The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton

M. Perri; D. Guetta; L. A. Antonelli; A. Cucchiara; V. Mangano; J. Reeves; L. Angelini; A. P. Beardmore; P. Boyd; D. N. Burrows; S. Campana; M. Capalbi; G. Chincarini; G. Cusumano; P. Giommi; J. E. Hill; S. T. Holland; V. La Parola; T. Mineo; A. Moretti; J. A. Nousek; J. P. Osborne; C. Pagani; P. Romano; P. W. A. Roming; R. L. C. Starling; G. Tagliaferri; E. Troja; L. Vetere; N. Gehrels

doi:10.1051/0004-6361:20066227

The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton

M. Perri, D. Guetta, L. A. Antonelli, A. Cucchiara, V. Mangano, J. Reeves, L. Angelini, A. P. Beardmore, P. Boyd, D. N. Burrows, S. Campana, M. Capalbi, G. Chincarini, G. Cusumano, P. Giommi, J. E. Hill, S. T. Holland, V. La Parola, T. Mineo, A. MorettiJ. A. Nousek, J. P. Osborne, C. Pagani, P. Romano, P. W. A. Roming, R. L. C. Starling, G. Tagliaferri, E. Troja, L. Vetere, N. Gehrels

Research output: Contribution to journal › Article › peer-review

16 Scopus citations

Abstract

Aims. We observed the high redshift (z = 3.969) GRB 050730 with Swift and XMM-Newton to study its prompt and afterglow emission. Methods. We carried out a detailed spectral and temporal analysis of Swift and XMM-Newton observations. Results. The X-ray afterglow of GRB 050730 was found to decline along with time with superimposed intense flaring activity that extended over more than two orders of magnitude in time. Seven distinct re-brightening events starting from 236 s and up to 41.2 ks after the burst were observed. The underlying decay of the afterglow was well described by a double broken power-law model with breaks at t₁ = 237 ±20 s and t₂ = 10.1_-2.2 ^+4.6 ks. The temporal decay slopes before, between and after these breaks were α₁ = 2.1 ±0.3, α₂ = 0.44_-0.08^+0.14 and α₃ = 2.40 _-0.07^+0.09, respectively. The spectrum of the X-ray afterglow was well described by a photoelectrically absorbed power-law with an absorbing column density N_H^Z=(1.28_-0.25 ^+0.26) × 10²² cm^-2 in the host galaxy. Evidence was found of flaring activity in the early UVOT optical afterglow, simultaneous with that observed in the X-ray band. Strong X-ray spectral evolution during the flaring activity was present. The rise and decay power-law slopes of the first three flares were in the range 0.8-1.8 using as zero times the beginning and the peak of the flares, respectively. In the majority of flares (6/7), the ratio Δt/t_p between the duration of the event and the time when the flare peaks was nearly constant and ∼ 0.6-0.7. We showed that the observed spectral and temporal properties of the first three flares are consistent with being due both to high-latitude emission, as expected if the flares were produced by late internal shocks, and to refreshed shocks, i.e. late time energy injections into the main afterglow shock by slow moving shells ejected from the central engine during the prompt phase. The event fully satisfies the E_p-E_iso Amati relation but is not consistent with the E_p vs. E_jet Ghirlanda relation.

Original language	English
Pages (from-to)	83-92
Number of pages	10
Journal	Astronomy and Astrophysics
Volume	471
Issue number	1
DOIs	https://doi.org/10.1051/0004-6361:20066227
State	Published - Aug 2007
Externally published	Yes

Keywords

gamma rays : bursts
X-rays : individuals : GRB050730

Access to Document

10.1051/0004-6361:20066227

Cite this

Perri, M., Guetta, D., Antonelli, L. A., Cucchiara, A., Mangano, V., Reeves, J., Angelini, L., Beardmore, A. P., Boyd, P., Burrows, D. N., Campana, S., Capalbi, M., Chincarini, G., Cusumano, G., Giommi, P., Hill, J. E., Holland, S. T., La Parola, V., Mineo, T., ... Gehrels, N. (2007). The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton. Astronomy and Astrophysics, 471(1), 83-92. https://doi.org/10.1051/0004-6361:20066227

