2014A&A...566A.102S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST18:57:14

2014A&A...566A.102S - Astronomy and Astrophysics, volume 566A, 102-102 (2014/6-1)

GRB 120422A/SN 2012bz: Bridging the gap between low- and high-luminosity gamma-ray bursts.

SCHULZE S., MALESANI D., CUCCHIARA A., TANVIR N.R., KRUEHLER T., DE UGARTE POSTIGO A., LELOUDAS G., LYMAN J., BERSIER D., WIERSEMA K., PERLEY D.A., SCHADY P., GOROSABEL J., ANDERSON J.P., CASTRO-TIRADO A.J., CENKO S.B., DE CIA A., ELLERBROEK L.E., FYNBO J.P.U., GREINER J., HJORTH J., KANN D.A., KAPER L., KLOSE S., LEVAN A.J., MARTIN S., O'BRIEN P.T., PAGE K.L., PIGNATA G., RAPAPORT S., SANCHEZ-RAMIREZ R., SOLLERMAN J., SMITH I.A., SPARRE M., THOENE C.C., WATSON D.J., XU D., BAUER F.E., BAYLISS M., BJOERNSSON G., BREMER M., CANO Z., COVINO S., D'ELIA V., FRAIL D.A., GEIER S., GOLDONI P., HARTOOG O.E., JAKOBSSON P., KORHONEN H., LEE K.Y., MILVANG-JENSEN B., NARDINI M., NICUESA GUELBENZU A., OGURI M., PANDEY S.B., PETITPAS G., ROSSI A., SANDBERG A., SCHMIDL S., TAGLIAFERRI G., TILANUS R.P.J., WINTERS J.M., WRIGHT D. and WUYTS E.

Abstract (from CDS):

At low redshift, a handful of gamma-ray bursts (GRBs) have been discovered with luminosities that are substantially lower (Liso≲1048.5erg/s) than the average of more distant ones (Liso>1049.5erg/s). It has been suggested that the properties of several low-luminosity (low-L) GRBs are due to shock break-out, as opposed to the emission from ultrarelativistic jets. This has led to much debate about how the populations are connected. The burst at redshift z=0.283 from 2012 April 22 is one of the very few examples of intermediate-L GRBs with a γ-ray luminosity of Liso∼1049.6–49.9erg/s that have been detected up to now. With the robust detection of its accompanying supernova SN 2012bz, it has the potential to answer important questions on the origin of low- and high-L GRBs and the GRB-SN connection. We carried out a spectroscopy campaign using medium- and low-resolution spectrographs with 6-10-m class telescopes, which covered a time span of 37.3-days, and a multi-wavelength imaging campaign, which ranged from radio to X-ray energies over a duration of ∼270-days. Furthermore, we used a tuneable filter that is centred at Hα to map star-formation in the host and the surrounding galaxies. We used these data to extract and model the properties of different radiation components and fitted the spectral energy distribution to extract the properties of the host galaxy. Modelling the light curve and spectral energy distribution from the radio to the X-rays revealed that the blast wave expanded with an initial Lorentz factor of Γ0∼50, which is a low value in comparison to high-L GRBs, and that the afterglow had an exceptionally low peak luminosity density of ≲2x1030erg/s/Hz in the sub-mm. Because of the weak afterglow component, we were able to recover the signature of a shock break-out in an event that was not a genuine low-L GRB for the first time. At 1.4hr after the burst, the stellar envelope had a blackbody temperature of kBT∼16eV and a radius of ∼7x1013cm (both in the observer frame). The accompanying SN 2012bz reached a peak luminosity of MV=-19.7mag, which is 0.3mag more luminous than SN 1998bw. The synthesised nickel mass of 0.58M, ejecta mass of 5.87M, and kinetic energy of 4.10x1052erg were among the highest for GRB-SNe, which makes it the most luminous spectroscopically confirmed SN to date. Nebular emission lines at the GRB location were visible, which extend from the galaxy nucleus to the explosion site. The host and the explosion site had close-to-solar metallicity. The burst occurred in an isolated star-forming region with an SFR that is 1/10 of that in the galaxy's nucleus. While the prompt γ-ray emission points to a high-L GRB, the weak afterglow and the low Γ0 were very atypical for such a burst. Moreover, the detection of the shock break-out signature is a new quality for high-L GRBs. So far, shock break-outs were exclusively detected for low-L GRBs, while GRB 120422A had an intermediate Liso of ∼1049.6–49.9erg/s. Therefore, we conclude that GRB 120422A was a transition object between low- and high-L GRBs, which supports the failed-jet model that connects low-L GRBs that are driven by shock break-outs and high-L GRBs that are powered by ultra-relativistic jets.

