Comic Gamma-Ray Background from Dark Matter Annihilation
|
|
- Lorraine Sullivan
- 6 years ago
- Views:
Transcription
1 TeV Particle Astrophysics II Madison (Aug. 29, 2006) Comic Gamma-Ray Background from Dark Matter Annihilation Shin ichiro Ando (California Institute of Technology) S. Ando & E. Komatsu, Phys. Rev. D 73, (2006) S. Ando, E. Komatsu, T. Narumoto & T. Totani, to be submitted
2 1. Introduction
3 Cosmic gamma-ray background (CGB) Extragalactic Diffuse γ-ray Background 0.0 HEAO A2,A4(LED) E2 dj/de (kev2/(cm2-s-kev-sr) ASCA HEAO-A4 (MED).0 COMPTEL EGRET 1.0 v Photon Energy (kev) Strong et al Fig. 3. Extragalactic X-ray and γ-ray spectrum. Data compilation from Sreekumar et al. (1998) except for (Weidenspointner et al. 2000) and EGRET 30 MeV 20 GeV (this work). (1998). Fig. 3 shows the extragalactic X- and ground, using the compilation by Sreekumar e but using our new EGRET values, and al COMPTEL results (Weidenspointner et al. 2 Discovered with EGRET at GeV region Same photon intensity coming from all the directions Table 3. EGRB intensity. 6 Eγ, MeV Intensity, cm 2 sr 1 s 1 MeV 1 Total error FURTHER CHECKS FOR SYSTEMATICS MODEL In order to check the robustness of our mates, we compare estimates based on data hemispheres and four quarter spheres (Tab tests for the presence of apparent anisotro EGRB values, and thus gives an independe
4 Origin of CGB at GeV region: Candidates 1. Blazars AGN population beaming towards Earth ~50 detected as point sources by EGRET 2. Galaxy clusters Either pp collisions or electron inverse-compton 3. Dark matter annihilation Good candidate motivated by particle physics (e.g., supersymmetric neutralino) Energy spectrum is characteristic
5 Blazar contribution Luminosity function constructed with the detected EGRET blazar properties he 68%, 95% and 99% C.L. regions for the PLE model parameters [the faint-end slope index γ1 and the mean gamma-ray 0 (Lγ /Lr )"]. The best-fit values, (!p",γ1 ) = (3.28,0.69), are shown by the cross. The dashed contours correspond to.33, respectively, where η is the ratio of the normalizations of the gamma-ray to radio luminosity functions. GAMMA-RAY LUMINOSITY FUNCTION OF BLAZARS Narumoto & Totani dn/d(logz) 1.2 LDDE model PLE model SS96 model EGRET blazars LDDE model PLE model SS96 model EGRET blazars dn/d(logl!) Redshift z log (L! [erg s"1]) F IG. data. 6. The Luminosity of the blazars. Thefor line are the same as Figure 5. The luminosity is νl EGRET blazars. The histogram is the EGRET solid anddistribution dashed curves areegret the best-fit models themarkings LDDE and 1σ Poisson error. elihood analysis. The dotted curve is obtained from the blazar GLF model of SS96. The error bars are 1σ Poisson error. Luminosity-dependent density evolution (LDDE) model is more prefered
6 Blazar contribution Best LDDE model explains only ~25% of the CGB above 0 MeV Most CGB still can only be explained, although such a model is disfavored at ~2σ level Still, the excess around 3 GeV cannot be attributed to blazars
7 [32]. The blazar model also would imply 00 sources with a > 300 GeV flux of the order of a typical Whipplesource, whereas the steeper power law alone corresponds to 40 sources. The first number seems worryingly large in view of the confirmed sources, in spite of excessive observation campaigns on candidate sources from Dark matter annihilation? Annihilation into gamma rays in all the observable dark halos Is the excess due to this signal? Constraint by the Galactic center (Ando 2005, PRL 94, ) can be avoided by Elsässer & Mannheim 2005 FIG. 2: Extragalactic gamma-ray background: spectrum as determined from EGRET data by Strong et al. (data points); substructure (Oda, Totani & Nagashima 2005), or minispikes around IMBH (Horiuchi & Ando 2006; see also, Bertone, Zentner & Silk 2005)
