Abstract
GRB 060105 was detected with the BAT instrument on-board Swift. The Suzaku follow-up observation started just 5.3 hours after the trigger with the XIS and HXD instruments. The XIS detected an uncatalogued fading source and its position was consistent with that previously reported by Swift XRT. We performed the spectral analyses using the data derived from Suzaku XIS and Swift XRT, and found that the spectrum of X-ray afterglow was well reproduced by the absorbed power law model. The best-fit spectral index and absorption are β = 2.15 ± 0.03 and NH = (3.74 ± 0.03) × 1021 cm-2, respectively. The observed decay curve by Suzaku XIS is fully consistent with the Swift XRT result. The Suzaku and Swift observations imply the possibility of the jet break at t = 3500 s, and the brightening of afterglow around t = 40000 s likely due to the refreshed shock. We see neither significant spectral evolution during the decay, nor evidence of emission line feature.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 1531-1533 |
| Number of pages | 3 |
| Journal | Nuovo Cimento della Societa Italiana di Fisica B |
| Volume | 121 |
| Issue number | 12 |
| DOIs | |
| State | Published - Dec 1 2006 |
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All Science Journal Classification (ASJC) codes
- Physics and Astronomy(all)
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Detailed analyses of GRB 060105 X-ray afterglow observed by Suzaku. / Nakagawa, Y. E.; Tashiro, M.; Abe, K.; Yoshida, A.; Yamaoka, K.; Nakazawa, K.; Murakami, T.; Yonetoku, D.; Kawai, N.; Nousek, J.; Ishikawa, N.; Urata, Y.; Onda, K.; Tamagawa, T.; Suzuki, M.; Kuwahara, M.; Takahashi, T.; Yamauchi, M.; Sonoda, E.; Maeno, S.; Kinugasa, K.; Kohmura, T.; Torii, K.; Ueda, Y.; Kubota, K.; Sugiyasu, K.; Kodaira, H.; Okuno, S.; Yoshinari, S.; Shimokawabe, T.; Ishimura, T.; Ricker, G. R.; Reeves, J. N.; Angelini, L.; Kaluzienski, L. J.; Kelley, R. L.
In: Nuovo Cimento della Societa Italiana di Fisica B, Vol. 121, No. 12, 01.12.2006, p. 1531-1533.Research output: Contribution to journal › Article
TY - JOUR
T1 - Detailed analyses of GRB 060105 X-ray afterglow observed by Suzaku
AU - Nakagawa, Y. E.
AU - Tashiro, M.
AU - Abe, K.
AU - Yoshida, A.
AU - Yamaoka, K.
AU - Nakazawa, K.
AU - Murakami, T.
AU - Yonetoku, D.
AU - Kawai, N.
AU - Nousek, J.
AU - Ishikawa, N.
AU - Urata, Y.
AU - Onda, K.
AU - Tamagawa, T.
AU - Suzuki, M.
AU - Kuwahara, M.
AU - Takahashi, T.
AU - Yamauchi, M.
AU - Sonoda, E.
AU - Maeno, S.
AU - Kinugasa, K.
AU - Kohmura, T.
AU - Torii, K.
AU - Ueda, Y.
AU - Kubota, K.
AU - Sugiyasu, K.
AU - Kodaira, H.
AU - Okuno, S.
AU - Yoshinari, S.
AU - Shimokawabe, T.
AU - Ishimura, T.
AU - Ricker, G. R.
AU - Reeves, J. N.
AU - Angelini, L.
AU - Kaluzienski, L. J.
AU - Kelley, R. L.
PY - 2006/12/1
Y1 - 2006/12/1
N2 - GRB 060105 was detected with the BAT instrument on-board Swift. The Suzaku follow-up observation started just 5.3 hours after the trigger with the XIS and HXD instruments. The XIS detected an uncatalogued fading source and its position was consistent with that previously reported by Swift XRT. We performed the spectral analyses using the data derived from Suzaku XIS and Swift XRT, and found that the spectrum of X-ray afterglow was well reproduced by the absorbed power law model. The best-fit spectral index and absorption are β = 2.15 ± 0.03 and NH = (3.74 ± 0.03) × 1021 cm-2, respectively. The observed decay curve by Suzaku XIS is fully consistent with the Swift XRT result. The Suzaku and Swift observations imply the possibility of the jet break at t = 3500 s, and the brightening of afterglow around t = 40000 s likely due to the refreshed shock. We see neither significant spectral evolution during the decay, nor evidence of emission line feature.
AB - GRB 060105 was detected with the BAT instrument on-board Swift. The Suzaku follow-up observation started just 5.3 hours after the trigger with the XIS and HXD instruments. The XIS detected an uncatalogued fading source and its position was consistent with that previously reported by Swift XRT. We performed the spectral analyses using the data derived from Suzaku XIS and Swift XRT, and found that the spectrum of X-ray afterglow was well reproduced by the absorbed power law model. The best-fit spectral index and absorption are β = 2.15 ± 0.03 and NH = (3.74 ± 0.03) × 1021 cm-2, respectively. The observed decay curve by Suzaku XIS is fully consistent with the Swift XRT result. The Suzaku and Swift observations imply the possibility of the jet break at t = 3500 s, and the brightening of afterglow around t = 40000 s likely due to the refreshed shock. We see neither significant spectral evolution during the decay, nor evidence of emission line feature.
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U2 - 10.1393/ncb/i2007-10316-8
DO - 10.1393/ncb/i2007-10316-8
M3 - Article
AN - SCOPUS:35349011131
VL - 121
SP - 1531
EP - 1533
JO - Nuovo Cimento della Societa Italiana di Fisica B
JF - Nuovo Cimento della Societa Italiana di Fisica B
SN - 1594-9982
IS - 12
ER -