Recent Observations of Supernova Remnants

Size: px
Start display at page:

Download "Recent Observations of Supernova Remnants"

Transcription

1 1 Recent Observations of Supernova Remnants with VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (

2 2 Contents Supernova Remnants and the Galactic CR acceleration Results Crab Nebula Cassiopeia A IC 443 Summary

3 Supernova Remnants and Galactic Cosmic Ray Acceleration 3 Composition of cosmic rays Protons (86%) and heavy nuclei (12%) for energies below 1015 ev (1 particle per m 2 second) Small fraction is gamma rays and neutrinos 2 (1 particle per m year ) Cosmic rays below the knee are galactic in origin (1 particle per km 2 year ) Supernova remnants are prime candidates for CR acceleration >diffuse shock acceleration models, amplified magnetic fields >accelerate electrons or charged particles

4 Gamma Rays from a Pulsar Wind Nebula (Plerion) 4 A PWN is a supernova remnant with a pulsar, which is injecting continuously electrons into its nebula, where electrons get shock accelerated to high energies through this mechanism. These electrons interact with ambient photons and up scatter them to very high energies. X ray / Chandra Optical / Palomar Radio / VLT

5 5 Gamma Rays from Shell type Supernova Remnants No electrons supplied by the pulsar wind X ray image Shells of the remnants possibly hadron or electron acceleration sites Gamma rays from hadrons through π0 γγ Gamma rays from electrons through inverse Compton scattering Gamma ray signal from shell regions may give hints for hadron acceleration Signal could be enhanced by shell interacting with nearby molecular clouds Gamma ray source spectrum

6 6 VERITAS at F.L. Whipple Observatory in Amado, Arizona Geographic Location: North, West, Altitude: 1268 masl. u a ry n Ja T T1 T4 April m 108m 85m 85m December 2006 T3 109m FoV: 3.5 Energy Range: 100 GeV 30 TeV Point source Sensitivity: 1% of the Crab Nebula detected at 5 in 50 hours at 20 zenith

7 The Crab Nebula: A Plerion as Standard Candle 7 VERITAS Observations 3 telescope data from January February 2007 Sensitivity: 30.4 hrs Gamma ray rate: 6.93 /min 4 telescope data from Fall 2007 Sensitivity: 30.9 hrs Gamma ray rate: 7.86 /min More results on the Crab Nebula > see O.Celik's talk. Point like gamma ray emission = 0.07 ± 0.01

8 Cassiopeia A: A Young Shell type Supernova Remnant 8 Youngest known supernova remnant in our galaxy (First record in 1680) Cas A (X ray Image) CHANDRA picture (NASA) Distance = 3.4 kpc Brightest shell type remnant in radio waveband Strong X ray source SNR shell diameter is 4' (4 pc at 3.4 kpc) X ray measurements revealed central object

9 Cassiopeia A TeV Gamma ray Observations 9 HEGRA Observations and detection in hours of observations Flux(>1 TeV) is 3 % of the Crab Nebula MAGIC Observations between July 2006 and January hours of observation Significance 5.2 Flux and spectral index in agreement with HEGRA

10 10 Cassiopeia A VERITAS Results VERITAS 4 telescope data from September to November 2007 Average zenith angle: 32 Observation Time: 21 hours Point Source Search: ² ² Significance: 9.2 PSF Gamma ray Rate: 0.09 ±0.01 /min Background Rate: 0.08 ± 0.02 bkg/min Flux(>300 GeV) is 3 % of the Crab Nebula

11 Cassiopeia A: Extension of the Gamma ray Emission 11 2D Gaussian fit location RA = ± (0.05 )stat ± (0.05 )sys Dec =+58.6 ± (0.05 )stat ± (0.05 )sys Point like profile of the gamma ray emission, fit simple gauss function to theta squared plot = ±(0.015 )stat ± (0.04 )sys

12 CHANDRA picture (NASA) IC 443: A Supernova Remnant Interacting with Molecular Clouds 12 An SNR within dense molecular cloud region and some OB associations Distance = 1.5 kpc, Age = 3 30 kyrs Strong X ray source SNR shell diameter is 20 pc (45' for 1.5 kpc) Associated with neutron star CXOU J Associated with an unidentified EGRET source (E > 100 MeV) X ray / Chandra Optical Radio

13 IC 443 TeV Gamma ray Observations IC MAGIC J Observed between December 2006 and January hours of observation Significance 5.7 VLA Radio ROSAT X ray Molecular Clouds Flux Measurement d /de = (1.0 ± 0.2) (E/0.4 TeV) 3.1±0.3 cm 2 s 1 TeV 1 MAGIC, astro ph/ v1 MAGIC, ApJ, 664, L87 L90 (2007)

14 14 IC 443 VERITAS Results 3 telescope data February March 2007 and 4 telescope data October November 2007 Average zenith angle: 18 Point Source Search: ² ² Max Significance Position: RA: 94.19, Dec: PSF Combined Significance: 8.6 Gamma ray rate: 0.18 ±0.03 /min Background rate: 0.93 ±0.01 bkg/min Flux(>300 GeV) is 3 % of the Crab Excluded 3rd magnitude star Nebula (HIP29655), 0.5 away from the remnant location

15 15 IC 443: Extension of the Gamma ray Emission Intrinsic Extension: ( ² IC443)Measured = ( ²Crab)Measured+ ( ² IC443) Intrinsic Measured Extension by fitting simple Gaussian = 0.18 ± (0.05 )stat ± (0.04 )sys Intrinsic extension of IC 443 = 0.17 ± (0.05 )stat ± (0.04 )sys

16 16 IC 443: Extension of the Gamma ray Emission Asymmetric Source Morphology Max Excess fit location RA = ± (0.07 )stat ± (0.05 )sys Dec = ± (0.07 )stat ± (0.05 )sys Work ongoing! PSF

