Interstellar molecules uncover cosmic rays properties
|
|
- Alan Green
- 5 years ago
- Views:
Transcription
1 Interstellar molecules uncover cosmic rays properties Solenn Vaupre, P. Hily-Blant, C. Ceccarelli, G. Dubus, S. Gabici and T. Montmerle Institute of Planetology and Astrophysics of Grenoble (IPAG) Oct 30, 2014 Solenn Vaupre (IPAG) ISM molecules uncover CR properties PCMI /10/30 1 / 26
2 Today 15 orders of magnitude in energy from radio observations to cosmic rays properties Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 2 / 26
3 Interest in cosmic-rays Star formation Disk turbulence ISM chemistry Space weather High energy physics... ζ Solenn Vaupre (IPAG) ISM molecules uncover CR properties PCMI /10/30 3 / 26
4 Effects of cosmic-rays on dense gas MeV unknown spectrum GeV known spectrum TeV gas ionisation γ photon emission CR CR γ H 2 H + 2 H + 3 [...] H 2 π 0 Energy γ IRAM molecular spectrosopy FERMI-LAT, AGILE (satellites) HESS, MAGIC, VERITAS (Cherenkov) Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 4 / 26
5 CR-induced chemistry of DCO + and HCO + cosmic-rays [ζ] H + 2 (He +, H + ) H 2 HD H + 3 H 2 D + H 2 H 2 CO CO e DCO + HCO 1 H 2 D H HCO + DCO + αx(hd) βx(e )+γx(co)+δe 220/T e H, D, H 2, HD, CO Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 5 / 26
6 CR-induced chemistry of DCO + and HCO + observations DCO + HCO 1 H 2 D H T dependent αx(hd) βx e +γx(co)+δe 220/T e abundance { abundance ratio DCO + /HCO + + temperature } electron abundance x e x e ζ/n H need physical conditions to make sure no ionization by UV/X (i.e. high CO column density) Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 6 / 26
7 Chemistry summary DCO + /HCO + is determined by electrons and gas temperature e abundance is linked to ζ through gas density make sure high column density so ionization is dominated by CR We need physical conditions and DCO + /HCO + ratio to derive ζ Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 7 / 26
8 Program 1 Source: W28 SNR/MC association 2 CR ionization rate ζ from radio observations 3 CR properties Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 8 / 26
9 Galactic view Source: W28 SNR/MC association Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 9 / 26
10 Galactic view Source: W28 SNR/MC association Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 10 / 26
11 The W28 complex Source: W28 SNR/MC association Full Moon to scale + Observed positions [GeV- TeV CR γ-ray] HESS contours (TeV emission) [MeV-GeV CR ionization] molecular cloud (CO) [ 5-15, km s 1 ] Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 11 / 26
12 The W28 complex Source: W28 SNR/MC association Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 12 / 26
13 Program CR ionization rate ζ from radio observations 1 Source: W28 SNR/MC association 2 CR ionization rate ζ from radio observations 3 CR properties Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 13 / 26
14 Method CR ionization rate ζ from radio observations CO radiative transfer (LVG) n H, T, A V DCO +, HCO + LVG DCO + /HCO + chemical modeling x e, ζ mm observations [1mm 1meV] physical conditions, abundance ratios ionization Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 14 / 26
15 Spectra CR ionization rate ζ from radio observations Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 15 / 26
