D. Dewey 5/031 SNR E0102: Measured Velocities and Geometric Musings by Dan Dewey, MIT  Extraction of spatial-velocity information from HETGS observation.

Slides:

Advertisements

Similar presentations

CH 10: Rotation.

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.

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

Tsing Hua University, Taiwan Solar Acoustic Holograms January 2008, Tucson Dean-Yi Chou.

X-ray Emission due to Charge Exchange between Solar Wind and Earth Atmosphere on September Hironori Matsumoto (Kobayashi-Maskawa Institute, Nagoya.

A Narrow Field Lobster Eye Telescope Dick Willingale – AXRO December 2014 A Narrow Field Lobster Eye Telescope (for SVOM and similar) Dick Willingale Adrian.

Image reconstruction and analysis for X-ray computed microtomography Lucia Mancini 1, Francesco Montanari 2, Diego Dreossi 3 1 Elettra - Trieste 2 A.R.P.A.

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal April ACIS Calibration: Recent Updates, Planned Updates, & Future Issues 2.E0102: Joint.

Geometric aspects of variability. A simple building system could be schematically conceived as a spatial allocation of cells, each cell characterized.

GG450 April 22, 2008 Seismic Processing.

Imaging Arp 220 in CO 6-5 and dust at 100 pc resolution with ALMA C. Wilson, (McMaster); N. Rangwala, J. Glenn, P. Maloney, J. R. Kamenetzky (Colorado);

High Resolution X-ray Spectroscopy of SN 1006 X-ray Diagnostics of Astrophysical Plasmas Jacco Vink (SRON Nat. Inst. for Space Research) Cambridge Ma,

24 Oct 2001 A Cool, Dense Flare T. S. Bastian 1, G. Fleishman 1,2, D. E. Gary 3 1 National Radio Astronomy Observatory 2 Ioffe Institute for Physics and.

X-ray Emission and Absorption in Massive Star Winds Constraints on shock heating and wind mass-loss rates David Cohen Swarthmore College.

Line Shapes in Hot Stars: Hydrodynamics & Wind Mass-Loss Rates David Cohen Swarthmore College with Maurice Leutenegger, Stan Owocki, Rich Townsend, Emma.

Measuring the Wilson effect: observations and modeling with RHESSI H. Jabran Zahid M. D. Fivian H. S. Hudson.

The remarkable soft X-ray emission of the Broad Line Radio Galaxy 3C445 BLRG in the Unification Scheme of AGN: Is the circumnuclear gas in BLRG different.

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

Electron Heating Mechanisms and Temperature Diagnostics in SNR Shocks Martin Laming, Cara Rakowski, NRL Parviz Ghavamian, STScI.

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal October Comparison of RGS Model for 1E to the HETG data 2.BI CCD CTI Correction.

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,

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Update on ACIS Calibration 1) Update to the ACIS contamination model 2) Temperature-dependent.

Levels of organization: Stellar Systems Stellar Clusters Galaxies Galaxy Clusters Galaxy Superclusters The Universe Everyone should know where they live:

Pat Arnott, ATMS 749 Atmospheric Radiation Transfer CH4: Reflection and Refraction in a Homogenous Medium.

02/25/05© 2005 University of Wisconsin Last Time Meshing Volume Scattering Radiometry (Adsorption and Emission)

Chapter 23 Properties of Light. Section 1: Objectives Use ray diagrams to show how light is reflected or refracted. Compare plane mirrors, concave mirrors,

The planetary nebula M2-9: Balmer line profiles of the nuclear region Silvia Torres-Peimbert 1 Anabel Arrieta 2 Leonid Georgiev 1 1 Instituto de Astronomía,

Computer Vision – Fundamentals of Human Vision Hanyang University Jong-Il Park.

The Influence of the Return Current and the Electron Beam on the X-Ray Flare Spectra Elena Dzifčáková, Marian Karlický Astronomical Institute of the Academy.

