Investigation of jet break features in Swift gamma-ray bursts

G. Sato; R. Yamazaki; K. Ioka; T. Sakamoto; T. Takahashi; K. Nakazawa; T. Nakamura; K. Toma; D. Hullinger; M. Tashiro; A. M. Parsons; H. A. Krimm; S. D. Barthelmy; N. Gehrels; D. N. Burrows; P. T. O'Brien; J. P. Osborne; G. Chincarini; D. Q. Lamb

Investigation of jet break features in Swift gamma-ray bursts

G. Sato, R. Yamazaki, K. Ioka, T. Sakamoto, T. Takahashi, K. Nakazawa, T. Nakamura, K. Toma, D. Hullinger, M. Tashiro, A. M. Parsons, H. A. Krimm, S. D. Barthelmy, N. Gehrels, D. N. Burrows, P. T. O'Brien, J. P. Osborne, G. Chincarini, D. Q. Lamb

Waseda Research Institute for Science and Engineering

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

Abstract

We analyze Swift gamma-ray bursts (GRBs) and X-ray afterglows for three GRBs with spectroscopic redshift determinations - GRB 050401, XRF 050416a, and GRB 050525a. We find that the relation between spectral peak energy and isotropic energy of prompt emissions (the Amati relation) is consistent with that for the bursts observed in pre-Swift era. However, we find that the X-ray afterglow lightcurves, which extend up to 10-70 days, show no sign of the jet break that is expected in the standard framework of collimated outflows. We do so by showing that none of the X-ray afterglow lightcurves in our sample satisfies the relation between the spectral and temporal indices that is predicted for the phase after jet break. The jet break time can be predicted by inverting the tight empirical relation between the peak energy of the spectrum and the collimation-corrected energy of the prompt emission (the Ghirlanda relation). We find that there are no temporal breaks within the predicted time intervals in X-ray band. This requires either that the Ghirlanda relation has a larger scatter than previously thought, that the temporal break in X-rays is masked by some additional source of X-ray emission, or that it does not happen because of some unknown reason.

Original language	English
Title of host publication	11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity
Pages	2033-2035
Number of pages	3
Publication status	Published - 2008
Event	11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories, MG 2006 - Berlin Duration: 2006 Jul 23 → 2006 Jul 29

Other

Other	11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories, MG 2006
City	Berlin
Period	06/7/23 → 06/7/29

ASJC Scopus subject areas

Nuclear and High Energy Physics

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Sato, G., Yamazaki, R., Ioka, K., Sakamoto, T., Takahashi, T., Nakazawa, K., Nakamura, T., Toma, K., Hullinger, D., Tashiro, M., Parsons, A. M., Krimm, H. A., Barthelmy, S. D., Gehrels, N., Burrows, D. N., O'Brien, P. T., Osborne, J. P., Chincarini, G., & Lamb, D. Q. (2008). Investigation of jet break features in Swift gamma-ray bursts. In 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity (pp. 2033-2035)

Investigation of jet break features in Swift gamma-ray bursts. / Sato, G.; Yamazaki, R.; Ioka, K.; Sakamoto, T.; Takahashi, T.; Nakazawa, K.; Nakamura, T.; Toma, K.; Hullinger, D.; Tashiro, M.; Parsons, A. M.; Krimm, H. A.; Barthelmy, S. D.; Gehrels, N.; Burrows, D. N.; O'Brien, P. T.; Osborne, J. P.; Chincarini, G.; Lamb, D. Q.

11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity. 2008. p. 2033-2035.

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

Sato, G, Yamazaki, R, Ioka, K, Sakamoto, T, Takahashi, T, Nakazawa, K, Nakamura, T, Toma, K, Hullinger, D, Tashiro, M, Parsons, AM, Krimm, HA, Barthelmy, SD, Gehrels, N, Burrows, DN, O'Brien, PT, Osborne, JP, Chincarini, G & Lamb, DQ 2008, Investigation of jet break features in Swift gamma-ray bursts. in 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity. pp. 2033-2035, 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories, MG 2006, Berlin, 06/7/23.

Sato, G. ; Yamazaki, R. ; Ioka, K. ; Sakamoto, T. ; Takahashi, T. ; Nakazawa, K. ; Nakamura, T. ; Toma, K. ; Hullinger, D. ; Tashiro, M. ; Parsons, A. M. ; Krimm, H. A. ; Barthelmy, S. D. ; Gehrels, N. ; Burrows, D. N. ; O'Brien, P. T. ; Osborne, J. P. ; Chincarini, G. ; Lamb, D. Q. / Investigation of jet break features in Swift gamma-ray bursts. 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity. 2008. pp. 2033-2035