16 Results CR ionization rate ζ from radio observations Pos. v nh2 Tkin N(C 18 O) AV N(H 13 CO + ) N(DCO + [DCO ) + ] [HCO + ] ζ [ km s 1 ] [10 3 cm 3 ] [K] [10 15 cm 2 ] [mag] [10 12 cm 2 ] [10 12 cm 2 ] [10 17 s 1 ] N {0.2 1} 15 ± 5 4 {2 6} 21 {11 32} < 0.22 < N {2 5} 10 ± 2 3 {2 8} 16 {11 32} N {2 6} 13 ± 3 6 {4 20} 32 {21 105} N2 5.0 > 2 16 ± 2 20 {15 30} 105 {79 158} N {2 5} 10 ± 2 4 {3 10} 21 {16 53} < 0.25 < N {0.6 2} 8 ± 1 3 {2 4} 16 {11 21} < 0.2 < N {4 10} 8 ± 1 6 {5 7} 32 {26 37} < 0.35 < N {0.6 4} 12 ± 3 2 {2 3} 11 {5 16} < 0.35 < SE {1 5} 19 ± 5 6 {5 20} 32 {26 105} SE {2 10} 8 ± {0.4 20} 5 {2 105} < 0.2 < SW {1 4} 20 ± 4 4 {3 10} 21 {16 53} < 0.1 < SW {4 10} 16 ± {1 3} 5 {5 16} < 0.25 < Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 16 / 26
17 CR ionization rate ζ from radio observations ζ from observations (astrochem code) Zoom box DCO + /HCO + x(dco + ) x(e ) ζ [s 1 ] [DCO + ] / [HCO + ] ζ [s 1 ] Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 17 / 26
18 CR ionization rate ζ from radio observations ζ from observations (astrochem code) DCO + /HCO x(dco + ) x(e ) High-IP ζ [s 1 ] [DCO + ] / [HCO + ] ζ [s 1 ] Low- Ionization Phase 10 1 Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 17 / 26
19 CR ionization rate ζ from radio observations ζ from observations (astrochem code) 10 1 Low- Ionization Phase 10 2 DCO + /HCO x(dco + ) x(e ) High-IP ζ [s 1 ] [DCO + ] / [HCO + ] SE1 N5 N ζ [s 1 ] Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 17 / 26
20 Artist view CR ionization rate ζ from radio observations If DCO + /HCO + lies on the LIP OK but can t exclude some HIP If DCO + not detected no LIP on the line of sight If DCO + /HCO + not on LIP HIP dominant on the line of sight structure [DCO + ] / [HCO + ] SE1 N5 N ζ [s 1 ] Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 18 / 26
21 CR ionization rate ζ from radio observations Artist view If DCO + /HCO + lies on the LIP OK but can t exclude some HIP Molecular cloud LIP HIP HIP If DCO + not detected no LIP on the line of sight If DCO + /HCO + not on LIP HIP dominant on the line of sight structure Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 18 / 26
22 Results CR ionization rate ζ from radio observations Pos. v nh2 Tkin N(C 18 O) AV N(H 13 CO + ) N(DCO + [DCO ) + ] [HCO + ] ζ [ km s 1 ] [10 3 cm 3 ] [K] [10 15 cm 2 ] [mag] [10 12 cm 2 ] [10 12 cm 2 ] [10 17 s 1 ] N {0.2 1} 15 ± 5 4 {2 6} 21 {11 32} < 0.22 < > 13 N {2 5} 10 ± 2 3 {2 8} 16 {11 32} N {2 6} 13 ± 3 6 {4 20} 32 {21 105} N2 5.0 > 2 16 ± 2 20 {15 30} 105 {79 158} N {2 5} 10 ± 2 4 {3 10} 21 {16 53} < 0.25 < > 130 N {0.6 2} 8 ± 1 3 {2 4} 16 {11 21} < 0.2 < N {4 10} 8 ± 1 6 {5 7} 32 {26 37} < 0.35 < > 260 N {0.6 4} 12 ± 3 2 {2 3} 11 {5 16} < 0.35 < > 40 SE {1 5} 19 ± 5 6 {5 20} 32 {26 105} SE {2 10} 8 ± {0.4 20} 5 {2 105} < 0.2 < SW {1 4} 20 ± 4 4 {3 10} 21 {16 53} < 0.1 < SW {4 10} 16 ± {1 3} 5 {5 16} < 0.25 < Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 19 / 26
23 Results CR ionization rate ζ from radio observations N6 ζ [s 1 ] N5 N3 N7 N4 N1 SE Standard value in dense clouds ζ s Approx. projected distance to shock [pc] Assumed distance to W28: 2 kpc Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 20 / 26
24 Results CR ionization rate ζ from radio observations Diffuse clouds Dense clouds High AV objects ζ [s 1 ] N(H2) [cm 2 ] Padovani&Galli (20013) collection of observations Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 21 / 26
25 Program CR properties 1 Source: W28 SNR/MC association 2 CR ionization rate ζ from radio observations 3 CR properties Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 22 / 26
26 CR properties (1) CR ionization Padovani+ (2009), Fig. 14 contribution of CR to ionization GeV γ-rays in the North, NOT in the South (FERMI - Abdo et al. 2010) TeV γ-rays in the North AND in the South (HESS - Rowell et al. 2007) ionization by GeV CR [Some of these same CR also contribute to γ emission (E > 0.28 GeV)] Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 23 / 26