17 17 IC 443: Multi wavelength Comparison ROSAT PWN CO Data MAGIC 3EG J Spatial overlap between the peak of the gamma ray excess and the CO data Declination (J2000) [degrees] VERITAS detected gamma ray excess region consistent with MAGIC gamma ray position and the optical and X ray counterpart Models of gamma ray production Right Ascension (J2000) [degrees] by pion decay that is a product of proton interactions. by interactions of relativistic electrons from the SNR with the ambient photons Some modeling papers: Bartko & Bednarek MNRAS, 385, (2008), D.F. Torres, astro ph/

18 18 Conclusion Supernova Remnants are candidate sites of galactic CR acceleration From the observations from 2007 Fall to 2008 Spring VERITAS detected two supernova remnants each having gamma ray fluxes of 3% of the Crab Nebula The shell type supernova remnant Cassiopeia A has a point like gamma ray extension IC 443 is a slightly extended gamma ray source that might be interacting with the surrounding molecular clouds Detailed extension and spectral analysis is ongoing! Sensitive measurements of the spectra of these sources might help constraining the gamma ray emission mechanisms

19 19 Backup Slide: IC 443 VERITAS Results VERITAS 3 telescope data from February March 2007 VERITAS 4 telescope data from October November 2007 Average Zenith Angle: 20 Observation Time: 17.8 hours Average Zenith Angle: 16 Observation Time: 17.5 hours Significance: 7.4 Significance: 6.7 Gamma ray rate: 0.24 ±0.03 /min Gamma ray rate: 0.19 ±0.03 min Background rate: 0.92 ±0.01 bkg/min Max Significance Position RA: 94.22, Dec: Background rate: 1.00 ± 0.01 bkg/min Max Significance Position RA: 94.26, Dec: 22.46

20 20 VERITAS TIME ALLOCATION About 800 hours allocated for science observations and ~ 90 hours for Group engineering per year. Proposals 40% Key Science Projects Sky Survey (Preliminary scan and follow up observations) Dark Matter (Deep observations of selected candidate sources) Supernova Remnants (Intensive observations, search for new sources) Blazars (MWL campaign for large flare, intensive observation of some AGN, search for new blazars) DDT 10% Key Science Projects 50% Groups proposals administered by VERITAS Time Allocation Committee (TAC) Director s discretionary time (DDT) for engineering, ToO.

21 21 The Telescope Design 345 Mirror Facets Camera 499 PMTs 12 m 3.5 Mirror Area: 110 m2 12 m Mirror Reflectivity: (at 320 nm) > 90 % PMT size Light Collector Reflectivity: (at 260 nm) > 85 % Light Collector Tracking Accuracy: 0.02 PSF: ~ 0.06 FWHM measured at Polaris (elevation 31 ) Camera Pixel Spacing: 0.15 Energy Threshold: ~100 GeV

22 22 Stereoscopic Reconstruction Angular Resolution (energy dependent) Core Location Precision ~15 25 m (energy dependent) Energy Resolution %

23 23 The Crab Nebula Effective Area: m2 Flux of the Crab Nebula (3 telescopes) d E = 0 where E 0=1TeV de E0 0=(3.87± 0.10stat) cm 2 s 1 TeV 1 = 2.46± 0.03stat Analysis Energy Threshold: ~ 200 GeV O.Celik, HEAD 2008

24 24 VERITAS Performance Sensitivity Crab Nebula detected (5 ) Flux of the Crab Nebula (3 telescopes) with 3 telescopes in 1.9 minutes. d E = 0 where E 0 =1TeV For 5 detection of a source de E0 having 10 % of the Crab stat =(3.63± 0.15 ) 10 cm s TeV Nebula flux 3.3 hours (2 telescopes) = 2.54± 0.05stat 1.2 hours (3 telescopes) (> 1 TeV)=(2.35± 0.12stat) cm 2 s 1 <1 hours (4 telescopes) Effective Area: m2 Analysis Energy Threshold: ~ 200 GeV

25 Comparison of H.E.S.S. and VERITAS Performances HESS Crab Nebula detection at zenith: 0.01 Crab : ~25 h 0.05 Crab : ~1 h 0.10 Crab : ~15 min 1.00 Crab : ~10 s VERITAS A source having 1% of the Crab Nebula flux is detected at 5 in less than 50 hours for observations ~ 20. For 5 detection of a source having 10 % of the Crab Nebula flux 3.3 hours (2 telescopes) 1.2 hours (3 telescopes) <1 hours (4 telescopes) 25

TEV GAMMA RAY ASTRONOMY WITH VERITAS

TEV GAMMA RAY ASTRONOMY WITH VERITAS 1 TEV GAMMA RAY ASTRONOMY WITH VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration 2 Contents The VERITAS Experiment Results and the Performance Galactic Sources

More information

OBSERVATIONS OF VERY HIGH ENERGY GAMMA RAYS FROM M87 BY VERITAS

OBSERVATIONS OF VERY HIGH ENERGY GAMMA RAYS FROM M87 BY VERITAS OBSERVATIONS OF VERY HIGH ENERGY GAMMA RAYS FROM M87 BY VERITAS 1 Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) APOD, 2004 December

More information

VERITAS Observations of Supernova Remnants

VERITAS Observations of Supernova Remnants VERITAS Observations of Supernova Remnants Reshmi Mukherjee 1 for the VERITAS Collaboration 1 Barnard College, Columbia University Chandra SNR Meeting, Boston, Jul 8, 2009 Outline (Quick) introduction

More information

Galactic sources in GeV/TeV Astronomy and the new HESS Results

Galactic sources in GeV/TeV Astronomy and the new HESS Results Galactic sources in GeV/TeV Astronomy and the new HESS Results Martin Tluczykont for the HESS Collaboration LLR Ecole Polytechnique Joint Symposium on GeV-TeV Astrophysics in the GLAST Era Stanford, September

More information

H.E.S.S. Unidentified Gamma-ray Sources in a Pulsar Wind Nebula Scenario And HESS J

H.E.S.S. Unidentified Gamma-ray Sources in a Pulsar Wind Nebula Scenario And HESS J H.E.S.S. Unidentified Gamma-ray Sources in a Pulsar Wind Nebula Scenario And HESS J1303-631 Matthew Dalton Humboldt University at Berlin For the H.E.S.S. Collaboration TeV Particle Astrophysics, Paris.

