Dark Matter - II. Workshop Freudenstadt shedding (Cherenkov) light on dark matter. September 30, 2015

Size: px
Start display at page:

Download "Dark Matter - II. Workshop Freudenstadt shedding (Cherenkov) light on dark matter. September 30, 2015"

Transcription

1 Dark Matter - II GRK 1694: Elementarteilchenphysik bei höchster Energie und höchster Präzision Workshop Freudenstadt 2015 September 30, 2015 Guido Guido Drexlin, Drexlin, Institut Institut für für für Experimentelle Kernphysik shedding (Cherenkov) light on dark matter KIT University of the State of Baden-Württemberg and National Research Center of the Helmholtz Association

2 log cross section (s int /1pb) WIMP WIMP candidates weak interaction s EW < 1 pb ( = cm 2 ) energy-dependent neutrino n neutralino c MSSM Standard Model particles: neutrino cross section: s n,ew = cm 2 = pb supersymmetric particles: neutralino cross section: s c = cm 2 = pb ~ 10-2 s n,ew kev GeV M GUT M Pl suppressed relative to s n,ew due to mixing effects log particle mass (M / 1GeV) 2 Sept. 30, 2015 G. Drexlin DM1

3 log cross section (s int /1pb) WIMP WIMP candidates weak interaction s EW < 1 pb ( = cm 2 ) energy-dependent neutrino n MSSM kev GeV M GUT M Pl log particle mass (M / 1GeV) 3 Sept. 30, 2015 G. Drexlin DM1

4 log cross section (s int /1pb) WIMPzilla WIMP WIMP candidates axion light ( ev) WIMP, produced by non-thermal processes, solves the strong CP-problem (Peccei-Quinn) neutrino n Neutralino c MSSM axino -15 SUSY partner of axion, from decays of SUSY particles gravitino SUSY partner of graviton, only gravitational interaction WIMPzilla extremly massive, non-thermal relics (curvature effects) 4 Sept. 30, 2015 G. Drexlin DM axion axino gravitino kev GeV M GUT M Pl log particle mass (M / 1GeV)

5 outline of today s lecture Dark Matter 2: indirect searches for dark matter - modelling of physics (signal) - modelling of astrophysics (halo, background) - messenger particles: gammas, positrons, anti-protons, neutrinos - FERMI gamma-ray observatory - GC: a model case for signal & background - gammas at the TeV-scale: Atmospheric Cherenkov Telescopes - charged messengers & neutrinos 5 Sept. 30, 2015 G. Drexlin DM2

6 LHC experimental WIMP searches annihilation of neutralinos in CDM halos ~ c 0 c 0 generation of neutralinos at LHC indirect f - f scattering of galactic neutralinos in detector direct 6 Sept. 30, 2015 G. Drexlin DM2

7 indirect detection methods Indirect detection of CDM: observation of secondary particles from WIMP annihilation processes in the local group of galaxies _ - gammas (g), neutrinos (n), antiprotons (p) & positrons (e + ) c 0 c 0 supersymmetric neutralinos quarks u,d leptons e,µ,t gauge bosons W,Z 0 low-energy photons gamma rays gamma rays decay positrons electrons neutrinos antiprotons protons electrons/positrons from: - hadronic decays - pair production - direct production neutrinos from: - hadronic/leptonic decays gammas from: - hadronic decays - bremsstrahlung protons/antiprotons from: - hadronisation & jets - decays of gauge boson 7 Sept. 30, 2015 G. Drexlin DM2

8 WIMP annihilation modelling of signal detection of WIMP annihilation requires precise modelling of a) c 0 -signal: particle physics (decay modes) how: WIMP decays into quarks, leptons, bosons WIMP annihilation 8 Sept. 30, 2015 G. Drexlin DM2

9 Neutralino annihilation processes annihilation into fermion pairs (quarks, Leptons) c c _ f f _ f t-channel c c Z 0 f _ f c c s-channel A f _ f s-channel - Z 0 boson - pseudoscalar Higgs A t-channel - sfermions annihilation into gauge boson pairs W ± Z 0 c c W c c + n c c W c Z 0 W W c W h,h W c t-channel: charginos, neutralinos Z 0 c n Z 0 c h,h c Z 0 Z 0 9 Sept. 30, 2015 G. Drexlin DM2

10 Neutralino annihilation processes an extract of further annihilation channels 10 Sept. 30, 2015 G. Drexlin DM2

11 E 2 flux (GeV cm -2 s -1 sr -1 ) Gammas from WIMP annihilations ~ ~ Neutralino annihilation c 0 c 0 qq : fragmentation of quarks leads to ~30-40 gammas (GeV-energies) gamma spectrum depends on annihilation channel ( bb, ZZ) Spektren für _ m(c 0 ) = 100 GeV bb _ M = 100 GeV W + W - t + t - cc _ - decay channels depend on: a) WIMP mass M(c 0 ) b) WIMP flavour composition (bino, wino, higgsino) Z 0 Z g-energy (GeV) - c 0 -decays to light quarks u,d, (and massless g s) are helicity suppressed 11 Sept. 30, 2015 G. Drexlin DM2

