Cosmic Ray Anomalies from the MSSM?

Size: px
Start display at page:

Download "Cosmic Ray Anomalies from the MSSM?"

Transcription

1 Cosmic Ray Anomalies from the MSSM? Randy Cotta (Stanford/SLAC) In collaboration with: J.A. Conley (Bonn) J.S. Gainer (ANL/NU) J.L. Hewett (SLAC) T.G. Rizzo (SLAC) Based on:

2 Positron Fraction: e + / (e - + e + ) p / p The Astrophysical Theory Curve PAMELA PAMELA Anomalous Cosmic Ray Data? Measurements deviate from expected curves Excess CR antimatter could be a signal of DM annihilation E 3 * (e - + e + ) (GeV 2 m -2 s -1 sr -1 ) FERMI-LAT

3 Are We Seeing MSSM WIMPs? The Lore: No. i) Need: <σv> cm 3 s -1, MSSM: <σv> ~ cm 3 s -1 => Boost: B*<σv> ii) Need: DM DM (lepton) - (lepton) + DM DM quark quark Studied MSSM models not especially leptophilic. But: BUT: MSSM== msugra!! Also: Discovering DM Indirectly is very hard. LOTS of uncertainty unrelated to the particle model: Halo?????? particle????????????? astrophysics msugra: see e.g. Barger etal. ( )

4 # Models MLSP M_χi (GeV) <σv> (10-26 cm3s-1) SUSY Without Prejudice C.F. Berger, J.S. Gainer, J.L. Hewett, T.G. Rizzo (Re. Also: My Phuong Le s Talk) General Models Ωh2 Ωh2 LSP >= 0.1 (Ωh2 LSP ~ Ωh2 WMAP ) Ωh2 LSP <σv>*(ρ2/ρo2) (10-26cm3s-1) # Models LSP > 0.1 Models LSP Mass (GeV) Thermal Rescaling: ρ2=ρo2*(ωh2 LSP /Ωh2WMAP)2 ρo ~ 0.3GeV/cm3 LSP Mass (GeV)

5 Diverse Annihilation Phenomenology ~1.4M Annihilation cross sections from DarkSUSY <σv>*(ρ 2 /ρ o 2 )*BRi (cm 3 s -1 ) General Models Ωh 2 LSP >0.1 Models Annihilation Channel

6 Diverse Annihilation Phenomenology ~1.4M Annihilation cross sections from DarkSUSY <σv>*(ρ 2 /ρ o 2 )*BRi (cm 3 s -1 ) General Models Ωh 2 LSP >0.1 Models pmssm Model #11417 Annihilation Channel

7 Diverse Annihilation Phenomenology Studies often take: Br(χχ --> bb) ~ 80% Br(χχ --> τ + τ - ) ~ 20% Leptophilia? <σv> τ+τ- /<σv> bbbar 80%/20% General Models Ωh 2 LSP >0.1 Models <σv> τ+τ- *(ρ 2 /ρ o2 ) cm 3 s -1

8 Dealing with The Astrophysical Background Astrophysical background models have been VERY uncertain until VERY recently. E 3 * (e - + e + ) (GeV 2 m -2 s -1 sr -1 )!!! Grasso et al. (FERMI) ( ) With anomalies in the data we want to make sure we re not tuning background models to fit BG+Signal!! Positron Fraction: e + / (e - + e + ) Grasso et al. (FERMI) ( )!!!

9 Designing Astro-Models GALPROP/DarkSUSY, Scan+Constraints just like pmssm, but NOT without prejudice, we look for pars. that are better for SUSY. Par. Type Par. Names Constrained By Also Note First Proton Source N n, γ n Proton Abs. Flux (AMS01,ATIC,BESS, CAPRICE) Diffusion z h, D 0xx, δ, V A, V c B/C (HEAO-3, ATIC, CREAM) Electron Source N e, γ e e+/(e + +e - ), (e + +e - ) B-Field N B e+/(e + +e - ), (e + +e - ) Diffuse γ s ISRF (u FIR +u optical ), e+/(e + +e - ), (e + +e - ) u optical /u FIR Diffuse γ s These are fixed at the beginning and never floated thereafter z h and D 0xx are degenerate, we scan z h. Radio clocks: z h >~2Kpc. δ expected in ~ Here δ=0.33 N B ~ few µg (u FIR,u optical ) ~ default, Scan similar to Blandford etal. ( ) e+/(e + +e - ), (e + +e - ), pbar/p, fit above 10GeV Last

