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Suzaku Observation of X-ray Afterglow: Spectral and Temporal Behaviors

Suzaku Observation of X-ray Afterglow: Spectral and Temporal Behaviors. See also the posters Y. Nakagawa & M. S. Tashiro. Suzaku GRB ToO Team:. D. Yonetoku , T. Murakami , H. Kodaira, S. Okuno, S. Yoshinari ( Kanazawa U. )

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Suzaku Observation of X-ray Afterglow: Spectral and Temporal Behaviors

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  1. Suzaku Observation of X-ray Afterglow:Spectral and Temporal Behaviors See also the posters Y. Nakagawa & M. S. Tashiro Suzaku GRB ToO Team: D. Yonetoku, T. Murakami, H. Kodaira, S. Okuno, S. Yoshinari (Kanazawa U.) A. Yoshida, Y. Nakagawa, K. Yamaoka, N. Ishikawa (Aoyama G. U.), M. S. Tashiro, Y. Urata, K. Abe, K. Onda (Saitama U.) T. Tamagawa, M. Kuwahara, M. Suzuki (RIKEN) M. Yamauchi, E. Sonoda, S. Maeno (Miyazaki U.) T. Takahashi, K. Nakazawa (ISAS/JAXA) Y. Ueda, K. Sugiyasu, K. Kubota (Kyoto U.) N. Kawai, T. Shimokawabe, T. Ishimura (Tokyo Tech.) K. Torii (Osaka U.), K. Kinugasa (Gunma Obs.), T. Kohmura (Kougakuin U.) L. Angelini, L. J. Kaluzienski, R. L. Kelley, J. N. Reeves (GSFC/NASA), J. Nousek (Penn-State U.), G. Ricker (MIT) 36 Members and Suzaku GRB ToO Members 14 Institute/University

  2. Suzaku Satellite Aoyama

  3. Suzaku’s Characteristics We can realize the broad band observation (0.2 – 600 keV) with the ultra-low-noise instruments. For the X-ray afterglow observation, Suzaku is the best tool to investigate (1) the emission lines, (2) the spectral variance. XIS (X-ray CCD) – Effective Area SuzakuXIS HXD – Sensitivity XMM Chandra

  4. Scientific Objectives very steep shallow classical (1) Spectral change in early break of X-ray afterglow transition from hard to soft … ? We try to provide the existence of continuous energy injection with broad band spectroscopy (XIS+HXD). Nousek et al. (2) Emission lines in the X-ray afterglow • Prominent iron emission line/edge is independently reported. • XMM-Newton shows emission lines of light element, and no iron line. • Almost all X-ray afterglows show NO emission lines… Using the best condition of Suzaku-XIS to detect the emission lines, we try to CLOSE this chaotic issue.

  5. GRB970508 (Piro et al.) GRB970828 (Yoshida et al.) GRB011211 (Reeves et al.) GRB000214 (Antonelli et al.) GRB991216 (Piro et al.) GRB030227 (Watson et al.) GRB990705 (Amati et al.) GRB001025A (Watson et al.)

  6. Suzaku Observation – GRB060105 06:50:14(UT) : HETE-2 Trigger Notice . 05/Jan/2006 06:49:28(UT) : GRB detection (+0) 06:49:44(UT) : BAT Notice (+16sec) 06:50:23(UT) : XRT Notice (+55sec) 08:55:14(UT) : Contact with Suzaku steering committee (+2.1 hrs) 12:10:00(UT) : Suzaku Obs. START (+5.35 hrs) 06/Jan/2006 12:00:00(UT) : Suzaku Obs. END (+29.2 hrs) Total exposure : 46.4 ksec

  7. t –2.29±0.24 t –0.71±0.02 t –2.39±0.13 -100 -50 0 50 100 GRB060105 X-ray afterglow tbreak = 0.04 days

  8. GRB060105 Afterglow Spectrum average spectrum hardness ratio 0.8 – 1.5 keV Γ= 2.01±0.11 nH = (2.4±0.5)×1021 cm–2 1.5 – 8.0 keV HR χ2ν/dof = 1.12/170 • We found no emission line features, even if we perform the time-resolved spectral analysis. EW < a few 10 eV in any energy range. • The hardness ratio is stable in the Suzaku observation. The X-ray flux at the PIN energy band is less than 1% of background level. We set only upper-limit flux for GRB060105.

  9. Conclusions Details are in Nakagawa’s & Tashiro’s Poster • Suzaku satellite was successfully launched in 10/July/2006. • Our scientific objectives are: (1) Early break in lightcurve of X-ray afterglows (2) Emission lines in the X-ray afterglows • We performed the very quick ToO observation for GRB060105. Combined with XRT/Swift, lightcurve shows (1) early jet-like break at 3,500 sec. (2) late hump around 40,000 sec. Spectrum show (1) no emission line features (2) no spectral evolution during the entire observation time.

  10. Suzaku ToO Strategy (1) GCN Notice from Swift BAT Detection (SWIFT_BAT_POSITION) XRT Detection (SWIFT_XRT_POSITION) Sun angle distribution : 65 – 110 degree (Suzaku constraint) X-ray flux @ T+100 sec > 1×10 –11 erg/cm2/sec (2) Time Window open at 8 hrs before the 1st contact pass close at the end of the 2nd contact pass (3) Operation Constraints No time critical observation will be pushed out. ToO will be officially triggered by the Suzaku steering committee

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