Methods and results of an automatic analysis of a complete sample of<i>Swift</i>-XRT observations of GRBs

Evans, P. A.; Beardmore, A. P.; Page, K. L.; Osborne, J. P.; O’Brien, P. T.; Willingale, R.; Starling, R. L. C.; Burrows, D. N.; Godet, O.; Vetere, L.; Racusin, J. L.; Goad, M. R.; Wiersema, K.; Angelini, L.; Capalbi, M.; Chincarini, G.; Gehrels, N.; Kennea, J. A.; Margutti, R.; Morris, David C.; Mountford, C. J.; Pagani, C.; Perri, M.; Romano, P.; Tanvir, N. R.

doi:10.1111/j.1365-2966.2009.14913.x

Cited by 1,519 publications

(1,269 citation statements)

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“…1, together with the monitoring observations provided by Swift/XRT (0.5-10 keV). The latter data were retrieved from the Leicester University on-line analysis tool (Evans et al 2009) and used only to compare the monitoring provided by the Swift and IN-TEGRAL satellites. We refer the reader to Tetarenko et al (2016) for more details on the Swift data and the corresponding analysis.…”

Section: Integralmentioning

confidence: 99%

XMM-Newtonand INTEGRAL view of the hard state of EXO 1745−248 during its 2015 outburst

Matranga

Papitto

Salvo

et al. 2017

A&A

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Context. Transient low-mass X-ray binaries (LMXBs) often show outbursts lasting typically a few-weeks and characterized by a high X-ray luminosity (L x ≈ 10 36 − 10 38 erg s −1 ), while for most of the time they are found in X-ray quiescence (L X ≈ 10 31 − 10 33 erg s −1 ). EXO 1745-248 is one of them. Aims. The broad-band coverage, and the sensitivity of instrumet on board of XMM-Newton and INTEGRAL, offers the opportunity to characterize the hard X-ray spectrum during EXO 1745-248 outburst. Methods. In this paper we report on quasi-simultaneous XMM-Newton and INTEGRAL observations of the X-ray transient EXO 1745-248 located in the globular cluster Terzan 5, performed ten days after the beginning of the outburst (on 2015 March 16th) shown by the source between March and June 2015. The source was caught in a hard state, emitting a 0.8-100 keV luminosity of ≃ 10 37 erg s −1 . Results. The spectral continuum was dominated by thermal Comptonization of seed photons with temperature kT in ≃ 1.3 keV, by a cloud with moderate optical depth τ ≃ 2 and electron temperature kT e ≃ 40 keV. A weaker soft thermal component at temperature kT th ≃ 0.6-0.7 keV and compatible with a fraction of the neutron star radius was also detected. A rich emission line spectrum was observed by the EPIC-pn on-board XMM-Newton; features at energies compatible with K-α transitions of ionized sulfur, argon, calcium and iron were detected, with a broadness compatible with either thermal Compton broadening or Doppler broadening in the inner parts of an accretion disk truncated at 20 ± 6 gravitational radii from the neutron star. Strikingly, at least one narrow emission line ascribed to neutral or mildly ionized iron is needed to model the prominent emission complex detected between 5.5 and 7.5 keV. The different ionization state and broadness suggest an origin in a region located farther from the neutron star than where the other emission lines are produced. Seven consecutive type-I bursts were detected during the XMM-Newton observation, none of which showed hints of photospheric radius expansion. A thorough search for coherent pulsations from the EPIC-pn light curve did not result in any significant detection. Upper limits ranging from a few to 15% on the signal amplitude were set, depending on the unknown spin and orbital parameters of the system.