8 Quick summary on CGB EGRET confirmed the existence of diffuse extragalactic gamma-ray emission (CGB) The CGB would contributed by either astrophysical sources such as blazars, or annihilating dark matter GLAST could pinpoint the origin Better understanding of blazars Potentially a smoking gun of dark matter annihilation Spectrum might not be sufficient for such a strong claim
9 2. Anisotropy as a Smoking Gun
10 Anisotropy from dark matter annihilation Rate of annihilation depends on density squared A characteristic very different from ordinary astrophysical objects The CGB anisotropy should also be quite different This could provide more stringent evidence of particle dark matter
11 Angular power spectrum Dark matter halo Projected along the line of sight is the CGB intensity Angular power spectrum, Cl, is related to the spatial power spectrum via Limber s equation 3D correlation can be modeled, using θ (= π / l) halo mass function, and density profile in each halo
12 A few equations..., if you want Gamma-ray intensity: I γ (ˆn, E γ ) = dr δ 2 (r, ˆnr)W ([1 + z]e γ, r) Spherical harmonic expansion: δi γ (ˆn) I γ = lm a lm Y lm (ˆn) C l = a lm 2 Limber s equation: dr I γ 2 C l = {W ([1 + z]e γ, r)} 2 P f r 2 f = δ 2 δ 2 (k = lr ; r )
13 3D power spectrum (z=0) 2 f (k) = k3 P f (k) 2π 2 δ 2 2 Ando & Komatsu, PRD 73, (2006)
14 Angular power spectrum M min is the lower mass cutoff, below which no dark halos are formed M min = 6 Msun is set by the free-streaming of the neutralino M min = 6 Msun is set by the Jeans mass of the baryon, below which halos might be tidally disrupted Ando & Komatsu, PRD 73, (2006)
15 3. Detectability
16 What are backgrounds? From Detector background!"##$%&'#($)*'+#,&-'.$,%*'%.+(&/',0' 1&2&-+,&/' $2/ Negligible, being 5% of the CGB above 0 MeV (even smaller at GeV) (01567'.0--&.,&/'58&97
17 -3 EB 6-4 What are backgrounds? energy, MeV bremss 1! " MeV -1 s -1 sr -2. intensity, cm 2 E MeV -1 s -1 sr -2. intensity, cm 2 E galdef ID 44_ IC galdef ID 44_ IC deg 1 total EB bremss! " 2 total EB 2! " deg <l<179.75, <l< <b<-20.25, 20.25<b< energy, MeV 0.25<l<179.75, <l< <b<-60.25, 60.25<b< energy, MeV Strong et al described in Table 2: top row H A B, middle row Galactic cosmic rays a foreground It strongly depends on the galactic latitude The flux is about one order of magnitude smaller than CGB for b > 20 deg, safely negligible
18 Detectability: Pure dark matter case Ando & Komatsu, PRD 73, (2006) Adopted GLAST parameters: Aeff 4 cm 2 Ωfov 2.4 sr θres T 1 yr
19 Detectability: Lower Cutoff Ando & Komatsu, PRD 73, (2006)
20 Mixed case with blazars Mmin = 6 Msun Mmin = 6 Msun Ando et al., to be submitted
21 4. Conclusions
22 The CGB anisotropy would be a key to revealing the origin of CGB, and potentially be a smoking gun of annihilating dark matter The resulting angular spectrum would be very different from the case of other sources We developed a new formalism for that calculation We showed that if the annihilating dark matter is a main CGB constituent, GLAST can detect anisotropy in a few years This is also true even with the existence of other sources like blazars, if the current dark matter contribution exceeds 30% at GeV
Hunting for Dark Matter in Anisotropies of Gamma-ray Sky: Theory and First Observational Results from Fermi-LAT
Hunting for Dark Matter in Anisotropies of Gamma-ray Sky: Theory and First Observational Results from Fermi-LAT Eiichiro Komatsu (Texas Cosmology Center, Univ. of Texas at Austin) MPA Seminar, September
More informationGamma-ray background anisotropy from Galactic dark matter substructure
Gamma-ray background anisotropy from Galactic dark matter substructure Shin ichiro Ando (TAPIR, Caltech) Ando, arxiv:0903.4685 [astro-ph.co] 1. Introduction Dark matter annihilation and substructure Dark
