Dust Properties In Afterglow Of GRB 071025 At z 5

Details Dust Properties In Afterglow Of GRB 071025 At z 5 Dust Properties In Afterglow Of GRB 071025 At z 5

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21914201j&link_type=abstract

American Astronomical Society, AAS Meeting #219, #142.01

Astronomy and Astrophysics

Astronomy

Scientific paper

Core-collapse supernovae (SNe) are suspected to be the dominant source of dust production at high redshift where AGB stars cannot contribute to dust formation. However, some observations indicate that the dust production by SNe is inefficient, which casts doubts on the existence of abundant SNe-dust in the early universe. Perley et al. (2010) previously reported that the afterglow of GRB 071025 - an unusually red GRB at z 5 - shows evidence for the existence of SNe-dust. Although it might be the only high redshift GRB that exhibits compelling evidence for SNe-dust, the result could easily be changed by small systematics in photometry. Thus, we re-examined the extinction properties of GRB 071025 using our own optical/near-infrared data at a different epoch. In addition, we tested various SNe-dust models with different progenitor masses and dust destruction varying ambient gas density to constrain the dust formation mechanisms. By searching for the best-fit model of the spectral energy distribution of the afterglow, we confirm the previous claim that the dust in GRB 071025 is most likely to originate from SNe. We also find that the SNe-dust model of 13 or 25Msol without dust destruction fits the extinction property of GRB 071025 best whereas pair-instability SNe (PISNe) models with a 170Msol progenitor result in poor fits. Our results indicate that, at least in some systems at high redshift, the SNe with intermediate masses within 10 - 30Msol were the main contributors of the dust enrichment, and the dust destruction effect due to reverse shock was negligible.

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