27 CR properties (2) CR escape GeV CR TeV CR SNR GeV CR TeV CR GeV CR still bound to SNR shell TeV CR escape sooner ionizing CR have not reached the southern cloud yet diffusion coeff estimate Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 24 / 26
28 Specific results on CR CR properties Diffusion coefficient ( ) 2 ( ) 1 R t D ( 10 GeV) pc 10 4 cm 2 /s, yr substantial agreement with e.g. Nava&Gabici (2013) Ionization losses timescale τ ion 14 ( n H 10 3 cm 3 ) 1 ( ) 3/2 E yr. MeV D R 2 d /τ ion only CR 100 MeV can spread over 3 pc Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 25 / 26
29 Conclusion Conclusion From radio to CR properties upper limit on DCO + /HCO + lower limit on ζ observation of energy-dependent CR diffusion away from the SNR high ionization due to GeV cosmic-rays Perspectives Increase number of sources (W28, W51C, W44,...) Increase number of species to characterize ζ (tracers) See Vaupré+ (2014), A&A, 568 See also [W51C]: Ceccarelli+ (2011), ApJL, 740 ; Dumas+ (2014), ApJL, 786 Solenn Vaupré (IPAG) ISM molecules uncover CR properties PCMI /10/30 26 / 26
Interaction rayons cosmiques - MIS le contexte hautes énergies
Interaction rayons cosmiques - MIS le contexte hautes énergies Guillaume Dubus remerciements à Pierrick Martin Atelier Astrochimie IPAG 24-25 novembre 2011 Institut de Planétologie et d Astrophysique de
More informationConstraints 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 informationGamma-Rays and the ISM (Mopra, ATCA, ASKAP... and others)
Gamma-Rays and the ISM (Mopra, ATCA, ASKAP... and others) Gavin Rowell High Energy Astrophysics Group, School of Physical Sciences University of Adelaide CTA/MWL Meeting (Adelaide) Sept. 2016 Image Credit:
More informationGamma ray emission from supernova remnant/molecular cloud associations
Gamma ray emission from supernova remnant/molecular cloud associations Stefano Gabici APC, Paris stefano.gabici@apc.univ-paris7.fr The Origin of galactic Cosmic Rays Facts: the spectrum is (ALMOST) a single
More informationA 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 informationVERITAS 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 informationRemnants 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 informationMOLECULES IN THE CIRCUMNUCLEAR DISK OF THE GALACTIC CENTER
MOLECULES IN THE CIRCUMNUCLEAR DISK OF THE GALACTIC CENTER Implications from Chemical Modeling Nanase Harada 1, Denise Riquelme 1, Serena Viti 2, Karl Menten 1, Miguel Requena-Torres 1, Rolf Güsten 1,
More informationCTA and the ISM. Gavin Rowell. High Energy Astrophysics Group, School of Chemistry & Physics
CTA and the ISM Gavin Rowell High Energy Astrophysics Group, School of Chemistry & Physics Nanten2 Meeting (Adelaide) Feb. 2014 CTA Integral Flux Sensitivity Bernloehr etal 2013 CTA : 50 hours HAWC : 1
More informationCosmic Rays in the Interstellar Medium. Nick Indriolo University of Illinois at Urbana- Champaign
Cosmic Rays in the Interstellar Medium Nick Indriolo University of Illinois at Urbana- Champaign November 3, 2010 Stormy Cosmos Cosmic Ray Basics Energetic charged particles and nuclei protons, alpha particles,
More informationRadio 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 informationObservations 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 informationHigh energy radiation from molecular clouds (illuminated by a supernova remnant
High energy radiation from molecular clouds (illuminated by a supernova remnant A. Marcowith (L.P.T.A. Montpellier) collaboration with S. Gabici (D.I.A.S.) 1 Outlook Introduction: Scientific interests.