10 Our Astro-Background Scan (NO SUSY added) Antiproton/Proton Flux Ratio Boron/Carbon CR Flux Ratio Energy (GeV) ASTRO-ONLY E 3 * (e - + e + ) (GeV 2 m -2 s -1 sr -1 ) E 2 *(Flux) (MeV m -2 sr -1 s -1 ) Our Models (qty. 524) ASTRO-ONLY Energy (GeV) Diffuse Midlat. Gammas (10 o < b <20 o, 0 o <b<360 o ) Benchmark Model 1 Grasso et al. (FERMI, ) ASTRO-ONLY Energy (MeV)

11 Our Astro-Background Scan (NO SUSY added) Antiproton/Proton Flux Ratio Boron/Carbon CR Flux Ratio Positron Fraction: e + / (e - + e + ) Energy (GeV) Energy (GeV) ASTRO-ONLY ASTRO-ONLY E 3 * (e - + e + ) (GeV 2 m -2 s -1 sr -1 ) Our Models (qty. 524) E 2 *(Flux) (MeV m -2 sr -1 s -1 ) Energy (GeV) Our Models (qty. 524) ASTRO-ONLY Energy (GeV) Diffuse Midlat. Gammas (10 o < b <20 o, 0 o <b<360 o ) Benchmark Model 1 Grasso et al. (FERMI, ) Benchmark Model 1 Grasso et al. (FERMI, ) ASTRO-ONLY Energy (MeV)

12 Global Fit (Astro)X(SUSY) The SUSY-Added fits do significantly better than the ASTRO-ONLY fits. Most cases: a significantly better fit to the PAMELA positron fraction data χ 2 (posi. frac.) / χ2 (tot.) ASTRO+SUSY fits All Astro Models and all SUSY Models ASTRO-ONLY fits Global Fit χ 2 /dof (dof=36) Benchmark Model 1 and Our SUSY Model Set BEST FITS: χ 2 /dof = 1.54 With boosts in: B ~ Best Fit Boost Factor B<500, χ 2 /dof <2.0 Global Fit χ 2 /dof (dof=36)

13 TEN Best SUSY Models 1) annihilate dominantly to τ + τ - 2) Most important to have a light stau. <σv> τ+τ- /<σv> bbbar 3) (Ωh 2 LSP ~ Ωh2 WMAP ), some co-annihilation 4) LSP is a (mostly bino) bino-higgsino admixture <σv> τ+τ- *(ρ 2 /ρ o2 )cm 3 s -1 5) Rest of spectrum => Leptophilic.

14 Best-Fit CR Spectra for My Favorite SUSY Model e+/(e + +e - ) (e + +e - ) B=156 B=156 Diffuse Midlat. Gammas (10 o < b <20 o, 0 o <b<360 o ) E 2 *(Flux) (MeV m -2 sr -1 s -1 ) B=156 pbar/p B=156

15 Best-Fit CR Spectra for My Favorite SUSY Model e+/(e + +e - ) B=156 (e + +e - ) B=156 E 2 *(Flux) (MeV m -2 sr -1 s -1 ) For Much More: Diffuse Midlat. Gammas (10 o < b <20 o, 0 o <b<360 o ) pbar/p B=156 B=156

16 Backup Slides

17 So how do we choose δ e +/- are not as simple as stable nuclei but 1D result gives rough idea: diffusion convection reacceleration energy losses decay fragm. Many more e - than e + Background Positron Fraction: e+/(e + +e - ) ~ e+/e - ~ 2 ary /1 ary ~ E γ e γ n - δ Signal Positrons (SUSY): e + SUSY ~ E - γ s - δ Small δ is desirable for SUSY visibility in e+/(e + +e - ) with lower Boosts. We use δ=0.33 δ=0.33 δ=0.40 δ=0.50