12 WIMP annihilation modelling of signal detection of WIMP annihilation requires precise modelling of a) c 0 -signal: particle physics (decay modes) & astrophysics (halo model) where: NFW halo profile (triaxial halo, sub-halos)? 12 Sept. 30, 2015 G. Drexlin DM2

13 DMA-sources & halo profile N Ann ~ ds 2 CDM line of sight number N Ann of WIMP annihilations in DM-halo (per unit time/volume): N Ann ~ ~ s s Ann Ann v v n 2 CDM m 2 CDM 2 CDM CMD v s Ann from NFW profile of the CDM halo WIMP velocity profile in the halo cross section from theoretical calculations WIMP annihilation rate in DM halos: G Ann ~ 2 CDM searching in areas with DM overdensities - galactic centre - sub-halo centres: dwarf galaxies, 13 Sept. 30, 2015 G. Drexlin DM2

14 DM density DM (GeV/cm³) DMA-sources & halo profile WIMP-density profile in inner DM-halo strongly model-dependent! N Ann ~ ds 2 CDM line of sight Moore Einasto NFW isothermal r sun - DMA-signal rates are model-dependent: different parameterisations of the radial WIMP halo profile DM,sun distance r from galactic centre (kpc) 14 Sept. 30, 2015 G. Drexlin DM2

15 WIMP annihilation: line-of-sight energy-dependent flux F AP,i of WIMP annihilation products (g, n) is given by the integration along the line-of-sight: F AP, i 1 dni 2 ( E) ~ s Ann v ds 2 4 m de CDM line of sight dn/de: energy spectrum 1 pb 1 TeV F AP, ( E, ) i 12 cm 2 s 1 : solid angle small flux of particles from DMA 15 Sept. 30, 2015 G. Drexlin DM2

16 integral along line-of-sight WIMP annihilation: line-of-sight energy-dependent flux F AP,i of WIMP annihilation products (g, n) is given by the integration along the line-of-sight: F AP, i 1 dni 2 ( E) ~ s Ann v ds 2 4 m de CDM line of sight dn/de: energy spectrum galactic centre dominant source Andromeda sub-halo dwarf galaxy Virgo galactic centre d = 7.6 kpc angle q Andromeda d = 780 kpc 16 Sept. 30, 2015 G. Drexlin DM2

17 WIMP annihilation modelling of background detection of WIMP annihilation requires precise modelling of b) astrophysical background (sources, background mechanism) how: energy distribution of background, processes? inverse Compton effect low-energy photon gamma high-energy electron e + g where: location of pulsars, SNRs, CR-sources? background: pulsars, SNR 17 Sept. 30, 2015 G. Drexlin DM2

18 WIMP annihilation: gamma background astrophysical background processes for g s - are generated by the production and reactions of the (non-thermal) cosmic radiation - various galactic sources: a) SN-shock waves in SNRs (SuperNova Remnant) b) pulsar winds, ms-pulsars c) processes in the interstellar medium (ISM), - extragalactic a) active galactic nuclei electrons: pulsar wind SN1006 in g-rays (GeV) 18 Sept. 30, 2015 G. Drexlin DM2 protons: SNR

19 WIMP annihilation modelling of transport detection of WIMP annihilation requires precise modelling of c) propagation of (anti-)protons & electron/positrons in galactic B-fields super-bubbles propagation 19 Sept. 30, 2015 G. Drexlin DM2

20 WIMP annihilation modelling of detection detection of WIMP annihilation requires precise modelling of d) efficiency of detectors at GeV-TeV scale super-bubbles propagation Cherenkovshowers TeV-gammas detection telescopes 20 Sept. 30, 2015 G. Drexlin DM2

21 DMA detection: uncertainties systematic effects from astrophysics & particle physics in detecting DMA: ASTRO SUSY DM halo profile (sub-halos?) WIMP-properties: - mass ~ ~ - flavour (B 0, W 0 ) - s Ann v - decay channels - background sources (pulsars, SNR, ) DM propagation (energy losses, B-fields) 21 Sept. 30, 2015 G. Drexlin DM2

22 WIMP annihilation: modelling of signal modelling of different contributions to DMA signal galactic centre WIMP halo sub-halos sum 22 Sept. 30, 2015 G. Drexlin VL11

23 DMA: antiprotons, positrons Satellit: Fermi c c g, p, e n,,... DM annihilation in galactic centre, in CDM sub-halos ISS: AMS-02 e + _ p antiprotons, positrons: - deflection in galactic B-field - energy losses (e + : local origin only) - rather small backgroud (antiprotons) & well-defined (e/m) signal - atmosphere shields p and e + : satellites with strong B-field (GeV) 23 Sept. 30, 2015 G. Drexlin DM2

24 DMA: Gammas g c c g, p, e n,,... DM annihilation in galactic centre, in CDM sub-halos Gamma-rays: - point back to their region of origin (source) - no energy losses (no inelastic scattering) - no deflection in galactic B-fields - gamma energies extend up to m(c) - but: atmosphere shields GeV-TeV g s: satellites (GeV) & Cherenkov-telescopes (TeV) g upper atmosphere 24 Sept. 30, 2015 G. Drexlin DM2

