Confirmation of the E peak src-E iso (Amati) relation from the X-ray flash XRF 050416A observed by Swift/BAT

T. Sakamoto; L. Barbier; S. Barthelmy; J. Cummings; E. Fenimore; N. Gehrels; D. Hullinger; H. Krimm; C. Markwardt; D. Palmer; A. Parsons; G. Sato; J. Tueller

doi:10.1063/1.2207958

Confirmation of the E _peak ^src-E _iso (Amati) relation from the X-ray flash XRF 050416A observed by Swift/BAT

T. Sakamoto^*, L. Barbier, S. Barthelmy, J. Cummings, E. Fenimore, N. Gehrels, D. Hullinger, H. Krimm, C. Markwardt, D. Palmer, A. Parsons, G. Sato, J. Tueller

^*Corresponding author for this work

Waseda Research Institute for Science and Engineering

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

1 Citation (Scopus)

Abstract

We report Swift Burst Alert Telescope (BAT) observations of the X-ray Flash (XRF) XRF 050416A. The fluence ratio between the 15-25 and 25-50 keV bands of this event is 1.1, thus making it the softest gamma-ray burst (GRB) observed by BAT so far. The spectrum is well fitted by the Band function with E _peak ^obs of 15.6 _-2.7 ^+2.3keV. Assuming the redshift of the host galaxy (z=0.6535), the isotropic-equivalent energy E _iso and the E _peak energy at the GRB rest frame (E _peak ^src) of XRF 050416A are not only consistent with the correlation found by Amati et al. and extended to XRFs by Sakamoto et al., but also fill-in the gap of this relation around 30-80 keV range of E _peak ^src. This result tightens the validity of the E _peak ^src-E _iso relation form XRFs to GRBs.

Original language	English
Title of host publication	AIP Conference Proceedings
Pages	578-581
Number of pages	4
Volume	836
DOIs	https://doi.org/10.1063/1.2207958
Publication status	Published - 2006 May 19
Event	GAMMA-RAY BURSTS IN THE SWIFT ERA: 16th Maryland Astrophysics Conference - Washington, D.C. Duration: 2005 Nov 29 → 2005 Dec 2

Other

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

Keywords

Prompt gamma-ray emission
X-ray flash

ASJC Scopus subject areas

Physics and Astronomy(all)

Access to Document

10.1063/1.2207958

Cite this

Sakamoto, T., Barbier, L., Barthelmy, S., Cummings, J., Fenimore, E., Gehrels, N., Hullinger, D., Krimm, H., Markwardt, C., Palmer, D., Parsons, A., Sato, G., & Tueller, J. (2006). Confirmation of the E _peak ^src-E _iso (Amati) relation from the X-ray flash XRF 050416A observed by Swift/BAT. In AIP Conference Proceedings (Vol. 836, pp. 578-581) https://doi.org/10.1063/1.2207958

Sakamoto, T, Barbier, L, Barthelmy, S, Cummings, J, Fenimore, E, Gehrels, N, Hullinger, D, Krimm, H, Markwardt, C, Palmer, D, Parsons, A, Sato, G & Tueller, J 2006, Confirmation of the E _peak ^src-E _iso (Amati) relation from the X-ray flash XRF 050416A observed by Swift/BAT. in AIP Conference Proceedings. vol. 836, pp. 578-581, GAMMA-RAY BURSTS IN THE SWIFT ERA: 16th Maryland Astrophysics Conference, Washington, D.C., 05/11/29. https://doi.org/10.1063/1.2207958

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title = "Confirmation of the E peak src-E iso (Amati) relation from the X-ray flash XRF 050416A observed by Swift/BAT",

abstract = "We report Swift Burst Alert Telescope (BAT) observations of the X-ray Flash (XRF) XRF 050416A. The fluence ratio between the 15-25 and 25-50 keV bands of this event is 1.1, thus making it the softest gamma-ray burst (GRB) observed by BAT so far. The spectrum is well fitted by the Band function with E peak obs of 15.6 -2.7 +2.3keV. Assuming the redshift of the host galaxy (z=0.6535), the isotropic-equivalent energy E iso and the E peak energy at the GRB rest frame (E peak src) of XRF 050416A are not only consistent with the correlation found by Amati et al. and extended to XRFs by Sakamoto et al., but also fill-in the gap of this relation around 30-80 keV range of E peak src. This result tightens the validity of the E peak src-E iso relation form XRFs to GRBs.",

keywords = "Prompt gamma-ray emission, X-ray flash",

author = "T. Sakamoto and L. Barbier and S. Barthelmy and J. Cummings and E. Fenimore and N. Gehrels and D. Hullinger and H. Krimm and C. Markwardt and D. Palmer and A. Parsons and G. Sato and J. Tueller",

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T1 - Confirmation of the E peak src-E iso (Amati) relation from the X-ray flash XRF 050416A observed by Swift/BAT

AU - Sakamoto, T.

AU - Barbier, L.

AU - Barthelmy, S.

AU - Cummings, J.

AU - Fenimore, E.

AU - Gehrels, N.

AU - Hullinger, D.

AU - Krimm, H.

AU - Markwardt, C.

AU - Palmer, D.

AU - Parsons, A.

AU - Sato, G.

AU - Tueller, J.

PY - 2006/5/19

Y1 - 2006/5/19

N2 - We report Swift Burst Alert Telescope (BAT) observations of the X-ray Flash (XRF) XRF 050416A. The fluence ratio between the 15-25 and 25-50 keV bands of this event is 1.1, thus making it the softest gamma-ray burst (GRB) observed by BAT so far. The spectrum is well fitted by the Band function with E peak obs of 15.6 -2.7 +2.3keV. Assuming the redshift of the host galaxy (z=0.6535), the isotropic-equivalent energy E iso and the E peak energy at the GRB rest frame (E peak src) of XRF 050416A are not only consistent with the correlation found by Amati et al. and extended to XRFs by Sakamoto et al., but also fill-in the gap of this relation around 30-80 keV range of E peak src. This result tightens the validity of the E peak src-E iso relation form XRFs to GRBs.

AB - We report Swift Burst Alert Telescope (BAT) observations of the X-ray Flash (XRF) XRF 050416A. The fluence ratio between the 15-25 and 25-50 keV bands of this event is 1.1, thus making it the softest gamma-ray burst (GRB) observed by BAT so far. The spectrum is well fitted by the Band function with E peak obs of 15.6 -2.7 +2.3keV. Assuming the redshift of the host galaxy (z=0.6535), the isotropic-equivalent energy E iso and the E peak energy at the GRB rest frame (E peak src) of XRF 050416A are not only consistent with the correlation found by Amati et al. and extended to XRFs by Sakamoto et al., but also fill-in the gap of this relation around 30-80 keV range of E peak src. This result tightens the validity of the E peak src-E iso relation form XRFs to GRBs.

KW - Prompt gamma-ray emission

KW - X-ray flash

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