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 perspective

(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 ?

GCXE GCXE GRXE GRXE

LP

HP

5—8 keV Fe I (6.4 keV)

Fe XXV-Ka Fe XXVI-Lya

S XV-Ka S XVI-Lya

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)

GCXE0.5 deg

l

b

5 deg 0.5 deg

50 deg l

GRXE17-60 keV band (Integral) scale height ~10 deg. (Krivonos et al. 2007) Astro-H (HXI)

GCXE GRXEkTH (keV) 7.4 6.7 kTL (keV) 0.98 1.45 Ab (solar) 1.35 0.71EMH/EML 0.37 0.42Γ 2.1EW6.4 (eV) 445

2-kT plasma + 6.4 keV line

(Uchiyama et al. 2012 in preparation)

GC

GR

GC

GR

S Ar Ca Fe

S Ar Ca Fe

Using this strong line (single), we measure the Galactic rotation curve. ΔV ~ 10 km/sDoes Hot plasma show similar rotation as hose of stars, cold gas, star clusters or same ? expansion ?

Lugten et al. 1986Crawford etal. 1985

Plasma states (collisional ex, recombination, & temperature). So Astro-H can determine more reliableparameters

6

Past flare of Sgr A* indicated by the 6.4keV Line

BSgr D A C E

Nobukawa et al. 2011

Ponti et al. 2010Capelli et al. 2012

Hard X-ray=Compton Scattered Component

Sgr B2(20-60 keV)

calibratorFe K line(Inui et al. 2009)

Terrier et al. 2010

Activity of Sgr A*(SMBH)

In the Past, at Present, and in near Future 　

Light Curve of Sgr A*

Past Present-10-100

Time (yr)

-1000

1040

1039

1038

1037

1036

1035

1034

1033

Sgr

A*

Lum

inosi

ty (

erg

s/s)

1041

1042

-104

Sgr B, CSgr A ？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 methods2) EW6.4 = 850ZFe/ (1 + cos 2θ) (eV), ZFe ~ NFe (iron edge)3) Compton shoulder of the 6.4 keV line, Eedge=6.4/(1.013+ 0.013cos θ ) (keV)

Sgr A*

Behind

Front

プラ

ズマ

成分

Absorbed

MC

Ryu et al. 2010 ,2012

very delicate spectrum analysis. We need accuratespectra (Astro-H SXS)

X-ray Tomography

Observer

e- (keV)σ∼0 eV

p (MeV)σ∼10 eV

XRN (Sgr B2, Radio Arc) : Detection of Compton shoulder --> cos θ and NFe Other regions: Separation of the 6.4 keV and Thermal Plasmas

If NFE is small, then origin may be electron or proton

Sgr B2 Radio Arc

NFE

NFE

Compton shoulder

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 keV 30-40 keV

40-56 keV 56-85 keV

Integral (IBIS/ISGRI)

Compton Mirror of Sgr A*Neronov et al. 2005 Revnivtsev et al. 2004

Sgr A

Sgr B2(Mirror of Sgr A* when it was 105-6 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.

Fermi Bubble & Jet

Su et al.2010

These past activities possibly had large impacts on the GC plasma . Even at present, theGC plasma may be transient or in dynamical phase.

GP

120 pc

kTz > kTe= 0.58 keVnt= 7.9×1011 s/cc

Si-Lyα RRC

Jet of Recombining Plasma ?

Nakashima et al. 2012, in pre.

Senda et al. 2006

1’

kTz =kTe= 0.66 keV

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”.