Collaborators: Michael Muno (UCLA) Frederick Baganoff (MIT) Yoshitomo Maeda (ISAS) Mark Morris (UCLA) George Chartas (Penn State) Divas Sanwal (Penn State)

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

Suzaku Discovery of Fe K-Shell Line from the O-rich SNR G Arxiv: Fumiyoshi Kamitukasa et al.

Millisecond pulsar population and related high energy phenomena 王伟 (NAOC) July 2009, Pulsar Summer School Beijing.

X-ray Properties of Sgr A* Flares A Detailed X-ray View of the Central Parsecs Frederick Baganoff MIT Kavli Institute MIT Mark Bautz George Ricker Zhongxiang.

2009 July 8 Supernova Remants and Pulsar Wind Nebulae in the Chandra Era 1 Modeling the Dynamical and Radiative Evolution of a Pulsar Wind Nebula inside.

X-ray Properties of Five Galactic SNRs arXiv: Thomas G. Pannuti et al.

SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS JOHN R. DICKEL UNIVERSITY OF NEW MEXICO AND ROSA MURPHY WILLIAMS COLUMBUS STATE UNIVERSITY Preliminary SNR.

Supernova Remnants in the ChASeM33 X-ray Survey of M33 Knox S. Long, William P. Blair, P. Frank Winkler, and the ChASeM33 team.

Rie Yoshii ( RIKEN/Tokyo Univ. of Science) すざくで観測した N103B Observation of N103B by Suzaku 〜 together with SNR and SNR (type Ia SNRs.

October 10, 2002COSPAR Houston, TX1 X-Ray Spectral Morphologies of Young Supernova Remnants John P. Hughes Rutgers University  Cara Rakowski, Rutgers.

Supernova Remnants in the ChASeM33 X-ray Observations of M33 Knox Long, Bill Blair, Frank Winkler, Terry Gaetz, David Helfand, Jack Hughes, Kip Kuntz,

What Are the Faint X-ray Transients Near the Galactic Center? Michael Muno (UCLA/Hubble Fellow) Fred Baganoff (MIT), Eric Pfahl (UVa), Niel Brandt, Gordon.

I. Balestra, P.T., S. Ettori, P. Rosati, S. Borgani, V. Mainieri, M. Viola, C. Norman Galaxies and Structures through Cosmic Times - Venice, March 2006.

A young pulsar with a long radio trail emerging from SNR G F. Camilo, C.-Y. NG et al. arxiv : v1.

Facts about SNe and their remnants Evolution of an SNR sensitively depends on its environment. Observed SNRs are typically produced by SNe in relative.

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.

IR Shell Surrounding the Pulsar Wind Nebula G SNRs and PWNe in the Chandra Era Boston, July 8, 2009 Tea Temim (CfA, Univ. of MN) Collaborators:

March 11-13, 2002 Astro-E2 SWG 1 John P. Hughes Rutgers University Some Possible Astro-E2 Studies of Supernova Remnants.

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.

Summary Candidate supernova remnants G and G23.5–0.0 were observed by XMM-Newton in the course of a snap-shot survey of plerionic and composite.

January 8, st AAS Meeting1 Nucleosynthesis, Pulsars, Cosmic Rays, and Shock Physics: High Energy Studies of Supernova Remnants with Chandra and.

May 6, 2003Constellation-X Workshop1 Spatial/Spectral Studies of Supernova Remnants with Chandra and XMM-Newton John P. Hughes Rutgers University.

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.

An X-ray Study of the Bright Supernova Remnant G with XMM-Newton SNRs and PWNe in the Chandra Era Boston, MA – July 8 th, 2009 Daniel Castro,

Jeng-Lwen, Chiu Institute of Astronomy, NTHU 2005/05/05 Periodicity Search from the compact central object CXOU J

February 20, 2003Carnegie Symposum1 X-Ray Studies of Nucleosynthesis and Abundances in Supernova Remnants John P. Hughes Rutgers University.

Tycho’s SNR SNR G "To make an apple pie from scratch, you must first invent the universe." ~Carl Sagan.

Outline: Introduction into the problem Status of the identifications Summary Identification of Very high energy gamma-ray sources.

The Hot Plasma in the Galactic Center with Suzaku Masayoshi Nobukawa, Yoshiaki Hyodo, Katsuji Koyama, Takeshi Tsuru, Hironori Matsumoto (Kyoto Univ.)