25 DMA: Gammas extra-galactic: good statistics diffuse background galactic centre: very good statistics many bright sources galactic halo: good statistics diffuse background 25 Sept. 30, 2015 G. Drexlin DM2

26 DMA: gammas E > 10 GeV ~500 sources DMA? Geminga Vela Crab galaxis: 38 g/cm 2 atmosphere: 1000 g/cm 2 GeV 3C454 3 TeV 26 Sept. 30, 2015 G. Drexlin DM2

27 Fermi-Gamma-Observatory Fermi-g-Observatory - principle: pair conversion - successor of Compton-GRO with major improvements: - larger effective area - better angular resolution - higher g energies Fermi key parameters data taking since mid-2008 altitude 560 km dimensions 2.8 m(h) 2.5 m(ø) weight 4.3 t g-energy interval 20 MeV 300 GeV effective area 1 m 2 angular resolution ~ 1 LAT 27 Sept. 30, 2015 G. Drexlin DM2

28 Fermi Large Area Telescope LAT LAT: large area covered solid angle d ~ 20% (at any time) - 4 coverage every 3 hours - 16 single towers single tower g g-conversion (16 W-foils) Si-strips (tracker) gamma-direction e - e + calorimeter (8.6 L 0 ) CsJ-crystals Gamma energy anti-coincidence 28 Sept. 30, 2015 G. Drexlin DM2

29 FERMI results after 3 years 3-year data taking with FERMI galactic chart in multi-gev gammas energy spectrum shows no clear hints for DM annihilation PSR J DMA? Geminga Geminga Vela Vela Crab Crab 3C C454 3 E > 10 GeV - ms Pulsare - g-pulsare ~500 sources 29 Sept. 30, 2015 G. Drexlin DM2

30 events / 1 1 Fermi results after 3.7 years Data taking from 8/2008 4/2012: gamma map from GeV - more than 500 point sources eliminated from dat definition of ROIs around galactic centre R3-3 / R16-6 / R Likelihood analyses to search for line sources 30 Sept. 30, 2015 G. Drexlin DM2

31 95%CL limit flux F g (cm -2 s -1 ) Fermi results after 3.7 years Data taking from 8/2008 4/2012: gamma map from GeV - no significant g-line in overall dat-set observed expected limit 68% CL 95% CL 133 GeV? R16-results (3.7 Jahre) E g (GeV) - weak hints for g-line at E g = 133 GeV (most prominent in R3) - signal also observed (but weaker) in direction of earth horizon! - actual significance s (depends on interval & model) 31 Sept. 30, 2015 G. Drexlin DM2

32 Fermi 2014 update on results excess of g-events in energy range 1-3 GeV, extending up to 1.5 kpc from GC - interpreted as decay of WIMP with M = GeV bb quarks (the hooperon : lead author Dan Hooper, Fermilab) 32 Sept. 30, 2015 G. Drexlin DM2

33 E 2 g dn g /de g (GeV) Fermi 2014 update on results _ modelling of gamma spectra from 30 GeV WIMP-decays: bb-channel? M c = 30 GeV E g (GeV) 33 Sept. 30, 2015 G. Drexlin DM2

34 E 2 g dn g /de g (10-6 GeV/cm²/s/sr) Fermi 2014 update on results Fit to FERMI data by Hooper et al. for galactic NFW profile: a hooperon? 3 M c = GeV 2 _ bb 1 s v = cm³/s for local = 0.3 GeV/cm³ E g (GeV) 34 Sept. 30, 2015 G. Drexlin DM2

35 Fermi 2014 update on results Fit to FERMI data by Hooper et al. for galactic NFW profile: centered on GC 35 Sept. 30, 2015 G. Drexlin DM2

36 s v (10-26 cm³/s) Fermi 2014 update on results Fit to FERMI data by Hooper et al. for galactic NFW profile: the parameters m c (GeV) 36 Sept. 30, 2015 G. Drexlin DM2

37 Fermi 2014/15 update on results excess of g-events in energy range 1-3 GeV, extending up to 1.5 kpc from GC - could also stem from much more massive (200 GeV) neutralinos in MSSM - annihilation cross section s v = ( ) cm³ s -1 - conventional scenario based on unresolved population of ms-pulsars (Weniger et al, arxiv: ) ms-pulsars emit g s with E g ~ 2 GeV, distinct sources give a better fit DMA of hooperon ms-pulsars 2 GeV g 37 Sept. 30, 2015 G. Drexlin DM2

38 Fermi 2015 results from KIT excess of g-events in energy range 1-3 GeV disappears by proper modelling - g-excess in galactic plane correlates with regions of Al-26 production (SNR) - scenario: excess due to old CRs in dense environment of GMCs - hard component with E -2.1 slope from fresh CRs shows same morphology - conclusion by de Boer / Gebauer: excess at GC disappears when GMC with high column density are correctly described arxiv: ( ) DMA of hooperon no excess in de Boer et al. 38 Sept. 30, 2015 G. Drexlin DM2 Al-26

39 gamma flux (TeV -1 cm -2 s -1 ) WIMP annihilation: IACTs & satellites IACT sensitivity is ideal for high g-energies in the multi-tev-region MeV/GeV: satellites TeV: IACTs Fermi gamma energy (TeV) 39 Sept. 30, 2015 G. Drexlin DM2