More informationFermi-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 informationCTA 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 informationCosmic ray electrons from here and there (the Galactic scale)
Cosmic ray electrons from here and there (the Galactic scale) Julien Lavalle Department of Theoretical Physics Torino University and INFN Outline: (i) local electrons (ii) comments on synchrotron [based
More informationThe 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 informationRecent Observations of Supernova Remnants
1 Recent Observations of Supernova Remnants with VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) 2 Contents Supernova Remnants
More informationSupernova 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 informationPACIFIC 2014, Moorea, French Polynesia, Sep Efficient CR Acceleration and High-energy Emission at Supernova Remnants
PACIFIC 2014, Moorea, French Polynesia, 15-20 Sep 2014 Efficient CR Acceleration and High-energy Emission at Supernova Remnants Anatomy of an SNR Emission from an SNR High-energy non-thermal emission =
More informationA 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 informationParticle 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 informationQuestions 1pc = 3 ly = km
Cosmic Rays Historical hints Primary Cosmic Rays: - Cosmic Ray Energy Spectrum - Composition - Origin and Propagation - The knee region and the ankle Secondary CRs: -shower development - interactions Detection:
More informationSupernova 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 informationSupernova 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 informationShell supernova remnants as cosmic accelerators: II
Shell supernova remnants as cosmic accelerators: II Stephen Reynolds, North Carolina State University I. Observational tools II. Radio inferences III. X ray synchrotron emission IV. MeV GeV observations
More informationobservation of Galactic sources
AGILE observation of Galactic sources Andrea Giuliani Istituto Astrofisica Spaziale e Fisica Cosmica, Milano ( INAF ) on behalf of the AGILE Team Summary of the Presentation The AGILE Mission The diffuse
More informationAbsorption spectroscopy with Herschel/HIFI and IRAM-PdBI : Promises for ALMA
PRISMAS PRobing InterStellar Molecules with Absorption line Studies Absorption spectroscopy with Herschel/HIFI and IRAM-PdBI : Promises for ALMA Maryvonne Gerin Why Absorption Spectroscopy? Sensitivity
More informationThe 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 informationExploring the Ends of the Rainbow: Cosmic Rays in Star-Forming Galaxies
Exploring the Ends of the Rainbow: Cosmic Rays in Star-Forming Galaxies Brian Lacki With Todd Thompson, Eliot Quataert, Eli Waxman, Abraham Loeb 21 September 2010 The Cosmic SED Nonthermal Thermal Nonthermal
More informationSep. 13, JPS meeting
Recent Results on Cosmic-Rays by Fermi-LAT Sep. 13, 2010 @ JPS meeting Tsunefumi Mizuno (Hiroshima Univ.) On behalf of the Fermi-LAT collaboration 1 Outline Introduction Direct measurement of CRs CRs in
More informationFermi measurements of diffuse gamma-ray emission: results at the first-year milestone
SciNeGHE 2009 Assisi, October 7th Fermi measurements of diffuse gamma-ray emission: results at the first-year milestone Luigi Tibaldo luigi.tibaldo@pd.infn.it INFN Sezione di Padova Dip. di Fisica G. Galilei,
More informationRecent 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 informationRecent 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 informationHigh-Energy Plasma Astrophysics and Next Generation Gamma-Ray Observatory Cherenkov Telescope Array
High-Energy Plasma Astrophysics and Next Generation Gamma-Ray Observatory Cherenkov Telescope Array FAPESP CUNY Week, New York, November 2018 M82 Star Formation- Clouds-SNRturbulence connection Sun & Stars
More informationObserving 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 informationLecture 14 Cosmic Rays
Lecture 14 Cosmic Rays 1. Introduction and history 2. Locally observed properties 3. Interactions 4. Demodulation and ionization rate 5. Midplane interstellar pressure General Reference MS Longair, High
More informationGamma rays from supernova remnants in clumpy environments.! Stefano Gabici APC, Paris
Gamma rays from supernova remnants in clumpy environments!! Stefano Gabici APC, Paris Overview of the talk Galactic cosmic rays Gamma rays from supernova remnants Hadronic or leptonic? The role of gas
More informationMaria Cunningham, UNSW. CO, CS or other molecules?