18 Is δ=0.33 OK? CR e +/- and CR nuclei probe different regions of the galaxy E>10GeV e +/- are cooled very efficiently by synchrotron, IC and brem. => e +/- come from the local ~ kpc. Nucleonic CRs radiate negligibly => diffuse substantially throughout the galaxy. B/C probes the average condition of a large portion of the galaxy. Very tricky to associate the δ describing B/C with the δ that should be used to propagate local CR e +/- Fraction of Local Signal Dist to Origin (kpc) ~ 0.5Kpc Delahaye etal, Irvine, CA.

19 SUSY ONLY Signals Shown: positron and antiproton fluxes from a single SUSY model for each astro-model used Our Model Propagation E*(Pbar Flux) (m -2 sr -1 s -1 ) Model 1 ( ) Propagation E 2 *(Positron Flux) (GeV m -2 sr -1 s -1 ) Energy (GeV) Energy (GeV) Green s functions appropriate to each custom astro-model are used to compute the SUSY signals (i.e. GALPROP -> DarkSUSY )

20 We Have More Ways to Fit the Data Scanning over loss parameters widens the basin of fit that one would get by tuning γ e alone A wider variety of astrophysical backgrounds to which we ll add our signal A wider variety of green s functions with which we ll propagate our signal. On to the Results

21 Astro AND SUSY, Gammas Diffuse Midlat. Gammas (10 o < b <20 o, 0 o <b<360 o ) Assuming the SAME B applies diffuse mid-latitude γs SUSY Contribution to diffuse mid-lat. γs: Some tension with FERMI preliminary data E 2 *(Flux) (MeV m -2 sr -1 s -1 ) B=156 But Components from IC, π 0 -decay, Brem., point sources uncertainties in the normalization of each component. Did not use this quantity in the global fit b/c Astro-BGs bad fit to all data sets, new GALPROP default model will fit the FERMI data together, but all models built on the assumption of NO SUSY SIGNAL, all ordinary astrophysics.

22 Astro AND SUSY, Gammas OLD Assuming the SAME B applies to dwarf galaxies Dwarfs: boosted signals near LAT detection, pure τ models are hardest to see. NEW Dwarfs may be the fastest way to obtain believable evidence for these scenarios! Essig etal

23 Direct Detection? Ten best pmssm models span a sizeable range of DD cross sections. Cross sections highlighted here DO NOT include Boosts. Appropriate boost factor depends on the considered origin of the boost

24 Awaiting More Data AMS-02 can measure CR antimatter better than any previous experiment. AMS-02: size, duration and combination of sub-detectors => high acceptance with proton e + /p + ~ Expected Performance (Superconducting)

25 Charge-Sign Dependent Solar Modulation Sign-INdependent solar modulation factors out of the positron fraction. Clem etal. ApJ 464 (1996) Our strategy: avoid data below 10 GeV!! G. Tarle, UCLA DM 2010 Conf., paper to appear

26 3BFSs Channels w/ extra W/Z compete with direct channels as the extra vector lifts the helicity suppression Very interesting! Calculated in a toy model that does a pretty good job reflecting the MSSM result But Bell, etal For our models annihilation to taus will always dominate over annihilation to electrons. The numerator is universal: f(m W /M χ ), denominator is not: ~ (M f /M χ ) 2

pmssm Dark Matter Searches On Ice! Randy Cotta (Stanford/SLAC) In collaboration with: K.T.K. Howe (Stanford) J.L. Hewett (SLAC) T.G.

pmssm Dark Matter Searches On Ice! Randy Cotta (Stanford/SLAC) In collaboration with: K.T.K. Howe (Stanford) J.L. Hewett (SLAC) T.G. pmssm Dark Matter Searches On Ice! χ ~ 0 1 Randy Cotta (Stanford/SLAC) In collaboration with: K.T.K. Howe (Stanford) J.L. Hewett (SLAC) T.G. Rizzo (SLAC) Based on: 1104.XXXX (next week or bust.) In case