40 atmospheric Cherenkov telescopes ground-based gamma astronomy at TeV-scale with IACTs: Imaging Atmospheric Cherenkov Telescope search for TeV-gammas from DMA at galactic centre (GC) - range of TeV-g s: ~ 100 Mpc - 1Gpc (o.k. for c 0 -annihilation) - telescope operation: only in clear moonless nights (~ 1000 h / year) GC 40 Sept. 30, 2015 G. Drexlin DM2

41 atmospheric Cherenkov telescopes Ground-based gamma astronomy at TeV-scale with IACTs: - TeV gammas initiate airshower cascades & generate charged particles - cascade process: g e + e - (pair production) g (bremsstrahlung) - relativistic e + e - emit Cherenkov-photons into a narrow cone (~1 ) TeV-gamma ray TeV-g air shower air shower ~10 km photons m -2 GeV -1 reflector area ~ 100 m 2 41 Sept. 30, 2015 G. Drexlin DM2

42 TeV Gamma-observatories Veritas MAGIC Milagro H.E.S.S. CANGAROO III 42 Sept. 30, 2015 G. Drexlin DM2

43 H.E.S.S. galactic centre in TeV gammas HESS observes a clear TeV g signal from the galactic centre Sgr A* after subtraction of this source extended regions of TeV-g-emission are visible: interactions of CR protons with giant molecular clouds 43 Sept. 30, 2015 G. Drexlin DM2

44 H.E.S.S. galactic centre in TeV light search for mono-energetic DMA-line from TeV in central 1 around galactic centre (avoiding galactic plane) over t = 112 h in inner increased g-rate due to HE cosmic rays supernova explosions activity of central SMBH phenomenological description G(x), P(x) of g-energy spectrum no signal 44 Sept. 30, 2015 G. Drexlin DM2 total background G(x) MC for 2 TeV g-line DMA P(x) 1 10 gamma energy (TeV)

45 CTA observatory CTA : world-wide flagship project of TeV gamma astronomy Cherenkov Telescope Array CTA: (10 GeV 100 TeV) - new observatory: 1 southern, 1 northern hemisphere - more than 100 Cherenkov telescopes of different size - commissioning and first data-taking ~ 2020, will look for DMA 45 Sept. 30, 2015 G. Drexlin DM2

46 CTA observatory search for DMA in specific target regions: - galactic centre - galactic halo - dwarf spheroidal galaxies - diffuse emission focus on high energies ~ 1-10 TeV 46 Sept. 30, 2015 G. Drexlin DM2

47 CTA observatory search for DMA in specific target regions: - galactic centre - galactic halo - dwarf spheroidal galaxies - diffuse emission 47 Sept. 30, 2015 G. Drexlin DM2

M. Lattanzi. 12 th Marcel Grossmann Meeting Paris, 17 July 2009

M. 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 information

Project Paper May 13, A Selection of Dark Matter Candidates

Project Paper May 13, A Selection of Dark Matter Candidates A688R Holly Sheets Project Paper May 13, 2008 A Selection of Dark Matter Candidates Dark matter was first introduced as a solution to the unexpected shape of our galactic rotation curve; instead of showing

More information

Dark Matter in the Universe

Dark 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 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

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

Neutrino bounds on dark matter. Alejandro Ibarra Technische Universität München

Neutrino bounds on dark matter. Alejandro Ibarra Technische Universität München Neutrino bounds on dark matter Alejandro Ibarra Technische Universität München NOW 2012 10 September 2012 Introduction Many pieces of evidence for particle dark matter. However, very little is known about

More information

Neutrinos and DM (Galactic)

Neutrinos and DM (Galactic) Neutrinos and DM (Galactic) ArXiv:0905.4764 ArXiv:0907.238 ArXiv: 0911.5188 ArXiv:0912.0512 Matt Buckley, Katherine Freese, Dan Hooper, Sourav K. Mandal, Hitoshi Murayama, and Pearl Sandick Basic Result

More information

Indirect dark matter searches with the Cherenkov Telescope Array

Indirect dark matter searches with the Cherenkov Telescope Array Indirect dark matter searches with the Cherenkov Telescope Array Jennifer Gaskins GRAPPA, University of Amsterdam for the CTA Consortium For more details, please see: arxiv:1508.06128 Carr et al. 2015

More information

Indirect Dark Matter Detection

Indirect Dark Matter Detection Indirect Dark Matter Detection Martin Stüer 11.06.2010 Contents 1. Theoretical Considerations 2. PAMELA 3. Fermi Large Area Telescope 4. IceCube 5. Summary Indirect Dark Matter Detection 1 1. Theoretical

More information

Searching for Dark Matter in the Galactic Center with Fermi LAT: Challenges

Searching for Dark Matter in the Galactic Center with Fermi LAT: Challenges Searching for Dark Matter in the Galactic Center with Fermi LAT: Challenges Simona Murgia University of California, Irvine Debates on the Nature of Dark Matter Sackler 2014 19-22 May 2014 arxiv:0908.0195

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

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

Spectra of Cosmic Rays

Spectra 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 information

EGRET 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 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 information