Maria Cunningham, UNSW CO, CS or other molecules? Wide field Surveys at mm wavelengths: pu8ng the whole picture together Follow chemical abundances through the whole ISM. Follow energy transfer through
More informationThe High-Energy Interstellar Medium
The High-Energy Interstellar Medium Andy Strong MPE Garching on behalf of Fermi-LAT collaboration Cosmic Ray Interactions: Bridging High and Low Energy Astrophysics Lorentz Centre Workshop March 14-18
More informationAstro2020 Science White Paper Prospects for the detection of synchrotron halos around middle-age pulsars
Astro2020 Science White Paper Prospects for the detection of synchrotron halos around middle-age pulsars Thematic Areas: Planetary Systems Star and Planet Formation Formation and Evolution of Compact Objects
More informationA Far-ultraviolet Fluorescent Molecular Hydrogen Emission Map of the Milky Way Galaxy
A Far-ultraviolet Fluorescent Molecular Hydrogen Emission Map of the Milky Way Galaxy (The Astrophysical Journal Supplement Series, 231:21 (16pp), 2017 August) November 14, 2017 Young-Soo Jo Young-Soo
More informationThe XMM-Newton (and multiwavelength) view of the nonthermal supernova remnant HESS J
The XMM-Newton (and multiwavelength) view of the nonthermal supernova remnant HESS J- Gerd Pühlhofer Institut für Astronomie und Astrophysik Kepler Center for Astro and Particle Physics Tübingen, Germany
More informationDiscovery 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 informationCosmic Rays, Photons and Neutrinos
Cosmic Rays, Photons and Neutrinos Michael Kachelrieß NTNU, Trondheim [] Introduction Outline Plan of the lectures: Cosmic rays Galactic cosmic rays Basic observations Acceleration Supernova remnants Problems
More informationGalactic 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 informationThe Physics of the Interstellar Medium
The Physics of the Interstellar Medium Ulrike Heiter Contact: 471 5970 ulrike@astro.uu.se www.astro.uu.se Matter between stars Average distance between stars in solar neighbourhood: 1 pc = 3 x 1013 km,
More informationHigh Energy Astrophysics: A View on Chemical Enrichment, Outflows & Particle Acceleration. (Feedback at work)
High Energy Astrophysics: A View on Chemical Enrichment, Outflows & Particle Acceleration (Feedback at work) Jacco Vink Utrecht University High Energy Astrophysics HEA aims at understanding the extreme
More informationParticle acceleration in Supernova Remnants
Particle acceleration in Supernova Remnants Anne Decourchelle Service d Astrophysique, CEA Saclay Collaborators: J. Ballet, G. Cassam-Chenai, D. Ellison I- Efficiency of particle acceleration at the forward
More informationMASSIVE STARS IN COLLIDING WIND SYSTEMS: THE HIGH-ENERGY GAMMA-RAY PERSPECTIVE
MASSIVE STARS IN COLLIDING WIND SYSTEMS: THE HIGH-ENERGY GAMMA-RAY PERSPECTIVE Anita Reimer, HEPL & KIPAC, Stanford University Scineghe 2008, Padova, Oct. 2008 Massive Stars......are hot (~3-6 10 4 K),
More informationGamma-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 informationTHE TeV GAMMA-RAY MILKY WAY
Publications of the Korean Astronomical Society pissn: 1225-1534 30: 553 557, 2015 September eissn: 2287-6936 c 2015. The Korean Astronomical Society. All rights reserved. http://dx.doi.org/10.5303/pkas.2015.30.2.553
More informationChemical Diagnostics of Star Forming Regions
School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES Chemical Diagnostics of Star Forming Regions Paola Caselli N 2 H + (1-0) Di Francesco et al. 2004 N 2 H + (3-2) Bourke et al.
