The first survey of X-ray flares from gamma-ray bursts observed by Swift: Temporal properties and morphology

G. Chincarini, A. Moretti, P. Romano, A. D. Falcone, D. Morris, J. Racusin, S. Campana, S. Covino, C. Guidorzi, G. Tagliaferri, D. N. Burrows, C. Pagani, M. Stroh, D. Grupe, M. Capalbi, G. Cusumano, N. Gehrels, P. Giommi, V. La Parola, V. ManganoT. Mineo, J. A. Nousek, P. T. O'Brien, K. L. Page, M. Perri, E. Troja, R. Willingale, B. Zhang

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Abstract

We present the first systematic investigation of the morphological and timing properties of flares in GRBs observed by Swift XRT. We consider a large sample drawn from all GRBs detected by Swift, INTEGRAL, and HETE-2 prior to 2006 January 31, which had an XRT follow-up and which showed significant flaring. Our sample of 3 3 GRBs includes long and short, at low and high redshift, and a total of 69 flares. The strongest flares occur in the early phases, with a clear anticorrelation between the flare peak intensity and the flare time of occurrence. Fitting each X-ray flare with a Gaussian model, we find that the mean ratio of the width and peak time is ( Δt/t) = 0.13 ± 0.10, albeit with a large scatter. Late flares at times >2000 s have long durations, Δr > 300 s, and can be very energetic compared to the underlying continuum. We further investigated whether there is a clear link between the number of pulses detected in the prompt phase by BAT and the number of X-ray flares detected by XRT, finding no correlation. However, we find that the distribution of intensity ratios between successive BAT prompt pulses and that between successive XRT flares is the same, an indication of a common origin for gamma-ray pulses and X-ray flares. All evidence indicates that flares are indeed related to the workings of the central engine and, in the standard fireball scenario, originate from internal shocks rather than external shocks. While all flares can be explained by long-lasting engine activity, 29/69 flares may also be explained by refreshed shocks. However, 10 can only be explained by prolonged activity of the central engine.

Original languageEnglish (US)
Pages (from-to)1903-1920
Number of pages18
JournalAstrophysical Journal
Volume671
Issue number2
DOIs
StatePublished - Dec 20 2007

Fingerprint

gamma ray bursts
flares
engine
x rays
energetics
engines
shock
pulses
fireballs
indication
time measurement
occurrences
gamma rays
continuums

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Chincarini, G. ; Moretti, A. ; Romano, P. ; Falcone, A. D. ; Morris, D. ; Racusin, J. ; Campana, S. ; Covino, S. ; Guidorzi, C. ; Tagliaferri, G. ; Burrows, D. N. ; Pagani, C. ; Stroh, M. ; Grupe, D. ; Capalbi, M. ; Cusumano, G. ; Gehrels, N. ; Giommi, P. ; La Parola, V. ; Mangano, V. ; Mineo, T. ; Nousek, J. A. ; O'Brien, P. T. ; Page, K. L. ; Perri, M. ; Troja, E. ; Willingale, R. ; Zhang, B. / The first survey of X-ray flares from gamma-ray bursts observed by Swift : Temporal properties and morphology. In: Astrophysical Journal. 2007 ; Vol. 671, No. 2. pp. 1903-1920.
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Chincarini, G, Moretti, A, Romano, P, Falcone, AD, Morris, D, Racusin, J, Campana, S, Covino, S, Guidorzi, C, Tagliaferri, G, Burrows, DN, Pagani, C, Stroh, M, Grupe, D, Capalbi, M, Cusumano, G, Gehrels, N, Giommi, P, La Parola, V, Mangano, V, Mineo, T, Nousek, JA, O'Brien, PT, Page, KL, Perri, M, Troja, E, Willingale, R & Zhang, B 2007, 'The first survey of X-ray flares from gamma-ray bursts observed by Swift: Temporal properties and morphology', Astrophysical Journal, vol. 671, no. 2, pp. 1903-1920. https://doi.org/10.1086/521591

The first survey of X-ray flares from gamma-ray bursts observed by Swift : Temporal properties and morphology. / Chincarini, G.; Moretti, A.; Romano, P.; Falcone, A. D.; Morris, D.; Racusin, J.; Campana, S.; Covino, S.; Guidorzi, C.; Tagliaferri, G.; Burrows, D. N.; Pagani, C.; Stroh, M.; Grupe, D.; Capalbi, M.; Cusumano, G.; Gehrels, N.; Giommi, P.; La Parola, V.; Mangano, V.; Mineo, T.; Nousek, J. A.; O'Brien, P. T.; Page, K. L.; Perri, M.; Troja, E.; Willingale, R.; Zhang, B.

