the galactic center is a treasure box of high energy physics the nearest agn and star burst galaxy....
TRANSCRIPT
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 ?
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”.