The Energetics and Host Galaxies of X-Ray Flashes

Details The Energetics and Host Galaxies of X-Ray Flashes The Energetics and Host Galaxies of X-Ray Flashes

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003cxo..prop.1474f&link_type=abstract

Chandra Proposal ID #05500900

Mathematics

Logic

Chandra Proposal Id #05500900

Scientific paper

The X-ray flashes (XRFs) occur at the cosmological distances of gamma-ray bursts (GRBs), but possess a non-thermal prompt emission spectrum that peaks in the X-ray (0.1 keV < E < 20 keV) rather than the gamma-ray band. With roughly the same energy release as GRBs and supernovae, the XRFs appear to couple an intermediate fraction of their energy to highly relativistic ejecta. After the XRFs were identified as a distinct class in 2001, we discovered the first three XRF afterglows and their likely host galaxies. Chandra observations of HETE-2 XRF positions will localize more such events and enable measurement of their energetics via the luminosity of the X-ray afterglow. These observations will help clarify the nature of the XRFs, the most likely link between GRBs and supernovae.

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