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ASCA-SIS

The Scientific Results of MAXI/SSC Hiroshi Tomida and the MAXI/SSC team e-mail : tomida.hiroshi@jaxa.jp. MAXI-SSC. ASCA-SIS.

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ASCA-SIS

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  1. The Scientific Results of MAXI/SSCHiroshi Tomida and the MAXI/SSC team e-mail : tomida.hiroshi@jaxa.jp MAXI-SSC ASCA-SIS SSC (Solid-state Slit Camera) is an X-ray CCD camera on MAXI. In the first year observation from Aug 2009, SSC has detected over 70 sources. SSC is sensitive to ~0.5keV. Some of the SSC sources are not deteced with MAXI/GSC. In this poster, the initial scientific results (all-sky map, light cirves, and spectra) obatained with MAXI/SSC are presented. Suzaku-XIS Sco X-1 GX5-1 MAXI image of Sco X-1 2010-07-20 deep absorption expanded spectrum (5-8keV) scan scan No significant structure!! ~6.7keV GSC 4-10keV anode#2-5 SSc spectra of Sco X-1 SSC full band energy (keV) The PSF of the SSC is smaller than that of GSC. The SSC is suitable for the source detection in the confused region (Gal center) and near the bright sources. 5 6 7 Sco X-1 is a bright Galactic LMXB. Suzuki et al (1984) and White et al (1985) reported the broad Fe line emission (6.7keV) from Sco X-1. The SSC observed Sco X-1 without pile-up for the first time as CCD camera. The spectrum, however, shows no significant excess around 6-7keV. Around the galactic center region, X-ray objects have absorbed spectra. The SSC can determine the absorption parameters No BGD subtraction No exposure correction SSC All-Sky Image (12 month) red : 0.7-1.85keV green : 1.85-4keV blue : 4-7keV preliminary!! The bgd subtraction and the exposure correction is now undergoing. Cyg X-1 Cyg X-2 GSC light curve soft (hight) state (2010Jun25 - Jul15) hard (low) state (2010Feb06-26, Apr05-May05) SSC spectrum GSC and SSC light curve 2-20keV NEW!! SSC-H SSC 0.7-1.7keV GSC 2-4keV GSC SSC 2-10keV SSC-H SSC 4-10keV diskbb(0.4keV)+PL 4-10keV GSC diskbb(0.2keV)+PL GSC low energy limit 10-20keV 10-20keV 2010-06-26 Cyg X-2is a bright X-ray binary source. SSC can monitor the low energy region (<2keV) where the GSC does not cover !! MAXI detected the high state of Cyg X-1 in Jun 2010. SSC can determine the disk temperature. The temperature of 0.4keV is lower than the ASCA result (soft state [1]), and the higher than the Suzaku results (hard state [2]). It is likely that Cyg X-1 was in the intermediate state. SSC View of SRNs Cygnus Region Vela / Pup-A CasA (a comparison with other camera） SSC GSC Cyg X-1 Vela X-1 Cyg X-3 Vela SNR Cygnus Loop Pup-A Cyg X-2 Vela pulsar SSC GSC The detection efficiency of SSC for hard X-rays is comparable to that of Suzaku/XIS. Cygnus Loop, Vela SNR and Pup-A are dim in the GSC image, but they are bright in the SSC image since the SNRs have very soft spectrum (kT<1keV). SSC can observe the whole region of the largely extended SNRs with the moderate energy resolution of the CCD for the first time!! Si References [1] Dotani et al (1997) ApJ 485 87 [2] Makishima et al (2008) PASJ 60 585 [3] Suzuki et al (1984) PASJ 36 761 [4] White et al (1985) ApJ 296 475 S Fe-L and Ne Mg

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