X-ray flare in XRF 050406: Evidence for prolonged engine activity

P. Romano; A. Moretti; P. L. Banat; D. N. Burrows; S. Campana; G. Chincarini; S. Covino; D. Malesani; G. Tagliaferri; A. D. Falcone; M. Capalbi; G. Cusumano; P. Giommi; V. La Parola; V. Mangano; M. Perri; C. Pagani

doi:10.1063/1.2207956

X-ray flare in XRF 050406: Evidence for prolonged engine activity

P. Romano, A. Moretti, P. L. Banat, D. N. Burrows, S. Campana, G. Chincarini, S. Covino, D. Malesani, G. Tagliaferri, A. D. Falcone, M. Capalbi, G. Cusumano, P. Giommi, V. La Parola, V. Mangano, M. Perri, C. Pagani

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

We present observations of XRF 050406, an X-ray flash with a relatively low fluence (∼ 10^-7 erg cm^-2 in the 15-350 keV band), a soft spectrum (photon index Γ_γ = 2.65), no significant flux above ∼ 50 keV and a peak energy E_p < 15 keV. XRF 050406 is the first burst detected by Swift clearly showing a flare in its X-ray light curve. The flare peaks 210 s after the BAT trigger, presents a flux variation δF/F ∼ 6 in a timescale δt/t_peak ≪ 1 and a measured fluence of 1-15% of the prompt one. We argue that the producing mechanism is late internal shocks, which implies that the central engine is still active at 210 s, though with a reduced power with respect to the prompt emission. The X-ray light curve flattens to a more shallow slope with a decay index of ∼ 0.5 after ∼ 4400 s, also supporting continued central engine activity.

Original language	English (US)
Title of host publication	GAMMA-RAY BURSTS IN THE SWIFT ERA
Subtitle of host publication	Sixteenth Maryland Astrophysics Conference
Pages	570-573
Number of pages	4
DOIs	https://doi.org/10.1063/1.2207956
Publication status	Published - May 19 2006
Event	GAMMA-RAY BURSTS IN THE SWIFT ERA: 16th Maryland Astrophysics Conference - Washington, D.C., United States Duration: Nov 29 2005 → Dec 2 2005

Publication series

Name	AIP Conference Proceedings
Volume	836
ISSN (Print)	0094-243X
ISSN (Electronic)	1551-7616

Other

Other	GAMMA-RAY BURSTS IN THE SWIFT ERA: 16th Maryland Astrophysics Conference
Country	United States
City	Washington, D.C.
Period	11/29/05 → 12/2/05

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All Science Journal Classification (ASJC) codes

Physics and Astronomy(all)

Cite this

Romano, P., Moretti, A., Banat, P. L., Burrows, D. N., Campana, S., Chincarini, G., ... Pagani, C. (2006). X-ray flare in XRF 050406: Evidence for prolonged engine activity. In GAMMA-RAY BURSTS IN THE SWIFT ERA: Sixteenth Maryland Astrophysics Conference (pp. 570-573). (AIP Conference Proceedings; Vol. 836). https://doi.org/10.1063/1.2207956

Romano, P. ; Moretti, A. ; Banat, P. L. ; Burrows, D. N. ; Campana, S. ; Chincarini, G. ; Covino, S. ; Malesani, D. ; Tagliaferri, G. ; Falcone, A. D. ; Capalbi, M. ; Cusumano, G. ; Giommi, P. ; La Parola, V. ; Mangano, V. ; Perri, M. ; Pagani, C. / X-ray flare in XRF 050406 : Evidence for prolonged engine activity. GAMMA-RAY BURSTS IN THE SWIFT ERA: Sixteenth Maryland Astrophysics Conference. 2006. pp. 570-573 (AIP Conference Proceedings).

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title = "X-ray flare in XRF 050406: Evidence for prolonged engine activity",

abstract = "We present observations of XRF 050406, an X-ray flash with a relatively low fluence (∼ 10-7 erg cm-2 in the 15-350 keV band), a soft spectrum (photon index Γγ = 2.65), no significant flux above ∼ 50 keV and a peak energy Ep < 15 keV. XRF 050406 is the first burst detected by Swift clearly showing a flare in its X-ray light curve. The flare peaks 210 s after the BAT trigger, presents a flux variation δF/F ∼ 6 in a timescale δt/tpeak ≪ 1 and a measured fluence of 1-15{\%} of the prompt one. We argue that the producing mechanism is late internal shocks, which implies that the central engine is still active at 210 s, though with a reduced power with respect to the prompt emission. The X-ray light curve flattens to a more shallow slope with a decay index of ∼ 0.5 after ∼ 4400 s, also supporting continued central engine activity.",

author = "P. Romano and A. Moretti and Banat, {P. L.} and Burrows, {D. N.} and S. Campana and G. Chincarini and S. Covino and D. Malesani and G. Tagliaferri and Falcone, {A. D.} and M. Capalbi and G. Cusumano and P. Giommi and {La Parola}, V. and V. Mangano and M. Perri and C. Pagani",

year = "2006",

month = "5",

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doi = "10.1063/1.2207956",

language = "English (US)",

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series = "AIP Conference Proceedings",

pages = "570--573",

booktitle = "GAMMA-RAY BURSTS IN THE SWIFT ERA",

note = "GAMMA-RAY BURSTS IN THE SWIFT ERA: 16th Maryland Astrophysics Conference ; Conference date: 29-11-2005 Through 02-12-2005",

