1. The Best Performance of XIS is the
best S/N ratio at hard X-rays: 　e.g. GC
Suzaku:　180 ksec
Chandra 600ksec (Muno et al. 2004)
XMM ksec (Tanaka)

2. Ｏｒｉｇｉｎ ｏｆ GCDX＆GRDX： Ｉｆ Diffuse, we need huge Energy  Point Source ?
Results of PV– AO3 (Long　Project)　
Ｉｍａｇｅ

3. We Ｓｅｐａｒａｔｅd　GCDX＆GRDX （flux and the Kα/Lα: l = 1-2）
Origin is not the same　!
Key Project：　Ｅｘｔｅｎｄ　ｔｏ　ｔｈｅ　
Ｇａｌａｃｔｉｃ　Ｒｉｄｇｅ　
FeXXV-Kα
FeXXVI-Lα/FeXXV-Kα
FeXXVI-Lα

4. Two Scale-Heights in the GCＤＸ (but ＧＲＤＸ ?)
　　　　　　Small : SN, GC Flare　　Large : WD, Active star　
l =-1.2: ? ?
Scale heights
as a function
of the galactic longitude

5. Key Ｐｒｏｊｅｃｔ Determine the Scale Height & Spectrum (for both the GC&GR
And
Large & Small Scale
Height ) Key for the
Origin

6. （１） Quantitatively separate 6.4keV-line+continuum (XRN?) &
New method and subject
（１） Quantitatively separate
6.4keV-line+continuum (XRN?) &
6.7keV-line+continuum (hot plasma)
 Origin/correlation of the 6.4keV-line
to the molecular cloud/TeV Diffuse
= new frontier of high energy Galaxy
6.7 keV-line
6.4 keV-line
Scale height =0.5 deg
This HESS　UID is a GC source
6.7 keV+0.5×6.4-keV

7. （２） Absorption vs the 6.4 keV line  3-dimensional Cloud Positions
2.5—3.5 keV band
(absorption）
6.3—6.5 keV band
(6.4 keV-line)
CS-line
Submitted to PASJ
Structure
of the
GMZ/GC

8. This project is highly Productive
1) G (Fukuoka), submitted
2) Sgr B a Face-on View (Ryu), submitted
3) Super bubble candidate In the GC (Mori) submitted
4) 6.4 keV line and Sgr B complex (Ryu) , in prep.
5) Neutral K-shell lines (Nobukawa) in prep.
6) keV distribution Letter (Uchiyama) in prep.
7) 1 keV GC plasma structure (Uchiyama)
8) 2.45 keV loop in Sgr C (Tsuru)
9) 0.6 keV Foreground Emission (Matsumoto)
10) Unidentified HESS (Matsumoto)
11) 6. 4keV emission from Sgr E (Tsuru)
12) Tornado Emission (Sawada)
13) G SNR (?)
14) keV distribution Full paper (Uchiyama)
15) 6.4 keV Jet of Great Annihilator (Nobukawa)
16) Discrete Sources or SNRs (Osaka)
17) Hard X-ray (Saitama)
　　Key project, 30papers , in total
This project is highly Productive
I said when I proposed the Long project （ＧＣ）that;
(1) I will write 20 Refereed Papers with in 1 year　　　　　
　　　　　　　After one year , 21 Papers
(2) With the long Project data I will write 20
papers
(The data of the Long project have just came in,
But even from QL, I can pick up 17 subjects ）
Yes We have done
what we said

9. Ｓｕｒｖｅｙ　ｏｆ　 GRＤＸ: 　 Search for possible connections between diffuse X-rays (Faint & Non-Thermal) and TeV/Fermi/Radio Sources
All these Sources are on the Galactic Ridge, so even if we get upper limit, the data itself is GRDX
= Crisis Management (Important Concept of KP)

10. Survey of Diffuse Hard Sources in GC/GR
(1) Discovery　of New Sources （surely exist）
(2) Extended TeV Sources
(3) Extended Fermi Sources
(4) Radio SNRs (X-ray faint, Non-Thermal)
Systematic Study of these Objects will surely
produce the Suzaku Legacy
1. “Suzaku Catalog of
the K-shell line Sources
in the GC”
2. “---in the Galaxy”　（Ｋｅｙ　Ｐｒｏｊｅｃｔ）
Yes
You can
Yes we can work
out
SNR candidates
XRN candidates

11. ”the X-ray” is the Flagship Satellite/Group in Space Japan
Ｒｅｆｅｒｅｅｄ　Ｊｏｕｒｎａｌ　 of
ASCA and Suzaku
The former director Prof. Tsuruta said “I approved Astro-E Astro-E2 (Suzaku) because
”the X-ray” is the Flagship Satellite/Group in Space Japan
Papers
If the Suzaku Papers
< 1/3 of the ASCA,
we may not be the
Flagship Satellite/Group
in the Space of Japan.
The GC/GR Project will
largely increase this ratio.
Years after launch
Papers
Summary PV—AO2
Observations Papers
Total 35 Msec
GC 1.5 Msec
Ratio 4 % %
21×35/1.5= 490
Ｒｅｆｅｒｅｅｄ　Ｊｏｕｒｎａｌ　
of GC and Total
Years after launch

12. Suzaku Statistics (by the end of Feb. 2009)
(Except Gamma-Ray Burst, Instr, Cal)　　
Target Exposure Papers
(Msec) (refereed)
Extra Diff
Extra Com
Gal Diff
Gal Com
Total

13. Suzaku Statistics (by the end of Feb 2009) (Except Gamma-Ray Burst, Instr, Cal)