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The Late-time Afterglow Evolution of Long Gamma-Ray Bursts GRB 160625B and GRB 160509A

AuthorsKangas, Tuomas; Fruchter, Andrew S.; Cenko, S. Bradley; Corsi, Alessandra; Ugarte Postigo, Antonio de ; Pe'er, Asaf; Vogel, Stuart N.; Cucchiara, Antonino; Gompertz, Benjamin; Graham, John; Levan, Andrew; Misra, Kuntal; Perley, Daniel A.; Racusin, Judith; Tanvir, Nial
KeywordsGamma-ray bursts
Relativistic jets
Issue Date2020
PublisherIOP Publishing
CitationAstrophysical Journal 894(1): 43 (2020)
AbstractWe present post-jet-break Hubble Space Telescope, Very Large Array, and Chandra observations of the afterglow of the long gamma-ray bursts GRB 160625B (between 69 and 209 days) and GRB 160509A (between 35 and 80 days). We calculate the post-jet-break decline rates of the light curves and find the afterglow of GRB 160625B is inconsistent with a simple t(-3/4) steepening over the break, expected from the geometric effect of the jet edge entering our line of sight. However, the favored optical post-break decline is also inconsistent with the f(nu) proportional to t(-p) decline (where p 2.3 from the pre-break light curve), which is expected from exponential lateral expansion of the jet; perhaps suggesting lateral expansion that only affects a fraction of the jet. The post-break decline of GRB 160509A is consistent with both the t(-3/4) steepening and with f(nu) proportional to t(-p). We also use boxfit to fit afterglow models to both light curves and find both to be energetically consistent with a millisecond magnetar central engine, but the magnetar parameters need to be extreme (i.e., E similar to 3 x 10(52) erg). Finally, the late-time radio light curves of both afterglows are not reproduced well by boxfit and are inconsistent with predictions from the standard jet model; instead, both are well represented by a single power-law decline (roughly f(nu) proportional to t(-1)) with no breaks. This requires a highly chromatic jet break and possibly a two-component jet for both bursts.© 2020. The American Astronomical Society. All rights reserved.
Publisher version (URL)http://dx.doi.org/10.3847/1538-4357/ab8799
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