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

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

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

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

Cosmic Ray Excess From Multi-Component Dark Matter

Cosmic Ray Excess From Multi-Component Dark Matter Cosmic Ray Excess From Multi-Component Dark Matter Da Huang Physics Department, NTHU @ LeCosPA PRD89, 055021(2014) [arxiv: 1312.0366] PRD91, 095006 (2015) [arxiv: 1411.4450] Mod. Phys. Lett. A 30 (2015)

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

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

a cosmic- ray propagation and gamma-ray code

a cosmic- ray propagation and gamma-ray code GALPROP: a cosmic- ray propagation and gamma-ray code A. Strong, MPE Garching Tools for SUSY, Annecy, June 28 2006 The basis: cosmic-ray production & propagation in the Galaxy intergalactic space HALO

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

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

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

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

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

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

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

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

PAMELA from Dark Matter Annihilations to Vector Leptons

PAMELA from Dark Matter Annihilations to Vector Leptons PAMELA from Dark Matter Annihilations to Vector Leptons phalendj@umich.edu With Aaron Pierce and Neal Weiner University of Michigan LHC and Dark Matter Workshop 2009 University of Michigan Outline PAMELA

More information

Interstellar 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 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 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

EGRET excess of diffuse Galactic Gamma Rays interpreted as Dark Matter Annihilation

EGRET excess of diffuse Galactic Gamma Rays interpreted as Dark Matter Annihilation EGRET excess of diffuse Galactic Gamma Rays interpreted as Dark Matter Annihilation Wim de Boer, Christian Sander, Valery Zhukov Univ. Karlsruhe From CMB + SN1a + Dmitri Kazakov, Alex Gladyshev structure

More information

Monthly Proton Flux. Solar modulation with AMS. Veronica Bindi, AMS Collaboration

Monthly Proton Flux. Solar modulation with AMS. Veronica Bindi, AMS Collaboration Solar modulation with AMS Monthly Proton Flux Veronica Bindi, AMS Collaboration Physics and Astronomy Department University of Hawaii at Manoa Honolulu, Hawaii, US 1 AMS on the ISS May 19, 2011 and for

More information

Cosmic ray electrons from here and there (the Galactic scale)

Cosmic 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 information

Astrophysical 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? 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 information

Constraining Dark Matter annihilation with the Fermi-LAT isotropic gamma-ray background

Constraining 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 information

Do Gamma Rays reveal our Galaxy s DM?

Do Gamma Rays reveal our Galaxy s DM? Do Gamma Rays reveal our Galaxy s DM? We don t know it, because we don t see it! WdB, C. Sander, V. Zhukov, A. Gladyshev, D. Kazakov, EGRET excess of diffuse Galactic Gamma Rays as Tracer of DM, astro-ph/0508617,

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

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

arxiv: v1 [astro-ph.he] 29 Jan 2015 arxiv:1501.07485v1 [astro-ph.he] 29 Jan 2015 Fitting the Fermi-LAT GeV excess: on the importance of the propagation of electrons from dark matter UPMC-CNRS, UMR7095, Institut d Astrophysique de Paris,

More information

LATE DECAYING TWO-COMPONENT DARK MATTER (LD2DM) CAN EXPLAIN THE AMS-02 POSITRON EXCESS

LATE DECAYING TWO-COMPONENT DARK MATTER (LD2DM) CAN EXPLAIN THE AMS-02 POSITRON EXCESS LATE DECAYING TWO-COMPONENT DARK MATTER (LD2DM) CAN EXPLAIN THE AMS-02 POSITRON EXCESS (WITH A FEW BONUS FEATURES!) (BASED ON 1609.04821 W/ P. RALEGANKAR AND V. RENTALA) JATAN BUCH (BROWN U.) 1 THE DARK

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

Gamma-ray and neutrino diffuse emissions of the Galaxy above the TeV

Gamma-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 information

Indirect Search for Dark Matter with AMS-02

Indirect Search for Dark Matter with AMS-02 Indirect Search for Dark Matter with AMS-02 A. Malinin, UMD For the AMS Collaboration SUSY06, UC Irvine, June 14, 2006 Alpha Magnetic Spectrometer science The AMS is a particle physics experiment in space.