More informationSearching for dark matter. with gamma-ray anisotropies
Image Credit: NASA/DOE/International LAT Team Searching for dark matter with gamma-ray anisotropies Jennifer Siegal-Gaskins CCAPP, Ohio State University with Brandon Hensley (Caltech!Princeton) Eiichiro
More informationDiffuse Gamma-Ray Emission
Diffuse Gamma-Ray Emission Debbijoy Bhattacharya Manipal Centre for Natural Sciences (MCNS) Manipal University 5 Sept 2014 Observational Gamma-Ray Astronomy Atmospheric Window 00 11 00 11 Figure: Atmospheric
More informationGLAST - Exploring the high- energy gamma-ray Universe
GLAST - Exploring the high- energy gamma-ray Universe Julie McEnery NASA/GSFC (many thanks to the members of the LAT DM&NP working group for figures and suggestions for this talk) Julie McEnery 1 Outline
More informationConstraints and Signals from the Diffuse Gamma Ray and X-ray Backgrounds
Constraints and Signals from the Diffuse Gamma Ray and X-ray Backgrounds Kevork Abazajian University of California, Irvine!! KICP High-Energy Messengers Workshop June 10, 2014 The Diffuse Gamma Ray Background
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 informationEBL Studies with the Fermi Gamma-ray Space Telescope
EBL Studies with the Fermi Gamma-ray Space Telescope Luis C. Reyes KICP The Extragalactic Background Light (EBL) What is it? Accumulation of all energy releases in the form of electromagnetic radiation.
More informationConstraints on dark matter annihilation cross section with the Fornax cluster
DM Workshop@UT Austin May 7, 2012 Constraints on dark matter annihilation cross section with the Fornax cluster Shin ichiro Ando University of Amsterdam Ando & Nagai, arxiv:1201.0753 [astro-ph.he] Galaxy
More informationResolving the Extragalactic γ-ray Background
Resolving the Extragalactic γ-ray Background Marco Ajello Clemson University On behalf of the Fermi-LAT collab. (with a few additions by Jack) Ackermann+2015, ApJ, 799, 86 Ajello+2015, ApJL, 800,27 Ackermann+2016,
More informationMattia Di Mauro. Fermi-LAT point source population studies and origin of the Fermi-LAT gamma-ray background. Trieste, May, 3, 2016
Fermi-LAT point source population studies and origin of the Fermi-LAT gamma-ray background Mattia Di Mauro On behalf of the Fermi- LAT Collaboration 1 Trieste, May, 3, 2016 THE ISOTROPIC GAMMA RAY BACKGROUND
More informationCross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background
Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background Masato Shirasaki (Univ. of Tokyo) with Shunsaku Horiuchi (UCI), Naoki Yoshida (Univ. of Tokyo, IPMU) Extragalactic Gamma-Ray Background
More informationDark matter indirect searches: Multi-wavelength and anisotropies
Journal of Physics: Conference Series PAPER OPEN ACCESS Dark matter indirect searches: Multi-wavelength and anisotropies To cite this article: Shin ichiro Ando 2016 J. Phys.: Conf. Ser. 718 022002 Related
More informationHigh energy resolution GeV gamma ray detector Satoko Osone Funabashi, Chiba, , JAPAN
High energy resolution GeV gamma ray detector Satoko Osone Funabashi, Chiba, 273-0865, JAPAN osone@icrr.u-tokyo.ac.jp Abstract We design a GeV gamma ray detector based on an electron-positron pair measurement
More informationSearch for exotic process with space experiments
Search for exotic process with space experiments Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata Rencontres de Moriond, Very High Energy Phenomena in the Universe Les Arc, 20-27
More informationM. Lattanzi. 12 th Marcel Grossmann Meeting Paris, 17 July 2009
M. Lattanzi ICRA and Dip. di Fisica - Università di Roma La Sapienza In collaboration with L. Pieri (IAP, Paris) and J. Silk (Oxford) Based on ML, Silk, PRD 79, 083523 (2009) and Pieri, ML, Silk, MNRAS
More informationHow bright can the brightest neutrino source be?