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Romano, P, Moretti, A, Banat, PL, Burrows, DN, Campana, S, Chincarini, G, Covino, S, Malesani, D, Tagliaferri, G, Falcone, AD, Capalbi, M, Cusumano, G, Giommi, P, La Parola, V, Mangano, V, Perri, M & Pagani, C 2006, X-ray flare in XRF 050406: Evidence for prolonged engine activity. in GAMMA-RAY BURSTS IN THE SWIFT ERA: Sixteenth Maryland Astrophysics Conference. AIP Conference Proceedings, vol. 836, pp. 570-573, GAMMA-RAY BURSTS IN THE SWIFT ERA: 16th Maryland Astrophysics Conference, Washington, D.C., United States, 11/29/05. https://doi.org/10.1063/1.2207956

X-ray flare in XRF 050406 : Evidence for prolonged engine activity. / Romano, P.; Moretti, A.; Banat, P. L.; Burrows, D. N.; Campana, S.; Chincarini, G.; Covino, S.; Malesani, D.; Tagliaferri, G.; Falcone, A. D.; Capalbi, M.; Cusumano, G.; Giommi, P.; La Parola, V.; Mangano, V.; Perri, M.; Pagani, C.

GAMMA-RAY BURSTS IN THE SWIFT ERA: Sixteenth Maryland Astrophysics Conference. 2006. p. 570-573 (AIP Conference Proceedings; Vol. 836).

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

TY - GEN

T1 - X-ray flare in XRF 050406

T2 - GAMMA-RAY BURSTS IN THE SWIFT ERA: 16th Maryland Astrophysics Conference

AU - Romano, P.

AU - Moretti, A.

AU - Banat, P. L.

AU - Burrows, D. N.

AU - Campana, S.

AU - Chincarini, G.

AU - Covino, S.

AU - Malesani, D.

AU - Tagliaferri, G.

AU - Falcone, A. D.

AU - Capalbi, M.

AU - Cusumano, G.

AU - Giommi, P.

AU - La Parola, V.

AU - Mangano, V.

AU - Perri, M.

AU - Pagani, C.

PY - 2006/5/19

Y1 - 2006/5/19

N2 - We present observations of XRF 050406, an X-ray flash with a relatively low fluence (∼ 10-7 erg cm-2 in the 15-350 keV band), a soft spectrum (photon index Γγ = 2.65), no significant flux above ∼ 50 keV and a peak energy Ep < 15 keV. XRF 050406 is the first burst detected by Swift clearly showing a flare in its X-ray light curve. The flare peaks 210 s after the BAT trigger, presents a flux variation δF/F ∼ 6 in a timescale δt/tpeak ≪ 1 and a measured fluence of 1-15% of the prompt one. We argue that the producing mechanism is late internal shocks, which implies that the central engine is still active at 210 s, though with a reduced power with respect to the prompt emission. The X-ray light curve flattens to a more shallow slope with a decay index of ∼ 0.5 after ∼ 4400 s, also supporting continued central engine activity.

AB - We present observations of XRF 050406, an X-ray flash with a relatively low fluence (∼ 10-7 erg cm-2 in the 15-350 keV band), a soft spectrum (photon index Γγ = 2.65), no significant flux above ∼ 50 keV and a peak energy Ep < 15 keV. XRF 050406 is the first burst detected by Swift clearly showing a flare in its X-ray light curve. The flare peaks 210 s after the BAT trigger, presents a flux variation δF/F ∼ 6 in a timescale δt/tpeak ≪ 1 and a measured fluence of 1-15% of the prompt one. We argue that the producing mechanism is late internal shocks, which implies that the central engine is still active at 210 s, though with a reduced power with respect to the prompt emission. The X-ray light curve flattens to a more shallow slope with a decay index of ∼ 0.5 after ∼ 4400 s, also supporting continued central engine activity.

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U2 - 10.1063/1.2207956

DO - 10.1063/1.2207956

M3 - Conference contribution

AN - SCOPUS:33845581600

SN - 0735403260

SN - 9780735403260

T3 - AIP Conference Proceedings

SP - 570

EP - 573

BT - GAMMA-RAY BURSTS IN THE SWIFT ERA

Y2 - 29 November 2005 through 2 December 2005

ER -

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10.1063/1.2207956