Relativistic ejecta from XRF 060218 and the rate of cosmic explosions

Details Relativistic ejecta from XRF 060218 and the rate of cosmic explosions Relativistic ejecta from XRF 060218 and the rate of cosmic explosions

2006-04-18

arxiv.org/abs/astro-ph/0604389v3

Nature 442:1014-1017,2006

Astronomy and Astrophysics

Astrophysics

To appear in Nature on August 31 2006 (15 pages, 3 figures, 1 table, including Supplementary Information)

Scientific paper

10.1038/nature05087

Over the last decade, long-duration gamma-ray bursts (GRBs) including the subclass of X-ray flashes (XRFs) have been revealed to be a rare variety of Type Ibc supernova (SN). While all these events result from the death of massive stars, the electromagnetic luminosities of GRBs and XRFs exceed those of ordinary Type Ibc SNe by many orders of magnitude. The essential physical process that causes a dying star to produce a GRB or XRF, and not just an SN, remains the crucial open question. Here we present radio and X-ray observations of XRF 060218 (associated with SN 2006aj), the second nearest GRB identified to-date, which allow us to measure its total energy and place it in the larger context of cosmic explosions. We show that this event is 100 times less energetic but ten times more common than cosmological GRBs. Moreover, it is distinguished from ordinary Type Ibc SNe by the presence of 10^48 erg coupled to mildly-relativistic ejecta, along with a central engine (an accretion-fed, rapidly rotating compact source) which produces X-rays for weeks after the explosion. This suggests that the production of relativistic ejecta is the key physical distinction between GRBs/XRFs and ordinary SNe, while the nature of the central engine (black hole or magnetar) may distinguish typical bursts from low-luminosity, spherical events like XRF 060218.

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