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X-ray follow-ups of TeV unID sources using Suzaku

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X-ray follow-ups of TeV unID sources using Suzaku. Aya, T. Bamba (ISAS/JAXA, Japan) R. Yamazaki, K. Kohri, H. Matsumoto, H. Yamaguchi, G. Pühlhofer, S. J. Wagner. 1.1. Origin of Cosmic rays. Who and how to accelerate cosmic rays up to knee ?

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slide1
X-ray follow-ups of TeV unID sources

using Suzaku

Aya, T. Bamba

(ISAS/JAXA, Japan)

R. Yamazaki, K. Kohri, H. Matsumoto, H. Yamaguchi,

G. Pühlhofer, S. J. Wagner

slide2
1.1. Origin of Cosmic rays

Who and how to accelerate cosmic rays up to knee ?

diffusive shock acc. in shocks ? = biggest problem !

difficulties: rg ~ pc in interstellar B

-> we cannot point out accelerators

How to search for accelerators ?

TeV electron

IS B. (~mG)

synchrotron X-rays

Inverse Compt. (e)

piondecay (p)

TeV gamma-rays

hard X-rays and TeV gamma-rays are the best

for the accelerator search.

slide3
1.2. New Candidates:

TeV unID sources

A lot of sources are

discovered from the GP

They are not

known PSRs, PWNe

known SNRs

known SF regions

known EGRET source

“TeV unID sources”

“dark particle accelerators”

(Aharonian+ 2006)

X-ray follow-ups are needed !

slide4
1.3. X-ray follow-ups of TeV unIDs (1): known categories

PWN !!

HESS J1718-3825

XMM-Newton

(Hinton+ 2007)

HESS J1837-069

Chandra

(Gotthelf+ 2008)

HESS J1813-178

XMM-Newton

(Funk+ 2007)

(See also Pühlhofer’s invited talk, Uchiyama+ poster D12)

SNR !!

Many samples are PWN

CTB37B

Suzaku

(Nakamura+

submitted)

slide5
1.4. X-ray follow-ups of TeV unIDs (2): unknown categories

Some source but unID !!

No counterpart !!

HESS J1614-518

Suzaku (Matsumoto+ 2008)

HESS J1616-508

Suzaku (Matsumoto+ 2007)

Compact unID sources !!

Molecular cloud ??

HESS J1804-218: Suzaku (Bamba+ 2007)

Galactic center region

radio obs. (Aharonian+ 2006)

Many kinds of TeV unIDs !

slide6
2.1. One of the most mysterious TeV unIDs

: HESS J1745-303

  • Discovered by H.E.S.S. (Aharonian+ 2005)
  • Near the Galactic Center
  • One of the most extended source (~0.5 deg)
  • Rather soft (Gamma=2.7) and bright (5.2x10-12ergs cm-2s-1)
  • No couterpart !

-> Suzaku is the best toolfor the counter part search: low and stable bgd

0.5 deg

This one !

50ks x 4 pointing

mapping obs.

color: TeV

contour: molecular cloud

slide7
2.2. Suzaku image of HESS J1745-303 (1)

No X-ray !

SNRs

G359.0-0.9, G359.1-0.5

(Bamba+ 2000)

ROSAT sources

0.5-2.0 keV (Suzaku)

contour: HESS

slide8
2.3. Suzaku image of HESS J1745-303 (2)

No X-ray !

2.0-8.0 keV (Suzaku)

contour: HESS

slide9
2.4. Suzaku image of HESS J1745-303 (3)

6.4 keV ion line (Suzaku)

contour: HESS

Some excess on HESS J1745-303 ??

slide10
3.1. Spectral Analysis (1)

continuum comp.

src

Src: TeV peak region

bgd: TeV free region

bgd1

bgd2

Compare the flux

(Assuming Gamma = 2.0)

F2-10 keV < 2.1 x 10-13 ergs cm-2s-1

c.f. F1-10TeV = 5.2 x 10-12 ergs cm-2s-1

one of the mostX-ray faint

TeV unIDs!

F1-10TeV

F2-10keV

> 25

slide11
3.2. Spectral Analysis (2) neutral iron line

src

6.4 keV flux density 6.7 keV flux density 6.4/6.7

(ph/cm2/s/arcmin2) (ph/cm2/s/arcmin2)

src: 6.5e-8 ± 0.7e-8 1.1e-7 ± 0.08e-7 0.58 ± 0.03

bgd1: 5.9e-8 ± 2.2e-8 1.2e-7 ± 0.2e-7 0.49 ± 0.20

bgd1

Src region has stronger 6.4 keV line

although the statistics is not enough …

bgd2

6.7keV

(He-like Fe)

6.4keV

(neutral Fe)

5.9keV

(MnKa: bgd)

Src

Ni Ka

(bfd)

total excess:

6.1x10-6 ph cm-2s-1

bgd1

slide12
4.1. Discussion 1: Nonthermal continuum emission

F2-10 keV < 2.1 x 10-13 ergs cm-2s-1

F1-10TeV = 5.2 x 10-12 ergs cm-2s-1

different from known sources (SNR/PWN …)

c.f. Crab: FTeV/FX ~3x10-3

RXJ1713: FTeV/FX ~ 0.06

The TeV gamma-ray emission from the GC MCs

MC are faint in nonthermal X-rays

HESS J1745 coinsides with MC

(Aharonian+ 2008)

HESS J1745 could emit TeV gamma-rays

in the same way of the TeV GC emission

F1-10TeV

F2-10keV

> 25

(Bitran+ 1997)

(Aharonian+ 2008)

slide13
4.2. Discussion 2: neutral iron line

neutral iron line near the GC, coinside with MC

= reflection on the MC by the past bright GC

(Koyama+ invited talk, Murakami+ 2001)

Sgr B2 HESSJ1745

line Int. 5.6e-5 6.1e-6

MMC 6e6 Mo 5e4 Mo

size 0.05 deg. 0.3 deg.

d from GC 0.7 deg. 1.2 deg.

line int. ~ mass x viewing angle

~ mass x (size)2 x (distance)-2

HESSJ1745:

7.0e-6 ph cm-2s-1

The neutral iron line can be explained

by X-ray reflection of the past bright GC

HESS J1745-303 – MC association in the GC region !

could be similar source to the TeV GC emission

Cosmic rays make TeV emission with attacking MC ???

(Aharonian+ 2006)

Where is the CR source ?? G359.1-0.5 ??

slide14
5. Summary
  • The origin of TeVunID sources are still unknown.
  • HESS J1745-303 is one of the most interesting source
                  • near the Galactic center.
  • We made deep X-ray follow-ups of HESS J1745-303
                  • with Suzaku.
  • We made tight upper-limit in the X-ray band.
  • The excess of neutral iron line is found from the MC,
              • which could associate the TeVunID.
                • HESS J1745-303 could be TeV emission from a MC
        • with CR attacking like GC diffuse TeV emission.
  • In order to pinpoint the origin of this interesting source,
    • more follow-ups are needed in other wavelengths.
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