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

Cosmic Antiproton and Gamma-Ray Constraints on Effective Interaction of the Dark matter

Cosmic Antiproton and Gamma-Ray Constraints on Effective Interaction of the Dark matter Cosmic Antiproton and Gamma-Ray Constraints on Effective Interaction of the Dark matter Authors: Kingman Cheung, Po-Yan Tseng, Tzu-Chiang Yuan Physics Department, NTHU Physics Division, NCTS Institute

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

Dark Matter Searches with AMS-02. AMS: Alpha Magnetic Spectrometer

Dark Matter Searches with AMS-02. AMS: Alpha Magnetic Spectrometer Dark Matter Searches with AMS-02 AMS: Alpha Magnetic Spectrometer 2007/2008 Wim de Boer on behalf of the AMS collaboration University of Karlsruhe July, 20. 2004 COSPAR, Paris, W. de Boer, Univ. Karlsruhe

More information

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

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

More information

Excess of EGRET Galactic Gamma Ray Data interpreted as Dark Matter Annihilation

Excess of EGRET Galactic Gamma Ray Data interpreted as Dark Matter Annihilation Excess of EGRET Galactic Gamma Ray Data interpreted as Dark Matter Annihilation Wim de Boer, Marc Herold, Christian Sander, Valery Zhukov Univ. Karlsruhe Alex Gladyshev, Dmitri Kazakov Dubna Outline (see

More information

Dark Matter and Supersymmetry

Dark Matter and Supersymmetry Dark Matter and Supersymmetry We don t know it, because we don t see it! WdB, C. Sander, V. Zhukov, A. Gladyshev, D. Kazakov, EGRET excess of diffuse Galactic Gamma Rays as Tracer of DM, astro-ph/0508617,

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

What is known about Dark Matter?

What is known about Dark Matter? What is known about Dark Matter? 95% of the energy of the Universe is non-baryonic 23% in the form of Cold Dark Matter From CMB + SN1a + surveys Dark Matter enhanced in Galaxies and Clusters of Galaxies

More information

Antiproton Limits on Decaying Gravitino Dark Matter

Antiproton Limits on Decaying Gravitino Dark Matter Antiproton Limits on Decaying Gravitino Dark Matter Michael Grefe Departamento de Física Teórica Instituto de Física Teórica UAM/CSIC Universidad Autónoma de Madrid Particle Theory Journal Club Rudolf

More information

Anisotropy signatures of dark matter annihilation

Anisotropy signatures of dark matter annihilation Anisotropy signatures of dark matter annihilation Le Zhang (University of Wisconsin-Madison) Based on L. Zhang, G. Sigl; arxiv:0807.3429; JCAP09(2008)027 L. Zhang, F. Miniati, G. Sigl; arxiv:1008.1810

More information

Evidence of Stochastic Acceleration of Secondary. Antiprotons by Supernova Remnants! Ilias Cholis, 08/09/2017

Evidence of Stochastic Acceleration of Secondary. Antiprotons by Supernova Remnants! Ilias Cholis, 08/09/2017 C [ ] -4 Evidence of Stochastic Acceleration of Secondary 2.2 1.0 2.0 1.8 1.6 1.4 1.2 C k p p Φ /Φ ratio fit Antiprotons by Supernova Remnants! 0.8 0.6 0.4 0.2 0.0-6 - 1 k [ GV ] -1 AMS-02 PAMELA Fermi

