1. Suzaku Observation of the Galactic Center Region Takeshi Go Tsuru (Kyoto University) 20110722_Suzaku2011_GC_v14.key R.Fukuoka, Y.Hyodo, T.Inui, K.Koyama, S.Nakashima, M.Nobukawa, T.Ohnishi, S.G.Ryu, M.Sawada, Y.Takizawa (Kyoto), S. Yamauchi, (Nara WU), H.Uchiyama, T.Yuasa (Tokyo), H.Matsumoto, H.Mori (Nagoya), M.Tsujimoto (ISAS), J.Miura (Chuo), H.Nakajima (Osaka), D.Chernysov, V.Dogiel (P.N. Lebedev Institute) and more

2. Sgr C 1deg Observation of the GC region with Suzaku 197pointings, 5.26Msec SWG, AO, LP, KP (|l|<3°, |b|<5°)

3. Fe 24+ Kα Fe 25+ Kα Fe 24+ Kβ FeI Kα Ni 26+ Kα FeI Kβ Fe 25+ Kβ Ni 27+ Kα NiI Kα Si 12+ Kα Si 12+ Kβ Ar 16+ Kβ Ar 16+ Kα Si 13+ Kα Ca 18+ Kα Ca 19+ Kα Ar 17+ Kα S 15+ Kα S 14+ Kβ Energy Koyama+07 234 (keV) 768 (keV) S 14+ Kα Narrow Line Mapping High Spectral Resolution, Large Collecting Area, Low and Stable Non-X-ray Background The Galactic center region is the best target for Suzaku to take the most advantage of its Superiorities.

5. 5 Papers and Thesis using the GC data Published or Accepted In prep. or Submitted 5 30 Doctor Thesis : 6Nakajima, Inui, Hyodo, Uchiyama, Nobukawa, Yuasa

6. 6 Our Talk Plans (Tsuru & Nobukawa) Discoveries of New SNR candidates New Aspects of Peculiar Diffuse Sources 6.7keV and 6.9keV line distribution Discoveries and Revisits of 6.4 keV clumps Discovery of diffuse 6.4keV emission from the intercloud region Discovery of neutral Ar, Ca, Cr and Mn lines Time variabilities of 6.4keV and Hard X-ray emission from XRNe. 3D-distribution of the XRNe Nobukawa-san’s Talk

7. 7 1. Discovery of SNR candidates Young (<1000 y) SNR G0.61+0.01 kT= 3.2 keV, Z(Fe) = 5.1 Middle-Aged (<10000 y) SNRs kT~1 keV, Z 〜 1 G0.61+0.01 (Koyama+07) G359.79-0.26 (Mori+08) G359.77- 0.09 (Mori+09) G0.42−0.04 (Nobukawa+08) G359.41−0.12 (Tsuru+09) G359.12-0.05 (Nakashima+1 0) G1.2-0.0 (Sawada09+)

8. 8 Tsuru+09 “Chimney” 2. New Aspects of Peculiar Sources (1) Sgr A* Elliptical Ring Like Structure Mori+09 Super Bubble Both have similar spectra. Physically Connecting. E(thermal) = 1e51 ergs Candidate for a Super Bubble Diffuse and Chimney-like Structure SNR and associated outflow

9. At the Head and Tail Twin Plasma kT= 0.6-0.7 9 G395.1-0.5 near HESS J1745- 303 2. New Aspects of Peculiar Sources (2) Molecular Clouds Remnant of the bipolar flow from a compact object. Strong Mg, Si and S RRC Extremely Over- Ionized Plasma Ohnishi+11 Ohnishi #27 Tornado Peculiar radio source with strong polarization Sawada+11

10. Image Divided into small areas and made spectra, fit the individual spectrum with a power-law + Gaussians. Fluxes (F) F 6.7 : 6.7 keV line F 6.9 : 6.95 keV line 3. Fe-K Lines (6.7, 6.9 keV) Distributions Truly Diffuse or Point Sources ?

11. Surface brightness (10 -6 ph/s/cm 2 /arcmin 2 ) B ： East R ： West Ridge: Yamauchi GC: Nobukawa+ The border between GC and GR is located at l = 1 〜 2deg. The temperature of GC would be higher than GR. Nobukawa, Hyodo+, Yamauchi+09

12. 6.7keV Line Profile vs Stellar Mass Distribution Origin of 6.7keV line in GC is different from GR Nuclear stellar cluster Nuclea r stellar disk Galactic bulge Galactic disk Nuclear bulge A new population of point sources with a strong 6.7keV line. Truly diffuse plasma or (at b =0.0) * Uchiyama+11 Uchiyama #35 6.7keV Lines Excess at GC x4 〜 x 10 6.7keV (at l =-0.114) *

13. ( ｂ ) The 6.7 keV line flux vs Integrated point source flux (Chandra deep exposure) Near GC ( < 0.3 deg) l-distribution b-distribution 10 x 6.7 keV line (EW=0.5 keV) Sgr A* Nobukawa, Hyodo+ The 6.7keV has more extended distribution than point sources. Distribution of Point source flux (4.8-8 keV)

14. Size ~ 50pc x 30pc L 2-10 ~ 2×10 36 ergs/s n ave ~ 0.1cm -3 n peak ~ 0.4cm -3 E gas ~ 3×10 52 ergs Plasma Parameters (assuming Z Fe =1.2) ~0.36° ~0.70° R: 6.7keV, G:2.45keV, B: 6.4keV Escape Time scale (latutude) τ esc = Size/Cs = 2×10 4 yr Heating Rate = E gas /τ esc ~ 5×10 40 ergs/s ~ 10 -3 SN yr - 1 Much higher than the current activity of Sgr A * and ~10 -5 SN yr -1 expected from the stellar mass in this region. Plasma is in the ionization equilibrium or not ? (eg. Koyama+96) Tsuru+ (Suzaku2007)

15. Sgr B1 E.W : 1–2keV K-edge : 2–10 x 10 23 cm -2 X-ray reflection is more likely. 4. 6.4 keV clumps : New and Revisit Nobukawa+0 8 Nakashima+1 1 Nakajima+09Inui+09 Hyodo+08 Takigawa+ Ryu prep Uchiyama+11 Uchiyama #35

16. Fig. 2b: 4-6 keV image →Electron bombardment is conceivable ! Since Radio Arc is a site of relativistic electrons, it may also include Low Energy Cosmic Ray electrons (LECRe). 4.735GHz (radio) image Fukuoka+09 Fe EW(Fe) 〜 0.20 keV Γ=2.5(1.9-2.7)

17. example 6.4 keV 1 0.5 0 -0.5 -1 ( l deg) 5. Discovery of diffuse 6.4keV emission from the intercloud regoin. Uchiyama+11 Uchiyama #35 ABDCE 6.4 keV line intensity Diffuse 6.4keV line emission exits in the intercloud region.

18. 18 Summary of My Talk 6 Middle-Aged and 1 young SNR candidates Discovered a Super bubble, “Chimney”, Strong RRC of G359.1-0.5 and Diffuse Thermal Emission of Tornado Origin of He-Fe-Kα in the GC is different from GR Discovered or Revisited 12 XRNe Discovery of a 6.4keV clump due to Electron bombardment. Discovery of diffuse 6.4keV emission from the intercloud region. Nobukawa-san’s Talk The data are open. A lot of (new) themes can be found. Please join us and explore new sciences in the GC region.

19. Thank you.