D. Dewey et al.4 years of Chandra Observations, Sept Towards a 3D Model of SNR E D. Dewey, C.R. Canizares, K.A. Flanagan, A. Fredericks,

SPIE Optics for EUV, X-Ray, and Gamma-Ray Astronomy VI

The Influence of the Return Current and Electron Beam on the EUV and X-Ray Flare Emission E. Dzifčáková, M. Karlický Astronomical Institute of the Academy.

An introduction to the MULTI radiative transfer code Lars Heggland Institute of Theoretical Astrophysics, University of Oslo Kwasan Observatory, Kyoto.

Feature based deformable registration of neuroimages using interest point and feature selection Leonid Teverovskiy Center for Automated Learning and Discovery.

: Chapter 11: Three Dimensional Image Processing 1 Montri Karnjanadecha ac.th/~montri Image.

Imaging Molecular Gas in a Nearby Starburst Galaxy NGC 3256, a nearby luminous infrared galaxy, as imaged by the SMA. (Left) Integrated CO(2-1) intensity.

Spectral Signature of Emergent Magnetic Flux D1 神尾精 Solar Seminar Balasubramaniam,K.S., 2001, ApJ, 557, 366. Chae, J. et al., 2000, ApJ, 528,

Evolution of Flare Ribbons and Energy Release Rate Ayumi ASAI 1, Takaaki YOKOYAMA 2, Masumi SHIMOJO 3, Satoshi MASUDA 4, and Kazunari SHIBATA 1 1:Kwasan.

Physics 1C Lecture 27A. Interference Treating light as a particle (geometrical optics) helped us to understand how images are formed by lenses and mirrors.

Black Holes in Other Galaxies. The giant elliptical galaxy M87 is located 50 million light-years away in the constellation Virgo. By measuring the rotational.

Simulations Report E. García, UIC. Run 1 Geometry Radiator (water) 1cm x 2cm x 2cm with optical properties Sensitive Volume (hit collector) acrylic (with.

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.

Chandra X-Ray Observatory CXC Paul Plucinsky IACHEC March Thermal SNR Working Group: Summary Report Paul Plucinsky on behalf of the IACHEC Thermal.

Is the velocity of the wave shown above. For reflection of light, we have the situation shown in Figure 1. The two plane mirrors in Figure 2 are at 90.

Interference and Diffraction

1. If the amount of water increases, then the height of the plant will increase. This is an example of A hypothesis.

Barrel or Bilateral-shaped SNRs Jiangtao Li May 6th 2009.

X-ray observation of the Cygnus Loop with Suzaku and XMM-Newton

Dan DeweySNORE talk, Dec.1, SNR E0102: Building a Supernova Remnant A SNORE talk by Dan Dewey MIT Center for Space Research "SNR-3D" Collegues at.

Perception and VR MONT 104S, Fall 2008 Lecture 8 Seeing Depth

14 may 2007Simbol-X workshop - Bologna1 44 Ti nucleosynthesis γ –ray lines with Simbol-X Matthieu Renaud Max-Planck-Institute für Kernphysik Heidelberg,

Opacity Correction (1/20/09) Schumacher, Ovchinnikov Materials: Copper (1/e absoption length taken as 22  ), Aluminum (72.4  ). Targets: Slab sandwich,

Formation and evolution of dust in Type IIb SN: Application to Cas A Takaya Nozawa (IPMU, Univ. of Tokyo) Collaborators; T. Kozasa (Hokkaido Univ.), N.

X-ray Line Profile Diagnostics of Shock Heated Stellar Winds Roban H. Kramer 1,2, Stephanie K. Tonnesen 1, David H. Cohen 1,2, Stanley P. Owocki 3, Asif.

2/5/16Oregon State University PH 212, Class #151 Snell’s Law This change in speed when light enters a new medium means that its wavefronts will bend, as.

1. Science Science is a way of learning about the natural world that provides possible explanations to questions.

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.

Principal planes method For the purposes of finding images, we can reduce any* optical system to a thin lens. Principal plane distances p 1 and p 2 are.

Micro-structural size properties of Saturn’s rings determined from ultraviolet measurements made by the Cassini Ultraviolet Imaging Spectrograph Todd Bradley.

