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J/ApJ/788/30       Gamma-ray burst flares: X-ray flaring        (Swenson+, 2014)

Gamma-ray burst flares: X-ray flaring. II. Swenson C.A., Roming P.W.A. <Astrophys. J., 788, 30 (2014)> =2014ApJ...788...30S (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays ; Stars, flare ; X-ray sources ; Redshifts Keywords: gamma-ray burst: general Abstract: We present a catalog of 498 flaring periods found in gamma-ray burst (GRB) light curves taken from the online Swift X-Ray Telescope GRB Catalogue (Evans et al. 2007A&A...469..379E, 2009, J/MNRAS/397/1177). We analyzed 680 individual light curves using a flare detection method developed and used on our UV/optical GRB Flare Catalog. This method makes use of the Bayesian Information Criterion to analyze the residuals of fitted GRB light curves and statistically determines the optimal fit to the light curve residuals in an attempt to identify any additional features. These features, which we classify as flares, are identified by iteratively adding additional "breaks" to the light curve. We find evidence of flaring in 326 of the analyzed light curves. For those light curves with flares, we find an average number of ∼1.5 flares per GRB. As with the UV/optical, flaring in our sample is generally confined to the first 1000 s of the afterglow, but can be detected to beyond 105 s. Only ∼50% of the detected flares follow the "classical" definition of Δt/t≤0.5, with many of the largest flares exceeding this value. Description: For the purposes of this study, we will use the publicly available XRT light curves from the online Swift-XRT GRB Catalogue (Evans et al. 2007A&A...469..379E; 2009, J/MNRAS/397/1177). We downloaded the light curves for the time period covering 2005 January through 2012 December, as well as the best-fit parameters for each burst. We calculated the light curve residuals using the best-fit parameters and perform our flare-finding analysis on these residuals. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 72 498 X-ray Flares
See also: J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009) J/ApJS/209/20 : Swift GRB catalog with X-ray data (Grupe+, 2013) J/MNRAS/428/729 : GRB Swift X-ray light curves analysis (Margutti+, 2013) J/ApJS/224/20 : 10yr of Swift/XRT obs. of GRBs (Yi+, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1 A1 --- FP [Y/N] Flaring Period observed; Y/N 3- 12 A10 --- Name Source name (GRB YYMMDDA) (1) 14- 19 F6.4 --- z ? Redshift 21- 29 F9.2 s Tpeak Flare peak time (2) 31- 39 F9.2 s Tstart Lower limit on flare start time (2) 41- 50 F10.2 s Tstop Upper limit on flare stop time (2) 52- 57 F6.2 --- Delt/t The (Tstop-Tstart)/Tpeak ratio 59- 65 F7.2 --- FRatio Flux ratio (3) 67- 72 F6.4 --- Conf Confidence measure (4)
Note (1): Flares are listed in chronological order by GRB date, then sorted by confidence. Note (2): Our analysis identifies a specific data point in the light curve as being associated with these quantities. The large number of digits reported for Tpeak, Tstart and Tstop are not reflective of our confidence in their determination, but are rather the timestamp associated with the data point identified. We have chosen not to round these values for two reasons: 1) any rounding decision we make would be arbitrary, and 2) the relative effect of the rounding on each value would differ depending on the size of the value. This also prevents the introduction of an arbitrary bias to the data. All times are relative to the time of the initial burst trigger. Note (3): Calculated as the flux at the flare peak time divided by the extrapolated flux of the underlying light curve at the same time, normalized using the flux of the underlying light curve, and is a lower limit of the actual peak flux ratio. Note (4): Represents the fraction of times the flare was identified during the 10000 Monte Carlo simulations. The first column identifies whether the identified feature comes from an overlapping `flaring period'.
History: From electronic version of the journal References: Swenson et al., Paper I, 2013ApJ...774....2S
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 03-Jul-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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