2012A&A...539A..76O


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.15CET12:45:33

2012A&A...539A..76O - Astronomy and Astrophysics, volume 539A, 76-76 (2012/3-1)

The fast evolution of SN 2010bh associated with XRF 100316D.

OLIVARES E.F., GREINER J., SCHADY P., RAU A., KLOSE S., KRUEHLER T., AFONSO P.M.J., UPDIKE A.C., NARDINI M., FILGAS R., NICUESA GUELBENZU A., CLEMENS C., ELLIOTT J., KANN D.A., ROSSI A. and SUDILOVSKY V.

Abstract (from CDS):

The first observational evidence of a connection between supernovae (SNe) and gamma-ray bursts (GRBs) was found about a decade ago. Since then, only half a dozen spectroscopically confirmed associations have been discovered and XRF 100316D/SN 2010bh is among the latest. We constrain the progenitor radius, the host-galaxy extinction, and the physical parameters of the explosion of XRF 100316D and its associated SN 2010bh at z=0.059. We study the brightness and colours of SN 2010bh in the context of GRB-SNe. We began observations 12h after the GRB trigger and continued until 80 days after the burst. The Gamma-Ray burst Optical and Near-infrared Detector (GROND) provided excellent photometric data of XRF 100316D/SN 2010bh in six filter bands covering a wavelength range from approximately 350 to 1800nm, significantly expanding the pre-existing data set for this event. Combining GROND and Swift data, the early broad-band spectral energy distribution (SED) is modelled with a blackbody and afterglow component attenuated by dust and gas absorption. The temperature and radius evolution of the thermal component are analysed and combined with earlier measurements available from the literature. Templates of SN 1998bw are fitted to the SN itself to directly compare the light-curve properties. Finally, a two-component parametrised model is fitted to the quasi-bolometric light curve, which delivers physical parameters of the explosion. The best-fit models to the broad-band SEDs imply moderate reddening along the line of sight through the host galaxy (AV,host=1.2±0.1mag). Furthermore, the parameters of the blackbody component reveal a cooling envelope at an apparent initial radius of 7x1011cm, which is compatible with a dense wind surrounding a Wolf-Rayet star. A multicolour comparison shows that SN 2010bh is 60-70% as bright as SN 1998bw. It proves to be the most rapidly evolving GRB-SNe to date, reaching maximum brightness at 8-9 days after the burst in the blue bands. Modelling of the quasi-bolometric light curve yields MNi=0.21±0.03M and Mej=2.6±0.2M, typical of values within the GRB-SN population. The kinetic energy is Ek=(2.4±0.7)x1052erg, which is making this SN the second most energetic GRB-SN after SN 1998bw. This supernova has one of the earliest peaks ever recorded and thereafter fades more rapidly than other GRB-SNe, hypernovae, or typical type-Ic SNe. This implies that a thin envelope is possibly expanding at very high velocities and is, therefore, unable to retain the γ-rays that would prolong the duration of the SN event.

Abstract Copyright:

Journal keyword(s): gamma-ray burst: general - gamma-ray burst: individual: XRF 100316D - supernovae: individual: SN 2010bh - supernovae: general

Simbad objects: 40

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Number of rows : 40

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SN 2010ma SN* 00 48 55.35 -34 33 59.5           SNIc 109 1
2 GRB 050824 gB 00 48 56.100 +22 36 32.00 19.66 21.03 20.46     ~ 151 0
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9107 1
4 GRB 041006 gB 00 54 50.17 +01 14 07.0           ~ 184 2
5 SN 2002ap SN* 01 36 23.85 +15 45 13.2   13.11 14.54     SN.Ic-bl 482 1
6 GRB 040924 gB 02 06 22.52 +16 08 48.8           ~ 145 1
7 SN 2009nz SN* 02 26 19.87 -18 57 08.6           SN.? 218 1
8 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SN.Ic-bl 807 1
9 GRB 970228 gB 05 01 46.7 +11 46 53           ~ 623 1
10 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14348 1
11 GRB 060729 gB 06 21 31.850 -62 22 12.69           ~ 241 0
12 GRB 080109 gB 06 31 29.0 +70 37 14           ~ 30 0
13 SN 2010bh SN* 07 10 30.63 -56 15 19.7           SNIc 223 1
14 Anon J071031-5615 G 07 10 31 -56 15.3           ~ 5 0
15 SN 2003lw SN* 08 02 30.1 -39 51 03       20.23   SN.Ic: 498 0
16 SN 2002lt SN* 08 08 59.858 +06 43 37.52           SN.Ic:(~) 334 1
17 GRB 980326 gB 08 36 34.3 -18 51 24           ~ 255 0
18 SN 2008D SN* 09 09 30.625 +33 08 20.16     17.5     SNIb 323 1
19 SNLS 04D2dc SN* 10 00 16.681 +02 12 18.52           ~ 29 0
20 SN 2010aq SN* 10 02 09.742 +01 14 00.93           SNIIP 17 1
21 SN 2009bb SN* 10 31 33.92 -39 57 28.2           SNIc 127 1
22 SN 2003dh SN* 10 44 50.030 +21 31 18.15     16.2     SN.IcPec 1097 2
23 SN 2010dh SN* 10 56 37.19 +20 14 41.9           ~ 11 1
24 GRB 011121 gB 11 34 26.67 -76 01 41.6       23.0   ~ 253 1
25 SN 2004aw SN* 11 57 50.24 +25 15 55.1   18.06       SNIc 155 1
26 SN 2008ax SN* 12 30 40.80 +41 38 16.1   23.6 23.5 14.1 22.6 SN.IIb 200 1
27 SN 2010ay SN* 12 35 27.19 +27 04 02.8           SNIc 41 1
28 GRB 050509B gB 12 36 18.000 +29 01 24.00           ~ 269 1
29 SN 1994I SN* 13 29 54.072 +47 11 30.50     12.9     SNIc 557 1
30 GRB 020405 gB 13 58 03.12 -31 22 22.2   21.9 21.5     ~ 231 1
31 GRB 050525A gB 18 32 32.560 +26 20 22.34 14.19 15.17 13.91     SN.Ic: 342 1
32 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1616 2
33 ESO 184-82 G 19 35 04.416 -52 50 38.04   15.17   14.26   ~ 96 2
34 GRB 090618 gB 19 36 01.80 +78 21 07.1           ~ 262 0
35 GRB 060614 gB 21 23 32.140 -53 01 36.10 18.89 20.12 19.54     ~ 490 1
36 GRB 060505 gB 22 07 03.440 -27 48 51.89           ~ 215 1
37 SN 2008hw SN* 22 39 50.39 -40 08 49.1           SNIc 137 1
38 GRB 020903 gB 22 48 42.34 -20 46 09.3           ~ 211 1
39 GRB 050709 gB 23 01 26.960 -38 58 39.50           ~ 247 1
40 XRF 100316D gB ~ ~           ~ 24 0

    Equat.    Gal    SGal    Ecl

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2019.11.15-12:45:33

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