@article{1c3e6257447b4ad7af998b5808349774,

title = "The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton",

abstract = "Aims. We observed the high redshift (z = 3.969) GRB 050730 with Swift and XMM-Newton to study its prompt and afterglow emission. Methods. We carried out a detailed spectral and temporal analysis of Swift and XMM-Newton observations. Results. The X-ray afterglow of GRB 050730 was found to decline along with time with superimposed intense flaring activity that extended over more than two orders of magnitude in time. Seven distinct re-brightening events starting from 236 s and up to 41.2 ks after the burst were observed. The underlying decay of the afterglow was well described by a double broken power-law model with breaks at t1 = 237 ±20 s and t2 = 10.1-2.2 +4.6 ks. The temporal decay slopes before, between and after these breaks were α1 = 2.1 ±0.3, α2 = 0.44-0.08+0.14 and α3 = 2.40 -0.07+0.09, respectively. The spectrum of the X-ray afterglow was well described by a photoelectrically absorbed power-law with an absorbing column density NHZ=(1.28-0.25 +0.26) × 1022 cm-2 in the host galaxy. Evidence was found of flaring activity in the early UVOT optical afterglow, simultaneous with that observed in the X-ray band. Strong X-ray spectral evolution during the flaring activity was present. The rise and decay power-law slopes of the first three flares were in the range 0.8-1.8 using as zero times the beginning and the peak of the flares, respectively. In the majority of flares (6/7), the ratio Δt/tp between the duration of the event and the time when the flare peaks was nearly constant and ∼ 0.6-0.7. We showed that the observed spectral and temporal properties of the first three flares are consistent with being due both to high-latitude emission, as expected if the flares were produced by late internal shocks, and to refreshed shocks, i.e. late time energy injections into the main afterglow shock by slow moving shells ejected from the central engine during the prompt phase. The event fully satisfies the Ep-Eiso Amati relation but is not consistent with the Ep vs. Ejet Ghirlanda relation.",

keywords = "gamma rays : bursts, X-rays : individuals : GRB050730",

author = "M. Perri and D. Guetta and Antonelli, {L. A.} and A. Cucchiara and V. Mangano and J. Reeves and L. Angelini and Beardmore, {A. P.} and P. Boyd and Burrows, {D. N.} and S. Campana and M. Capalbi and G. Chincarini and G. Cusumano and P. Giommi and Hill, {J. E.} and Holland, {S. T.} and {La Parola}, V. and T. Mineo and A. Moretti and Nousek, {J. A.} and Osborne, {J. P.} and C. Pagani and P. Romano and Roming, {P. W. A.} and Starling, {R. L. C.} and G. Tagliaferri and E. Troja and L. Vetere and N. Gehrels",

year = "2007",

month = aug,

doi = "10.1051/0004-6361:20066227",

language = "אנגלית",

volume = "471",

pages = "83--92",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

number = "1",

}

Perri, M, Guetta, D, Antonelli, LA, Cucchiara, A, Mangano, V, Reeves, J, Angelini, L, Beardmore, AP, Boyd, P, Burrows, DN, Campana, S, Capalbi, M, Chincarini, G, Cusumano, G, Giommi, P, Hill, JE, Holland, ST, La Parola, V, Mineo, T, Moretti, A, Nousek, JA, Osborne, JP, Pagani, C, Romano, P, Roming, PWA, Starling, RLC, Tagliaferri, G, Troja, E, Vetere, L & Gehrels, N 2007, 'The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton', Astronomy and Astrophysics, vol. 471, no. 1, pp. 83-92. https://doi.org/10.1051/0004-6361:20066227

TY - JOUR

T1 - The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton

AU - Perri, M.

AU - Guetta, D.

AU - Antonelli, L. A.

AU - Cucchiara, A.

AU - Mangano, V.

AU - Reeves, J.

AU - Angelini, L.

AU - Beardmore, A. P.

AU - Boyd, P.

AU - Burrows, D. N.

AU - Campana, S.

AU - Capalbi, M.

AU - Chincarini, G.

AU - Cusumano, G.

AU - Giommi, P.

AU - Hill, J. E.

AU - Holland, S. T.

AU - La Parola, V.

AU - Mineo, T.

AU - Moretti, A.

AU - Nousek, J. A.

AU - Osborne, J. P.

AU - Pagani, C.

AU - Romano, P.

AU - Roming, P. W. A.

AU - Starling, R. L. C.

AU - Tagliaferri, G.

AU - Troja, E.