Neutralino Dark Matter as the Source of the WMAP Haze

Neutralino Dark Matter as the Source of the WMAP Haze Neutralino Dark Matter as the Source of the WMAP Haze Gabriel Caceres Penn State University & Fermilab Based on work with Dan Hooper INT Summer School 2009 Dark Matter: The Evidence The Search Direct Detection

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

Dark matter and LHC: complementarities and limitations

Dark matter and LHC: complementarities and limitations Dark matter and LHC: complementarities and limitations,1,2, F. Mahmoudi 1,2,3, A. Arbey 1,2,3, M. Boudaud 4 1 Univ Lyon, Univ Lyon 1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574,

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

The Cherenkov Telescope Array (CTA)

The Cherenkov Telescope Array (CTA) The Cherenkov Telescope Array (CTA) The CTA Consortium1, represented by Andreas Reisenegger2 1 2 see http://www.cta observatory.org/consortium_authors/authors_2018_01.html for full author list Instituto

More information

Dark Matter Decay and Cosmic Rays

Dark Matter Decay and Cosmic Rays Dark Matter Decay and Cosmic Rays Christoph Weniger Deutsches Elektronen Synchrotron DESY in collaboration with A. Ibarra, A. Ringwald and D. Tran see arxiv:0903.3625 (accepted by JCAP) and arxiv:0906.1571

More information

Dark Matter in the Galactic Center

Dark Matter in the Galactic Center Dark Matter in the Galactic Center Tim Linden University of Chicago along with: Eric Carlson, Ilias Cholis, Dan Hooper, Manoj Kaplinghat, Stefano Profumo, Jennifer Siegal-Gaskins, Tracy Slatyer, Hai-Bo

More information

DARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1

DARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1 DARK MATTER Martti Raidal NICPB & University of Helsinki 28.05.2010 Tvärminne summer school 1 Energy budget of the Universe 73,4% - Dark Energy WMAP fits to the ΛCDM model Distant supernova 23% - Dark

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

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

PHY326/426 Dark Matter and the Universe. Dr. Vitaly Kudryavtsev F9b, Tel.:

PHY326/426 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 information

Measuring Dark Matter Properties with High-Energy Colliders

Measuring 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 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

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

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

Using 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 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 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

High-energy neutrino detection with the ANTARES underwater erenkov telescope. Manuela Vecchi Supervisor: Prof. Antonio Capone

High-energy neutrino detection with the ANTARES underwater erenkov telescope. Manuela Vecchi Supervisor: Prof. Antonio Capone High-energy neutrino detection with the ANTARES underwater erenkov telescope Supervisor: Prof. Antonio Capone 1 Outline Neutrinos: a short introduction Multimessenger astronomy: the new frontier Neutrino

More information

Nikolay Topchiev for the GAMMA-400 Collaboration High-energy gamma-ray studying with GAMMA-400

Nikolay Topchiev for the GAMMA-400 Collaboration High-energy gamma-ray studying with GAMMA-400 Nikolay Topchiev for the GAMMA-400 Collaboration High-energy gamma-ray studying with GAMMA-400 July 12-20, 2017, ICRC2017, Busan, Korea High-energy gamma-ray studying Distribution of 3033 discrete sources

More information

Lecture 14. Dark Matter. Part IV Indirect Detection Methods

Lecture 14. Dark Matter. Part IV Indirect Detection Methods Dark Matter Part IV Indirect Detection Methods WIMP Miracle Again Weak scale cross section Produces the correct relic abundance Three interactions possible with DM and normal matter DM Production DM Annihilation

More information

Indirect searches for dark matter with the Fermi LAT instrument

Indirect searches for dark matter with the Fermi LAT instrument Indirect searches for dark matter with the Fermi LAT instrument M. Nicola Mazziotta INFN-Bari mazziotta@ba.infn.it 2nd international workshop on HERD Beijing Dec 2-3, 2013 Indirect Dark Matter Search +

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

Measurement of the CR e+/e- ratio with ground-based instruments

Measurement of the CR e+/e- ratio with ground-based instruments Measurement of the CR e+/e- ratio with ground-based instruments Pierre Colin Max-Planck-Institut für Physik CR Moon shadow MPP retreat - 21 January 2014 Cosmic ray electrons Observation: Above the atmosphere:

More information

Signals from Dark Matter Indirect Detection

Signals from Dark Matter Indirect Detection Signals from Dark Matter Indirect Detection Indirect Search for Dark Matter Christian Sander Institut für Experimentelle Kernphysik, Universität Karlsruhe, Germany 2nd Symposium On Neutrinos and Dark Matter

More information

Searching for dark matter annihilation lines with HESS II. Knut Dundas Morå for the HESS collaboration

Searching for dark matter annihilation lines with HESS II. Knut Dundas Morå for the HESS collaboration Searching for dark matter annihilation lines with HESS II Knut Dundas Morå for the HESS collaboration Outline Indirect Dark Matter detection Dark Matter signatures Dark Matter distributions Fermi Line

More information

Very High-Energy Gamma- Ray Astrophysics

Very High-Energy Gamma- Ray Astrophysics Very High-Energy Gamma- Ray Astrophysics David A. Williams Santa Cruz Institute for Particle Physics UC Santa Cruz Quarknet July 12, 2013 Detecting High Energy Gamma Rays High Sensitivity HESS, MAGIC,