The TeV view of the Galactic Centre R. Terrier APC.

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.),

A Neutron Star with a Massive Progenitor in the Star Cluster Westerlund 1 Michael Muno (UCLA/Hubble Fellow) J. S. Clark (Open U)R. de Grijs (U Sheffield)

Classification of SN Progenitors Optical obs of SNe Classification is relatively straightforward - Spectrum (historically well established) - Luminosity.

A New Magnetar Candidate Located Outside the Galactic Plane? Joe Callingham | Sean Farrell | Bryan Gaensler | Geraint Lewis Sydney Institute for Astronomy.

Extreme soft X-ray emission from the broad-line quasar REJ R.L.C. Starling 1*, E.M. Puchnarewicz 1, K.O. Mason 1 & E. Romero- Colmenero 2 1 Mullard.

Chandra Observations of Sgr A* Frederick Baganoff Massachusetts Institute of Technology MITMark Bautz George Ricker Penn StateNiel Brandt Gordon Garmire.

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.

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.

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.

Observations of AXPs and SGRs: 1E and SGR Andrea Tiengo (IASF-MI, Univ. Milano) S. Mereghetti, G. L. Israel, L. Stella, S. Zane, A.

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.

Associations of H.E.S.S. VHE  -ray sources with Pulsar Wind Nebulae Yves Gallant (LPTA, U. Montpellier II, France) for the H.E.S.S. Collaboration “The.

C. Y. Hui & W. Becker X-Ray Studies of the Central Compact Objects in Puppis-A & RX J Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse.

Antimatter in our Galaxy unveiled by INTEGRAL

A Pulsar Wind Nebula Origin for Luminous TeV Source HESS J Joseph Gelfand (NYUAD / CCPP) Eric Gotthelf, Jules Halpern (Columbia University), Dean.

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

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,

「すざく」による超新星残骸 RCW86 の観測 Suzaku Observations of Supernova Remnant RCW86 山口弘悦（理研） Hiroya Yamaguchi (RIKEN) ← Preliminary image of the Suzaku mapping observation.

Cornelia C. Lang University of Iowa collaborators:

A deep view of the iron line and spectral variability in NGC 4051 James Reeves Collaborators:- Jane Turner, Lance Miller, Andrew Lobban, Valentina Braito,

The Magnetic Field of an Isolated Neutron Star from X-ray Cyclotron Absorption Lines G.F.Bignami (1,2) P.A.Caraveo (3) A.De Luca (3,4) S.Mereghetti (3)

Boston 2009 Patrick Slane (CfA) SNRs and PWNe in the Chandra Era Observations of Pulsar Bowshock Nebulae Collaborators: B. M. Gaensler T. Temim J. D. Gelfand.

Neutral Atomic Hydrogen Gas at Forbidden Velocities in the Galactic Plane Ji-hyun Kang NAIC Seoul National University Supervisor :Bon-Chul Koo 213 th AAS.

Damien Parent – Moriond, February PSR J , PSR J , and their cousins -- young & noisy gamma ray pulsars Damien Parent on behalf of.

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.

The X-Ray Universe 2008, Granada, Spain, May 28, 2008 Chandra Monitoring of X-Ray Evolution of SNR 1987A Sangwook Park Department of Astronomy & Astrophysics.

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.

Asami Hayato (RIKEN / Tokyo Univ. of Sci.)

XMM-Newton Observation of the composite SNR G0. 9+0

Suzaku perspective on the Galactic Center

The X-ray perspective on young stellar populations in objects

X-rays from the Galactic Center

Galactic Center Diffuse X-rays with Suzaku

Cornelia C. Lang University of Iowa collaborators:

Presentation transcript:

Collaborators: Michael Muno (UCLA) Frederick Baganoff (MIT) Yoshitomo Maeda (ISAS) Mark Morris (UCLA) George Chartas (Penn State) Divas Sanwal (Penn State) David Burrows (Penn State) Gordon Garmire (Penn State) A Candidate Neutron Star & Its Association with Sgr A East High Energy Phenomena in the Galactic Center, High Energy Phenomena in the Galactic Center, Paris, France, June 15, 2005 Sangwook Park Department of Astronomy & Astrophysics The Pennsylvania State University