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title = "Investigation of jet break features in Swift gamma-ray bursts",

abstract = "We analyze Swift gamma-ray bursts (GRBs) and X-ray afterglows for three GRBs with spectroscopic redshift determinations - GRB 050401, XRF 050416a, and GRB 050525a. We find that the relation between spectral peak energy and isotropic energy of prompt emissions (the Amati relation) is consistent with that for the bursts observed in pre-Swift era. However, we find that the X-ray afterglow lightcurves, which extend up to 10-70 days, show no sign of the jet break that is expected in the standard framework of collimated outflows. We do so by showing that none of the X-ray afterglow lightcurves in our sample satisfies the relation between the spectral and temporal indices that is predicted for the phase after jet break. The jet break time can be predicted by inverting the tight empirical relation between the peak energy of the spectrum and the collimation-corrected energy of the prompt emission (the Ghirlanda relation). We find that there are no temporal breaks within the predicted time intervals in X-ray band. This requires either that the Ghirlanda relation has a larger scatter than previously thought, that the temporal break in X-rays is masked by some additional source of X-ray emission, or that it does not happen because of some unknown reason.",

author = "G. Sato and R. Yamazaki and K. Ioka and T. Sakamoto and T. Takahashi and K. Nakazawa and T. Nakamura and K. Toma and D. Hullinger and M. Tashiro and Parsons, {A. M.} and Krimm, {H. A.} and Barthelmy, {S. D.} and N. Gehrels and Burrows, {D. N.} and O'Brien, {P. T.} and Osborne, {J. P.} and G. Chincarini and Lamb, {D. Q.}",

year = "2008",

language = "English",

isbn = "9812834265",

pages = "2033--2035",

booktitle = "11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity",

note = "11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories, MG 2006 ; Conference date: 23-07-2006 Through 29-07-2006",

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TY - GEN

T1 - Investigation of jet break features in Swift gamma-ray bursts

AU - Sato, G.

AU - Yamazaki, R.

AU - Ioka, K.

AU - Sakamoto, T.

AU - Takahashi, T.

AU - Nakazawa, K.

AU - Nakamura, T.

AU - Toma, K.

AU - Hullinger, D.

AU - Tashiro, M.

AU - Parsons, A. M.

AU - Krimm, H. A.

AU - Barthelmy, S. D.

AU - Gehrels, N.

AU - Burrows, D. N.

AU - O'Brien, P. T.

AU - Osborne, J. P.

AU - Chincarini, G.

AU - Lamb, D. Q.

PY - 2008

Y1 - 2008

N2 - We analyze Swift gamma-ray bursts (GRBs) and X-ray afterglows for three GRBs with spectroscopic redshift determinations - GRB 050401, XRF 050416a, and GRB 050525a. We find that the relation between spectral peak energy and isotropic energy of prompt emissions (the Amati relation) is consistent with that for the bursts observed in pre-Swift era. However, we find that the X-ray afterglow lightcurves, which extend up to 10-70 days, show no sign of the jet break that is expected in the standard framework of collimated outflows. We do so by showing that none of the X-ray afterglow lightcurves in our sample satisfies the relation between the spectral and temporal indices that is predicted for the phase after jet break. The jet break time can be predicted by inverting the tight empirical relation between the peak energy of the spectrum and the collimation-corrected energy of the prompt emission (the Ghirlanda relation). We find that there are no temporal breaks within the predicted time intervals in X-ray band. This requires either that the Ghirlanda relation has a larger scatter than previously thought, that the temporal break in X-rays is masked by some additional source of X-ray emission, or that it does not happen because of some unknown reason.

AB - We analyze Swift gamma-ray bursts (GRBs) and X-ray afterglows for three GRBs with spectroscopic redshift determinations - GRB 050401, XRF 050416a, and GRB 050525a. We find that the relation between spectral peak energy and isotropic energy of prompt emissions (the Amati relation) is consistent with that for the bursts observed in pre-Swift era. However, we find that the X-ray afterglow lightcurves, which extend up to 10-70 days, show no sign of the jet break that is expected in the standard framework of collimated outflows. We do so by showing that none of the X-ray afterglow lightcurves in our sample satisfies the relation between the spectral and temporal indices that is predicted for the phase after jet break. The jet break time can be predicted by inverting the tight empirical relation between the peak energy of the spectrum and the collimation-corrected energy of the prompt emission (the Ghirlanda relation). We find that there are no temporal breaks within the predicted time intervals in X-ray band. This requires either that the Ghirlanda relation has a larger scatter than previously thought, that the temporal break in X-rays is masked by some additional source of X-ray emission, or that it does not happen because of some unknown reason.

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M3 - Conference contribution

AN - SCOPUS:84892974067

SN - 9812834265

SN - 9789812834263

SP - 2033

EP - 2035

BT - 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories - Proc. of the MG11 Meeting on General Relativity

T2 - 11th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation and Relativistic Field Theories, MG 2006

Y2 - 23 July 2006 through 29 July 2006

ER -