More information

Observing Galactic Sources at GeV & TeV Energies (A Short Summary)

Observing Galactic Sources at GeV & TeV Energies (A Short Summary) 1 Observing Galactic Sources at GeV & TeV Energies (A Short Summary) Tülün Ergin Univ. of Massachusetts, Amherst Air Cherenkov Telescopes 2 Past IACTs: HEGRA, Whipple, CANGAROO Present/Future IACTs: H.E.S.S.,

More information

Fermi: Highlights of GeV Gamma-ray Astronomy

Fermi: Highlights of GeV Gamma-ray Astronomy Fermi: Highlights of GeV Gamma-ray Astronomy Dave Thompson NASA GSFC On behalf of the Fermi Gamma-ray Space Telescope Large Area Telescope Collaboration Neutrino Oscillation Workshop Otranto, Lecce, Italy

More information

VERITAS: exploring the high energy Universe

VERITAS: exploring the high energy Universe VERITAS: exploring the high energy Universe K. Ragan McGill University Queen's - March '09 VERITAS 1 Outline Beyond the optical Very high-energy (VHE) gamma-ray astrophysics Ground-based observations Cherenkov

More information

Gamma-ray Astrophysics with VERITAS: Exploring the violent Universe

Gamma-ray Astrophysics with VERITAS: Exploring the violent Universe Gamma-ray Astrophysics with VERITAS: Exploring the violent Universe K. Ragan McGill University Soup & Science 11-Jan-2008 Soup & Science Jan. '08 1 How do we know about the Universe? Historically, all

More information

Pulsar Wind Nebulae as seen by Fermi-Large Area Telescope

Pulsar Wind Nebulae as seen by Fermi-Large Area Telescope Pulsar Wind Nebulae as seen by Fermi-Large Area Telescope Marie-Hélène Grondin Centre d'etudes Nucléaires de Bordeaux- Gradignan SNR/PWN Workshop Montpellier, 2010 June 1 th M.-H. Grondin, SNR/PWN Wokshop,

More information

Status of the MAGIC telescopes

Status of the MAGIC telescopes SNOWPAC 2010 Status of the MAGIC telescopes Pierre Colin for the MAGIC collaboration Max-Planck-Institut für physik (Munich) Status of the MAGIC telescopes MAGIC-1 MAGIC-2 Outline: Recent results of the

More information

Potential Neutrino Signals from Galactic γ-ray Sources

Potential Neutrino Signals from Galactic γ-ray Sources Potential Neutrino Signals from Galactic γ-ray Sources, Christian Stegmann Felix Aharonian, Jim Hinton MPI für Kernphysik, Heidelberg Madison WI, August 28 31, 2006 TeV γ-ray Sources as Potential ν Sources

More information

Galactic Sources with Milagro and HAWC. Jordan Goodman for the HAWC and Milagro Collaborations

Galactic Sources with Milagro and HAWC. Jordan Goodman for the HAWC and Milagro Collaborations Galactic Sources with Milagro and HAWC Jordan Goodman for the HAWC and Milagro Collaborations Snowpack 2010 Milagro and HAWC Milagro was a first generation wide-field gamma-ray telescope: Proposed in 1990

More information

VERITAS Observations of Starburst Galaxies. The Discovery of VHE Gamma Rays from a Starburst Galaxy

VERITAS Observations of Starburst Galaxies. The Discovery of VHE Gamma Rays from a Starburst Galaxy VERITAS Observations of Starburst Galaxies The Discovery of VHE Gamma Rays from a Starburst Galaxy Wystan Benbow for the VERITAS Collaboration 1 Harvard-Smithsonian Center for Astrophysics 1 see R.A. Ong

More information

Recent highlights from VERITAS

Recent highlights from VERITAS Recent highlights from VERITAS K. Ragan McGill University RICAP 2011, Rome, 26-May-2011 K. Ragan VERITAS RICAP '11 1 Outline Very high-energy (VHE) gamma-ray astrophysics Ground-based observations with

More information

Recent Results from VERITAS

Recent Results from VERITAS Recent Results from VERITAS Physics Department, McGill University, Montreal, Canada E-mail: hanna@physics.mcgill.ca VERITAS (Very Energetic Radiation Imaging Telescope Array System) is an array of four

More information

Constraints on cosmic-ray origin from gamma-ray observations of supernova remnants

Constraints on cosmic-ray origin from gamma-ray observations of supernova remnants Constraints on cosmic-ray origin from gamma-ray observations of supernova remnants Marianne Lemoine-Goumard (CENBG, Université Bordeaux, CNRS-IN2P3, France) On behalf of the Fermi-LAT and HESS Collaborations

More information

PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY. Paolo Lipari Vulcano 27 may 2006

PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY. Paolo Lipari Vulcano 27 may 2006 PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY Paolo Lipari Vulcano 27 may 2006 High Energy Neutrino Astrophysics will CERTAINLY become an essential field in a New Multi-Messenger Astrophysics What is

More information

TeV γ-ray observations with VERITAS and the prospects of the TeV/radio connection

TeV γ-ray observations with VERITAS and the prospects of the TeV/radio connection TeV γ-ray observations with VERITAS and the prospects of the TeV/radio connection Matthias Beilicke for the VERITAS collaboration Washington University in St.Louis, Physics Department and McDonnell Center

More information

Remnants and Pulsar Wind

Remnants and Pulsar Wind High Energy Supernova Remnants and Pulsar Wind Nebulae F. Giordano Dipartimento Interateneo di Fisica and INFN Sez. Bari For the Fermi-LAT Collaboration Scineghe 2010 The Afterlife of a star IC443 Crab

More information

Discovery of TeV Gamma-ray Emission Towards Supernova Remnant SNR G Last Updated Tuesday, 30 July :01