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Section: Integralmentioning

confidence: 99%

XMM-Newtonand INTEGRAL view of the hard state of EXO 1745−248 during its 2015 outburst

Matranga

Papitto

Salvo

et al. 2017

A&A

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“…9 XRT continued observing the afterglow for 4.7 days in photon counting mode. We extract XRT PC-mode spectra using the online tool on the Swift website (Evans et al 2007(Evans et al , 2009. 10 We downloaded the event and response files generated by the online tool in these time bins, and fit them using the HEASOFT (v6.19) software package and corresponding calibration files.…”

Section: Grb Properties and Observationsmentioning

confidence: 99%

“…Whereas the rapid response of Swift has yielded prompt X-ray afterglow localization and rich X-ray light curves, and ground-based facilities have improved the detection and characterization of optical light curves (Nousek et al 2006;Liang et al 2007Liang et al , 2008Evans et al 2009;Margutti et al 2013;Zaninoni et al 2013), detailed observations of afterglows in the radio and millimeter have resulted in a low detection rate of about 30%, with sensitivity being the primary challenge (Chandra & Frail 2012;de Ugarte Postigo et al 2012).…”

Section: Introductionmentioning

confidence: 99%

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

Laskar

Berger

Chornock

et al. 2018

ApJ

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We present the first results from a recently concluded study of GRBs at z  5 with the Karl G. Jansky Very Large Array (VLA). Spanning 1 to 85.5 GHz and 7 epochs from 1.5 to 82.3 days, our observations of GRB140311A are the most detailed joint radio and millimeter observations of a GRB afterglow at z  5 to date. In conjunction with optical/near-IR and X-ray data, the observations can be understood in the framework of radiation from a single blast wave shock with energy »É 8.5 10 K,iso 53 erg expanding into a constant density environment with density, » n 8 0 -cm 3 . The X-ray and radio observations require a jet break at » t 0.6 jet days, yielding an opening angle of q »  4 jet and a beaming-corrected blast wave kinetic energy of »É 2.2 10 K 50 erg. The results from our radio follow-up and multiwavelength modeling lend credence to the hypothesis that detected high-redshift GRBs may be more tightly beamed than events at lower redshift. We do not find compelling evidence for reverse shock emission, which may be related to fast cooling driven by the moderately high circumburst density.

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“…Another important phenomenon observed by Swift/XRT is the jet break of X-ray afterglow at late time. We use the light curve analysis result from UK Swift Science Data Centre, in which the jet break time is determined to be 1.8 ± 0.5 × 10 6 s (Evans et al 2007(Evans et al , 2009). With the isotropic Energy E γ and the jet break time t j , the half-opening angle of the jet can be estimated by (Sari & Piran 1999;Frail et al 2001):…”

Section: Information From the Afterglowmentioning

confidence: 99%

Evaluating the Bulk Lorentz Factors of Outflow Material: Lessons Learned from the Extremely Energetic Outburst GRB 160625B

Wang

Zhang

et al. 2017

ApJ

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GRB 160625B is an extremely-bright outburst with well-monitored afterglow emission. The geometrycorrected energy is high up to ∼ 5.2 × 10 52 erg or even ∼ 8 × 10 52 erg, rendering it the most energetic GRB prompt emission recorded so far. We analyzed the time-resolved spectra of the prompt emission and found that in some intervals there were likely thermal-radiation components and the high energy emission were characterized by significant cutoff. The bulk Lorentz factors of the outflow material are estimated accordingly. We found out that the Lorentz factors derived in the thermal-radiation model are consistent with the luminosity-Lorentz factor correlation found in other bursts as well as in GRB 090902B for the time-resolved thermal-radiation components. While the spectral cutoff model yields much lower Lorentz factors that are in tension with the constraints set by the electron pair Compoton scattering process. We then suggest that these spectral cutoffs are more likely related to the particle acceleration process and that one should be careful in estimating the Lorentz factors if the spectrum cuts at a rather low energy (e.g., ∼ tens MeV). The nature of the central engine has also been discussed and a stellar-mass black hole is favored.

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Methods and results of an automatic analysis of a complete sample ofSwift-XRT observations of GRBs

Cited by 1,519 publications

References 55 publications

XMM-Newtonand INTEGRAL view of the hard state of EXO 1745−248 during its 2015 outburst

XMM-Newtonand INTEGRAL view of the hard state of EXO 1745−248 during its 2015 outburst

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

Evaluating the Bulk Lorentz Factors of Outflow Material: Lessons Learned from the Extremely Energetic Outburst GRB 160625B

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