1. Publication List (refereed Journal) using the GC data 1 Sawada et al.2011,PASJ (submited) 2 Uchiyama et al.2011,PASJ (submited) 3 Ohnishi et al.2011,PASJ (submited) 4 Dogiel et al. 2011,PASJ (accepted) 5 Uchiyama et al. 2011,PASJ (accepted) 6 Nobukawa et al.2011,ApJ (submited) 7 Nakashima et al.2010,PASJ,62,971 8 Nobukawa et al.2010,PASJ,62,423 9 Ryu et al.2009,PASJ,61,751 10 Mori et al.2009,PASJ,61,687 11 Fukuoka et al.2009,PASJ,61,593 12 Nobukawa et al.2009, AdSpR,43,1045 13 Koyama et al.2009,PASJ,61,255 14 Inui et al.2009,PASJ,61,241 15 Nakajima et al.2009,PASJ,61,233 16 Yamauchi et al.2009,PASJ,61,225 17 Tsuru et al.2009,PASJ,61,219 18 Sawada et al.2009,PASJ,61,209 19 Hyodo et al.2009,PASJ,61,99 20 Nobukawa et al.2009,PASJ,61,93 21Koyama et al.2008, AN,.329,182 22 Yuasa et al.2008,PASJ,60,207 23 Koyama et al.2008,PASJ,60,201 24 Nobukawa et al.2008,PASJ,60,191 25 Mori et al.2008,PASJ,60,183 26 Hyodo et al.2008,PASJ,60,173 27 Miura et al.2008,PASJ,60,49 28 Koyama et al.2007,PASJ,59,245 29 Koyama et al.2007,PASJ,59,237 30 Tsujimoto et al.2007,PASJ,59,229 31 Koyama et al.2007,PASJ,59,221 The Galactic Center Key Project Katsuji Koyama, Kyoto University

2. Topics of my Talk 1. Discoveries of New SNR Candidates: Fe 6.7 keV line Si, S lines (ref: 7, 10, 12, 17, 18, 4, 25, 29, 31) 2. New Aspects of Peculiar Sources: G359.1-0.5 & Tornado (ref: 1, 3) 3. 6.7 keV, 6.9 keV line distribution : Origin of GCDX is different from GRXE (ref: 2, 13, 15, 31) 4. 6.4 keV Cloud: New discoveries : Sgr A--E (ref 2: 11, 15, 24, 31) 5. 3D-distribution of the XRN: Sgr B, Radio Src and Sgr C (ref: 9) 6. Time variability of 6.4 keV and Hard X-ray (ref: 4, 14, 21)

3. 1. Discoveries of SNR Candidates Midle-Aged (<10000 y) SNRs (kT~1 keV) e.g. G359.79-0.26 (Mori et al. 2008) G359.12-0.05 G359.77-0.09 G359.41−0.12 G1.2-0.0 G0.42−0.04 Young (<1000 y) SNR G0.61+0.01 (Koyama et al. 2007) kT= 3.2 keV, Fe abundance= 5.1 Twin of Sgr A East ?

4. G395.1-0.5 Extremely Over- Ionized Plasma (RRC) This source is near HESS J1745-303 Tornado Twin Plasma (blue) kT= 0.6-0.7 ~ solar abundance N H = 7x10 22 at the Head and Tail of the Tornado 2. New Aspects of Peculiar Sources

5. Image Divided into many segments, fit the individual spectrum with a power-law + Gaussians. Fluxes (F) F 6.9 : 6.95 keV line F 6.7 : 6.7 keV line 3. Fe-Ka Lines (6.7, 6.9 keV) Distributions Diffuse or Point Sources ?

6. FeXXV Kα Line Profile vs Stellar Mass Distributi on KαExcess at GCDX Origin of GREX is different from GCDX Same analysis for Fe XXVI Kα found that the excess ratio is larger than that of FeXXV kT of GCDX > GREX 0.01 0.1 1 10 0.1 1 2 Ｌｏｎｇｉｔｕｄｅ Ｌａｔｉｔｕｄｅ

7. GCDX Divided into 2 x 16 regions Fit the spectra with power-law + Gaussians. Gamma, Fluxes (F) and Equivalent width (EW) F 5-10 : 5-10 keV band : F 6.4, EW 6.4 : 6.4 keV line F 6.7, EW 6.7 : 6.7 keV line 6.7 keV vs 6.4 keV lines

8. F 5-10 F 6.7 + 0.5F 6.4 100F 6.7 10F 6.4 In the GC region, about 2/3 (~1/1.5) of the 5-10 keV flux is associated with the 6.7 keV line, and the other 1/3 (~0.5/1.5) is associated with the 6.4 keV line.

9. F 6.7 +0.5F 6.4 Deviation is found In the low flux side (GRXE) Same Analysis, but for the whole GC and GR regions GRXE is different from GCDX

10. l-distribution of the 6.4 keV lines Sgr A 4. Discoveries of New 6.4 keV Clouds Sgr B2 Sgr B1 M0.74-0.09 M359.43-0.07 M359.47-0.15 M359.43-0.12 M359.38-0.00 M359.23-0.04 M0.1-0.1 Arches G0.174-0.223 G0.162-0.127

11. Parabola x 2 +y 2 = (300-y) 2 (Unit is light-year) 5. 3-D distribution of the 6.4 keV-Cloud Face-on View (Ryu et al. 2009, and this conference)

12. 6. Time Variable 6.4 keV line & Hard X-rays 2005 2009

13. Thank you for your attention

14. 1994 年 2000 年 2004 年 2005 年 X-ray front

15. F 6.4 ∝ Fc F 6.7 ∝ Fc

16. Iron line difference between GC/GR and bright CVs (> 10 31 erg/s) EW6.7 GC & GR 450—550 eV (mean of 12: Yamauchi et al. 2009) m-CV 370 eV (mean of ~20 m-CVs: Ezuka et al. 1999)) Non-m CV250 eV (mean of 6 CVs: Rana et al. 2006) Thermal Plasma Fit GC & GR ~0.6-0.7 solar m-CV ~0.4 (mean of ~20 CVs: Ezuka et al. 1999) ~0.4 (mean of 16 CVs: Yuasa et al. 2010) Non –m CVs ~0.3 (mean of 7 CVs Baskill et al. )