Discovery of TeV Gamma-ray Emission Towards Supernova Remnant SNR G Last Updated Tuesday, 30 July :01 Background-subtracted gamma-ray count map of SNR G78.2+2.1 showing the VERITAS detection (VER2019+407). For details, see Figure 1 below. Reference: E. Aliu et al. (The VERITAS Collaboration), Astrophysical

More information

Gamma-ray Astrophysics

Gamma-ray Astrophysics Gamma-ray Astrophysics AGN Pulsar SNR GRB Radio Galaxy The very high energy -ray sky NEPPSR 25 Aug. 2004 Many thanks to Rene Ong at UCLA Guy Blaylock U. of Massachusetts Why gamma rays? Extragalactic Background

More information

On the scientific motivation for a wide field-of-view TeV gamma-ray observatory in the Southern Hemisphere

On the scientific motivation for a wide field-of-view TeV gamma-ray observatory in the Southern Hemisphere On the scientific motivation for a wide field-of-view TeV gamma-ray observatory in the Southern Hemisphere for the HAWC collaboration E-mail: miguel@psu.edu Observations of high energy gamma rays are an

More information

VERITAS Design. Vladimir Vassiliev Whipple Observatory Harvard-Smithsonian CfA

VERITAS Design. Vladimir Vassiliev Whipple Observatory Harvard-Smithsonian CfA VERITAS Design Vladimir Vassiliev Whipple Observatory Harvard-Smithsonian CfA VERITAS design goals VERITAS is a ground-based observatory for gamma-ray astronomy VERITAS design is derived from scientific

More information

Radio Observations of TeV and GeV emitting Supernova Remnants

Radio Observations of TeV and GeV emitting Supernova Remnants Radio Observations of TeV and GeV emitting Supernova Remnants Denis Leahy University of Calgary, Calgary, Alberta, Canada (collaborator Wenwu Tian, National Astronomical Observatories of China) outline

More information

Very-High-Energy Gamma-Ray Astronomy with VERITAS. Martin Schroedter Iowa State University

Very-High-Energy Gamma-Ray Astronomy with VERITAS. Martin Schroedter Iowa State University Very-High-Energy Gamma-Ray Astronomy with VERITAS Martin Schroedter Iowa State University Summary Very-high-energy astronomy began 20 years ago with 1 source. Now ~80 more VHE discoveries have been made

More information

The VelaX pulsar wind nebula in the TeV regime. Bernhard Glück for the H.E.S.S. Collaboration July 8th, 2009, Boston

The VelaX pulsar wind nebula in the TeV regime. Bernhard Glück for the H.E.S.S. Collaboration July 8th, 2009, Boston The VelaX pulsar wind nebula in the TeV regime Bernhard Glück for the H.E.S.S. Collaboration July 8th, 2009, Boston Outline The H.E.S.S. Experiment Results for PWN VelaX from observation 2004 to 2006 Follow

More information

CTB 37A & CTB 37B - The fake twins SNRs

CTB 37A & CTB 37B - The fake twins SNRs Annecy le vieux CTB 37A & CTB 37B - The fake twins SNRs LAPP Annecy CTB 37: a complex complex 843 MHz MGPS map (Green et al. 1999) Bright region in radio emission Thought to be 2 SNRs plus a bridge and

More information

HAWC Observation of Supernova Remnants and Pulsar Wind Nebulae

HAWC Observation of Supernova Remnants and Pulsar Wind Nebulae HAWC Observation of Supernova Remnants and Pulsar Wind Nebulae a, and H. Zhou a for the HAWC Collaboration b a Department of Physics, Michigan Technological University 1400 Townsend Drive, Houghton, MI,

More information

Supernova Remnants and Cosmic. Rays

Supernova Remnants and Cosmic. Rays Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants

More information

Fermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars

Fermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars Fermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars Marie-Hélène Grondin CENBG, Bordeaux (France) on behalf of the Fermi-LAT Collaboration and the Pulsar Timing

More information

Non-thermal emission from pulsars experimental status and prospects

Non-thermal emission from pulsars experimental status and prospects Non-thermal emission from pulsars experimental status and prospects # γ!"# $%&'() TeV γ-ray astrophysics with VERITAS ( $γ" *$%&'() The charged cosmic radiation - how it all began... Discovery: Victor

More information

GLAST and beyond GLAST: TeV Astrophysics

GLAST and beyond GLAST: TeV Astrophysics GLAST and beyond GLAST: TeV Astrophysics Outline: Greg Madejski Assistant Director for Scientific Programs, SLAC / Kavli Institute for Astrophysics and Cosmology Recent excitement of GLAST and plans for

More information

Very High Energy monitoring of the radio galaxy M87 with MAGIC during a low emission state between 2012 and 2015

Very High Energy monitoring of the radio galaxy M87 with MAGIC during a low emission state between 2012 and 2015 Very High Energy monitoring of the radio galaxy M87 with MAGIC during a low emission state between 2012 and 2015 ICRR, U-Tokyo and Max-Planck-Institute for Physics, Munich and P. Bangale, M. Manganaro,

More information

Cosmic Ray Electrons and GC Observations with H.E.S.S.

