Suzaku First Results on Galactic Diffuse Objects

Hironori Matsumoto (Kyoto Univ., Japan)

and

The Suzaku team

Contents

•The Suzaku Satellite•Galactic center region•Dark particle accelerators•SN1006•Cygnus Loop

The Suzaku SatelliteJapan 5th X-ray SatelliteLaunched July 10, 2005

God bird “Suzaku”from ancient

myths

InstrumentsXRT (X-Ray Telescope)

XIS (X-ray Imaging Spectrometers)

HXD (Hard X-ray Detector)

X-ray CCD x 4 (3FI + 1BI)

Low & stable background

Large Effective Area 255cm2x4

Wide range (10-600keV)Low background

Poster 18.24 Tsuru et al.

Poster 18.29 Kokubun et al.Poster 18.13 Mori et al.

XRT+XISBest for diffuse

and dim objects!

The Galactic Center RegionMany emission lines are detected for the first time!(neutral Ni Kα, He-like Ni Kα, He-like Fe Kγ etc.)

G.C. & SgrA east 5min

Galactic Center Image6.3-6.5 keV (Fe I Kα)

6.6-6.8 keV (He-like Fe Kα)

Cool Material ( ～ 10K)

What is the origin? Collisional excitation, or charge exchange?

Galactic center.

5min

Plasma DiagnosticCollisional excitation Charge exchange

r

f

i

fr

iHigh res. High res.Low res. (CCD) Low res. (CCD)

6666±5eV6680-6685eV

Suzaku XIS: He-like Fe Kα center 6680±1eV(stat.)±4eV(syst.)

The line center observed with Suzaku favors the collisional excitation = hot plasma (108K)

(See Koyama et al. 2006 PASJ in print; astro-ph/0609215)

Dark Particle Accelerator?

HESSJ1616-508 HESSJ1804-216

HESS image in the TeV band

XIS FOV

Both are bright and diffuse TeV Objects

(Thanks to Prof. W. Hoffman and Prof. S. Funk)

XIS ImagesHESSJ1616

No counterpart!

Very dim & compact counterpart?3-12 keV

HESSJ1808 Center of HESSJ1808

2-10 keV

Fx(2-10keV)<3.1e-13erg/s/cm2

1: Fx(2-10keV)=2e-13erg/s/cm2

2: Fx(2-10keV)=4e-13erg/s/cm2

1

2

Target FTeV/FX

HESSJ1616 >55

HESSJ1804 ~10

Crab (PWN) 3e-3

RXJ1713 (SNR) ~0.06

We see hadronic process?

Real Dark Accelerator!

Matsumoto et al. 2006 PASJ in print; astro-ph/0608475Bamba et al. 2006 PASJ in print; astro-ph/0608310

SN1006O-band image

FIBI

ONe

Mg Si

SAr

Ca Fe

First detection of emission lines from S, Ar, Ca, Fe!

Center energy of Fe: 6.43 keV low nt ( ～ 109cm-

3s) plasma

Cygnus Loop

ROSAT HRI

XIS FOV

First detection of C & N lines!

C dominant (C : N : O ～ 5 : 2: 1) He burning origin (massive star)?

log

linear

XIS BI spectrum

(Miyata et al. 2006 PASJ in print)

Summary

1. Suzaku XRT+XIS is the best combination for studying diffuse emission.

2. The origin of He-like Fe Kα emission at the Galactic center is the collisional excitation (i.e. hot gas).

3. Real dark particle accelerators are discovered.

4. First detection of S, Ar, Ca, and Fe lines from SN1006.

5. We found C and N lines from the Cygnus Loop.

You can see many other results from Suzaku !

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