More information

Search for exotic process with space experiments

Search 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 information

The positron and antiproton fluxes in Cosmic Rays

The positron and antiproton fluxes in Cosmic Rays The positron and antiproton fluxes in Cosmic Rays Paolo Lipari INFN Roma Sapienza Seminario Roma 28th february 2017 Preprint: astro-ph/1608.02018 Author: Paolo Lipari Interpretation of the cosmic ray positron

More information

Emmanuel Moulin! on behalf of the CTA Consortium!!! Rencontres de Moriond 2013! Very High Energy Phenomena in the Universe! March 9-16, La Thuile,

Emmanuel Moulin! on behalf of the CTA Consortium!!! Rencontres de Moriond 2013! Very High Energy Phenomena in the Universe! March 9-16, La Thuile, Emmanuel Moulin! on behalf of the CTA Consortium!!! Rencontres de Moriond 2013! Very High Energy Phenomena in the Universe! March 9-16, La Thuile, Italy Emmanuel Moulin CTA meeting, Zürich 2009 1 Core-energy

More information

Dark matter in split extended supersymmetry

Dark matter in split extended supersymmetry Dark matter in split extended supersymmetry Vienna 2 nd December 2006 Alessio Provenza (SISSA/ISAS) based on AP, M. Quiros (IFAE) and P. Ullio (SISSA/ISAS) hep ph/0609059 Dark matter: experimental clues

More information

Searching for Dark Matter Annihilation from Milky Way Dwarf Spheroidal Galaxies. Present status and future prospects

Searching for Dark Matter Annihilation from Milky Way Dwarf Spheroidal Galaxies. Present status and future prospects Searching for Dark Matter Annihilation from Milky Way Dwarf Spheroidal Galaxies. Present status and future prospects Aldo Morselli INFN Roma Tor Vergata CTA in the quest for Dark Matter and exotic phenomena

More information

Astro2020 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 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 information

Dark Matter searches with astrophysics

Dark Matter searches with astrophysics Marco Taoso IPhT CEA-Saclay Dark Matter searches with astrophysics IAP 24 February 2013 The cosmological pie Non baryonic Dark Matter dominates the matter content of the Universe Motivation to search for

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

Searching for spectral features in the g-ray sky. Alejandro Ibarra Technische Universität München

Searching for spectral features in the g-ray sky. Alejandro Ibarra Technische Universität München Searching for spectral features in the g-ray sky Alejandro Ibarra Technische Universität München Oslo 5 November 2014 Outline Motivation Indirect dark matter searches with gamma-rays. Overcoming backgrounds

More information

PoS(ICRC2017)933. Cosmic rays and new fermionic dark matters. Jae-Kwang Hwang 1

PoS(ICRC2017)933. Cosmic rays and new fermionic dark matters. Jae-Kwang Hwang 1 1 JJJ Physics Laboratory, Brentwood, TN 37027 USA E-mail: jkhwang.koh@gmail.com Three generations of leptons and quarks correspond to the lepton charges (LC) in the present work. Then, the leptons have

More information

Andrea Albert (The Ohio State University) on behalf of The Fermi LAT Collaboration. HEP Seminar University of Virginia 12/05/12

Andrea Albert (The Ohio State University) on behalf of The Fermi LAT Collaboration. HEP Seminar University of Virginia 12/05/12 Indirect Searches for Dark Matter with the Fermi Large Area Telescope Andrea Albert (The Ohio State University) on behalf of The Fermi LAT Collaboration HEP Seminar University of Virginia 12/05/12 Outline

More information

Astroparticle Anomalies

Astroparticle 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 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

The Cherenkov Telescope Array

The Cherenkov Telescope Array The Cherenkov Telescope Array Gamma-ray particle astrophysics Dark Matter Space time Cosmic rays...? Gamma-ray particle astrophysics Dark Matter Space time Cosmic rays...? Particle Dark Matter Direct Detection

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

Detecting or Limiting Dark Matter through Gamma-Ray Telescopes

Detecting or Limiting Dark Matter through Gamma-Ray Telescopes Detecting or Limiting Dark Matter through Gamma-Ray Telescopes Lars Bergström The Oskar Klein Centre for Cosmoparticle Physics Dept. of Physics Stockholm University lbe@physto.se Firenze, February 9, 2009

More information

MACRO Atmospheric Neutrinos

MACRO Atmospheric Neutrinos MACRO Atmospheric Neutrinos 1. Neutrino oscillations 2. WIMPs 3. Astrophysical point sources Barry Barish 5 May 00 µ Neutrino induced upward-travelling muons are identified by the time-of-fligth

More information

Justin Vandenbroucke (KIPAC, Stanford / SLAC) for the Fermi LAT collaboration

Justin Vandenbroucke (KIPAC, Stanford / SLAC) for the Fermi LAT collaboration Measurement of the cosmic ray positron spectrum with the Fermi LAT using the Earth s magnetic field Justin Vandenbroucke (KIPAC, Stanford / SLAC) for the Fermi LAT collaboration International Cosmic Ray

More information

Wino dark matter breaks the siege

Wino dark matter breaks the siege Wino dark matter breaks the siege Shigeki Matsumoto (Kavli IPMU) In collaboration with M. Ibe, K. Ichikawa, and T. Morishita 1. Wino dark matter (Motivation & Present limits) 2. Wino dark matter is really

More information

GALACTIC CENTER GEV GAMMA- RAY EXCESS FROM DARK MATTER WITH GAUGED LEPTON NUMBERS. Jongkuk Kim (SKKU) Based on Physics Letters B.

