identification of an intermediate class of sub-energetic GRBs, and the overall overlap in Nickel production between GRB-SNe and ordinary SNe Ibc suggest that the properties leading to the production of a relativistic engine are yet to be uncovered. A fundamental difference between the two classes of explosions may be imprinted in the overall geometry of the explosion. The relativistic component of GRBs is known to be highly collimated, but it is unclear if the SN blast is spherical or mildly collimated as well. Here we propose HST observations of the late >30 days decay tails of two GRB-SNe as an independent measure of the Nickel mass synthesized in the explosion. A comparison to the Nickel mass inferred from the peak brightness of the SNe will provide a direct measure of the explosion asymmetry, since at late time the explosion is essentially spherical. These observations will form the core of a multi-wavelength optical, X-ray, radio effort to fully characterize all aspects of the explosions, from the energy and geometry of the relativistic material VLA, Chandra to the early SN evolution Keck, Magellan. The proposed observations require two slow-response >30 days TOOs, ideally suited to the 2-gyro operations of HST.;

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