2006A&A...460..415P


Query : 2006A&A...460..415P

2006A&A...460..415P - Astronomy and Astrophysics, volume 460, 415-424 (2006/12-3)

Multi-wavelength afterglow observations of the high redshift GRB 050730.

PANDEY S.B., CASTRO-TIRADO A.J., McBREEN S., PEREZ-RAMIREZ M.D., BREMER M., GUERRERO M.A., SOTA A., COBB B.E., JELINEK M., DE UGARTE POSTIGO A., GOROSABEL J., GUZIY S., GUIDORZI C., BAILYN C.D., MUNOZ-DARIAS T., GOMBOC A., MONFARDINI A., MUNDELL C.G., TANVIR N., LEVAN A.J., BHATT B.C., SAHU D.K., SHARMA S., BOGDANOV O. and COMBI J.A.

Abstract (from CDS):

GRB 050730 is a long duration high-redshift burst (z=3.967) that was discovered by Swift. The afterglow shows variability and was well monitored over a wide wavelength range. We present comprehensive temporal and spectral analysis of the afterglow of GRB 050730 including observations covering the wavelength range from the millimeter to X-rays. We use multi-wavelength afterglow data to understand the complex temporal and spectral decay properties of this high redshift burst. Five telescopes were used to study the decaying afterglow of GRB 050730 in the B, V, r', R, i', I, J and K photometric pass bands. A spectral energy distribution was constructed at 2.9h post-burst in the B, V, R, I, J and K bands. X-ray data from the satellites Swift and XMM-Newton were used to study the afterglow evolution at higher energies. The early afterglow shows variability at early times and the slope steepens at 0.1-days (8.6ks) in the B, V, r', R, i', I, J and K passbands. The early afterglow light curve decayed with a powerlaw slope index α1=-0.60±0.07 and subsequently steepened to α2=-1.71±0.06 based on the R and I band data. A millimeter detection of the afterglow around 3-days after the burst shows an excess in comparison to theoretical predictions. The early X-ray light curve observed by Swift is complex and contains flares. At late times the X-ray light curve can be fit by a powerlaw decay with αx=-2.5±0.15 which is steeper than the optical light curve. A spectral energy distribution (SED) was constructed at ∼2.9h after the burst. An electron energy index, p, of ∼2.3 was calculated using the SED and the photon index from the X-ray afterglow spectra and implies that the synchrotron cooling frequency νc is above the X-ray band.

Abstract Copyright:

Journal keyword(s): gamma ray: bursts - techniques: photometric

Nomenclature: Table 3: [PCM2006] NN (Nos 1-10).

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 GRB 021004 gB 00 26 54.68 +18 55 41.6           ~ 537 0
2 GRB 050904 gB 00 54 50.794 +14 05 09.42           ~ 459 0
3 GRB 050319 gB 10 16 47.900 +43 32 53.80   18.02 17.01     ~ 252 0
4 GRB 000528 gB 10 45 08.0 -33 59 26           ~ 29 0
5 PG 1323-086 HS* 13 25 39.4669501176 -08 49 19.067387484 12.660 13.341 13.481 13.529 13.608 sdB3IHe8 139 1
6 [PCM2006] 1 * 14 08 10.90 -03 46 40.2   15.56 15.15 14.92 14.42 ~ 1 0
7 [PCM2006] 9 * 14 08 11.5652140632 -03 44 37.054728060   17.94 17.30 16.94 16.29 ~ 1 0
8 [PCM2006] 8 * 14 08 14.5243523280 -03 44 42.486131616   18.24 17.51 17.05 16.33 ~ 1 0
9 [PCM2006] 2 * 14 08 14.6257610184 -03 46 28.332922116   18.59 18.06 17.77 17.17 ~ 1 0
10 GRB 050730 gB 14 08 17.090 -03 46 18.90   20.32 17.68     ~ 303 0
11 [PCM2006] 3 * 14 08 17.20 -03 46 36.1   20.04 18.94 18.26 17.22 ~ 1 0
12 [PCM2006] 7 * 14 08 18.3371756016 -03 44 46.664370600   18.48 17.72 17.27 16.54 ~ 1 0
13 [PCM2006] 6 * 14 08 18.6671625864 -03 49 14.621417688   16.2 15.70 15.41 14.83 ~ 1 0
14 [PCM2006] 4 * 14 08 19.40 -03 45 43.9   19.58 19.02 18.67 17.95 ~ 1 0
15 [PCM2006] 5 * 14 08 22.0192525848 -03 48 16.915393188   17.24 16.11 15.44 14.50 ~ 1 0
16 [PCM2006] 10 * 14 08 26.7754987512 -03 46 51.773459844   17.27 16.56 16.15 15.49 ~ 1 0
17 GRB 010222 G 14 52 12.5 +43 01 06           ~ 347 1
18 GRB 000301C gB 16 20 18.5 +29 26 35           ~ 351 0
19 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 779 0

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2023.06.04-16:46:08

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