GALACTIC CENTER GEV GAMMA- RAY EXCESS FROM DARK MATTER WITH GAUGED LEPTON NUMBERS. Jongkuk Kim (SKKU) Based on Physics Letters B. GALACTIC CENTER GEV GAMMA- RAY EXCESS FROM DARK MATTER WITH GAUGED LEPTON NUMBERS Jongkuk Kim (SKKU) Based on Physics Letters B. 752 (2016) 59-65 In collaboration with Jong Chul Park, Seong Chan Park The

More information

Dark Matter Annihilation, Cosmic Rays and Big-Bang Nucleosynthesis

Dark Matter Annihilation, Cosmic Rays and Big-Bang Nucleosynthesis Dark Matter Annihilation, Cosmic Rays and Big-Bang Nucleosynthesis Institute for Cosmic Ray Research, University of Tokyo Kazunori Nakayama J.Hisano, M.Kawasaki, K.Kohri and KN, arxiv:0810.1892 J.Hisano,

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

Testing 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 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 information

Indirect 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 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 information

Astrophysics with GLAST: dark matter, black holes and other astronomical exotica

Astrophysics 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 information

The Egret Excess, an Example of Combining Tools

The Egret Excess, an Example of Combining Tools The Egret Excess, an Example of Combining Tools Institut für Experimentelle Kernphysik, Universität Karlsruhe TOOLS 2006-26th - 28th June 2006 - Annecy Outline Spectral Fit to EGRET data Problems: Rotation

More information

Ingredients to this analysis

Ingredients to this analysis The dark connection between Canis Major, Monoceros Stream, gas flaring, the rotation curve and the EGRET excess From EGRET excess of diffuse Galactic gamma rays Determination of WIMP mass Determination

More information

Fundamental Physics with GeV Gamma Rays

Fundamental 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 information

Indirect dark matter detection and the Galactic Center GeV Excess

Indirect 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 information

> News < AMS-02 will be launched onboard the Shuttle Endeavour On May 2nd 2:33 P.M. from NASA Kennedy space center!

> News < AMS-02 will be launched onboard the Shuttle Endeavour On May 2nd 2:33 P.M. from NASA Kennedy space center! > News < Anti-matter, dark matter measurement By measuring the cosmic rays (Mainly electron, positron, proton, anti-proton and light nuclei) AMS-02 will be launched onboard the Shuttle Endeavour On May

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

Indirect detection of decaying dark matter

Indirect detection of decaying dark matter Indirect detection of decaying dark matter Alejandro Ibarra Technical University of Munich Many thanks to Chiara Arina, Wilfried Buchmüller, Gianfranco Bertone, Laura Covi, Mathias Garny, Michael Grefe,

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

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

Search for Dark Matter from the Galactic Halo with the IceCube Neutrino Observatory Paper Review

Search for Dark Matter from the Galactic Halo with the IceCube Neutrino Observatory Paper Review Search for Dark Matter from the Galactic Halo with the IceCube Neutrino Observatory Paper Review Stephen Portillo Review of R. Abbasi et al. (IceCube Collaboration), Phys. Rev. D 84, 022004 (2011). Introduction

More information

Dark Matter and Dark Energy components chapter 7

Dark Matter and Dark Energy components chapter 7 Dark Matter and Dark Energy components chapter 7 Lecture 3 See also Dark Matter awareness week December 2010 http://www.sissa.it/ap/dmg/index.html The early universe chapters 5 to 8 Particle Astrophysics,

More information

Signatures 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 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 information

Cosmic Rays, Photons and Neutrinos

Cosmic 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 information

Sho IWAMOTO. 7 Nov HEP phenomenology joint Cavendish DAMTP U. Cambridge

Sho IWAMOTO. 7 Nov HEP phenomenology joint Cavendish DAMTP U. Cambridge MSSM scenario Sho IWAMOTO 7 Nov. 2016 HEP phenomenology joint Cavendish DAMTP seminar @ U. Cambridge Based on [1608.00283] in collaboration with M. Abdullah, J. L. Feng, and B. Lillard (UC Irvine) The

More information

Special Topics in Nuclear and Particle Physics

Special Topics in Nuclear and Particle Physics Special Topics in Nuclear and Particle Physics Astroparticle Physics Lecture 5 Gamma Rays & x-rays Sept. 22, 2015 Sun Kee Kim Seoul National University Gamma ray astronomy gamma ray synchrotron radition

More information

Dark Matter WIMP and SuperWIMP

Dark Matter WIMP and SuperWIMP Dark Matter WIMP and SuperWIMP Shufang Su U. of Arizona S. Su Dark Matters Outline Dark matter evidence New physics and dark matter WIMP candidates: neutralino LSP in MSSM direct/indirect DM searches,