More information

DIETRICH MÜLLER University of Chicago SLAC SUMMER INSTITUTE 2011

DIETRICH MÜLLER University of Chicago SLAC SUMMER INSTITUTE 2011 SEARCHES FOR ANTIMATTER DIETRICH MÜLLER University of Chicago SLAC SUMMER INSTITUTE 2011 OUTLINE Early History Baryon Asymmetry of the Universe? Current Limits on Antimatter Nuclei from Distant Galaxies

More information

Troy A. Porter Stanford University

Troy A. Porter Stanford University High-Energy Gamma-Rays from the Milky Way: 3D Spatial Models for the CR and Radiation Field Densities Troy A. Porter Stanford University What is GALPROP? Tool for modelling and interpreting cosmic-ray

More information

Indirect Dark Matter Detection with Dwarf Galaxies

Indirect Dark Matter Detection with Dwarf Galaxies Indirect Dark Matter Detection with Dwarf Galaxies Neelima Sehgal KIPAC-SLAC/Stanford SnowPAC, Utah 2010 Rouven Essig, NS, Louis Strigari, arxiv: 0902.4750, PRD 80, 023506 (2009) Rouven Essig, NS, Louis

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

Cosmic Ray panorama. Pamela.roma2.infn.it PAMELA (2012) Experimental challenges : e + /p ~ 10-3 e + /e - ~ 10-1

Cosmic Ray panorama.  Pamela.roma2.infn.it PAMELA (2012) Experimental challenges : e + /p ~ 10-3 e + /e - ~ 10-1 1912 1932 Cosmic Ray panorama http::// Pamela.roma2.infn.it PAMELA (2012) Experimental challenges : e + /p ~ 10-3 e + /e - ~ 10-1 Pamela : < 0.1 evt year/gev Flux E α α 2.7 / 3.3 Statistical precision

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

Dark Matter searches with radio observations

Dark 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 information

Instituto 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 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 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

Ingredients to this analysis

Ingredients to this analysis Dark Matter visible from diffuse Galactic gamma rays From EGRET excess of diffuse Galactic gamma rays Determination of WIMP mass Determination of WIMP halo (= standard halo + DM ring) Confirmation: Rotation

More information

Sep. 13, JPS meeting

Sep. 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 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

Quest for New Physics

Quest for New Physics Stefano Profumo UC Santa Cruz Santa Cruz Institute for Particle Physics T.A.S.C. [Theoretical Astrophysics in Santa Cruz] Cosmic Rays and the Quest for New Physics Scineghe 2010, Trieste, Italy Thursday,

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

Latest 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 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 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

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

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

Implication of AMS-02 positron fraction measurement. Qiang Yuan

Implication of AMS-02 positron fraction measurement. Qiang Yuan Implication of AMS-02 positron fraction measurement Qiang Yuan (yuanq@ihep.ac.cn) Institute of High Energy Physics, Chinese Academy of Sciences Collaborated with Xiaojun Bi, Guo-Ming Chen, Yi-Qing Guo,

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 Models. Stephen West. and. Fellow\Lecturer. RHUL and RAL

Dark Matter Models. Stephen West. and. Fellow\Lecturer. RHUL and RAL Dark Matter Models Stephen West and Fellow\Lecturer RHUL and RAL Introduction Research Interests Important Experiments Dark Matter - explaining PAMELA and ATIC Some models to explain data Freeze out Sommerfeld

More information

Dark matter annihilations and decays after the AMS-02 positron measurements

Dark matter annihilations and decays after the AMS-02 positron measurements Dark matter annihilations and decays after the AMS-02 positron measurements Anna S. Lamperstorfer Technische Universität München SISSA - International School for Advanced Studies of Trieste Workshop The

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

arxiv: v1 [astro-ph] 17 Nov 2008

arxiv: 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 information

Structure of Dark Matter Halos

Structure 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 information

Dynamical Dark Matter and the Positron Excess in Light of AMS

Dynamical Dark Matter and the Positron Excess in Light of AMS Dynamical Dark Matter and the Positron Excess in Light of AMS Brooks Thomas (University of Hawaii) K. R. Dienes, J. Kumar, BT [arxiv:1306.2959] The Positron Puzzle Positron Fraction PAMELA, AMS-02, and