TeV Particle Astrophysics Columbus, OH August, 2017 How bright can the brightest neutrino source be? Shin ichiro Ando University of Amsterdam Ando, Feyereisen, Fornasa, Phys. Rev. D 95, 3003 (2017) Lessons
More informationEnhancement of Antimatter Signals from Dark Matter Annihilation
Enhancement of Antimatter Signals from Dark Matter Annihilation around Intermediate Mass Black Holes Pierre Brun Laboratoire d Annecy-le-vieux de Physique des Particules CNRS/IN2P3/Université de Savoie
More informationPreheating in the Universe Suppressing High Energy Gamma-rays from Structure Formation
Preheating in the Universe Suppressing High Energy Gamma-rays from Structure Formation Tomonori Totani and Susumu Inoue Division of Theoretical Astrophysics, National Astronomical Observatory, Mitaka,
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 informationConstraining Dark Matter annihilation with the Fermi-LAT isotropic gamma-ray background
Constraining Dark Matter annihilation with the Fermi-LAT isotropic gamma-ray background Fiorenza Donato @ Physics Dept., Un. Torino The gamma-ray sky - Minneapolis, October 10, 2013 Plan of my talk What
More informationstringent constraint on galactic positron production
stringent constraint on galactic positron production the ohio state university Phys. Rev. Lett. 97, 071102 (2006) [astro-ph/0512411] in collaboration with john beacom Workshop on TeV Particle Astrophysics
More informationConservative Constraints on Dark Matter Self Annihilation Rate
Conservative Constraints on Dark Matter Self Annihilation Rate Thomas Jacques 2009-07-13, TeVPA 2009 Indirect Detection Indirect detection often focuses on choosing a model, and comparing predicted flux
More informationIndirect dark matter detection and the Galactic Center GeV Excess
Image Credit: Springel et al. 2008 Indirect dark matter detection and the Galactic Center GeV Excess Jennifer Siegal-Gaskins Caltech Image Credit: Springel et al. 2008 Jennifer Siegal-Gaskins Caltech Image
More informationSignal Model vs. Observed γ-ray Sky
Signal Model vs. Observed γ-ray Sky Springel+, Nature (2008) Two main dark matter signal components: 1. galactocentric diffuse 2. small structures Observed sky modeled with bremsstrahlung π 0 decay up-scattered
More informationDifficulties of Star-forming Galaxies as the Source of IceCube Neutrinos. Takahiro Sudoh (UTokyo)
Difficulties of Star-forming Galaxies as the Source of IceCube Neutrinos Takahiro Sudoh (UTokyo) IceCube Neutrino Astrophysical TeV - PeV neutrinos Isotropic arrival direction extragalactic origin? No
More informationGamma rays from Galactic pulsars: high- and lowlatitude
Francesca Calore Gamma rays from Galactic pulsars: high- and lowlatitude emission Conca Specchiulla, 8th September 2014 based on: F. Calore, M. Di Mauro & F. Donato, arxiv:1406.2706 F. Calore, I. Cholis
More informationVERITAS 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 informationSearches for WIMP annihilation with GLAST
SLAC-PUB-11289 Searches for WIMP annihilation with GLAST Larry Wai Stanford Linear Accelerator Center, Stanford, California representing the GLAST LAT Collaboration Abstract We describe signatures for
More informationDark Matter Electron Anisotropy: A universal upper limit
Seminari teorici del venerdì Enrico Borriello Università degli Studi di Napoli Federico II & INFN Sezione di Napoli Dark Matter Electron Anisotropy: A universal upper limit Based on Borriello, Maccione,
More informationWhat Can GLAST Say About the Origin of Cosmic Rays in Other Galaxies
SLAC-PUB-8660 October 2000 astro-ph/0003407 What Can GLAST Say About the Origin of Cosmic Rays in Other Galaxies Seth Digelaxb, Igor V. Moskalenko xc, and Jonathan F. Ormes, P. Sreekumard. and P. Roger
More informationParticle 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 information1. Motivation & Detector concept 2. Performance 3. Confirmation experiments 4. Summary
A. Takada, T. Tanimori, H. Kubo, J. D. Parker, T. Mizumoto, Y. Mizumura, T. Sawano, K. Nakamura, Y. Matsuoka, S. Komura, S. Nakamura, T. Kishimoto, M. Oda, T. Takemura, S. Miyamoto, K. Miuchi, S. Kurosawa