R. Maggiolo 1, M. Echim 1,2, D. Fontaine 3, A. Teste 4, C. Jacquey 5 1 Belgian Institute for Space Aeronomy (IASB-BIRA); 2 Institute.

Hale COLLAGE (CU ASTR-7500) “Topics in Solar Observation Techniques” Lecture 3: Basic concepts in radiative transfer & polarization Spring 2016, Part 1.

U.A. Dyudina, A.P. Ingersoll, California Institute of Technology Pasadena, CA, Objectives We study lightning on Jupiter using spatially resolved.

Chandra HETG Spectra of SN 1987A at 20 Years

A Coarse 3D Model of E Derived from HETG Data

The Universe in High-resolution X-ray Spectra

Foil thickness measurements

Yuki Takagi1*, Kazuo Shiokawa1, Yuichi Otsuka1, and Martin Connors2

The Elements of Art.

HETG Spectral-imaging of SN1987A

Presentation transcript:

D. Dewey 5/031 SNR E0102: Measured Velocities and Geometric Musings by Dan Dewey, MIT  Extraction of spatial-velocity information from HETGS observation  3-D modeling of E0102 Ne X emission  Are SNRs Optically thin? Everywhere?

D. Dewey 5/032 HETGS Observation of E0102

D. Dewey 5/033 Ne X line images Usefulness of plus, minus, and zeroth order data Asymmetry in Ne X image: simple explanation: Minus order Zeroth-order Plus order

D. Dewey 5/034 Something too complex to explain happens

D. Dewey 5/035 Color-velocity image results Regions of red and blue shift appear as displaced rings. –Red: 900 and 1800 km/s –Green: -900 km/s –Blue: km/s Interpretation as cylinder viewed almost end-on

D. Dewey 5/036 Contrast the E0102 velocities distribution with Cas A velocities (Willingale 2002, Figure 7) Cas A is an inclined ring with red and blue shifted emission generally segregated.

D. Dewey 5/037 3-D Modeling & Ne X distribution Purposes for modeling: –Visualization ("pretty") –Modeling ("quantitative") Building model data structures, "voxels" for optically thin volumes 3-D arrays of scalar (plasma) parameters… Data structures Pretty pic.s Ray-trace Input events Creation

D. Dewey 5/038 Visualizing E0102 cylinder model IDL project_vol.pro used here. Optically thick and thin views of the cylinder intensity array. Optically thick viewOptically thin view Maximum value along a ray is used. The material has an opacity. Depth cuing darkens distant points. Sum of values along a ray is used. The material has NO opacity. No change in intensity with distance.

D. Dewey 5/039 Model of E0102 nominal viewing angleE0102 Ne X image Middle of ring left out Projection with middle left out - mimics the intensity distribution from the high-V planes.

D. Dewey 5/0310 Are SNRs Optically thin? Everywhere? E0102 Ne optically thin? –Assuming 1 M_solar of Ne in the cylinder volume get n_Ne ~ 0.02/cm^3. Times length of cylinder, 1.6e+19 cm, gives n_H equiv for the Ne of ~ 0.3e+22 / cm^2: varabs shows 90% transmission above Ne edge - Yes, it’s THIN! Other [O-rich] SNR? (Cas A, N132D, G292,...) –G : metal rich knots: 1e+17 cm, n ~ /cm^3 (Parviz Ghavamian, CfA talk) –1e+18 ions/cm^2 is amount in "solar" N_H of 10^21(O) to 3x10^22(Si) O edge transmission = 60% for N_H = 1e+21 Si edge transmission = 85% for N_H = 3e+22

D. Dewey 5/0311 Comments E0102 Ne X (12A, 1keV) result made possible by: –spatial resolution at scale of few arc seconds –Sensitive to V ~ 900 km/s FWHM (E/dE > 300) –Second E0102 observation at 90 deg. Roll will improve Ne X; do Ne IX also; similar analysis for O VIII 3-D useful for Visualization and Astrophysics –Move beyond "uniform volume" models for SNR (and other objects!) Are SNRs optically thin? –Metal-rich features/knots may be quasi-thin… –Is there a way to make quantitative measures to confirm optically thin based on the images themselves?