Indirect Dark Matter searches in the PAMELA and Fermi era

Transcription

1 Indirect Dark Matter searches in the PAMELA and Fermi era Aldo Morselli INFN, Sezione di Roma Tor Vergata ILIAS 6th Annual Meeting February 16th - 19st, 2009 Dresden, Germany ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 1

2 Dark Matter in the era of precision cosmology Cold Dark Matter 20% CDM Baryons 4% Dark Energy 76% Ω CDM ~ 5 Ω b ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 2

3 An Inventory of Matter in the Universe 1% Stars 7% Gas in vir. structures 7% WH Gas in IGM Baryons 85% DARK MATTER Non-baryonic So, what is Dark Matter? ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 3

4 Dark Matter Candidates Kaluza-Klein DM in UED Kaluza-Klein DM in RS Axion Axino Gravitino Photino SM Neutrino Sterile Neutrino Sneutrino Light DM Little Higgs DM Wimpzillas Q-balls Mirror Matter Champs (charged DM) D-matter Cryptons Self-interacting Superweakly interacting Braneworld DM Heavy neutrino NEUTRALINO L. Roszkowski Messenger States in GMSB Branons Chaplygin Gas Split SUSY ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata Primordial Black Holes 4

5 Dark Matter Candidates Kaluza-Klein DM inued Kaluza-Klein DM in RS Axion Axino Gravitino Photino SM Neutrino Sterile Neutrino Sneutrino Light DM Little Higgs DM Wimpzillas Q-balls Mirror Matter Champs (charged DM) D-matter Cryptons Self-interacting Superweakly interacting Braneworls DM Heavy neutrino NEUTRALINO Messenger States in GMSB Branons Chaplygin Gas Split SUSY ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Primordial Black Holes Aldo Morselli, INFN Roma Tor Vergata 5

6 Neutralino WIMPs Assume χ present in the galactic halo χ is its own antiparticle => can annihilate in galactic halo producing gamma-rays, antiprotons, positrons. Antimatter not produced in large quantities through standard processes (secondary production through p + p --> p + X) So, any extra contribution from exotic sources (χ χ annihilation) is an interesting signature ie: χ χ --> p + X Produced from (e. g.) χ χ --> q / g / gauge boson / Higgs boson and subsequent decay and/ or hadronisation. ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 6

7 Antiproton/proton ratio 1997 Caprice coll. Astrophysics Journal, 487, 415, 1997 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 7

8 MASS Matter Antimatter Space Spectrometer ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 8

9 MASS 89 the calorimeter ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 9

10 MASS 89 flight ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 10

11 MASS 89 flight ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 11

12 MASS 89 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 12

13 PAMELA Payload for Antimatter Matter Exploration and Light Nuclei Astrophysics In orbit on June 15, 2006, on board of the DK1 satellite by a Soyuz rocket from the Bajkonour launch site. First switch-on on June From July 11 Pamela is in continuous data taking mode ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 13

14 Pamela Separating p from e - ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 14

15 PAMELA: Cosmic-Ray Antiparticle Measurements: Antiprotons an example in msugra fd: Clumpiness factors needed to disentangle a neutralino induced component in the antiproton flux f = the dark matter fraction concentrated in clumps d = the overdensity due to a clump with respect to the local halo density A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 ILIAS 6th [astro-ph/ ] Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 15

16 Supersymmetry introduces free parameters: In the MSSM, with Grand Unification assumptions, the masses and couplings of the SUSY particles as well as their production cross sections, are entirely described once 5 parameters are fixed: M 1/2 the mass parameter of supersymmetric partners of gauge fields (gauginos) µ the higgs mixing parameters that appears in the neutralino and chargino mass matrices m 0 A the common mass for scalar fermions at the GUT scale the trilinear coupling in the Higgs sector tang β = v 2 / v 1 = <H 2 > / <H 1 > the ratio between the two vacuum expectation values of the Higgs fields ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 16

17 msugra Signal Signal and Background are separated? YES tg(β)=55, sign(µ)=+1 Background NO Signal Background ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 17

18 msugra Signal and Background are separated? tg(β)=55, sign(µ)=+1 Signal Background Signal YES YES YES YES YES YES NO NO NO NO NO NO NO NO NO NO NO NO NO YES YES YES YES YES NO YES YES YES Background ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 18

19 msugra Signal and Background are separated? tg(β)=55, sign(µ)=+1 Signal Background Signal YES YES YES YES YES YES NO NO NO NO NO NO NO NO NO NO NO NO NO YES YES YES YES YES NO YES YES YES Background ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 19

