Suzaku perspective on the Galactic Center

Slides:



Advertisements
Similar presentations
(2) Profile of the Non-Thermal Filaments of SNRs =>High Energy Particle Acceleration =>High Energy Particle Acceleration In all the SNRs & GC Non Thermal.
Advertisements

Astro-E2 target: The Galactic Center Red: 1-3 keV Green: 3-5 keV Blue: 5-8 keV Sgr B2 Wang et al Yoshitomo Maeda Hiroshi Murakami 2 degree The Arches.
X-ray Astronomy with High Spectral Resolution: Astro-E2 / ISAS Y. Tanaka.
Science results. N. Produit INTEGRAL science results 2 INTEGRAL is on a 3-days orbit with apogee at km and perigee at km. Maximizes time.
Suzaku Discovery of Fe K-Shell Line from the O-rich SNR G Arxiv: Fumiyoshi Kamitukasa et al.
Fluorescent Iron-Line Emission in the Galactic Centre Bob Warwick University of Leicester, UK.
Q. Daniel Wang and Cornelia Lang (U. of Massachusetts) Eric Gotthelf (Columbia U.) Chandra X-ray Survey of the Galactic Center: On the Nature of the X-ray.
1 Origin of Variability of X-ray and γ-ray Spectra on Daily Scale Radovan Milinčić Astrophysics 711 May 3 rd 2005.
Discovery of New SNR Candidates in the Galactic Center Region with ASCA and Chandra Atsushi Senda 1, Hiroshi Murakami 2, Aya Bamba 1, Shin-ichiro Takagi.
Our Galaxy The Milky Way. The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band.
X-Ray Observations of SN1006 Koyama, K. Kyoto University Palmieri et al (1972) Ballon : The first X-ray detection Winkler and Laird : OSO7 The spectrum.
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,
Tycho’s SNR SNR G "To make an apple pie from scratch, you must first invent the universe." ~Carl Sagan.
The VHE gamma-ray sky viewed with H.E.S.S. Werner Hofmann MPI für Kernphysik Heidelberg © Philippe Plailly HESS = High Energy Stereoscopic System.
The Hot Plasma in the Galactic Center with Suzaku Masayoshi Nobukawa, Yoshiaki Hyodo, Katsuji Koyama, Takeshi Tsuru, Hironori Matsumoto (Kyoto Univ.)
Suzaku, XMM-Newton and Chandra Observations of the Central Region of M 31 Hiromitsu Takahashi (Hiroshima University, Japan) M. Kokubun, K. Makishima, A.
Suzaku Study of X-ray Emission from the Molecular Clouds in the Galactic Center M. Nobukawa, S. G. Ryu, S. Nakashima, T. G. Tsuru, K. Koyama (Kyoto Univ.),
Collaborators: Michael Muno (UCLA) Frederick Baganoff (MIT) Yoshitomo Maeda (ISAS) Mark Morris (UCLA) George Chartas (Penn State) Divas Sanwal (Penn State)
High Energy Sky with Advancing Technology The Galactic Center View From Tenma--Suzaku Hakucho (1979)96 kg Tenma (1983) 216kg Ginga ( 1987 ) 420 kg ASCA.
Discovery of K  lines of neutral sulfur, argon, and calcium atoms from the Galactic Center Masayoshi Nobukawa, Katsuji Koyama, Takeshi Go Tsuru, Syukyo.
Fe XXV Kα Fe I Kα S XV Kα Strong Fe XXV Kα, S XV Kα, and Fe I Kα  the GCXE consists of High Temperature Plasma (HP), Low Temperature Plasma (LP), and.
Sgr B2 Galactic Center Survey with Chandr Radio Arc 1 Sgr A East : Young SNR 2 The GC Hot Plasma : 10keV 3 Sgr B2, Radio Arc : Molecular Clouds ~2 x 1.
The Suzaku Results of the Galactic Center X-rays - Collisinal Excitation or Charge Exchange ? - Katusji Koyama, Kyoto University Nickname Suzaku An Ancient.
Spatial Distribution of the Galactic Diffuse X-Rays and the Spectral/Timing Study of the 6.4-keV Clumps Katsuji Koyama Department of Physics, Graduate.
Takayasu Anada ( anada at astro.isas.jaxa.jp), Ken Ebisawa, Tadayasu Dotani, Aya Bamba (ISAS/JAXA)anada at astro.isas.jaxa.jp Gerd Puhlhofer, Stefan.
X-ray observation of the Cygnus Loop with Suzaku and XMM-Newton
Hard X-Ray Emission of Quasi- Thermal Electrons from the Galactic Ridge V. A. Dogiel 1,2, Hajime Inoue 1, Kuniaki Masai 3, V. Schoenfelder 4, and A. W.
Discovery of K  lines of neutral S, Ar, Ca, Cr, & Mn atoms from the Galactic center with Suzaku Masayoshi Nobukawa, Katsuji Koyama, Takeshi Go Tsuru,
Recent Progress in Understanding X-ray Emission From Early-type Galaxies: The Hot Gas Component Jimmy A. Irwin University of Michigan X-rays From Nearby.
High Energy Astrophysics in the Next Decade International Workshop on NeXT and Future Missions Tokyo Metropolitan University June 21-23, 2006.
Eugenio Ursino on behalf of the UM Astrophysics Group University of Miami, USA Looking for the Missing Baryons.
1) Origin of 6.7/6.9 keV (He-like/H-like Fe Ka) Lines : Collisional Excitation or Charge Exchange 2) Discoveries of New SNR Candidates 3) Origin of 6.4.
Suzaku Observation of the Galactic Center Region Takeshi Go Tsuru (Kyoto University) _Suzaku2011_GC_v14.key R.Fukuoka, Y.Hyodo, T.Inui, K.Koyama,
The “youngest” Ia SNR in the Galaxy. The best to study early phase of Type Ia Cosmic Ray acceleration at the Shell The best to study the cosmic ray origin.
Publication List (refereed Journal) using the GC data 1 Sawada et al.2011,PASJ (submited) 2 Uchiyama et al.2011,PASJ (submited) 3 Ohnishi et al.2011,PASJ.
Galactic Center Diffuse Emission Katsuji Koyama, Kyoto University (1) FeXXV-Kα Line (6.7 keV) Diffuse or Point Sources ? Flux distribution Equivalent width.
The Galactic Center region The Galactic Center region K. Koyama and A. Senda (Kyoto-U) Y. Maeda and H. Murakami (ISAS / JAXA) Y. Maeda and H. Murakami.
Discovery of the X-ray emission from the darkest TeV object HESS J
High Energy Neutrinos and Gamma Rays from the Galactic Center
Chandra Science Highlights
NuSTAR + XMM Observations of NGC 1365: A Constant Inner Disc
Recent Suzaku Results on Strongly Magnetized Neutron Stars
Fermi Bubble Z.G.,Xiong.
Magnetar SGR By Christina Balanduk
A large XMM-Newton project on SN 1006
Asami Hayato (RIKEN / Tokyo Univ. of Sci.)
The Milky Way Galaxy.
Suzaku The Suzaku Results of the Galactic Center X-rays Nickname
Our Milky Way Galaxy.
A large XMM-Newton project on SN 1006
Suzaku First Results on Galactic Diffuse Objects
XMM-Newton Observation of the composite SNR G0. 9+0
Search for Bulk Motion in A2256 with Suzaku and ASTRO-H
X-ray Observations of the Dark Particle Accelerators
Suzaku Observations of our Milky Way Center
Galactic Center Diffuse X-rays with Suzaku
The X-ray perspective on young stellar populations in objects
X-rays from the Galactic Center
The Best Performance of XIS is the
Suzaku Observation of Tycho’s Supernova Remnant
超新星遗迹 的XTP 观测模拟 南京大学 陈阳、周平、张潇.
Our Galactic Center and its Environmemt K. Koyama A. Senda
Q. Daniel Wang and Cornelia Lang (U. of Massachusetts)
SNR 的XTP 观测模拟 南京大学 陈阳、周平、张潇.
The Galactic Diffuse X-Rays and Time Variability of the 6.4-keV Clumps
Target selection The GC hot plasma Sgr A East Sgr B2 / Radio arc
Katsuji Koyama Kyoto University X-ray or Electron irradiation ?
Galactic Center Diffuse X-rays with Suzaku
Cornelia C. Lang University of Iowa collaborators:
Presentation transcript:

Suzaku perspective on the Galactic Center The “40-keV Plasma” vs “10-keV Plasma” What is the Origin of the 6.7 keV-line Plasma ? Are the Galactic Center and Ridge emissions Same Origin ? Big bang of Sgr A* or Multi-SNe or ? (1) X-ray reflection Nebulae: Sgr B2, Sgr C, M0.01-0.09 (2) Supernovae and SNRs: Sgr A East, G359.8 G0.570 (3) Non Thermal Jets, Filaments, and Shell

What is our Galactic Center ? Who resembles the Milky Way ?      2   5           2  5    2 5 10 keV 6.64keV, EW=120eV Milky Way NGC253 NGC1068 6.4keV, EW=1200eV 6.7 1430eV 6.9 494eV     2   10 5    10  5 10  NGC253: Pietsch et al. 2001, M81:Page et al. 2004, M31: Takahashi et al. 2004, NGC1068: Matt et al. 2004

(1) X-ray Reflection Nebula Sgr B2 M0.01-0.09 Sgr C Under Construction

(1’) Other 6.4 keV line Clump

Kicked-off Neutron Star ? Foreground source (2) Sgr A East =Young SNR Thermal Plasma ( ~ 4 keV) Kicked-off Neutron Star ? Sgr A* Park et al. 2005 Sakano et al. 2004 Sgr A East (age ~1000 year) Maeda et al. 2002

(3) Non Thermal Structrue Shell of SNR ? like SN1006 or due to Nuclear Burst ? Sakano et al. 2003

1 2 3 Non Thermal X-ray       Jets and filaments

Key Questions on the iron line ASCA Mapping with thw3-iron Lines Key Questions on the iron line Which line is clumpy ? Only 6.4 keV line (XRN) ? How about 6.7 and 6.9 keV lines ? Are these intensities and the line ratio uniform ? Any non-thermal structure ? Suzaku Mapping of 6.4, 6.7 and 6.9 keV line with a unit scale of ~5 arc-min.

Sgr B2 other structure G0.570-0.018 Chandra 100 ksec XISx4 100 ksec

1 arcmin region spectra The East of Sgr A* Chandra 50 ksec XISx4 100 ksec

The West of Sgr A* and Sgr C XISx4 100 ksec

Hard Diffuse Component According to the latitudinal scanning observation of RXTE-PCA, the intensity of diffuse emission at the Galactic center can be estimated.