Introduction Sgr A East: Sgr A East: -Nonthermal radio shell -Nonthermal radio shell -X-ray detected by ROSAT, ASCA, Beppo-SAX -Chandra: Maeda et al. (2002) -Chandra: Maeda et al. (2002) MM SNR, kT=2 keV, CIE MM SNR, kT=2 keV, CIE E ~ 2 x ergs, M ~ 2 M sun E ~ 2 x ergs, M ~ 2 M sun Fe-rich center: He-like Fe line Fe-rich center: He-like Fe line Abund ratios => Type II SN Abund ratios => Type II SN -XMM: Sakano et al. (2004) -XMM: Sakano et al. (2004) SNR, central He- & H-like Fe SNR, central He- & H-like Fe => kT=1 keV & 4 keV, CIE => kT=1 keV & 4 keV, CIE Abund pattern =>Type Ia or II? Abund pattern =>Type Ia or II? “Neutral” Fe (6.4 keV) “Neutral” Fe (6.4 keV) ACIS-I: Sgr A* ACIS-I: Sgr A* ~ : ~ : 7 GTO & 5 GO obs 7 GTO & 5 GO obs => ~590 ks => ~590 ks Spatially-resolved spectroscopy Spatially-resolved spectroscopy with high photon statistics with high photon statistics - to test “Chandra vs XMM” - to test “Chandra vs XMM” - to test SN type - to test SN type Core-collapse SN: potential NS Core-collapse SN: potential NS => CXOGC J => CXOGC J (Muno et al. 2003) (Muno et al. 2003) Is CXOGC J Is CXOGC J a NS associated with SNR Sgr A East? a NS associated with SNR Sgr A East?

3-Color & Fe EW images Red: keV Green: keV Blue: keV He-like Fe XXV (E ~ 6.6 keV) Ar He  (3.1 keV) Ca He  (3.9 keV) Park et al. 2005, ApJ, in press

Sgr A East: Spectra & Fe Mass keV Plume Center kT=1.1 keV keV Fe=5.8 solar kT=1.3 keV Fe=1 solar Fe ejecta mass: EM => n Fe ~ 0.12 f -0.5 cm -3 M Fe < M sun Type Ia: M Fe ~ 0.5 – 0.8 M sun (Nomoto et al. 1997a) Type II: M Fe ~ 0.15 M sun for M star = 13 – 15 M sun M Fe ~ 0.05 – 0.08 M sun for M star = 18 – 70 M sun (Nomoto et al. 1997b) => Sgr A East is likely from a core-collapse SN.

Neutron Star Candidate: “the Cannonball” N E NS  =1.6 L x =3x10 33 ergs s -1 No varibility detected High velocity NS? - Tail: ~0.1 pc physical size - ~2’ from “center”: v ~ ( )/sin  km s -1 for SNR age ~ 5000 – yr - Mach number ~ 2.2: v ~ 880 km s -1 for ISM kT ~ 1 keV - Pressure balance: P PWN (E dot /   ) = P therm (2n e kT) = P ram (  v 2 ) where  = E dot -0.5 (Gotthelf 2003), v ~ 550 km s -1 =>Three velocities from independent estimates are consistent. =>Also consistent with typical Galactic high-velocity pulsars (e.g. Cordes & Chernoff 1998). The cannonball

Summary CXOGC J (the Cannonball): A High-V NS? CXOGC J (the Cannonball): A High-V NS? - Cometary morphology - Cometary morphology - X-ray spectrum: Hard, nonthermal continuum,  = X-ray spectrum: Hard, nonthermal continuum,  = X-ray luminosity L x = 3 x ergs s -1 - X-ray luminosity L x = 3 x ergs s -1 - No variability - No variability Associated with Sgr A East? Associated with Sgr A East? - Proximity to Sgr A East: estimated velocities are reasonable - Proximity to Sgr A East: estimated velocities are reasonable - Positional coincidence at the “tip” of Sgr A East Plume - Positional coincidence at the “tip” of Sgr A East Plume - Cometary tail extending toward Sgr A East - Cometary tail extending toward Sgr A East - Sgr A East is likely a core-collapse SNR: M Fe < 0.27 M sun - Sgr A East is likely a core-collapse SNR: M Fe < 0.27 M sun However, no evidence for a “pulsar”: - XMM/PN places an upper limit of ~40% on the pulsed fraction - XMM/PN places an upper limit of ~40% on the pulsed fraction at P > 147 ms. at P > 147 ms. => High time-resolution, high-sensitivity X-ray/radio => High time-resolution, high-sensitivity X-ray/radio observations are necessary. observations are necessary.