20 Antiproton-Proton Ratio antiproton / proton PAMELA data arxiv: ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 20

21 Antiproton-Proton Ratio Diffuse and Convention Propagation Model Upper and lower bounds A.Lionetto, A.Morselli, V.Zdravkovic JCAP09 (2005) 010 [astro-ph/ ] PAMELA data arxiv: ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 21

22 PAMELA WIMP Detection Sensitivity ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 22

23 Fermi PAMELA and LHC WIMP Detection Sensitivity arxiv: Fermi Region that Fermi will probe for boost factor 1 Fermi sensitivity in five years for a Navarro Frank and White (NFW) halo profile ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 23

24 Fermi PAMELA and LHC WIMP Detection Sensitivity arxiv: Fermi sensitivity in five years for a Navarro Frank and White (NFW) halo profile ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 24

25 msugra PAMELA WIMP Detection Sensitivity larger values of tg(b) gives larger signals both in antiprotons and gammas ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 25

26 Positron ratio ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 26

27 Positron ratio Solar modulation effects DC model A.Lionetto, A.Morselli, V.Zdravkovic JCAP09 (2005) 010 [astro-ph/ ] ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 27

28 electron + positron flux excess at about GeV by ATIC and PPB-BETS ATIC X PPB-BETS emulsion chambers Nature 456, 362, 2008 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 28

29 electron + positron flux excess at about GeV by ATIC and PPB-BETS and HESS results ATIC X PPB-BETS emulsion chambers Nature 456, 362, 2008 H.E.S.S. Coll. arxiv: ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 29

30 some articles about the positron excess 1. arxiv: Cosmic Ray Positrons from Cosmic Strings Robert Brandenberger, Yi-Fu Cai, Wei Xue, Xinmin Zhang 2. arxiv: Positrons and antiprotons from inert doublet model dark matter Emmanuel Nezri, Michel H.G. Tytgat, Gilles Vertongen 3. arxiv: On the cosmic electron/positron excesses and the knee of the cosmic rays - a key to the 50 years' puzzle? Hong-Bo Hu, Qiang Yuan, Bo Wang, Chao Fan, Jian-Li Zhang, Xiao-Jun Bi 4. arxiv: A Gamma-Ray Burst for Cosmic-Ray Positrons with a Spectral Cutoff and LineKunihito Ioka 5. arxiv: Is the PAMELA Positron Excess Winos? Phill Grajek, Gordon Kane, Dan Phalen, Aaron Pierce, Scott Watson 6. arxiv: Dissecting Pamela (and ATIC) with Occam's Razor: existing, well-known Pulsars naturally account for the "anomalous" Cosmic-Ray Electron and Positron Data Stefano Profumo 7. arxiv: Study of positrons from cosmic rays interactions and cold dark matter annihilations in the galactic environment Roberto A. Lineros thesis 8. arxiv: Gamma-ray and Radio Constraints of High Positron Rate Dark Matter Models Annihilating into New Light Particles Lars Bergstrom, Gianfranco Bertone, Torsten Bringmann, Joakim Edsjo, Marco Taoso 9. arxiv: A Relativistic Electron-Positron Outflow from a Tepid FireballKatsuaki Asano, Fumio Takahara 10. arxiv: Neutrino Signals from Annihilating/Decaying Dark Matter in the Light of Recent Measurements of Cosmic Ray Electron/Positron Fluxes Junji Hisano, Masahiro Kawasaki, Kazunori Kohri, Kazunori Nakayama 11. arxiv: High-energy Cosmic-Ray Positrons from Hidden-Gauge-Boson Dark Matter Chuan-Ren Chen, Fuminobu Takahashi, T. T. Yanagida 11. arxiv: Status of indirect searches in the PAMELA and Fermi era Aldo Morselli, Igor Moskalenko ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 30

