The nature of the X-ray flash of August 24 2005

Abstract

Aims. Our aim is to investigate the nature of the X-Ray Flash (XRF) of August 24, 2005. Methods. We present comprehensive photometric R-band observations of the fading optical afterglow of XRF 050824, from 11 min to 104 days 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. Results. The R-band lightcurve of the afterglow resembles the lightcurves of long duration Gamma-Ray Bursts (GRBs), i.e., a powerlaw, albeit with a rather shallow slope of α = 0.6 (F ν ∝ t −α ). Our late R-band images reveal the host galaxy. The rest-frame B-band luminosity is ∼0.5 L * . The star-formation rate as determined from the [O II] emission line is ∼1.8 M yr −1 . 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 (θ j > ∼ 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 (F ν ∝ ν −β ) shape with slope β = 0.56 ± 0.04. This can be compared to the X-ray spectral index which is β X = 1.0 ± 0.1. The curvature of the SED constrains the dust reddening towards the burst to A v < 0.5 mag.

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

“…The addition of Swift UVOT data (Schady et al 2005) allows us to create a more detailed SED than that presented by Sollerman et al (2007). From a fit without extinction, we find β 0 = 0.65 ± 0.07, in accordance, within errors, with the value found by Sollerman et al (2007), β 0 = 0.56 ± 0.04. These authors are unable to discern MW, LMC, and SMC extinction, and find A V = 0.4 ± 0.2 mag for SMC dust, albeit with β ≈ 0.…”

“…Clearly, an envelope is seen which traces the correlation found by Panaitescu & Vestrand (2008), but the scatter is much larger than what they find in their small sample, indicating that the significance of the correlation is much smaller than assumed. Applying rank correlation tests, we find Kendall's τ = 0.43 and Spearman's ρ = 0.62, indicating the existence of a correlation 72 Note that some XRFs show a normal, forward-shock-like decay from very early on, e.g., XRF 050406 ) and XRF 050824 (Sollerman et al 2007). (Figure 4).…”

“…We constructed the light curve and the SED with data from the following sources: Sollerman et al (2007), Schady et al (2005), and Lipunov et al (2005). The full light curve analysis (which also finds evidence for a rapid SN) can be found in Sollerman et al (2007).…”

“…We constructed the light curve and the SED with data from the following sources: Sollerman et al (2007), Schady et al (2005), and Lipunov et al (2005). The full light curve analysis (which also finds evidence for a rapid SN) can be found in Sollerman et al (2007). The addition of Swift UVOT data (Schady et al 2005) allows us to create a more detailed SED than that presented by Sollerman et al (2007).…”

“…The full light curve analysis (which also finds evidence for a rapid SN) can be found in Sollerman et al (2007). The addition of Swift UVOT data (Schady et al 2005) allows us to create a more detailed SED than that presented by Sollerman et al (2007). From a fit without extinction, we find β 0 = 0.65 ± 0.07, in accordance, within errors, with the value found by Sollerman et al (2007), β 0 = 0.56 ± 0.04.…”