More informationCosmic rays in the local interstellar medium
Cosmic rays in the local interstellar medium Igor V. Moskalenko Igor V. Moskalenko/NASA-GSFC 1 LMC (Magellanic Cloud Emission Nuclear Data-2004/09/28, Line Survey: Smith, Points) Santa Fe R - H G - [S
More informationFermi: 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 informationFUSE results concerning the diffuse and translucent clouds. Franck Le Petit
FUSE results concerning the diffuse and translucent clouds Franck Le Petit Outline I Diffuse and transluscent clouds a) Generalities b) The Meudon PDR code II Results of the FUSE survey a) H2 and HD in
More informationThe puzzling emission of γ-ray binaries
Credit: F. Reddy/NASA/GSFC The puzzling emission of γ-ray binaries Guillaume Dubus with special thanks to Benoît Cerutti & Astrid Lamberts Texas symposium, Dallas, dec. 2013 Institut de Planétologie et
More informationSupernova Remnant Studies with Fermi LAT
Supernova Remnant Studies with Fermi LAT J.W. Hewitt Univ. of North Florida on behalf of the Fermi LAT collaboration TeVPA 2017 Columbus, OH August 7, 2017 Fermi Larger Area Telescope (LAT) Large Area
More informationGamma-ray emission from cosmic rays and interstellar medium interactions in star-forming galaxies
Mem. S.A.It. Vol. 82, 888 c SAIt 2011 Memorie della Gamma-ray emission from cosmic rays and interstellar medium interactions in star-forming galaxies P. Martin 1 and K. Bechtol 2 on behalf of the Fermi/LAT
More informationThe role of cosmic rays on magnetic field diffusion and the formation of protostellar discs
CRIME workshop APC Paris, Nov 14 th 2014 The role of cosmic rays on magnetic field diffusion and the formation of protostellar discs Marco Padovani (LUPM Montpellier) in collaboration with Daniele Galli
More informationLecture 6: Molecular Transitions (1) Astrochemistry
Lecture 6: Molecular Transitions (1) Astrochemistry Ehrenfreund & Charnley 2000, ARA&A, 38, 427 Outline Astrochemical processes: The formation of H2 H3 formation The chemistry initiated by H3 Formation
More information19. Interstellar Chemistry
19. Interstellar Chemistry 1. Introduction to Interstellar Chemistry 2. Chemical Processes & Models 3. Formation & Destruction of H 2 4. Formation & Destruction of CO References Duley & Williams, "Interstellar
More informationGalactic Diffuse Gamma-Ray Emission
Galactic Diffuse Gamma-Ray Emission The Bright Gamma-Ray Sky 7 th AGILE Workshop 29 Sep - 1 Oct, 2009 Stanley D. Hunter NASA/GSFC stanley.d.hunter@nasa.gov Galactic Diffuse Emission The beginning: OSO
More informationThe VERITAS Dark M atter and Astroparticle Programs. Benjamin Zitzer For The VERITAS Collaboration
The VERITAS Dark M atter and Astroparticle Programs Benjamin Zitzer For The VERITAS Collaboration Introduction to VERITAS Array of four IACTs in Southern AZ, USA Employs ~100 Scientists in five countries
More informationIndirect Dark Matter Searches in the Milky Way Center with the LAT on board Fermi
Indirect Dark Matter Searches in the Milky Way Center with the LAT on board Fermi B. Cañadas, A. Morselli and V. Vitale on behalf of the Fermi LAT Collaboration Outline Gamma rays from Dark Matter Dark
More informationRevue sur le rayonnement cosmique
Revue sur le rayonnement cosmique Vladimir Ptuskin IZMIRAN Galactic wind termination shock GRB N cr ~ 10-10 cm -3 - total number density w cr ~ 1.5 ev/cm 3 - energy density E max ~ 3x10 20 ev - max. detected
More informationDark gas contribution to diffuse gamma-ray emission
Dark gas contribution to diffuse gamma-ray emission Masaki Mori ICRR CANGAROO group internal seminar, November 7, 2005 Adrian Cho S. Hunter, GLAST meeting, Oct.2004 The Galactic Diffuse Gamma-ray Emission...