AU - Vetere, L.

AU - Gehrels, N.

PY - 2007/8

Y1 - 2007/8

N2 - Aims. We observed the high redshift (z = 3.969) GRB 050730 with Swift and XMM-Newton to study its prompt and afterglow emission. Methods. We carried out a detailed spectral and temporal analysis of Swift and XMM-Newton observations. Results. The X-ray afterglow of GRB 050730 was found to decline along with time with superimposed intense flaring activity that extended over more than two orders of magnitude in time. Seven distinct re-brightening events starting from 236 s and up to 41.2 ks after the burst were observed. The underlying decay of the afterglow was well described by a double broken power-law model with breaks at t1 = 237 ±20 s and t2 = 10.1-2.2 +4.6 ks. The temporal decay slopes before, between and after these breaks were α1 = 2.1 ±0.3, α2 = 0.44-0.08+0.14 and α3 = 2.40 -0.07+0.09, respectively. The spectrum of the X-ray afterglow was well described by a photoelectrically absorbed power-law with an absorbing column density NHZ=(1.28-0.25 +0.26) × 1022 cm-2 in the host galaxy. Evidence was found of flaring activity in the early UVOT optical afterglow, simultaneous with that observed in the X-ray band. Strong X-ray spectral evolution during the flaring activity was present. The rise and decay power-law slopes of the first three flares were in the range 0.8-1.8 using as zero times the beginning and the peak of the flares, respectively. In the majority of flares (6/7), the ratio Δt/tp between the duration of the event and the time when the flare peaks was nearly constant and ∼ 0.6-0.7. We showed that the observed spectral and temporal properties of the first three flares are consistent with being due both to high-latitude emission, as expected if the flares were produced by late internal shocks, and to refreshed shocks, i.e. late time energy injections into the main afterglow shock by slow moving shells ejected from the central engine during the prompt phase. The event fully satisfies the Ep-Eiso Amati relation but is not consistent with the Ep vs. Ejet Ghirlanda relation.

AB - Aims. We observed the high redshift (z = 3.969) GRB 050730 with Swift and XMM-Newton to study its prompt and afterglow emission. Methods. We carried out a detailed spectral and temporal analysis of Swift and XMM-Newton observations. Results. The X-ray afterglow of GRB 050730 was found to decline along with time with superimposed intense flaring activity that extended over more than two orders of magnitude in time. Seven distinct re-brightening events starting from 236 s and up to 41.2 ks after the burst were observed. The underlying decay of the afterglow was well described by a double broken power-law model with breaks at t1 = 237 ±20 s and t2 = 10.1-2.2 +4.6 ks. The temporal decay slopes before, between and after these breaks were α1 = 2.1 ±0.3, α2 = 0.44-0.08+0.14 and α3 = 2.40 -0.07+0.09, respectively. The spectrum of the X-ray afterglow was well described by a photoelectrically absorbed power-law with an absorbing column density NHZ=(1.28-0.25 +0.26) × 1022 cm-2 in the host galaxy. Evidence was found of flaring activity in the early UVOT optical afterglow, simultaneous with that observed in the X-ray band. Strong X-ray spectral evolution during the flaring activity was present. The rise and decay power-law slopes of the first three flares were in the range 0.8-1.8 using as zero times the beginning and the peak of the flares, respectively. In the majority of flares (6/7), the ratio Δt/tp between the duration of the event and the time when the flare peaks was nearly constant and ∼ 0.6-0.7. We showed that the observed spectral and temporal properties of the first three flares are consistent with being due both to high-latitude emission, as expected if the flares were produced by late internal shocks, and to refreshed shocks, i.e. late time energy injections into the main afterglow shock by slow moving shells ejected from the central engine during the prompt phase. The event fully satisfies the Ep-Eiso Amati relation but is not consistent with the Ep vs. Ejet Ghirlanda relation.

KW - gamma rays : bursts

KW - X-rays : individuals : GRB050730

UR - http://www.scopus.com/inward/record.url?scp=34547944357&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20066227

DO - 10.1051/0004-6361:20066227

M3 - ???researchoutput.researchoutputtypes.contributiontojournal.article???

SN - 0004-6361

VL - 471

SP - 83

EP - 92

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 1

ER -

The exceptionally extended flaring activity in the X-ray afterglow of GRB 050730 observed with Swift and XMM-Newton

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this