2007A&A...466..839S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.05CEST07:15:37

2007A&A...466..839S - Astronomy and Astrophysics, volume 466, 839-846 (2007/5-2)

The nature of the X-ray flash of August 24 2005. Photometric evidence for an on-axis z = 0.83 burst with continuous energy injection and an associated supernova?

SOLLERMAN J., FYNBO J.P.U., GOROSABEL J., HALPERN J.P., HJORTH J., JAKOBSSON P., MIRABAL N., WATSON D., XU D., CASTRO-TIRADO A.J., FERON C., JAUNSEN A.O., JELINEK M., JENSEN B.L., KANN D.A., OVALDSEN J.E., POZANENKO A., STRITZINGER M., THOENE C.C., DE UGARTE POSTIGO A., GUZIY S., IBRAHIMOV M., JAERVINEN S.P., LEVAN A., RUMYANTSEV V. and TANVIR N.

Abstract (from CDS):

Our aim is to investigate the nature of the X-Ray Flash (XRF) of August 24, 2005. We present comprehensive photometric R-band observations of the fading optical afterglow of XRF050824, from 11min to 104days after the burst. In addition we present observations taken during the first day in the BRIK bands and two epochs of spectroscopy. We also analyse available X-ray data. The R-band lightcurve of the afterglow resembles the lightcurves of long duration Gamma-Ray Bursts (GRBs), i.e., a power-law, albeit with a rather shallow slope of α=0.6(Fν ∝t–α). Our late R-band images reveal the host galaxy. The rest-frame B-band luminosity is ∼0.5L*. The star-formation rate as determined from the [OII] emission line is ∼1.8M/yr. When accounting for the host contribution, the slope is α=0.65±0.01 and a break in the lightcurve is suggested. A potential lightcurve bump at 2 weeks can be interpreted as a supernova only if this is a supernova with a fast rise and a fast decay. However, the overall fit still shows excess scatter in the lightcurve in the form of wiggles and bumps. The flat lightcurves in the optical and X-rays could be explained by a continuous energy injection scenario, with an on-axis viewing angle and a wide jet opening angle (θj>10°). If the energy injections are episodic this could potentially help explain the bumps and wiggles. Spectroscopy of the afterglow gives a redshift of z=0.828±0.005 from both absorption and emission lines. The spectral energy distribution (SED) of the afterglow has a power-law (Fν∝ν–β) shape with slope β=0.56±0.04. This can be compared to the X-ray spectral index which is βX=1.0±0.1. The curvature of the SED constrains the dust reddening towards the burst to Av<0.5mag.

Abstract Copyright:

Journal keyword(s): cosmology: observations - gamma rays: bursts

CDS comments: Fig.1, Table 3: star A = USNO-B1.0 1125-0013373, star B = USNO-B1.0 1125-0013370, star C = USNO-B1.0 1126-0012719, star D = USNO-B1.0 1126-0012735.

Simbad objects: 18

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Number of rows : 18

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 USNO-B1.0 1125-00013370 * 00 48 52.5197390244 +22 35 15.099071092   18.17 17.29 16.83 16.18 ~ 1 0
2 USNO-B1.0 1125-00013373 * 00 48 53.6123500456 +22 35 30.368738059   17.42 16.60 16.18 15.60 ~ 1 0
3 USNO-B1.0 1126-00012719 * 00 48 55.8938693827 +22 37 09.251056088   21.1 20.23 19.14 17.75 ~ 1 0
4 [FJS2005] GRB 050824 abs 0.83 ALS 00 48 56.0 +22 36 32       23.70   ~ 2 0
5 GRB 050824 gB 00 48 56.100 +22 36 32.00 19.66 21.03 20.46     ~ 156 0
6 USNO-B1.0 1126-00012735 * 00 48 59.5536904163 +22 36 53.710638657   21.1 20.66 19.54 17.77 ~ 1 0
7 GRB 000210 gB 01 59 15 -40 40.0           ~ 164 0
8 [LDM2003] GRB J015915.5-403933 G 01 59 15.61 -40 39 33.1           ~ 13 0
9 GRB 050406 gB 02 17 52.200 -50 11 15.81     18.83     ~ 116 0
10 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SNIc-BL 828 1
11 GRB 030429 gB 12 13 07.495 -20 54 49.54           ~ 120 1
12 GRB 050416 gB 12 33 54.600 +21 03 26.69     19.12     ~ 253 1
13 EGGR 327 WD* 16 27 53.4891069739 +09 12 16.023160179 16.008 16.475 16.117 15.899 15.683 DA6.9 88 0
14 GRB 030528 gB 17 04 00.3 -22 37 10           ~ 84 1
15 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1650 2
16 GRB 050315 gB 20 25 54.100 -42 36 02.19           ~ 192 0
17 GRB 030723 gB 21 49 24.40 -27 42 47.4           ~ 120 0
18 GRB 020903 gB 22 48 42.34 -20 46 09.3           ~ 215 1

    Equat.    Gal    SGal    Ecl

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2020.07.05-07:15:37

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