More information

AMS-02 Antiprotons Reloaded

AMS-02 Antiprotons Reloaded AMS-02 Antiprotons Reloaded Martin W. Winkler in collaboration with R. Kappl and A. Reinert based on JCAP 09/2014 and arxiv:1506.04145 TAUP 2015 Torino September 9 2015 Martin W. Winkler (Bonn University)

More information

CMB constraints on dark matter annihilation

CMB constraints on dark matter annihilation CMB constraints on dark matter annihilation Tracy Slatyer, Harvard University NEPPSR 12 August 2009 arxiv:0906.1197 with Nikhil Padmanabhan & Douglas Finkbeiner Dark matter!standard cosmological model:

More information

Indirect Searches for Gravitino Dark Matter

Indirect Searches for Gravitino Dark Matter Indirect Searches for Gravitino Dark Matter Michael Grefe Departamento de Física Teórica Instituto de Física Teórica UAM/CSIC Universidad Autónoma de Madrid PLANCK 202 From the Planck Scale to the Electroweak

More information

Gamma ray and antiparticles (e + and p) as tools to study the propagation of cosmic rays in the Galaxy

Gamma ray and antiparticles (e + and p) as tools to study the propagation of cosmic rays in the Galaxy Gamma ray and antiparticles (e + and p) as tools to study the propagation of cosmic rays in the Galaxy INFN Sez. La Sapienza, Rome, Italy E-mail: paolo.lipari@roma1.infn.it The spectra of cosmic rays observed

More information

arxiv:hep-ph/ v2 9 Sep 2005

arxiv:hep-ph/ v2 9 Sep 2005 Indirect Signals from Dark Matter in Split Supersymmetry Asimina Arvanitaki and Peter W. Graham Institute for Theoretical Physics Department of Physics Stanford University Stanford, CA 94305 USA email:

More information

Supersymmetry Without Prejudice at the LHC

Supersymmetry Without Prejudice at the LHC Supersymmetry Without Prejudice at the LHC Conley, Gainer, JLH, Le, Rizzo arxiv:1005.asap J. Hewett, 10 09 Supersymmetry With or Without Prejudice? The Minimal Supersymmetric Standard Model has ~120 parameters

More information

Properties 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, 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 information

Astrophysical issues in indirect DM detection

Astrophysical issues in indirect DM detection Astrophysical issues in indirect DM detection Julien Lavalle CNRS Lab. Univers & Particules de Montpellier (LUPM), France Université Montpellier II CNRS-IN2P3 (UMR 5299) Service de Physique Théorique Université

More information

AMS-02 Antiprotons Reloaded

AMS-02 Antiprotons Reloaded AMS-02 Antiprotons Reloaded Rolf Kappl Bethe Center for Theoretical Physics & Physikalisches Institut der Universität Bonn based on RK, Annika Reinert, Martin Wolfgang Winkler JCAP 10 (2015) 034, arxiv:1506.04145

More information

Galactic cosmic rays phenomenology: nuclei, antimatter, dark matter

Galactic cosmic rays phenomenology: nuclei, antimatter, dark matter Galactic cosmic rays phenomenology: nuclei, antimatter, dark matter Fiorenza Donato Torino University and INFN NPQCD 1st Workshop Cortona, April 20, 2015 1. What are cosmic rays (CRs) 2. Searches for dark

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

Searches for Physics Beyond the Standard Model. Jay Wacker. APS April Meeting SLAC. A Theoretical Perspective. May 4, 2009

Searches for Physics Beyond the Standard Model. Jay Wacker. APS April Meeting SLAC. A Theoretical Perspective. May 4, 2009 Searches for Physics Beyond the Standard Model A Theoretical Perspective Jay Wacker SLAC APS April Meeting May 4, 2009 1 The Plan Motivations for Physics Beyond the Standard Model New Hints from Dark Matter