Cosmic Ray Electrons and GC Observations with H.E.S.S. Cosmic Ray Electrons and GC Observations with H.E.S.S. Christopher van Eldik (for the H.E.S.S. Collaboration) MPI für Kernphysik, Heidelberg, Germany TeVPA '09, SLAC, July 2009 The Centre of the Milky

More information

The Extreme Universe Rene A. Ong Univ. of Michigan Colloquium University of California, Los Angeles 23 March 2005

The Extreme Universe Rene A. Ong Univ. of Michigan Colloquium University of California, Los Angeles 23 March 2005 The Extreme Universe Rene A. Ong Univ. of Michigan Colloquium University of California, Los Angeles 23 March 2005 OUTLINE Introduction Messengers,, energy scales, & questions. Detecting Very High Energy

More information

Observations of Supernova Remnants with VERITAS

Observations of Supernova Remnants with VERITAS Observations of Supernova Remnants with VERITAS Presented by Nahee Park What do we want to learn? Are SNRs the main accelerators of the Galactic cosmic rays? Efficiency of cosmic-ray acceleration? Maximum

More information

Particle Acceleration in the Universe

Particle Acceleration in the Universe Particle Acceleration in the Universe Hiroyasu Tajima Stanford Linear Accelerator Center Kavli Institute for Particle Astrophysics and Cosmology on behalf of SLAC GLAST team June 7, 2006 SLAC DOE HEP Program

More information

TeV Gamma Rays from Synchrotron X-ray X

TeV Gamma Rays from Synchrotron X-ray X TeV Gamma Rays from Synchrotron X-ray X SNR Kyoto University Department of Physics Toru Tanimori (CANGAROO Collaboration) Introduction TeV Gamma Ray emissions in celestial objects Results of CANGAROO The

More information

Are supernova remnants PeV accelerators? The contribution of HESS observations

Are supernova remnants PeV accelerators? The contribution of HESS observations Are supernova remnants PeV accelerators? The contribution of HESS observations Marianne Lemoine Goumard Laboratoire Leprince Ringuet Ecole Polytechnique 1 Outline 1. VHE Gamma ray Astronomy & HESS 2. Clearly

More information

A New TeV Source in the Vicinity of Cygnus OB2

A New TeV Source in the Vicinity of Cygnus OB2 The Universe Viewed in Gamma-Rays 1 A New TeV Source in the Vicinity of Cygnus OB2 Gavin ROWELL and Dieter HORNS (for the HEGRA Collaboration) Max Planck Institut für Kernphysik, Heidelberg, Germany Abstract

More information

Diffuse TeV emission from the Cygnus region

Diffuse TeV emission from the Cygnus region Diffuse TeV emission from the Cygnus region References: Discovery of TeV gamma-ray emission from the Cygnus region of the Galaxy Abdo et al., astro-ph/0611691 Dissecting the Cygnus region with TeV gamma

More information

A New View of the High-Energy γ-ray Sky with the Fermi Telescope

A New View of the High-Energy γ-ray Sky with the Fermi Telescope A New View of the High-Energy γ-ray Sky with the Fermi Telescope Aurelien Bouvier KIPAC/SLAC, Stanford University On behalf of the Fermi collaboration SNOWPAC, 2010 The Fermi observatory Launch: June 11

More information

Supernova Remnants and GLAST

Supernova Remnants and GLAST SLAC-PUB-14797 Supernova Remnants and GLAST Patrick Slane Harvard-Smithsonian Center for Astrophysics Abstract. It has long been speculated that supernova remnants represent a major source of cosmic rays

More information

VERITAS Performance Gernot Maier

VERITAS Performance Gernot Maier VERITAS Performance Gernot Maier Alliance for Astroparticle Physics What scientific impact will VERITAS have in the next 3-5 years? Galactic long-term plan Performance Operations LTP & Performance May

More information

arxiv: v1 [astro-ph.he] 29 Aug 2015

arxiv: v1 [astro-ph.he] 29 Aug 2015 A detailed study of Gamma-ray emission from Cassiopeia A using VERITAS arxiv:1508.07453v1 [astro-ph.he] 29 Aug 2015 1 University of Delaware, 19716, USA E-mail: sajan@udel.edu Supernova remnants (SNRs)

More information

The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission

The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission 1 Outline Mainly from 2009 ApJ 697 1071 The Pair Conversion Telescope The Large Area Telescope Charged Background and Events

More information

A pulsar wind nebula associated with PSR J as the powering source of TeV J

A pulsar wind nebula associated with PSR J as the powering source of TeV J A pulsar wind nebula associated with PSR J2032+4127 as the powering source of TeV J2032+4130 Javier Moldón Netherlands Institute for Radio Astronomy Extreme Astrophysics in an Ever-Changing Universe Crete,

More information

Supernova Remnants as Cosmic Ray Accelerants. By Jamie Overbeek Advised by Prof. J. Finley

Supernova Remnants as Cosmic Ray Accelerants. By Jamie Overbeek Advised by Prof. J. Finley Supernova Remnants as Cosmic Ray Accelerants By Jamie Overbeek Advised by Prof. J. Finley Cosmic Rays Discovered by Victor Hess in 1911 during a balloon flight through Austria He used an electroscope to

More information

Calibrating Atmospheric Cherenkov Telescopes with the LAT

Calibrating Atmospheric Cherenkov Telescopes with the LAT Gamma-ray Large Area Space Telescope Calibrating Atmospheric Cherenkov Telescopes with the LAT S. W. Digel SLAC GLAST-for-Lunch, 21 April 2005 1 Outline IACTs vs. LAT Cross calibration Issues Advantages

More information

The Fermi Gamma-ray Space Telescope

The Fermi Gamma-ray Space Telescope Abstract The Fermi Gamma-ray Space Telescope Tova Yoast-Hull May 2011 The primary instrument on the Fermi Gamma-ray Space Telescope is the Large Area Telescope (LAT) which detects gamma-rays in the energy

More information

Galactic Accelerators : PWNe, SNRs and SBs

Galactic Accelerators : PWNe, SNRs and SBs TeV γ-ray Observations and Implications for Galactic Accelerators : PWNe, SNRs and SBs (co-chair, HESS working group on SNRs, pulsars and PWNe) LPTA, Montpellier, France Particle Acceleration in Astrophysical

More information

The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays

The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays Simona Murgia, SLAC-KIPAC for the Fermi LAT Collaboration Dark Matter Signatures in the Gamma-ray Sky Austin, Texas 7-8 May 2012 arxiv:0908.0195

More information

Extreme high-energy variability of Markarian 421

Extreme high-energy variability of Markarian 421 Extreme high-energy variability of Markarian 421 Mrk 421 an extreme blazar Previous observations outstanding science issues 2001 Observations by VERITAS/Whipple 10 m 2001 Light Curve Energy spectrum is