In: Astrophysical Journal, Vol. 671, No. 2, 20.12.2007, p. 1903-1920.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The first survey of X-ray flares from gamma-ray bursts observed by Swift

T2 - Temporal properties and morphology

AU - Chincarini, G.

AU - Moretti, A.

AU - Romano, P.

AU - Falcone, A. D.

AU - Morris, D.

AU - Racusin, J.

AU - Campana, S.

AU - Covino, S.

AU - Guidorzi, C.

AU - Tagliaferri, G.

AU - Burrows, D. N.

AU - Pagani, C.

AU - Stroh, M.

AU - Grupe, D.

AU - Capalbi, M.

AU - Cusumano, G.

AU - Gehrels, N.

AU - Giommi, P.

AU - La Parola, V.

AU - Mangano, V.

AU - Mineo, T.

AU - Nousek, J. A.

AU - O'Brien, P. T.

AU - Page, K. L.

AU - Perri, M.

AU - Troja, E.

AU - Willingale, R.

AU - Zhang, B.

PY - 2007/12/20

Y1 - 2007/12/20

N2 - We present the first systematic investigation of the morphological and timing properties of flares in GRBs observed by Swift XRT. We consider a large sample drawn from all GRBs detected by Swift, INTEGRAL, and HETE-2 prior to 2006 January 31, which had an XRT follow-up and which showed significant flaring. Our sample of 3 3 GRBs includes long and short, at low and high redshift, and a total of 69 flares. The strongest flares occur in the early phases, with a clear anticorrelation between the flare peak intensity and the flare time of occurrence. Fitting each X-ray flare with a Gaussian model, we find that the mean ratio of the width and peak time is ( Δt/t) = 0.13 ± 0.10, albeit with a large scatter. Late flares at times >2000 s have long durations, Δr > 300 s, and can be very energetic compared to the underlying continuum. We further investigated whether there is a clear link between the number of pulses detected in the prompt phase by BAT and the number of X-ray flares detected by XRT, finding no correlation. However, we find that the distribution of intensity ratios between successive BAT prompt pulses and that between successive XRT flares is the same, an indication of a common origin for gamma-ray pulses and X-ray flares. All evidence indicates that flares are indeed related to the workings of the central engine and, in the standard fireball scenario, originate from internal shocks rather than external shocks. While all flares can be explained by long-lasting engine activity, 29/69 flares may also be explained by refreshed shocks. However, 10 can only be explained by prolonged activity of the central engine.

AB - We present the first systematic investigation of the morphological and timing properties of flares in GRBs observed by Swift XRT. We consider a large sample drawn from all GRBs detected by Swift, INTEGRAL, and HETE-2 prior to 2006 January 31, which had an XRT follow-up and which showed significant flaring. Our sample of 3 3 GRBs includes long and short, at low and high redshift, and a total of 69 flares. The strongest flares occur in the early phases, with a clear anticorrelation between the flare peak intensity and the flare time of occurrence. Fitting each X-ray flare with a Gaussian model, we find that the mean ratio of the width and peak time is ( Δt/t) = 0.13 ± 0.10, albeit with a large scatter. Late flares at times >2000 s have long durations, Δr > 300 s, and can be very energetic compared to the underlying continuum. We further investigated whether there is a clear link between the number of pulses detected in the prompt phase by BAT and the number of X-ray flares detected by XRT, finding no correlation. However, we find that the distribution of intensity ratios between successive BAT prompt pulses and that between successive XRT flares is the same, an indication of a common origin for gamma-ray pulses and X-ray flares. All evidence indicates that flares are indeed related to the workings of the central engine and, in the standard fireball scenario, originate from internal shocks rather than external shocks. While all flares can be explained by long-lasting engine activity, 29/69 flares may also be explained by refreshed shocks. However, 10 can only be explained by prolonged activity of the central engine.

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U2 - 10.1086/521591

DO - 10.1086/521591

M3 - Article

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VL - 671

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EP - 1920

JO - Astrophysical Journal

JF - Astrophysical Journal

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