31 12. arxiv: Cosmic-Ray Positron from Superparticle Dark Matter and the PAMELA Anomaly Koji Ishiwata, Shigeki Matsumoto, Takeo Moroi 13. arxiv: The PAMELA Positron Excess from Annihilations into a Light Boson Ilias Cholis, Douglas P. Finkbeiner, Lisa Goodenough, Neal Weiner 14. arxiv: Possible causes of a rise with energy of the cosmic ray positron fraction Pasquale Dario Serpico 15. arxiv: TeV Gamma Rays from Geminga and the Origin of the GeV Positron Excess Hasan Yuksel, Matthew D. Kistler Todor Stanev 16. arxiv: Positron/Gamma-Ray Signatures of Dark Matter Annihilation and Big-Bang Nucleosynthesis Junji Hisano, Masahiro Kawasaki, Kazunori Kohri, Kazunori Nakayama 17. arxiv: Pulsars as the Sources of High Energy Cosmic Ray Positrons Dan Hooper, Pasquale Blasi, Pasquale Dario Serpico 18. arxiv: Galactic secondary positron flux at the Earth T. Delahaye, F. Donato, N. Fornengo, J. Lavalle, R. Lineros, P. Salati, R. Taillet, 19. arxiv: Two dark matter components in N_{DM}MSSM and dark matter extension of the minimal supersymmetric standard model and the high energy positron spectrum in PAMELA/HEAT data Ji-Haeng Huh, Jihn E. Kim, Bumseok Kyae 20. arxiv: On the 511 kev emission line of positron annihilation in the Milky Way N. Prantzos 22. arxiv: Gamma rays and positrons from a decaying hidden gauge boson Chuan-Ren Chen, Fuminobu Takahashi, T. T. Yanagida 23. arxiv: Minimal Dark Matter predictions and the PAMELA positron excessmarco Cirelli, Alessandro Strumia 24. arxiv: New Positron Spectral Features from Supersymmetric Dark Matter - a Way to Explain the PAMELA Data?Lars Bergstrom, Torsten Bringmann, Joakim Edsjo ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 31

32 Positron ratio Aharonian et al A&A 294 L Profumo, arxiv: Hooper et al., arxiv: Yuksel, Kistler. Stanev, arxiv: cut off : 2 TeV electrons from 300 pc Pre-Fermi era : Vela 500 pc ( 287 pc now ) t=2 10^4 yr ( now ^4 yr) require a very big diffusion coefficent D_10= 2 10^30 cm^/s and energy W=2 10^50 erg in e+e- (difficult) Geminga 100 pc (160 now ) t=3 10^5 yr D_10= ^26 cm^/s W=2 10^47 erg (may be? ) CTA ILIAS k pc 6th (no) Annual Meeting B , February? 16th st, pc (may Dresden be) Aldo Morselli, INFN Roma Tor Vergata 32

33 Why study γ s? γ rays offer a direct view into Nature s largest accelerators. the Universe is mainly transparent to γ rays with < 20 GeV that can probe cosmological volumes. Any opacity is energydependent for higher energy. Most particle relics of the early universe produce γ rays when they annihilate or decay. ~ 1.8m Large Area Telescope (LAT) Two Fermi instruments: LAT: 20 MeV 300 GeV GBM: 10 kev 30 MeV 5-year mission (10-year goal) 550km, ~25.6 o Fermi Burst Monitor (GBM) ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 33

34 The CAPRICE 94 flight 34 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 34

35 The TS93 and CAPRICE silicon-tungsten imaging calorimeter. 48 cm 48 cm 35 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 35

36 High Energy Gamma Experiments Experiments ~1993 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 36

37 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 37

38 GILDA ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 38

39 Elements of a pair-conversion telescope photons materialize into matter-antimatter pairs: E γ --> m e +c 2 + m e -c 2 electron and positron carry information about the direction, energy and polarization of the γ-ray (energy measurement) 39 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 39

40 Anti-Coincidence Dome SAS-2 11/1972-7/1973 Spark Chamber Trigger Telescope Cerenkov Counter Energy Calorimeter Cos-B 8/1975-4/1982 The gammaray missions EGRET 4/ ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 40

41 New Detector Technology Silicon strip detector Strip-shaped PN diode micron thick micron wide VLSI amplifier Stable particle tracker that allows micron-level tracking of gamma-rays Well known technology in Particle Physics experiments. Used by our collaboration in balloon experiments (MASS, TS93, CAPRICE), on MIR Space Station ( SilEye) and on satellite (NINA) ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 41

42 AGILE: inside the cube HARD X-RAY IMAGER (SUPER- AGILE) GAMMA-RAY IMAGER ANTICOINCIDENCE SILICON TRACKER (MINI) CALORIMETER ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 42

43 Fermi LAT: A Telescope Without Lenses Precision Si-strip Tracker (TKR) 70 m 2 of silicon detectors arranged in 36 planes. 880,000 channels. first 12 x y planes with 0.03 X 0 (thin part ) 4 x y planes with 0.18 X 0 (thick part ) last 2 planes without converter Hodoscopic CsI Calorimeter(CAL) 1536 CsI(Tl) crystals in 8 layers, total mass 1.5 tons. γ Tracker Segmented Anticoincidence Detector (ACD) 89 plastic scintillator tiles. Electronics System Includes flexible hardware trigger and onboard computing. ACD [surrounds 4x4 array of TKR towers] e + e Calorimeter Total power 650 W Total mass 2,789 kg ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 43