More informationarxiv: v1 [astro-ph] 17 Nov 2008
Dark Matter Annihilation in the light of EGRET, HEAT, WMAP, INTEGRAL and ROSAT arxiv:0811.v1 [astro-ph 1 Nov 008 Institut für Experimentelle Kernphysik, Universiät Karlsruhe E-mail: gebauer@ekp.uni-karlsruhe.de
More informationExtreme 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 informationThe Secondary Universe
Secondary photons and neutrinos from distant blazars and the intergalactic magnetic fields UC Berkeley September 11, 2011 The talk will be based on A new interpretation of the gamma-ray observations of
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 informationAstroparticle Anomalies
Astroparticle Anomalies Current Hints of Possible Dark Matter Signals Sheldon Campbell University of California, Irvine What is this talk really about? Isn t discussion of low-significance anomalies just
More informationAGILE Highlights. The AGILE Mission. Stefano Vercellone and the AGILE Team at IASF Milano
The AGILE Mission AGILE Highlights Stefano Vercellone and the AGILE Team at IASF Milano AGILE Highlights Visiting Committee Review - Milano, January 8 th, 2008 1 AGILE in a nutshell Super-AGILE AGILE-GRID
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 informationDM subhalos: The obser vational challenge
DM subhalos: The obser vational challenge Hannes-S. Zechlin and Dieter Horns Inst. f. Experimentalphysik, Universität Hamburg, Germany July 26th, 2012 DM subhalos in the Milky Way concordance cosmology
More informationTesting a DM explanation of the positron excess with the Inverse Compton scattering
Testing a DM explanation of the positron excess with the Inverse Compton scattering Gabrijela Zaharijaš Oskar Klein Center, Stockholm University Work with A. Sellerholm, L. Bergstrom, J. Edsjo on behalf
More informationCharged-particle and gamma-ray astronomy: deciphering charged messages from the world s most powerful
Charged-particle and gamma-ray astronomy: deciphering charged messages from the world s most powerful Charged-particle astronomy coming of age How it is done The sources The signals What we have learned
More informationBlazars as the Astrophysical Counterparts of the IceCube Neutrinos
Blazars as the Astrophysical Counterparts of the IceCube Neutrinos Maria Petropoulou Department of Physics & Astronomy, Purdue University, West Lafayette, USA Einstein Fellows Symposium Harvard-Smithsonian
More informationA New Look at the Galactic Diffuse GeV Excess
A New Look at the Galactic Diffuse GeV Excess Brian Baughman Santa Cruz Institute for Particle Physics 1 Overview Diffuse gamma-ray emission The Galactic diffuse gamma-ray GeV excess Discussion of the
More informationDark Matter in the Universe
Dark Matter in the Universe NTNU Trondheim [] Experimental anomalies: WMAP haze: synchrotron radiation from the GC Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron
More informationCOMPTON OBSERVATORY OBSERVATIONS OF AGN
COMPTON OBSERVATORY OBSERVATIONS OF AGN J. D. Kurfess Naval Research Laboratory Washington, DC 20375 ABSTRACT. The principal results on active galactic nuclei from the Phase 1 observations by the COMPTON
More informationEGRET Excess of diffuse Galactic Gamma Rays as a Trace of the Dark Matter Halo
EGRET Excess of diffuse Galactic Gamma Rays as a Trace of the Dark Matter Halo Indirect Search for Dark Matter W. de Boer 1, I. Gebauer 1, A.V. Gladyshev 2, D. Kazakov 2, C. Sander 1, V. Zhukov 1 1 Institut
More informationStructure of Dark Matter Halos
Structure of Dark Matter Halos Dark matter halos profiles: DM only: NFW vs. Einasto Halo concentration: evolution with time Dark matter halos profiles: Effects of baryons Adiabatic contraction Cusps and
More informationPERSPECTIVES 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 informationConstraining Galactic dark matter in the Fermi-LAT sky with photon counts statistics
Constraining Galactic dark matter in the Fermi-LAT sky with photon counts statistics Moriond Cosmology 2018 Silvia Manconi (University of Turin & INFN) March 20, 2018 In collaboration with: Hannes Zechlin,
