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Suzaku studies of SFXTs The X-ray Universe 2011 The University of Tokyo M.Sasano K.Nakajima, S.Yamada, T. Yuasa, K.Nakazawa, K. Makishima.

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Presentation on theme: "Suzaku studies of SFXTs The X-ray Universe 2011 The University of Tokyo M.Sasano K.Nakajima, S.Yamada, T. Yuasa, K.Nakazawa, K. Makishima."— Presentation transcript:

1 Suzaku studies of SFXTs The X-ray Universe 2011 The University of Tokyo M.Sasano K.Nakajima, S.Yamada, T. Yuasa, K.Nakazawa, K. Makishima

2 1. Introduction ~Power of Suzaku in SFXT studies~  Very drastic flares on short time scales ( 〜 a few hours), with flux increases by 2-3 orders of magnitude.  Sometimes very slow pulsations.  Highly absorbed hard spectra. The X-ray Universe 2011 SFXTs (Super-giant Fast X-ray Transients), a new class of High Mass X-ray Binary, show - Suchy et al. (2011) 1A Using Suzaku, we can study -  Absorption  Continuum  Iron lines Wide-band spectroscopy is essential in their studies.

3 2. SFXTs observed with Suzaku So far, Suzaku observed 6 SFXTs, and will observe 2 more. Data sets of 5 objects are publicly available. Two of the 5 objects exhibited flares typical of SFXTs. –IGR J Rampy et al. (2009)  The absorption fluctuated in the flare.  Fe-K EW < 14.2 eV (quiescence),< ** eV (flare). –AX J Morris et al.(2009)  A high absorption ( 〜 cm -2 ), with some changes in a flare.  Fe-K EW < 300 eV (quiescence),< 50 eV (flare). The X-ray Universe 2011 We perform detailed reanalysis of AX J focusing on the iron line. 1 Energy keV 40 count/s Time (hr) counts/s/keV χ

4 3.Light curves of AX J The X-ray Universe 2011 Time (ks) count/sec Hardness

5 3.Light curves of AX J The X-ray Universe 2011 Time (ks) count/sec Hardness A large flare was detected.

6 3.Light curves of AX J The X-ray Universe 2011 Time (ks) count/sec Hardness 〜 30 times

7 3.Light curves of AX J The X-ray Universe 2011 Time (ks) count/sec Hardness Duration 〜 4 hr

8 3.Light curves of AX J The X-ray Universe 2011 Time (ks) count/sec Hardness Rise time 〜 1.4 hr

9 3.Light curves of AX J The X-ray Universe 2011 Time (ks) count/sec Hardness Flare Quiescence

10 The X-ray Universe 2011 Flare Quiescence 4. Spectral analysis 4-1 Background-subtracted count spectra XIS HXD

11 The X-ray Universe Ratio between flare and quiescence Energy (keV) Ratio

12 The X-ray Universe Ratio between flare and quiescence Energy (keV) Ratio From 1.5 keV to 40 keV Spectral shape did not change.  Average N H remained nearly the same.

13 The X-ray Universe Focus on Iron line Energy (keV) Quiescence Flare

14 The X-ray Universe Focus on Iron line The narrow iron line was detected in quiescence Energy (keV) Flare Quiescence

15 The X-ray Universe Focus on Iron line However, in the flare, the narrow line almost disappeared. A broad one may be allowed. The narrow iron line was detected in quiescence Energy (keV) Quiescence Flare

16 The X-ray Universe 2011 count/s/keV 1e-4 1e Energy(keV) Model : wabs×(cutoffpl+Gaussian) 4-4. Model fitting 110

17 The X-ray Universe 2011 count/s/keV 1e-4 1e ± ±0.03 E c (keV) Energy(keV) 1 10 χ2χ2 0.97(529) Model : wabs×(cutoffpl+Gaussian) χ ν 4-4. Model fitting 0.95(535) N H (10 22 cm -2 ) Photon index E cut (keV) 19±3.1 23±5.5

18 4-5. Iron line EW and width The X-ray Universe 2011 EW eV 0.14 Width of iron line (keV) Flare 68% and 90% confidence contour map 0 The line is narrow and highly significant. EW is consistent with the UL by Morris et al. Quiescence A narrow lron line cannot have EW > 50 eV. Consistent with Morris et al. A broad one is allowed to have a consistent EW with the quiescent spectrum.

19 5. Discussion The X-ray Universe 2011 Our results The absorption was same within 15% between flare and quiescence. In the flare, the iron line decreased in EW, or broadened. Assuming clumpy wind model (in’t Zand 2005) The absorption should become higher in flares. Equivalent width of iron line should also increase. A simple clumpy wind model cannot explain our results. Assuming gated accretion model(Grebenev&Sunyaev2007,Bozzo+08) In quiescence, matters stored at Alfven radius can emit narrow Fe line. In flares, the matters fall onto the neutron star  line broadening. The gated accretion model is favored by our result.

20 6. Summary The X-ray Universe 2011 We reanalyzed Suzaku data of AX J which was studied by Morris et al. (2009). We compared spectra of the large flare with those of quiescence. The average N H remained same within 10%. In the flare, the iron line decreased in EW, or broadened. Our results prefer the gated accretion model to the clumpy wind model.

21 The X-ray Universe 2011

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