More informationGamma-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 informationHESS discovery of VHE γ-ray emission of a remarkable young composite SNR
HESS discovery of VHE γ-ray emission of a remarkable young composite SNR Arache Djannati-Ataï*, V. Marandon, R. Chaves, R. Terrier & N. Komin for the HESS Collaboration *Laboratoire d'astroparticule et
More informationDiffuse Interstellar Medium
Diffuse Interstellar Medium Basics, velocity widths H I 21-cm radiation (emission) Interstellar absorption lines Radiative transfer Resolved Lines, column densities Unresolved lines, curve of growth Abundances,
More informationGamma-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 informationON PROBABLE CONTRIBUTION OF NEARBY SOURCES TO ANISOTROPY AND SPECTRUM OF COSMIC RAYS AT TEV-PEV-ENERGIES
ON PROBABLE CONTRIBUTION OF NEARBY SOURCES TO ANISOTROPY AND SPECTRUM OF COSMIC RAYS AT TEV-PEV-ENERGIES SVESHNIKOVA L.G. 1, STRELNIKOVA O.N. 1, PTUSKIN V.S. 3 1 Lomonosov Moscow State University, SINP,
More informationDetailed Study of a Turbulent multiphase multicomponent ISM
Detailed Study of a Turbulent multiphase multicomponent ISM Dieter Breitschwerdt Collaborators Miguel de Avillez (Evora, Portugal) Verena Baumgartner (Vienna, Austria) Jan Bolte (TU Berlin, Germany) Jenny
More informationW.R. Webber. New Mexico State University, Astronomy Department, Las Cruces, NM 88003, USA
A Galactic Cosmic Ray Electron Spectrum at Energies from 2 MeV to 2 TeV That Fits Voyager 5-60 MeV Data at Low Energies and PAMELA and AMS-2 Data at 10 GeV Using an Electron Source Spectrum ~E -2.25 A
More informationObserving 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 informationInterstellar gamma rays. New insights from Fermi. Andy Strong. on behalf of Fermi-LAT collaboration. COSPAR Scientific Assembly, Bremen, July 2010
Interstellar gamma rays New insights from Fermi Andy Strong on behalf of Fermi-LAT collaboration COSPAR Scientific Assembly, Bremen, July 2010 Session E110: ' The next generation of ground-based Cerenkov
More informationPossible high energy phenomena related to the stellar capture by the galactic supermassive black holes. K S Cheng University of Hong Kong China
Possible high energy phenomena related to the stellar capture by the galactic supermassive black holes K S Cheng University of Hong Kong China Outline Introduction Swift J1644+57 Positron Annihilation
More informationGamma rays from star- forming regions. Jürgen Knödlseder (IRAP, Toulouse) 1
Gamma rays from star- forming regions Jürgen Knödlseder (IRAP, Toulouse) 1 Gamma- ray sources in star- forming regions Star forming regions as paracle accelerators Pulsars and wind nebulae Supernova remnants
More informationStudy of the very high energy gamma-ray diffuse emission in the central 200 pc of our galaxy with H.E.S.S.
