_ASJ_GC_ASTRO-H_v3.key

Transcription

1 X _ASJ_GC_ASTRO-H_v3.key

2 Counts s 1 kev deg Energy (kev)

3 中性鉄輝線 = 高エネルギー粒子が冷たい分子雲を照射 Inui+09 Nobukawa+08Hyodo+08 Takigawa+ Nakajima+09 Nakashima+11 Ryu prep Uchiyama+11 Sgr B1 E.W : 1 2keV K-edge : 2 x 23 cm-2 Sgr A*からのＸ線照射

4 4 (6.4 kev) l b= pm 0.05 deg ) 2 /arcmin 6.4 kev line flux 2 Intensity (1e-7 photons /s /cm Galactic Longitude l (deg) -3-4 Intensity (K km/s ) 2 13CO (NANTEN, Takeuchi+) Galactic longitude l (deg) -3-4

5 5 ASCA : Fe line center Maeda89 12CO (Oka+98) Sgr B Sgr C l = 3.2 Clump 2 l = 3.5 exhibits especially strong 6.4 kev line AO-7 (1Msec) or

6 6 Candidates for the ionizing particles 6.4 kev flux ~1e-7 ph/cm2/sec/arcmin2 is expected in the KP observing region XRN (X-ray Reflection Nebula) Already seen in the GC. Sgr A* Lx(Sgr A*) ~^41 ergs/s LECRp (Low Energy Cosmic Ray Proton) NH ~ 1e+24cm-2 (observed at Clump 2) Up > 75eV/cm3 equipartition with B > 50μG at R<400pc (Crocker+11) ~0.5e-7 ph/cm2/sec/arcmin2 LECRe (Low Energy Cosmic Ray Electron) cf. Valinia+00 Ue~1 ev/cm3 x NH 1e+23 cm-2 1e-7 ph/cm2/sec/arcmin2 All the three processes are possible.

7 EW (kev) 7 XRN LECR LECRe LECRp 2 Dogiel+11 p 1 e Spectral Index XRN: EW LECR: LECRe ev LECRp ev

8 LECRe LECRp 8 EW e or p ASTRO-H e - (kev) σ 0 ev p (MeV) σ ev O (MeV) σ 0 ev log( ) 6.4keV GeV/TeV γ p? kev MeV GeV TeV

9 If XRN 9 Sgr A* Luminosity (ergs/s) Light Curve of Sgr A* in years Clump 2 (Gillessen+12) Sgr B, C Sgr A Direct observation with Chandra Past Time (yr) Present Reveal the Activity of Sgr A* (SMBH) in 2000 years.

10 Plasma Parameters (assuming ZFe=1.2) Size = 52pc x 27pc ~0.70 L2- = 2 36 ergs/s nave ~ 0.1cm -3 ~0.36 npeak ~ 0.4cm -3 Egas ~ 3 52 ergs R: 6.7keV, G:2.45keV, B: 6.4keV Escape Time scale (latutude) τesc = Size/Cs = 2 4 yr Heating Rate = Egas/τesc ~ 5 40 ergs/s ~ -3 SN yr -1 Much higher than the current activity of Sgr A * (Lx=^33ergs/s) and ~ -5 SN yr -1 expected from the stellar mass in this region. Σ faint point sources? (CVs)

11 Global Distribution of Fe Kα Lines in the Galactic Center Region (b) 6.7keV Line Profile vs Stellar Mass Distribution Observed photons cm-s s-1 arcmin-2 x4 x (at b*=0.0) 6.7keV -6 x 6.7 kev line (EW=0.5 kev) ) This work Koyama+07 Yamauchi+09-5 Observed photons cm-s s-1 arcmin-2 Observed photons cm-s s-1 arcmin Distance from Sgr A* along the longitude l* (degree) Nuclear -5 stellar cluster Nuclear stellar disk Galactic Galactic This work bulge disk Koyama+07 Yamauchi+09-6 Nuclear bulge -7 Distribution of Point source flux (4.8-8 kev) * Distance from Sgr A along the latitude b* (degree) (d) -5-6 Truly diffuse plasma Nobukawa, Hyodo Sgr A* -8 Observed photons cm-s s-1 arcmin-2 a) Uchiyama

12 6.7keV He-Fe-Kα emission line P-V map of 6.7keV emission line Velocity 250km/s the Galactic rotation Point Sources Truly Diffuse Plasma (depending on a model) Position cf. Vthermal 120km/s 2deg ΔE=4eV (180km/s) is also important for the study of the plasma in the GC region.

13 13 2e+4yr x 0.1cm-3 ~ 0.1e+12 sec cm-3 ISM ( ) Ionizing Plasma rarefaction Recombining Plasma

14 Koyama, Hyodo et al. (2007) 6 8 He-Fe-Kβ/He-Fe-Kα kte=6.5kev Suzaku spectrum nτ > 2 12 sec cm -3 EI Normalizatino Ratio 6.9/6.7keV keV Center Energy kt=6.5kev ,-6eV 6.7-keV Line Center kt e =6.5keV Normalizatino Ratio 6.9/6.7keV 11 kt=6.5kev 12 VNEI 13 nt [sec/cm 3 ] 0.33±0.02 Line ratio 6.9/6.7-keV kt e =6.5keV nt [sec/cm 12 3 ] nt (sec cm -3 )

15 中性 Fe-Kα He-like Fe-Kα H-like Fe-Kα Edge Fe-Kβ Fe-Kβ, Ni Complex He-Ni-Kα He-Fe-Kβ H-Fe-Kβ He-Fe-Kγ H-Fe-Kγ 中性 Ni-Kα Koyama, Hyodo et al. (2007) He-Fe-RRC (8.8keV) H-Fe-RRC (9.2keV)

16 16 2e+4yr x 0.1cm-3 ~ 0.1e+12 sec cm-3 ISM ( ) Ionizing Plasma rarefaction Recombining Plasma IE

17 17 Pgas/k = 2e7 K/cm3 300μG B > 50μG at R<400pc (Crocker+11) ASTRO-H? P-V... No Info kt~1kev

18 Suzaku/XIS kev image Sgr A* Galactic Latitude (degree) 0.0 Jet? 銀河面 南北にのびる 360光年 巨大プラズマ Galactic Longitude (degree) GCからの噴出や爆発の証拠 Nakashima Murakami 再結合プラズマは無いのか

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