44 DoE NASA international partnership GLAST renamed Fermi by NASA on August 26, Enrico Fermi ( ) was an Italian physicist who immigrated to the United States. He was the first to suggest a viable way to produce high-energy particles in cosmic sources. Since gamma-rays are produced by interactions of such energetic particles, his work is the foundation for many of the studies being done with the Fermi Gamma-ray Space Telescope, formerly GLAST. ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 44

45 The Fermi Participating Institutions American Institutions SU-HEPL Stanford University, Hanson Experimental Physics Laboratory,, SU-SLAC Stanford Linear Accelerator Center, Particle Astrophysics group GSFC-NASA-LHEA Goddard Space Flight Center, Laboratory for High Energy Astrophysics NRL - U. S. Naval Research Laboratory, E. O. Hulburt Center for Space Research, X-ray and gamma-ray branches UCSC- SCIPP University of California at Santa Cruz, Santa Cruz Institute of Particle Physics SSU- California State University at Sonoma, Department of Physics & Astronomy, WUStL-Washington University, St. Louis UW- University of Washington, TAMUK- Texas A&M University-Kingsville, Italian Institutions Japanese Institutions French Institutions Swedish Institutions Ohio State University INFN - Istituto Nazionale di Fisica Nucleare and Univ. of Bari, Padova, Perugia, Pisa, Roma Tor Vergata, Trieste, Udine ASI - Italian Space Agency IASF- Milano, Roma University of Tokyo ICRR - Institute for Cosmic-Ray Research ISAS- Institute for Space and Astronautical Science Hiroshima University CEA/DAPNIA Commissariat à l'energie Atomique, Département d'astrophysique, de physique des Particules, de physique Nucliaire et de l'instrumentation Associée, CEA, Saclay IN2P3 Institut National de Physique Nucléaire et de Physique des Particules, IN2P3 IN2P3/LPNHE-X Laboratoire de Physique Nucléaire des Hautes Energies de l'école Polytechnique IN2P3/PCC Laboratoire de Physique Corpusculaire et Cosmologie, Collège de France IN2P3/CENBG Centre d'études nucléaires de Bordeaux Gradignan IN2P3/LPTA Laboratoire de Physique Theorique et Astroparticules, Montpellier KTH Royal Institute of Technology Stockholms Universitet Collaboration members: ~390 Members: 121 Affiliated Scientists ~96 Postdocs: 68 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, Graduate INFN Students Roma Tor Vergata

46 Fermi Prior to Fairing Installation ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 46

47 Fermi paper Model ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 47

48 Fermi inside the Delta 2 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 48

49 11 June 2008 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 49

50 11 June 2008 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 50

51 11 June 2008 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 51

52 11 June ILIAS th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 52

53 11 June ILIAS th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 53

54 11 June ILIAS th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 54

55 Fermi LAT MC Derived Performance thick+thin sections thick section thin section thick section thin section thick+thin sections thick section thin section ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 55

56 Vela Point Spread Function & Off-pulse emission The PSF becomes very sharp at high energy. Vela thick section Excellent agreement with pre-launch expectations. thin section The offpulse phase window shows very little flux. 10 o cut-outs On- and Off-pulse (0.3-3GeV) Good limit on PWN ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 56

57 LAT Working Very Well On Orbit! Total background rates very close to expectation (! non-trivial ) Spectacular chargedparticle hit efficiency: PSF on-orbit as expected (note intrinsic energy dependence => localization ( source-dependent is verify using on-pulse photons from Vela, compare with detailed MC simulation: On-orbit calorimeter calibration stable use cosmic ray heavy ions: Be B C N O Ne Mg Si Fe ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 57

58 Fermi LAT Sensitivity One-year integral sensitivity for the LAT (5σ, E> threshold energy), for a high latitude point source with an E -2 spectrum. ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 58

59 Energy versus time for X and Gamma ray detectors ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 59

60 Sensitivity of γ-ray detectors A.M.1-09 High galactic latitudes (background Φ b = γ cm -2 s -1 sr -1 (100 MeV/E) 1.1 ). Cerenkov telescopes sensitivities (Veritas, MAGIC, Whipple, Hess, Celeste, Stacee, Hegra) are for 50 hours of observations. Large field of view detectors sensitivities (AGILE, GLAST, Milagro, ARGO) are for 1 year of observation. ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 60