More information

CTA SKA Synergies. Stefan Wagner Landessternwarte (CTA Project Office) Heidelberg

CTA SKA Synergies. Stefan Wagner Landessternwarte (CTA Project Office) Heidelberg CTA SKA Synergies Stefan Wagner Landessternwarte (CTA Project Office) Heidelberg CTA SKA Synergies Stefan Wagner Landessternwarte (CTA Project Office) Heidelberg CTA SKA Synergies CTA Science: How and

More information

Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002

Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002 Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002 n High Energy Astronomy Multi-Messanger Astronomy Cosmic Rays

More information

Highlights from the ARGO-YBJ Experiment

Highlights from the ARGO-YBJ Experiment Highlights from the ARGO-YBJ Experiment Ivan De Mitri University of Salento and Istituto Nazionale di Fisica Nucleare Lecce, Italy On behalf of the ARGO-YBJ Collaboration 12th International Conference

More information

H.E.S.S. High Energy Stereoscopic System

H.E.S.S. High Energy Stereoscopic System H.E.S.S. High Energy Stereoscopic System MPI Kernphysik, Heidelberg Humboldt Univ. Berlin Ruhr-Univ. Bochum Univ. Hamburg Landessternwarte Heidelberg Univ. Kiel Ecole Polytechnique, Palaiseau College de

More information

Galactic Sources in Cygnus. Rene A. Ong (UCLA)

Galactic Sources in Cygnus. Rene A. Ong (UCLA) VERITAS Results on Galactic Sources in Cygnus (UCLA) for the VERITAS Collaboration ICRC 2013 (Rio de Janeiro) July 2013 OUTLINE VHE γ-rays as probes of Galactic CR origin The VERITAS Observatory The Cygnus

More information

Very high energy gamma-emission of Perseus Cluster

Very high energy gamma-emission of Perseus Cluster Very high energy gamma-emission of Perseus Cluster V.G. SINITSYNA, V.Y. SINITSYNA P. N. Lebedev Physical Institute, Leninsky prospect 53, Moscow, 119991 Russia VERY-HIGH ENERGY GAMMA-RAY ASTRONOMY of GALACTIC

More information

Prospects for Observations of Very Extended and Diffuse Sources with VERITAS. Josh Cardenzana

Prospects for Observations of Very Extended and Diffuse Sources with VERITAS. Josh Cardenzana Prospects for Observations of Very Extended and Diffuse Sources with VERITAS Josh Cardenzana New era of synergy ~0.5 at 1GeV to 10 GeV) Fermi ~0.15 at 150GeV to 1 TeV) VERITAS ~0.5 at 1TeV

More information

Particle acceleration during the gamma-ray flares of the Crab Nebular

Particle acceleration during the gamma-ray flares of the Crab Nebular Particle acceleration during the gamma-ray flares of the Crab Nebular SLAC Accelerator seminar SLAC 15 June 2011 R. Buehler for the LAT collaboration and A. Tennant, E. Costa, D. Horns, C. Ferrigno, A.

More information

Pulsars and Pulsar-Wind Nebulae: TeV to X-Ray Connection. Oleg Kargaltsev (University of Florida) George Pavlov (Penn State University)

Pulsars and Pulsar-Wind Nebulae: TeV to X-Ray Connection. Oleg Kargaltsev (University of Florida) George Pavlov (Penn State University) Pulsars and Pulsar-Wind Nebulae: TeV to X-Ray Connection Oleg Kargaltsev (University of Florida) George Pavlov (Penn State University) Pulsar Wind Nebulae. All active pulsars emit relativistic winds c

More information

Future Gamma-Ray Observations of Pulsars and their Environments

Future Gamma-Ray Observations of Pulsars and their Environments Future Gamma-Ray Observations of Pulsars and their Environments David J. Thompson NASA Goddard Space Flight Center GLAST Large Area Telescope Collaboration djt@egret.gsfc.nasa.gov D. Thompson 363 rd Heraeus

More information

Recent discoveries from TeV and X- ray non-thermal emission from SNRs

Recent discoveries from TeV and X- ray non-thermal emission from SNRs Recent discoveries from TeV and X- ray non-thermal emission from SNRs «From Neutrino to multimessenger astronomy» Marseille Fabio Acero LUPM (LPTA), Montpellier Fabio Acero 1 Outline Evidence of acceleration

More information

VERITAS. Tel 3. Tel 4. Tel 1. Tel 2

VERITAS. Tel 3. Tel 4. Tel 1. Tel 2 VHE Astrophysics with VERITAS VERITAS Tel 2 Tel 1 Tel 4 Tel 3 Rene A. Ong Caltech/Kellogg Seminar 29 Feb 2008 Outline Scientific Motivation A New Astronomy Physicist s Viewpoint Astrophysical TeV accelerators

More information

The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays

The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays The Inner Region of the Milky Way Galaxy in High Energy Gamma Rays Simona Murgia, SLAC-KIPAC for the Fermi LAT Collaboration UCLA Dark Matter 2012 Marina del Rey 22-24 February 2012 arxiv:0908.0195 Gamma

More information

Pulsars with MAGIC. Jezabel R. Garcia on behalf of the MAGIC collaboration

Pulsars with MAGIC. Jezabel R. Garcia on behalf of the MAGIC collaboration Pulsars with MAGIC Jezabel R. Garcia on behalf of the MAGIC collaboration Introduction to MAGIC - Energy range: ~50 GeV to 50 TeV - Energy resolution: 15% (@1TeV) 23% (@100 GeV) - Angular resolution: 0.06

More information

Gamma-ray observations of blazars with the Whipple 10 m telescope

Gamma-ray observations of blazars with the Whipple 10 m telescope Gamma-ray observations of blazars with the Whipple 1 m telescope, presented on behalf of the VERITAS collaboration. E-mail: edward.collins.hughes@gmail.com This paper presents a status update of the current

