2004MNRAS.351L..78F


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.31CET12:52:23

2004MNRAS.351L..78F - Mon. Not. R. Astron. Soc., 351, L78-L82 (2004/July-1)

Prediction on the very early afterglow of X-ray flashes.

FAN Y.Z., WEI D.M. and WANG C.F.

Abstract (from CDS):

In the past two years, tremendous progress in understanding X-ray flashes has been made. Now it is widely believed that X-ray flashes and gamma-ray bursts are intrinsically the same, and that their very different peak energy and flux may be merely due to our different viewing angles to them. Here we analytically calculate the very early afterglow of X-ray flashes, i.e. the reverse shock emission powered by the outflows interacting with the interstellar medium. Assuming z ∼ 0.3, we have shown that typically the R-band flux of reverse shock emission can be bright to ∼16-17th magnitude (the actual values are model-dependent and sensitive to the initial Lorentz factor of the viewed ejecta). That emission is bright enough to be detected by the telescope on work today such as Robotic Optical Transient Search Experiment (ROTSE-III) or the upcoming Ultraviolet and Optical Telescope (UVOT) carried by the Swift satellite, planned for launch in late 2004.

Abstract Copyright: 2004 RAS

Journal keyword(s): radiation mechanisms: non-thermal - gamma-rays: bursts - X-rays: general

Simbad objects: 4

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Number of rows : 4

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 2002lt SN* 08 08 59.858 +06 43 37.52           SNIc: 338 1
2 GRB 990123 gB 15 25 29 +44 45.0     8.95     ~ 964 1
3 GRB 030723 gB 21 49 24.40 -27 42 47.4           ~ 120 0
4 GRB 020903 gB 22 48 42.34 -20 46 09.3           ~ 215 1

    Equat.    Gal    SGal    Ecl

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2020.10.31-12:52:23

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