1. The Galactic Center is a Treasure Box of High Energy Physics The Nearest AGN and Star Burst Galaxy. I will report a current picture of the Galactic Center, then move on the Astro-H perspect ive (1) Global structure of GCXE and GRXE Origin ? --> Star Burst Activity or AGN? (2) AGN Activity : Kα line of neutral iron What can we learn with SXS and HXI+SXI ?

2. GCXE GRXE GRXE LPLP HPHP 5—8 keV Fe I (6.4 keV) Fe XXV -KaFe XXVI -Lya S XV -KaS XVI -Lya

3. l, b distribution of Low & High Temperature Plasma (LP, HP) and Neutral Iron (Uchiyama et al. 2012 in preparation) Soft (2.3-5 keV) S XV-VI Hard (5—8 keV) Fe XXV-VI Fe I (6.4 keV line) GCXE 0.5 deg l b 5 deg 0.5 deg 50 deg l GRXE 17-60 keV band (Integral) scale height ~10 deg. ( Krivonos et al. 2007)  Astro-H (HXI)

4. GCXEGRXE kT H (keV)7.4 6.7 kT L (keV)0.98 1.45 Ab (solar)1.350.71 EM H /EM L 0.370.42 Γ2.1 EW 6.4 (eV)445 2-kT plasma + 6.4 keV line (Uchiyama et al. 2012 in preparation) GC GR GC GR S Ar Ca Fe

5. Using this strong line (single), we measure the Galactic rotation curve. ΔV ~ 10 km/s Does Hot plasma show similar rotation as hose of stars, cold gas, star clusters or same ? expansion ? Lugten et al. 1986 Crawford etal. 1985 Plasma states (collisional ex, recombination, & temperature). So Astro-H can determine more reliable parameters

6. 6 Past flare of Sgr A* indicated by the 6.4keV Line B Sgr D A C E Nobukawa et al. 2011 Ponti et al. 2010 Capelli et al. 2012

7. Hard X-ray=Compton Scattered Component Sgr B2 (20-60 keV) calibrator Fe K line (Inui et al. 2009) Terrier et al. 2010

8. Activity of Sgr A*(SMBH) In the Past, at Present, and in near Future ？ 2014 ？ Clump2, Sgr D & E We need 3-D position (not only projected distance) and density of the molecular cloud. 1) Suzaku method  Astro-H methods 2) EW 6.4 = 850Z Fe / (1 + cos 2 θ) (eV), Z Fe ~ N Fe (iron edge) 3) Compton shoulder of the 6.4 keV line, E edge =6.4/(1.013+ 0.013cos θ ) (keV)

9. Sgr A* Behind Front プラズマ成分 Absorb ed MC Ryu et al. 2010,2012 very delicate spectrum analysis. We need accurate spectra (Astro-H SXS) X-ray Tomography Observer

10. e - (keV) σ ∼ 0 eV p (MeV) σ ∼ 10 eV XRN (Sgr B2, Radio Arc) : Detection of Compton shoulder --> cos θ and N Fe Other regions: Separation of the 6.4 keV and Thermal Plasmas If N FE is small, then origin may be electron or proton Sgr B2 Radio Arc N FE Compton shoulder

11. HXI:Hard X-ray Imaging Spectroscopy of Sgr A* and Sgr B Sgr B2 NGC 4151 (Sy-1 AGN) Revnivtsev et al. 2004 Zdziarski et al. 2002 Belanger et al. 2004, 2006 20-30 keV30-40 keV 40-56 keV 56-85 keV Integral (IBIS/ISGRI )

12. Compton Mirror of Sgr A* Neronov et al. 2005 Revnivtsev et al. 2004 Sgr A Sgr B2 (Mirror of Sgr A* when it was 10 5-6 times brighter) r = 6’ (Sgr A*+ diffuse) r = 15’’ (SgrA* only) Astro-H can observe Sgr A* both in the “active” and “quiescent” states. With Astro-H/HXI we can determine contamination(GCXE)-free Sgr A* (present) and Sgr B (past) spectra. Accretion on Sgr A* at present is RIAF, How was in the past flare.

13. Fermi Bubble & Jet Su et al.2010 These past activities possibly had large impacts on the GC plasma. Even at present, the GC plasma may be transient or in dynamical phase.

14. GP 120 pc kTz > kT e = 0.58 keV nt= 7.9×10 11 s/cc Si-Lyα RRC Jet of Recombining Plasma ? Nakashima et al. 2012, in pre. Senda et al. 2006 1’ kTz =kT e = 0.66 keV

15. Summary Galactic Center region is ideal laboratory for High energy Astronomy with many variety of active phenomena. These phenomena are closely related with each other, and hence these are “degenerated” The past instruments were not able to resolve the “degeneracy”. Astro-H is the first satellite to resolve the “degeneracy”.