More information

Fermi-LAT and WMAP observations of the SNR Puppis A

Fermi-LAT and WMAP observations of the SNR Puppis A Fermi-LAT and WMAP observations of the SNR Puppis A Marie-Hélène Grondin & Marianne Lemoine-Goumard Hewitt, J., Grondin, MH, et al. 2012, ApJ, accepted (arxiv:1210.4474) MODE-SNR-PWN workshop - November

More information

PoS(Extremesky 2011)036

PoS(Extremesky 2011)036 Univ. Complutense of Madrid E-mail: marcos@gae.ucm.es The MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes were designed to reach the lowest possible energy threshold using the ground-based

More information

Status and Future of the HESS experiment

Status and Future of the HESS experiment Status and Future of the HESS experiment Martin Tluczykont for the HESS Collaboration LLR Ecole Polytechnique Joint Symposium on GeV-TeV Astrophysics in the GLAST Era Stanford, September 2004 HESS Phase

More information

High Energy Emissions from the PSR /SS2883 Binary System

High Energy Emissions from the PSR /SS2883 Binary System High Energy Emissions from the PSR1259 63/SS2883 Binary System A. Kawachi, T. Naito and S. Nagataki Institute for Cosmic Ray Research, University of Tokyo, Chiba 277-8582, Japan Faculty of Management Information,

More information

Gamma-ray emission at the base of the Fermi bubbles. Dmitry Malyshev, Laura Herold Erlangen Center for Astroparticle Physics

Gamma-ray emission at the base of the Fermi bubbles. Dmitry Malyshev, Laura Herold Erlangen Center for Astroparticle Physics Gamma-ray emission at the base of the Fermi bubbles Dmitry Malyshev, Laura Herold Erlangen Center for Astroparticle Physics On behalf of the Fermi-LAT collaboration TeVPA 2018, Berlin Fermi bubbles surprise

More information

Recent Results from CANGAROO

Recent Results from CANGAROO 1 Recent Results from CANGAROO MASAKI MORI for the CANGAROO team Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, 277-8582 Chiba, Japan E-mail: morim@icrr.u-tokyo.ac.jp http://icrhp9.icrr.u-tokyo.ac.jp/

More information

TeV Future: APS White Paper

TeV Future: APS White Paper TeV Future: APS White Paper APS commissioned a white paper on the "Status and Future of very high energy gamma ray astronomy. For preliminary information, see http://cherenkov.physics.iastate.edu/wp Working

More information

Cherenkov Telescope Array ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP

Cherenkov Telescope Array ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP Cherenkov Telescope Array A SENSITIVE PROBE OF EXTREME UNIVERSE ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP 2015 1 The CTA Observatory SST ( 4m) LST ( 23m) MST ( 12m) South North

More information

VERITAS detection of VHE emission from the optically bright quasar OJ 287

VERITAS detection of VHE emission from the optically bright quasar OJ 287 VERITAS detection of VHE emission from the optically bright quasar OJ 287 S. Zola & NASA/JPL S. O Brien For The VERITAS Collaboration Outline 1. OJ 287 2. Historical Observations and Monitoring Programs

More information

Gamma-Ray Astronomy from the Ground

Gamma-Ray Astronomy from the Ground Gamma-Ray Astronomy from the Ground Dieter Horns University of Hamburg Introduction - summary Many new Results from ICRC 2015 No we haven't discovered dark matter, yet Yes we have discovered sources of

More information

Search for TeV Radiation from Pulsar Tails

Search for TeV Radiation from Pulsar Tails Search for TeV Radiation from Pulsar Tails E. Zetterlund 1 1 Augustana College, Sioux Falls, SD 57197, USA (Dated: September 9, 2012) The field of very high energy astrophysics is looking at the universe

More information

VHE γ-ray emitting pulsar wind nebulae discovered by H.E.S.S.

VHE γ-ray emitting pulsar wind nebulae discovered by H.E.S.S. SLAC-PUB-13255 VHE γ-ray emitting pulsar wind nebulae discovered by H.E.S.S. Y.A. Gallant, S. Carrigan, A. Djannati-Ataï, S. Funk, J.A. Hinton, S. Hoppe, O.C. de Jager, B. Khélifi, Nu. Komin, K. Kosack,

More information

Brian Humensky for the VERITAS Collaboration December 10, 2009

Brian Humensky for the VERITAS Collaboration December 10, 2009 Brian Humensky for the VERITAS Collaboration December 10, 2009 Univ ersit y of Chicago 1ES 0502+675 1ES 0229+200 27 Source Detections in 6 source classes, at least 10 in the Galactic Plane http://tevcat.uchicago.edu

More information

The origin of NORMAL cosmic rays First results from H.E.S.S. Werner Hofmann MPI für Kernphysik Heidelberg

The origin of NORMAL cosmic rays First results from H.E.S.S. Werner Hofmann MPI für Kernphysik Heidelberg The origin of NORMAL cosmic rays First results from H.E.S.S. Werner Hofmann MPI für Kernphysik Heidelberg High Energy Stereoscopic System 4 Cherenkov telescopes on a 120 m square located in Namibia full

More information

VERY HIGH-ENERGY GAMMA-RAY ASTRONOMY

VERY HIGH-ENERGY GAMMA-RAY ASTRONOMY VERY HIGH-ENERGY GAMMA-RAY ASTRONOMY Rene A. Ong Department of Physics and Astronomy, University of California, Los Angeles, Los Angeles, CA 90095, U.S.A. Very high-energy (VHE) γ-ray astronomy is an exciting

More information

HAWC: A Next Generation All-Sky VHE Gamma-Ray Telescope

HAWC: A Next Generation All-Sky VHE Gamma-Ray Telescope HAWC: A Next Generation All-Sky VHE Gamma-Ray Telescope VHE Astrophysics Energy range 10 GeV 10 TeV Non thermal processes in the universe Highly variable sources Particle acceleration Physics of extreme