More information

Topics. 1. Towards a unified picture of CRs production and propagation: 2. AMS-02 good candidates for Dark Matter space search

Topics. 1. Towards a unified picture of CRs production and propagation: 2. AMS-02 good candidates for Dark Matter space search Nicolò Masi Bologna University and INFN - 31 May 2016 Topics 1. Towards a unified picture of CRs production and propagation: Astrophysical uncertainties with GALPROP Local Interstellar Spectra: AMS-02

More information

DARK MATTER SEARCHES WITH AMS-02 EXPERIMENT

DARK MATTER SEARCHES WITH AMS-02 EXPERIMENT DARK MATTER SEARCHES WITH AMS-02 EXPERIMENT A.Malinin a, For AMS Collaboration IPST, University of Maryland, MD-20742, College Park, USA Abstract. The Alpha Magnetic Spectrometer (AMS), to be installed

More information

99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park

99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park 99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park #5 How do Cosmic Rays gain their energy? I. Acceleration mechanism of CR

More information

Recent Searches for Dark Matter with the Fermi-LAT

Recent Searches for Dark Matter with the Fermi-LAT Recent Searches for Dark Matter with the Fermi-LAT on behalf of the Fermi-LAT Collaboration CETUP* DM Workshop Deadwood, SD 7 July 2016 A One-Slide History of Dark Matter Particle Physics Astrophysics

More information

Sho IWAMOTO. 15 Sep Osaka University. Based on [ ] in collaboration with M. Abdullah, J. L. Feng, and B. Lillard (UC Irvine)

Sho IWAMOTO. 15 Sep Osaka University. Based on [ ] in collaboration with M. Abdullah, J. L. Feng, and B. Lillard (UC Irvine) MSSM scenario Sho IWAMOTO 15 Sep. 2016 Seminar @ Osaka University Based on [1608.00283] in collaboration with M. Abdullah, J. L. Feng, and B. Lillard (UC Irvine) The Standard Model of Particle Physics

More information

Neutrino Signals from Dark Matter Decay

Neutrino Signals from Dark Matter Decay Neutrino Signals from Dark Matter Decay Michael Grefe Deutsches Elektronen-Synchrotron DESY, Hamburg, Germany COSMO/CosPA 2010 The University of Tokyo 27 September 2010 Based on work in collaboration with

More information

The Dark Matter Puzzle and a Supersymmetric Solution. Andrew Box UH Physics

The Dark Matter Puzzle and a Supersymmetric Solution. Andrew Box UH Physics The Dark Matter Puzzle and a Supersymmetric Solution Andrew Box UH Physics Outline What is the Dark Matter (DM) problem? How can we solve it? What is Supersymmetry (SUSY)? One possible SUSY solution How

More information

The 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 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 information

An Auger Observatory View of Centaurus A

An Auger Observatory View of Centaurus A An Auger Observatory View of Centaurus A Roger Clay, University of Adelaide based on work particularly done with: Bruce Dawson, Adelaide Jose Bellido, Adelaide Ben Whelan, Adelaide and the Auger Collaboration

More information

Constraining 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 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 information

The Lightest Higgs Boson and Relic Neutralino in the MSSM with CP Violation

The Lightest Higgs Boson and Relic Neutralino in the MSSM with CP Violation The Lightest Higgs Boson and Relic Neutralino in the MSSM with CP Violation Stefano Scopel Korea Institute of Advanced Study (based on: J. S. Lee, S. Scopel, PRD75, 075001 (2007)) PPP7, Taipei, Taiwan,

More information

Dark Matter Annihilations in the Galactic Center

Dark Matter Annihilations in the Galactic Center Dan Hooper (Fermilab/University of Chicago) Debates on the Nature of Dark Matter, Harvard/CfA May 21, 2014 Dark Matter Annihilations in the Galactic Center This talk is based on: T. Daylan, D. Finkbeiner,

More information

Search for Astrophysical Neutrino Point Sources at Super-Kamiokande

Search for Astrophysical Neutrino Point Sources at Super-Kamiokande Search for Astrophysical Neutrino Point Sources at Super-Kamiokande Yusuke Koshio for Super-K collaboration Kamioka, ICRR, Univ. of Tokyo LNGS, INFN Super-Kamiokande detector Recent results of search for

More information

Mass Composition Study at the Pierre Auger Observatory

Mass Composition Study at the Pierre Auger Observatory OBSERVATORY Mass Composition Study at the Pierre Auger Observatory Laura Collica for the Auger Milano Group 4.04.2013, Astrosiesta INAF Milano 1 Outline The physics: The UHECR spectrum Extensive Air Showers

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

Astroparticle Physics with IceCube

Astroparticle 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 information

The 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 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 information

The High-Energy Interstellar Medium

The 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 information

HAWC and the cosmic ray quest

HAWC and the cosmic ray quest HAWC and the cosmic ray quest J.C. Arteaga-Velázquez for the HAWC Collaboration Instituto de Física y Matemáticas, Universidad Michoacana, Mexico Structure of the talk: 1) The HAWC gamma-ray observatory

More information