Sanders, Nathan E. 2011 SN 2010ay的观测

主要内容:
可能是和伽马暴成协的超新星

精彩摘抄:


文章信息:

· Find Similar Abstracts (with default settings below)

· arXiv e-print (arXiv:1110.2363)

· References in the Article

· Citations to the Article (2) (Citation History)

· Refereed Citations to the Article

· Also-Read Articles (Reads History)

·

· Translate This Page

Title:		SN 2010ay is a Luminous and Broad-lined Type Ic Supernova within a Low-metallicity Host Galaxy
Authors:		Sanders, Nathan E.; Soderberg, A. M.; Valenti, S.; Chomiuk, L.; Berger, E.; Smartt, S.; Hurley, K.; Barthelmy, S. D.; Chornock, R.;Foley, R. J.; Levesque, E. M.; Narayan, G.; Kirshner, R. P.; Botticella, M. T.; Briggs, M. S.; Connaughton, V.; Terada, Y.;Gehrels, N.; Golenetskii, S.; Mazets, E.; Cline, T.; von Kienlin, A.; Boynton, W.; Chambers, K. C.; Grav, T.; Heasley, J. N.;Hodapp, K. W.; Jedicke, R.; Kaiser, N.; Kudritzki, R. -P.; Luppino, G. A.; Lupton, R. H.; Magnier, E. A.; Monet, D. G.; Morgan, J. S.;Onaka, P. M.; Price, P. A.; Stubbs, C. W.; Tonry, J. L.; Wainscoat, R. J.; Waterson, M. F.
Publication:		eprint arXiv:1110.2363
Publication Date:		10/2011
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		18 pages, 10 figures, V2 has minor revisions; more information at https://www.cfa.harvard.edu/~nsanders/papers/2010ay/summary.html
Bibliographic Code:		2011arXiv1110.2363S

Abstract

[abridged] We report on our serendipitous pre-discovery detection and detailed follow-up of the broad-lined Type Ic supernova SN 2010ay at z\approx0.067 imaged by the Pan-STARRS1 3{\pi} survey just \sim3 days after explosion. We estimate the explosion date and the peak luminosity of the SN, MR\approx-20.2 mag, significantly brighter than known GRB-SNe and one of the most luminous SNe Ic ever discovered. We measure the photospheric expansion velocity of the explosion, v_ph\approx19.2x10^3 km/s at \sim40 days after explosion. In comparison with other broad-lined SNe, the characteristic velocity of SN 2010ay is 2-5x higher and similar to the measurements for GRB-SNe at comparable epochs. Moreover the velocity declines two times slower than other SNe Ic-BL and GRB-SNe. Assuming that the optical emission is powered by radioactive decay, the peak magnitude implies the synthesis of an unusually large mass of 56 Ni, M_Ni=0.9+0.2 M_solar. Our modeling of the light-curve points to a total ejecta mass, Mej\approx4.7M_solar, and total kinetic energy, E_K,51\approx11. Thus the ratio of MNi to Mej is at least twice as large for SN 2010ay than in GRB-SNe and may indicate an additional energy reservoir. We also measure the metallicity (log(O/H)+12=8.19) of the explosion site within the host galaxy, placing this SN in the low-metallicity regime populated by GRB-SNe, and \sim 0.2(0.5) dex lower than that typically measured for the host environments of normal (broad-lined) Ic supernovae. Despite striking similarities to the recent GRB-SN 100316D/2010bh, we show that gamma-ray observations rule out an associated GRB with a flux, F_gamma>6x10^-7 erg/cm^2 (25-150 keV). Similarly, our deep radio follow-up observations with the EVLA rule out relativistic ejecta with energy, E>10^48 erg. These observations challenge the importance of progenitor metallicity for the production of a GRB, and suggest that other parameters also play a key role.

---

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)