More information

CANGAROO Status of CANGAROO project

CANGAROO Status of CANGAROO project CANGAROO Status of CANGAROO project Masaki Mori ICRR, University of Tokyo CANGAROO Dec.11-12, 2003 Workshop New developments in Gamma-ray Astronomy with the CANGAROO telescope, Dec.11-12, Kyoto U. Brief

More information

Observing TeV Gamma Rays from the Jet Interaction Regions of SS 433 with HAWC

Observing TeV Gamma Rays from the Jet Interaction Regions of SS 433 with HAWC Observing TeV Gamma Rays from the Jet Interaction Regions of SS 433 with HAWC Chang Dong Rho University of Rochester TeVPA 2018 Berlin, Germany 08/28/2018 Overview 2 Microquasars as sources of TeV gamma

More information

TeV Gammas and Cosmic ray production in Tycho s SNR and Geminga

TeV Gammas and Cosmic ray production in Tycho s SNR and Geminga TeV Gammas and Cosmic ray production in Tycho s SNR and Geminga V. G. SINITSYNA, F.I. MUSIN, S. I. NIKOLSKY, G.F. PLATONOV, V. Y. SINITSYNA, P. N. Lebedev Physical Institute, Leninsky prospect 53, Moscow,

More information

TeV Astrophysics in the extp era

TeV Astrophysics in the extp era Institute of Astronomy and Astrophysics TeV Astrophysics in the extp era Andrea Santangelo* IAAT Kepler Center Tübingen Also at IHEP, CAS, Beijing High Throughput X-ray Astronomy in the extp Era, February

More information

arxiv:astro-ph/ v1 14 Jun 1999

arxiv:astro-ph/ v1 14 Jun 1999 Current Status of VHE Astronomy Gus Sinnis Los Alamos National Laboratory arxiv:astro-ph/9906242v1 14 Jun 1999 Very-high-energy astronomy studies the Universe at energies between 30 GeV and 100 TeV. The

More information

Multi-messenger studies of point sources using AMANDA/IceCube data and strategies

Multi-messenger studies of point sources using AMANDA/IceCube data and strategies Multi-messenger studies of point sources using AMANDA/IceCube data and strategies Cherenkov 2005 27-29 April 2005 Palaiseau, France Contents: The AMANDA/IceCube detection principles Search for High Energy

More information

Cherenkov Telescope Array Status Report. Salvatore Mangano (CIEMAT) On behalf of the CTA consortium

Cherenkov Telescope Array Status Report. Salvatore Mangano (CIEMAT) On behalf of the CTA consortium Cherenkov Telescope Array Status Report Salvatore Mangano (CIEMAT) On behalf of the CTA consortium Outline Very-High-Energy Gamma-Ray Astronomy Cherenkov Telescope Array (CTA) Expected Performance of CTA

More information

The Cygnus Region - a prime target for cosmic ray accelerators

The Cygnus Region - a prime target for cosmic ray accelerators The Cygnus Region - a prime target for cosmic ray accelerators DESY Zeuthen E-mail: maria.krause@desy.de Regions with prominent star formation activity are of great interest for understanding the properties

More information

Correlated GeV TeV Gamma-Ray Emission from Extended Sources in the Cygnus Region

Correlated GeV TeV Gamma-Ray Emission from Extended Sources in the Cygnus Region Correlated GeV TeV Gamma-Ray Emission from Extended Sources in the Cygnus Region Michigan Technological University E-mail: bhona@mtu.edu A. Robare Michigan Technological University E-mail: alrobare@mtu.edu

More information

Detectors for astroparticle physics

Detectors for astroparticle physics Detectors for astroparticle physics Teresa Marrodán Undagoitia marrodan@physik.uzh.ch Universität Zürich Kern und Teilchenphysik II, Zürich 07.05.2010 Teresa Marrodán Undagoitia (UZH) Detectors for astroparticle

More information

THE PATH TOWARDS THE CHERENKOV TELESCOPE ARRAY OBSERVATORY. Patrizia Caraveo

THE PATH TOWARDS THE CHERENKOV TELESCOPE ARRAY OBSERVATORY. Patrizia Caraveo THE PATH TOWARDS THE CHERENKOV TELESCOPE ARRAY OBSERVATORY Patrizia Caraveo 5 y integration of the gamma-ray sky Optical +TeV The TeV sky > 40, Active Galactic Nuclei (Blazars) AGN TeV by electrons (strong

More information

Sources of GeV Photons and the Fermi Results

Sources of GeV Photons and the Fermi Results Sources of GeV Photons and the Fermi Results 1. GeV instrumentation and the GeV sky with the Fermi Gamma-ray Space Telescope 2. First Fermi Catalog of Gamma Ray Sources and the Fermi Pulsar Catalog 3.

More information

Stellar Binary Systems and CTA. Guillaume Dubus Laboratoire d Astrophysique de Grenoble

Stellar Binary Systems and CTA. Guillaume Dubus Laboratoire d Astrophysique de Grenoble Stellar Binary Systems and CTA Guillaume Dubus Laboratoire d Astrophysique de Grenoble Barcelona Cherenkov Telescope Array Meeting, 24-25 January 2008 X-ray binaries picture by H. Spruit relativistic outflow

More information

Pulsar Wind Nebulae: A Multiwavelength Perspective

Pulsar Wind Nebulae: A Multiwavelength Perspective Pulsar Wind Nebulae: Collaborators: J. D. Gelfand T. Temim D. Castro S. M. LaMassa B. M. Gaensler J. P. Hughes S. Park D. J. Helfand O. C. de Jager A. Lemiere S. P. Reynolds S. Funk Y. Uchiyama A Multiwavelength

More information

Particle acceleration and pulsars

Particle acceleration and pulsars Meudon, nov. 2013 p. 1/17 Particle acceleration and pulsars Fabrice Mottez LUTH - Obs. Paris-Meudon - CNRS - Univ. Paris Diderot Meudon, nov. 2013 p. 2/17 Pulsars (PSR) and pulsar wind nebulae (PWNe) Mostly

More information