More informationSPATIAL UNIFORMITY OF THE GALACTIC GAMMA-RAY EXCESS. Manoj Kaplinghat, UC Irvine
SPATIAL UNIFORMITY OF THE GALACTIC GAMMA-RAY EXCESS Manoj Kaplinghat, UC Irvine Bas Observed Extended Counts Source Model THE GALACTIC CENTER EXCESS 0.69 0.95 GeV 0.95 1.29 GeV 1.29 1.76 GeV 1.76 2.40
More informationImpact of substructures on predictions of dark matter annihilation signals
Impact of substructures on predictions of dark matter annihilation signals Julien Lavalle Institute & Dept. of Theoretical Physics, Madrid Aut. Univ. & CSIC DESY Theory Astroparticle, Hamburg 16 V 2011
More informationProperties of Elementary Particle Fluxes in Cosmic Rays. TeVPA Aug. 7, Yuan-Hann Chang National Central University, Taiwan
Properties of Elementary Particle Fluxes in Cosmic Rays TeVPA Aug. 7, 2017 Yuan-Hann Chang National Central University, Taiwan Elementary Particles in Space There are hundreds of different kinds of charged
More informationAstrophysics with GLAST: dark matter, black holes and other astronomical exotica
Astrophysics with GLAST: dark matter, black holes and other astronomical exotica Greg Madejski Stanford Linear Accelerator Center and Kavli Institute for Particle Astrophysics and Cosmology (KIPAC) Outline:
More informationThe γ-ray sky after two years of the Fermi satellite Jean Ballet (AIM, CEA/DSM/IRFU/SAp) on behalf of the Fermi LAT Collaboration
The γ-ray sky after two years of the Fermi satellite Jean Ballet (AIM, CEA/DSM/IRFU/SAp) on behalf of the Fermi LAT Collaboration Marseille, April 4, 2011 The Fermi Observatory Large Area Telescope (LAT):
More informationTentative observation of a gamma-ray line at the Fermi Large Area Telescope
Tentative observation of a gamma-ray line at the Fermi Large Area Telescope arxiv:1203.1312 with T. Bringmann, X. Huang, A. Ibarra, S. Vogl (accepted for JCAP), arxiv:1204.2797 (accepted for JCAP) Christoph
More informationPreliminary results from gamma-ray observations with the CALorimeteric Electron Telescope (CALET)
Preliminary results from gamma-ray observations with the CALorimeteric Electron Telescope (CALET) Y.Asaoka for the CALET Collaboration RISE, Waseda University 2016/12/15 CTA-Japan Workshop The extreme
More informationMisaligned AGN with Fermi-Lat:
Misaligned AGN with Fermi-Lat: a different perspective on relativistic jets PAOLA GRANDI INAF/IASF BOLOGNA, ITALY on behalf of the FERMI LAT Collaboration Many thanks to : Torresi E., Migliori G., P. Malaguti,
More informationThe 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 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 informationCTA as a γ-ray probe for dark matter structures: Searching for the smallest clumps & the largest clusters
CTA as a γ-ray probe for dark matter structures: Searching for the smallest clumps & the largest clusters Moritz Hütten (MPP Munich) for the CTA consortium "The extreme Universe viewed in very-highenergy
More informationDark Matter searches with radio observations
Marco Taoso Dpt. of Physics and Astronomy UBC Vancouver Dark Matter searches with radio observations IDM 2012 Chicago, 23-27 July Search for DM with astrophysical observations Gamma- rays Microwave Radio
More informationThe Galactic diffuse gamma ray emission in the energy range 30 TeV 3 PeV
The Galactic diffuse gamma ray emission in the energy range 30 TeV 3 PeV Mount Rainier by Will Christiansen Silvia Vernetto & Paolo Lipari 35th ICRC 12-20 July 2017 - Busan - South Korea Gamma ray astronomy
More informationarxiv:astro-ph/ v1 3 Jun 2002
Gamma-Ray Constraints on Neutralino Dark Matter Clumps in the Galactic Halo Roberto Aloisio a,b,1 Pasquale Blasi c,b,2 Angela V. Olinto d,b,3 arxiv:astro-ph/0206036v1 3 Jun 2002 Abstract a INFN, Laboratori
More informationIndirect signatures of. Gravitino Dark Matter p.1/33
Indirect signatures of Gravitino Dark Matter Alejandro Ibarra DESY In collaboration with W. Buchmüller, L. Covi, K. Hamaguchi and T. Yanagida (JHEP 0703:037, 2007) G. Bertone, W. Buchmüller, L. Covi (JCAP11(2007)003)
More informationConstruction and Preliminary Application of the Variability Luminosity Estimator
