Target selection The GC hot plasma Sgr A East Sgr B2 / Radio arc

Slides:



Advertisements
Similar presentations
Charge Exchange Models for X-ray Spectroscopy with AtomDB v2.0 Randall Smith, Adam Foster & Nancy Brickhouse Smithsonian Astrophysical Observatory.
Advertisements

(2) Profile of the Non-Thermal Filaments of SNRs =>High Energy Particle Acceleration =>High Energy Particle Acceleration In all the SNRs & GC Non Thermal.
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.
Tom Esposito Astr Feb 09. Seyfert 1, Seyfert 2, QSO, QSO2, LINER, FR I, FR II, Quasars, Blazars, NLXG, BALQ…
Low Energy measurements of Cosmic Rays suggested by the HE group 1 1Tracing the distribution of matter in order to understand HE data Measurements of NH.
General Astronomy The Interstellar Medium Credits: Much of this slideset is modified from lectures by Dr. Peter Newbury (UBC)
Fluorescent Iron-Line Emission in the Galactic Centre Bob Warwick University of Leicester, UK.
Multiwavelength Sky by NASA. Radio Continuum (408 MHz). Intensity of radio continuum emission from surveys with ground- based radio telescopes (Jodrell.
CO J =1-0 + J =3-2 map (Oka+ 1999, 2007) Galactic Center Kunihiko Tanaka (1), Tomoharu Oka (1), Shinji Matsumura (1), Kazuhisa Kamegai (2), Makoto Nagai.
/72 X-ray Astronomy in our Galactic Center region Hironori Matsumoto Kobayashi-Maskawa Institute, Nagoya Univ. 1.
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.
The 511 keV Annihilation Emission From The Galactic Center Department of Physics National Tsing Hua University G.T. Chen 2007/1/2.
The HETGS view of the micro-quasar GRS Lee et al. 2002, ApJ., 567, 1102 COLLABORATORS : C.S. Reynolds (U. Maryland) R.A Remillard (MIT) N.S. Schulz.
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,
Nebular Astrophysics.
The Hot Plasma in the Galactic Center with Suzaku Masayoshi Nobukawa, Yoshiaki Hyodo, Katsuji Koyama, Takeshi Tsuru, Hironori Matsumoto (Kyoto Univ.)
1 Diagnostics of thermal plasma with eV-level Resolution Manabu ISHIDA Tokyo Metropolitan University.
The TeV view of the Galactic Centre R. Terrier APC.
About the 8 keV plasma at the Galactic Center CEA, Saclay Belmont R. Tagger M. UCLA Muno M. Morris M. Cowley S. High Energy Phenomena in the Galactic Center.
Summary(3) -- Dynamics in the universe -- T. Ohashi (Tokyo Metropolitan U) 1.Instrumentation for dynamics 2.Cluster hard X-rays 3.X-ray cavities 4.Dark.
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.),
1 Gabriele Ponti Marie Curie Fellow at University of Southampton High energy evidence for past activity from Sgr A* or its surroundings R. Terrier, A.
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.
ASTR112 The Galaxy Lecture 7 Prof. John Hearnshaw 11. The galactic nucleus and central bulge 11.1 Infrared observations (cont.) 11.2 Radio observations.
Internal Irradiation of the Sgr B2 Molecular Cloud Casey Law Northwestern University, USA A reanalysis of archived X-ray and radio observations to understand.
Discovery of K  lines of neutral sulfur, argon, and calcium atoms from the Galactic Center Masayoshi Nobukawa, Katsuji Koyama, Takeshi Go Tsuru, Syukyo.
The Interstellar Medium and Star Formation Material between the stars – gas and dust.
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.
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.
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.
Radio Galaxies part 4. Apart from the radio the thin accretion disk around the AGN produces optical, UV, X-ray radiation The optical spectrum emitted.
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,
Chapter 14 The Interstellar Medium. All of the material other than stars, planets, and degenerate objects Composed of gas and dust ~1% of the mass of.
Cornelia C. Lang University of Iowa collaborators:
Galaxies: Our Galaxy: the Milky Way. . The Structure of the Milky Way Galactic Plane Galactic Center The actual structure of our Milky Way is very hard.
Milky Way: Galactic Structure and Dynamics Milky Way has spiral structure Galactic Bulge surrounds the Center Powerful radio source Sagittarius A at Center.
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,
X-rays from Massive Star Fo r ming Region (YSO) ? Sgr B2 、 Arches, Mon R2 Herbig Ae/Be stars.
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.
天の川銀河の中心の星の運動 海王星くらいの 軌道で(5km/秒) 5000km/秒以上 太陽の400万倍 も重いブラック ホールがある.
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.
Tracing the coronal emission in AGN with VLT/NACO
The Milky Way Our Galactic Home.
The Interstellar Medium and Star Formation
Asami Hayato (RIKEN / Tokyo Univ. of Sci.)
Molecular Gas Distribution of our Galaxy: NANTEN Galactic Plane Survey
The Milky Way Galaxy.
Intimate Life in the Galactic Center
Suzaku The Suzaku Results of the Galactic Center X-rays Nickname
High Energy emission from the Galactic Center
The Milky Way Our Galactic Home.
Suzaku First Results on Galactic Diffuse Objects
Search for Bulk Motion in A2256 with Suzaku and ASTRO-H
Suzaku Observations of our Milky Way Center
Galactic Center Diffuse X-rays with Suzaku
Suzaku perspective on the Galactic Center
The X-ray perspective on young stellar populations in objects
X-rays from the Galactic Center
The Best Performance of XIS is the
Our Galactic Center and its Environmemt K. Koyama A. Senda
The Galactic Diffuse X-Rays and Time Variability of the 6.4-keV Clumps
A Timeline of the Early Building Blocks of Earth
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:

Target selection The GC hot plasma Sgr A East Sgr B2 / Radio arc plasma dynamics, galactic rotation Sgr A East SNR dynamics, galactic rotation Sgr B2 / Radio arc X-ray reflection nebula, Compton shoulder / recoil

        σ  Thermal motion ⇒ Vth~1700 km/s @10keV ⇒ σ~ 4 eV Turbulent Motion of the cloud ~70km/s ⇒ σ~ 1.5 eV        ΔE  Expanding Velocity of Hot Plasma  Galactic rotation curve ⇒ Vrot ~ 20 km/s @10 pc ⇒ ΔE ~ 0.4 eV

GC hot plasma Neutral Iron (6.4 keV) Trace the dynamics of the Cold Molecular cloud Galactic Rotation He/H-like Fe-K (6.7 / 6.9 keV) Trace the dynamics of the hot plasma ⇒ Dynamics of the hot plasma Galactic Rotation or Thermal motion ? Sgr A East Sgr A* GC hot Plasma Rotation curve near the GC region

Hot Plasma 100 ks 6.4 keV Lya 6.4 keV ±0.5 eV ±0.3 eV 6.7 keV ±0.5 eV Galactic rotation & Thermal Motion are detectable. 6.7 / 6.9 keV Line Ionization Temp. 6.7 keV / satellites Electron Temp. 6.7 & 6.7 width Ion Temp 6.4 keV Lya

Sgr A East resonance inter-combinations Line center error ±0.3 eV forbidden Line width error ±0.4 eV Li/Be-like satellites 20 km/s galactic rotation: detectable He-like Complex: 0.19 c/s/XRS He-like Resonance: 0.05 c/s/XRS He-like Resonance: 0.19 c/s/XRS

Sgr B2 / Radio Arc X-ray reflection nebulae (XRN) Compton shoulder of 6.4 keV line ⇒ Geometry of the Irradiation source & Cloud Compton recoil of 6.7 keV irradiation  ⇒ 3D configuration of Molecular cloud and Irradiating Source (Sgr A East). 3’ x1038 (year) Past luminosities of Sgr A*

Sgr B2 (100 ksec) Neutral iron line: 7x10-3 c/s/XRS line center 6.38 ±0.3 eV line width 1.7 ±0.4 eV (70km/s) Compton 6.37±10 eV Irradiation direction 10 %

Radio Arc (100 ksec) Neutral iron line 3.7x10-3 c/s He-like resonance Compton Recoil ? center ±0.3 eV width ±0.5 eV center ±1.2 eV width ±1.5 eV