Abstract Copyright:

Journal keyword(s): gamma-ray burst: individual: GRB 120422A - supernovae: individual: SN 2012bz - dust, extinction - galaxies: ISM - galaxies: individual: GRB 120422A

Simbad objects: 41

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Number of rows : 41

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 116 1
2 SN 2002ap SN* 01 36 23.85 +15 45 13.2   13.11 14.54     SNIc-BL 491 1
3 SN 2009nz SN* 02 26 19.87 -18 57 08.6           ~ 226 1
4 SN 2013ez SN* 02 53 56.70 +13 23 13.6           ~ 72 0
5 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3545 3
6 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SNIc-BL 828 1
7 SN 2012ap SN* 05 00 13.72 -03 20 51.2           SNIc 55 2
8 GRB 050826 gB 05 51 01.590 -02 38 35.40           ~ 109 0
9 GRB 060729 gB 06 21 31.850 -62 22 12.69           ~ 247 0
10 SN 2010bh SN* 07 10 30.63 -56 15 19.7           SNIc 230 1
11 GRB 070125 gB 07 51 17.80 +31 09 04.8           ~ 155 0
12 SN 2003lw SN* 08 02 30.1 -39 51 03       20.23   SNIc: 506 0
13 GRB 070612 gB 08 05.4 +37 15           ~ 11 0
14 QSO J0854+2006 BLL 08 54 48.8749311881 +20 06 30.642936668   15.91 15.43 15.56   ~ 2000 1
15 SN 2012bz SN* 09 07 38.38 +14 01 07.5           SNIb/c 130 1
16 4C 01.24B QSO 09 09 10.0921832543 +01 21 35.611559836   17.63 17.29 17.04   ~ 368 2
17 SN 2009bb SN* 10 31 33.92 -39 57 28.2           SNIc 134 1
18 SN 2003dh SN* 10 44 50.030 +21 31 18.15     16.2     SNIcpec 1117 2
19 SN 2010dh SN* 10 56 37.19 +20 14 41.9           ~ 11 1
20 SN 2013cq SN* 11 32 32.84 +27 41 56.2           SNIc 378 1
21 SN 2012au SN* 12 54 52.18 -10 14 50.2           SNIb 35 2
22 GRB 080319B gB 14 31 41.04 +36 18 09.2           ~ 421 0
23 GRB 000301C gB 16 20 18.5 +29 26 35           ~ 340 2
24 GRB 991208 gB 16 33 53.51 +46 27 21.5           ~ 243 1
25 GRB 000926 gB 17 04 15 +51 46.0           ~ 341 2
26 GRB 080605 gB 17 28 30.04 +04 00 56.9           ~ 153 0
27 SN 2005nc SN* 18 32 32.560 +26 20 22.34           SNIc: 347 1
28 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1650 2
29 GRB 071003 gB 20 07 24.50 +10 56 48.8           ~ 139 0
30 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 707 0
31 V* V1610 Cyg pA* 21 02 18.27 +36 41 37.0           F5Iae 830 1
32 GRB 060614 gB 21 23 32.140 -53 01 36.10 18.89 20.12 19.54     ~ 507 1
33 GRB 060505 gB 22 07 03.440 -27 48 51.89           ~ 222 1
34 GRB 990712 gB 22 31 53.061 -73 24 28.58           ~ 250 1
35 SN 2008hw SN* 22 39 50.39 -40 08 49.1           SNIc 144 1
36 GRB 020903 gB 22 48 42.34 -20 46 09.3           ~ 215 1
37 GRB 010921 gB 22 55 59.90 +40 55 52.9           ~ 159 1
38 GRB 020819 gB 23 00 12 -43 00.7           ~ 120 1
39 SN 2012eb SN* 23 41 38.35 -46 11 07.0           SNIb/c 39 1
40 SN 2013fu SN* 23 54 29.91 +29 25 47.6           SNIb/c 95 1
41 XRF 100316D gB ~ ~           ~ 25 0

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2020.07.14-18:57:14

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