Construction and Preliminary Application of the Variability Luminosity Estimator arxiv:astro-ph/0103255v2 19 Mar 2001 Daniel E. Reichart 1,2 and Donald Q. Lamb 3 1 Department of Astronomy, California Institute
More informationMeasuring Dark Matter Properties with High-Energy Colliders
Measuring Dark Matter Properties with High-Energy Colliders The Dark Matter Problem The energy density of the universe is mostly unidentified Baryons: 5% Dark Matter: 20% Dark Energy: 75% The dark matter
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 informationUri Keshet / CfA Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 2008
Uri Keshet / CfA Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 008 Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 008 Relaxed, cool
More informationCosmological Evolution of Blazars
Cosmological Evolution of Blazars Chuck Dermer Naval Research Laboratory The impact of high energy astrophysics experiments on cosmological physics Kavli Institute for Cosmological Physics University of
More informationUsing the Fermi-LAT to Search for Indirect Signals from Dark Matter Annihilation
Using the Fermi-LAT to Search for Indirect Signals from Dark Matter Annihilation Tim Linden UC - Santa Cruz Representing the Fermi-LAT Collaboration with acknowledgements to: Brandon Anderson, Elliott
More informationHigh-Energy Neutrinos from Gamma-Ray Burst Fireballs
High-Energy Neutrinos from Gamma-Ray Burst Fireballs Irene Tamborra GRAPPA Center of Excellence, University of Amsterdam TAUP 2015 Turin, September 9, 2015 Outline IceCube detection of high-energy neutrinos
More informationFundamental Physics with GeV Gamma Rays
Stefano Profumo UC Santa Cruz Santa Cruz Institute for Particle Physics T.A.S.C. [Theoretical Astrophysics, Santa Cruz] Fundamental Physics with GeV Gamma Rays Based on: Kamionkowski & SP, 0810.3233 (subm.
More informationFermi Source Analyses and Identifying VERITAS Candidates
Fermi Source Analyses and Identifying VERITAS Candidates 1 1 1. University of California, Berkeley 2 Overview Introduction VERITAS Fermi Analysis Likelihood Doppler Factor Estimation Motivations Blazars
More information10 Years. of TeV Extragalactic Science. with VERITAS. Amy Furniss California State University East Bay
55 555 56 565 57 55 555 56 565 57 55 555 56 565 57 572 574 576 578 57 5712 5714 5716 572 574 576 578 57 5712 5714 5716 5712 5713 5714 5715 5716 5712 5713 5714 5715 5716 5712 5713 5714 5715 5716 5712 5713
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 informationMattia Di Mauro Eric Charles, Matthew Wood
Characterizing the population of pulsars in the Galactic bulge with the Fermi Large Area Telescope ArXiv:1705.00009 Submitted to ApJ Mattia Di Mauro Eric Charles, Matthew Wood On behalf of the Fermi-LAT
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 informationBalloon-borne experiment for observation of sub-mev/mev gamma-rays from Crab Nebula using an Electron Tracking Compton Camera
Balloon-borne experiment for observation of sub-mev/mev gamma-rays from Crab Nebula using an Electron Tracking Compton Camera S. Komura, T. Tanimori, H. Kubo, A.Takada, S. Iwaki, S. Kurosawa, Y. Matsuoka,
More informationConstraints on Light WIMPs from Isotropic Diffuse γ-ray Emission
Constraints on Light WIMPs from Isotropic Diffuse γ-ray Emission Michel H.G. Tytgat Université Libre de Bruxelles Belgium Rencontres de Moriond: EW Interactions and Unified Theories March 2011 There are
More informationDark Matter. Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET)
Dark Matter Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET) 1 Dark Matter 1933 r. - Fritz Zwicky, COMA cluster. Rotation
More informationThe Plasma Physics and Cosmological Impact of TeV Blazars
The Plasma Physics and Cosmological Impact of TeV Blazars Philip Chang (UW-Milwaukee) Avery Broderick (Waterloo/Perimeter) Astrid Lamberts (UW-Milwaukee) Christoph Pfrommer (HITS-Heidelberg) Ewald Puchwein
More informationGamma-ray and neutrino diffuse emissions of the Galaxy above the TeV
Gamma-ray and neutrino diffuse emissions of the Galaxy above the TeV (with spatial dependent CR transport) D. Grasso (INFN, Pisa) with D. Gaggero, A. Marinelli, A. Urbano, M. Valli IceCube recent results
