Loading...
Please wait, while we are loading the content...
Similar Documents
Sn 2010ay is a luminous and broad-lined type ic supernova within a low-metallicity host galaxy
| Content Provider | NASA Technical Reports Server (NTRS) |
|---|---|
| Author | Berger, E. Heasley, J. N. Connaughton, V. Terada, Y. Foley, R. J. Chornock, R. Valenti, S. Narayan, G. Chomiuk, L. Grav, T. Soderberg, A. M. Mazets, E. Briggs, M. S. von Kienlin, A. Chambers, K. C. Barthelmy, S. D. Cline, T. Smartt, S. Golenetskii, S. Botticella, M. T. Sanders, N. E. Boynton, W. Gehrels, N. Levesque, E. M. Hurley, K. |
| Copyright Year | 2012 |
| Description | We report on our serendipitous pre-discovery detection and follow-up observations of the broad-lined Type Ic supernova (SN Ic) 2010ay at z = 0.067 imaged by the Pan-STARRS1 3pi survey just approximately 4 days after explosion. The supernova (SN) had a peak luminosity, MR approx. -20.2 mag, significantly more luminous than known GRB-SNe and one of the most luminous SNe Ib/c ever discovered. The absorption velocity of SN 2010ay is v Si (is) approx. 19Ã10(exp 3) km sâ1 at approximately 40 days after explosion, 2-5 times higher than other broad-lined SNe and similar to the GRB-SN 2010bh at comparable epochs. Moreover, the velocity declines approximately 2 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 56Ni, MNi = 0.9 solar mass. Applying scaling relations to the light curve, we estimate a total ejecta mass, Mej (is) approx. 4.7 solar mass, and total kinetic energy, EK (is) approx. 11 Ã 10(exp 51) erg. The ratio of MNi to Mej is approximately 2 times as large for SN 2010ay as typical GRB-SNe and may suggest an additional energy reservoir. The metallicity (log(O/H)PP04 + 12 = 8.19) of the explosion site within the host galaxy places SN 2010ay in the low-metallicity regime populated by GRB-SNe, and (is) approximately 0.5(0.2) dex lower than that typically measured for the host environments of normal (broad-lined) SNe Ic. We constrain any gamma-ray emission with E(gamma) (is) approximately less than 6 Ã 10(exp 48) erg (25-150 keV), and our deep radio follow-up observations with the Expanded Very Large Array rule out relativistic ejecta with energy E (is) approximately greater than 10(exp 48) erg. We therefore rule out the association of a relativistic outflow like those that accompanied SN 1998bw and traditional long-duration gamma-ray bursts (GRBs), but we place less-stringent constraints on a weak afterglow like that seen from XRF 060218. If this SN did not harbor a GRB, these observations challenge the importance of progenitor metallicity for the production of relativistic ejecta and suggest that other parameters also play a key role. |
| File Size | 462533 |
| Page Count | 16 |
| File Format | |
| Alternate Webpage(s) | http://archive.org/details/NASA_NTRS_Archive_20150008395 |
| Archival Resource Key | ark:/13960/t3wt3p77w |
| Language | English |
| Publisher Date | 2012-08-27 |
| Access Restriction | Open |
| Subject Keyword | Supernovae: Individual (2010ay) Supernovae: General Gamma-ray Burst: General Gamma Rays Light Emission Galaxies Afterglows Supernovae Very Large Array Vla Luminosity Light Curve Time Measurement Radioactive Decay Gamma Ray Bursts Radio Observation Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science |
| Content Type | Text |
| Resource Type | Article |