Study of the very high energy gamma-ray diffuse emission in the central 200 pc of our galaxy with H.E.S.S. Lemière A., Terrier R., Jouvin L., Marandon V, Lefranc V., Viana A. For the H.E.S.S. Collaboration
More informationFractionation in Infrared Dark Cloud Cores
15N Fractionation in Infrared Dark Cloud Cores Shaoshan (Sandy) Zeng, Izaskun Jiménez-Serra, Giuliana Cosentino, Serena Viti, Ashley Barnes, Jonathan Henshaw, Paola Caselli, Francesco Fontani, Piere Hily-Blant
More informationObservations of supernova remnants
Observations of supernova remnants Anne Decourchelle Service d Astrophysique, CEA Saclay I- Ejecta dominated SNRs: Cas A, Tycho and Kepler II- Synchrotron-dominated SNRs: SN 1006, G347.3-0.5 Young supernova
More informationCosmic 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 informationThe First Fermi LAT SNR Catalog SNR and Cosmic Ray Implications
The First Fermi LAT SNR Catalog SNR and Cosmic Ray Implications T. J. Brandt (1), F. Acero (2), (3,4), J. W. Hewitt (1,5), M. Renaud (6), on behalf of the Fermi LAT Collaboration (1) NASA Goddard Space
More informationThe 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 informationPulsar 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 informationMolecular properties of (U)LIRGs: CO, HCN, HNC and HCO +
Proceedings Astrophysical Masers and their Environments Proceedings IAU Symposium No. 242, 2007 J.M. Chapman & W.A. Baan, eds. c 2007 International Astronomical Union DOI: 000/X000000000000000X Molecular
More informationCTB 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 informationHESS J : A new gamma-ray binary?
HESS J0632+057: A new gamma-ray binary? Joanna Skilton MPIK Jim Hinton, Julia Brucker, M. Pommier, T. Cheung, A. Marcowith, G. Dubus, Y. Gallant, S. Funk, O. Reimer, A. Fiasson, F.A. Aharonian + many more!
More information22. Molecular Ions and Fractionation. 1. Review of Gas Phase Chemistry 2. Introduction to Molecular Ions 3. The Detection of H 3
22. Molecular Ions and Fractionation 1. Review of Gas Phase Chemistry 2. Introduction to Molecular Ions 3. The Detection of H 3 and the Cosmic-Ray Ionization Rate 4. Isotope Fractionation References Tielens,
More informationSpectral analysis of the 511 kev Line
Spectral analysis of the 511 kev Line Gillard William (C.E.S.R) From P. Jean et al. A&A, in press ( astro-ph/0509298 ) I. Introduction II. Annihilation spectrum 1. Independent model 2. Astrophysical model
More informationStellar 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 informationAstrophysical issues in the cosmic ray e spectra: Have we seen dark matter annihilation?
Astrophysical issues +/ in the cosmic ray e spectra: Have we seen dark matter annihilation? Julien Lavalle Department of Theoretical Physics University of Torino and INFN Collab: Torino: R. Lineros, F.
More informationFermi-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 informationNon-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 informationarxiv: v1 [astro-ph.he] 28 Nov 2011
Gamma-ray Astronomy: Implications for Fundamental Physics J. Rico Institució Catalana de Recerca i Estudis Avançats (ICREA) & Institut de Física d Altes Energies (IFAE), Bellaterra (Barcelona), 08193,
More informationDiffusive shock acceleration: a first order Fermi process. jan.-fév NPAC, rayons cosmiques E. Parizot (APC)
1 Diffusive shock acceleration: a first order Fermi process 2 Shock waves Discontinuity in physical parameters shock front n 2, p 2, T 2 n 1, p 1, T 1 v 2 v 1 downstream medium (immaterial surface) upstream
More informationParticle Acceleration at Supernova Remnants and Supernovae
Particle Acceleration at Supernova Remnants and Supernovae Gwenael Giacinti 1 & Tony Bell 2 1 MPIK, Heidelberg 2 Clarendon Laboratory, University of Oxford Giacinti & Bell, MNRAS 449, 3693 (2015); Bell,
More informationHigh-Energy GammaRays toward the. Galactic Centre. Troy A. Porter Stanford University
High-Energy GammaRays toward the Galactic Centre Troy A. Porter Stanford University Fermi LAT 5-Year Sky Map > 1 GeV Galactic Plane Galactic Centre Point Sources Diffuse γ-ray emission produced by cosmic
More informationThe LHAASO-KM2A detector array and physical expectations. Reporter:Sha Wu Mentor: Huihai He and Songzhan Chen
The LHAASO-KM2A detector array and physical expectations Reporter:Sha Wu Mentor: Huihai He and Songzhan Chen Outline 1. Introduction 2. The KM2A Detector Array 3. Physical Expectations 3.1 Sensitivity
More informationSources 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