More informationGamma Ray Physics in the Fermi era. F.Longo University of Trieste and INFN
Gamma Ray Physics in the Fermi era F.Longo University of Trieste and INFN Vulcano, May 22, 2018 F.Longo et al. -- 1 Gamma-ray astrophysics above 100 MeV AGILE Fermi 2 Picture of the day, Feb. 28, 2011,
More informationAstroparticle Physics with IceCube
Astroparticle Physics with IceCube Nick van Eijndhoven nickve.nl@gmail.com http://w3.iihe.ac.be f or the IceCube collaboration Vrije Universiteit Brussel - IIHE(ULB-VUB) Pleinlaan 2, B-1050 Brussel, Belgium
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 informationImplications of neutrino flux limits
Implications of neutrino flux limits by the AMANDA experiment Julia Becker for the IceCube collaboration August 2006 Contents I. Detection principle and detector II. Analysis methods and results I. point
More informationLatest Results on Dark Matter and New Physics Searches with Fermi. Simona Murgia, SLAC-KIPAC on behalf of the Fermi-LAT Collaboration
Latest Results on Dark Matter and New Physics Searches with Fermi Simona Murgia, SLAC-KIPAC on behalf of the Fermi-LAT Collaboration TeV Particle Astrophysics 2009 SLAC, July 13-16 2009 DM and New Physics
More informationInstituto de Fisica Teórica, IFT-CSIC Madrid. Marco Taoso. DM and the Galactic Center GeV excess
Instituto de Fisica Teórica, IFT-CSIC Madrid Marco Taoso DM and the Galactic Center GeV excess Frontier Objects in Astrophysics and Particle Physics Vulcano Workshop 26-05- 2016 How and where to look for
More informationDARK MATTER INTERACTIONS
DARK MATTER INTERACTIONS Jonathan H. Davis Institut d Astrophysique de Paris jonathan.h.m.davis@gmail.com LDMA 2015 Based on J.H.Davis & J.Silk, Phys. Rev. Lett. 114, 051303 and J.H.Davis, JCAP 03(2015)012
More informationAre TeV blazars heating the IGM?
Are TeV blazars heating the IGM? Ewald Puchwein! collaborators: Christoph Pfrommer, Avery Broderick, Phil Chang, Volker Springel TeV blazars unified AGN model: Photon-photon pair production e + e TeV blazar
More informationThe Gamma Large Area Space Telescope: GLAST
Chin. J. Astron. Astrophys. Vol.3 (2003), Suppl., 523 530 (http:/www.chjaa.org) Chinese Journal of Astronomy and Astrophysics The Gamma Large Area Space Telescope: GLAST Aldo Morselli 1 INFN Roma2 and
More informationPHY326/426 Dark Matter and the Universe. Dr. Vitaly Kudryavtsev F9b, Tel.:
PHY326/426 Dark Matter and the Universe Dr. Vitaly Kudryavtsev F9b, Tel.: 0114 2224531 v.kudryavtsev@sheffield.ac.uk Indirect searches for dark matter WIMPs Dr. Vitaly Kudryavtsev Dark Matter and the Universe
More informationSpectra of Cosmic Rays
Spectra of Cosmic Rays Flux of relativistic charged particles [nearly exactly isotropic] Particle density Power-Law Energy spectra Exponent (p, Nuclei) : Why power laws? (constraint on the dynamics of
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 informationSignatures of clumpy dark matter in the global 21 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:
Signatures of clumpy dark matter in the global 2 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:0808.088 Daniel Grin Ay. Journal Club /23/2009 /8 Signatures of clumpy dark matter in
More informationTHE MAGIC TELESCOPES. Major Atmospheric Gamma Imaging Cherenkov Telescopes
THE MAGIC TELESCOPES Observatorio del Roque de los Muchachos, La Palma (2200 m a.s.l.) System of two 17 m Cherenkov Telescopes for VHE γ-ray astronomy MAGIC-I operational since 2004, Stereo system since
More informationRecent results in very high energy gamma ray astronomy
Recent results in very high energy gamma ray astronomy J-F. GLICENSTEIN DSM/IRFU/SPP CEA-Saclay, F-91191 Gif-sur-Yvette, France The very high energy (E 5 GeV) gamma ray astronomy is an emerging field.
More informationWMAP Excess Interpreted as WIMP Annihilation
WMAP Excess Interpreted as WIMP Annihilation idm2004, Edinburgh September 9, 2004 Douglas Finkbeiner Princeton University Outline " " " WMAP ISM emission (expected) The Galactic synchrotron Haze (unexpected)
More information