More information

Positron Fraction from Dark Matter Annihilation in the CMSSM

Positron Fraction from Dark Matter Annihilation in the CMSSM Positron Fraction from Dark Matter Annihilation in the CMSSM W. de Boer a iekp]institut für Experimentelle Kernphysik, Universität Karlsruhe (TH), P.O. Box 6980, 7628 Karlsruhe, GermanyC. Sander b, M.Horn

More information

Cosmic Antimatter. Stéphane. Coutu The Pennsylvania State University. 3 rd. Astrophysics Arequipa,, Peru August 28-29, 29, 2008

Cosmic Antimatter. Stéphane. Coutu The Pennsylvania State University. 3 rd. Astrophysics Arequipa,, Peru August 28-29, 29, 2008 Cosmic Antimatter Stéphane Coutu The Pennsylvania State University 3 rd rd School on Cosmic Rays and Astrophysics Arequipa,, Peru August 28-29, 29, 2008 Outline Cosmic Rays Antimatter: Positrons, Antiprotons

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

Constraints on dark matter annihilation cross section with the Fornax cluster

Constraints 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 information

Fundamental Physics from the Sky

Fundamental Physics from the Sky Fundamental Physics from the Sky Based on: SP, 0812.4457 (PRD) Kamionkowski & SP, 0810.3233 (PRL) Jeltema & SP, 0808.2641 (JCAP) Jeltema & SP, 0805.1054 (ApJ) SP, 0801.0740 (PRD) Colafrancesco, SP & Ullio,

More information

Remnants and Pulsar Wind

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

More information

THE MAGIC TELESCOPES. Major Atmospheric Gamma Imaging Cherenkov Telescopes

THE 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 information

Global SUSY Fits with IceCube

Global SUSY Fits with IceCube Global SUSY Fits with IceCube Chris Savage * Oskar Klein Centre for Cosmoparticle Physics Stockholm University For the IceCube Collaboration * associate member Overview All processes depend on WIMP mass

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

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 STATUS OF NEUTRALINO DARK MATTER

THE STATUS OF NEUTRALINO DARK MATTER THE STATUS OF NEUTRALINO DARK MATTER BIBHUSHAN SHAKYA CORNELL UNIVERSITY CETUP 2013 Workshop June 25, 2013 Based on hep-ph 1208.0833, 1107.5048 with Maxim Perelstein, hep-ph 1209.2427 The favorite / most

More information

Probing the nature of Dark matter with radio astronomy. Céline Boehm

Probing the nature of Dark matter with radio astronomy. Céline Boehm Probing the nature of Dark matter with radio astronomy Céline Boehm IPPP, Durham LAPTH, Annecy SKA, Flic en Flac, May 2017 The DM Physics scale strong or weak / stable or decaying strong and stable Electromagnetic

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

High and low energy puzzles in the AMS-02 positron fraction results

High and low energy puzzles in the AMS-02 positron fraction results High and low energy puzzles in the AMS-02 positron fraction results Dario Grasso (INFN, Pisa) D. Gaggero (SISSA), L.Maccione (MPI, Munich), C. Evoli(DESY), G. Di Bernardo (Göteborg) AMS-02 positron fraction

More information

Cosmological and astrophysical probes of dark matter annihilation

Cosmological and astrophysical probes of dark matter annihilation Cosmological and astrophysical probes of dark matter annihilation Institute for Cosmic Ray Research, University of Tokyo Kazunori Nakayama J.Hisano, M.Kawasaki, K.Kohri and KN, Phys.Rev.D79,063514(2009)[0810.1892]

More information

Searching for Non-Colored SUSY at CMS. Alfredo Gurrola Vanderbilt University Dark Matter Workshop at Mitchell Institute TAMU, May 25, 2016

Searching for Non-Colored SUSY at CMS. Alfredo Gurrola Vanderbilt University Dark Matter Workshop at Mitchell Institute TAMU, May 25, 2016 Searching for Non-Colored SUSY at CMS Alfredo Gurrola Vanderbilt University Dark Matter Workshop at Mitchell Institute TAMU, May 25, 2016 1 30,000,000,000,000,000,000,000 stars in 350 billion large galaxies

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

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