61 Sensitivity of γ-ray detectors A.M.1-09 High galactic latitudes (background Φ b = γ cm -2 s -1 sr -1 (100 MeV/E) 1.1 ). Cerenkov telescopes sensitivities (Veritas, MAGIC, Whipple, Hess, Celeste, Stacee, Hegra) are for 50 hours of observations. Large field of view detectors sensitivities (AGILE, GLAST, Milagro, ARGO) are for 1 year of observation. ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 61

62 CTA: sensitivity gain with example configuration Cherenkov Telescope Array small = 14m large = 28m ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 62

63 Simulated Fermi LAT exposure for five years of all-sky scanning at 100 GeV cm 2 s ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 63

64 Energy Resolution normal incidence 60 0 off-axis The LAT sensitivity extends to higher energies (> 300 GeV) than that of any previous spacebased gamma-ray mission, opening the unexplored energy range above 30 GeV. The energy range of the LAT will overlap those of the next generation ground-based TeV gamma-ray instruments, allowing for inter-calibration between the LAT and these instruments. ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 64

65 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 65

66 205 Preliminary Fermi LAT Bright Sources 213th AAS Meeting Long Beach, CA. Crosses mark source locations, in Galactic coordinates. Fermi Coll. Submitted to ApJS, arxiv: ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 66

67 205 Preliminary LAT Bright Sources - Some Information EGRET on the Compton Observatory found fewer than 30 sources above 10 σ in its lifetime. Typical 95% error radius is less than 10 arcmin. For the brightest sources, it is less than 3 arcmin. Improvements are expected. About 1/3 of the sources show definite evidence of variability. More than 30 pulsars are identified by gamma-ray pulsations. Over half the sources are associated positionally with blazars. Some of these are firmly identified as blazars by correlated multiwavelength variability. Over 40 sources have no obvious associations with known gamma-ray emitting types of astrophysical objects. Fermi Coll. Submitted to ApJS, arxiv: ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 67

68 Vela Pulsar Phase-averaged SED N( E) = N 0 E " e!( E / E c ) b Consistent with b=1 (simple exponential) ! = " 1.51 " 0.04 E c = 2.9 ± 0.1 GeV b=2 (super-exponential) rejected at 16.5σ No evidence for magnetic pair attenuation: Near-surface emission ruled out Abdo et al. [Fermi Coll.] 2008 ApJ in press, arxiv: ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 68

69 Diffuse Galactic Gamma-ray Emission ~80% of total Milky Way luminosity at HE!!! Tracer of CR (p, e ) interactions in the ISM (π 0,IC,bremss): o o o o Study of CR species in distant locations (spectra & intensities) CR acceleration (SNRs, pulsars etc.) and propagation Emission from local clouds local CR spectra CR variations, Solar modulation May contain signatures of exotic physics (dark matter etc.) Cosmology, SUSY, hints for accelerator experiments Background for point sources (positions, low latitude sources ) Besides: o o o Diffuse emission from other normal galaxies (M31, LMC, SMC) Cosmic rays in other galaxies! Foreground in studies of the extragalactic diffuse emission Extragalactic diffuse emission (blazars?) may contain signatures of exotic physics (dark matter, BH evaporation etc.) Calculation requires knowledge of CR (p,e) spectra in the entire Galaxy ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 69

70 Gamma-ray background Galprop Conventional model Optimized: a model based on a renormalized CR proton flux (to fit antiprotons) and a CR electron flux ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 70

71 positrons Local Interstellar Spectra Optimized model (more positrons) Conventional model ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 71

72 Optimized model (more antiprotons) Conventional model ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 72

73 The Galactic Diffuse Emission Galprop conventional model Spectra shown for mid-latitude range GeV excess in this region of the sky is not confirmed. Sources are not subtracted but are a minor component. LAT errors are dominated by systematic uncertainties and are currently estimated to be ~10% this is preliminary. EGRET data is prepared as in Strong, et al with a 15% systematic error assumed to dominate (Esposito, et al. 1999). EG + instrumental is assumed to be isotropic and determined from fitting the data at b > 10. In order to use it for constraining DM one needs to understand the background model uncertainties which is a non trivial problem ( we are working on that). Guðlaugur ILIAS Jóhannesson 6th Annual for Meeting the Fermi, February LAT collaboration 16th - 19st, Jan Dresden th AAS Meeting Aldo Morselli, Long INFN Beach, Roma Tor CA. Vergata January

74 electron + positron flux excess at about GeV by ATIC and PPB-BETS ATIC X PPB-BETS emulsion chambers Nature 456, 362, 2008 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 74

75 electron + positron flux excess at about GeV by ATIC and PPB-BETS and HESS results ATIC X PPB-BETS emulsion chambers Nature 456, 362, 2008 H.E.S.S. Coll. arxiv: ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 75

76 Arnon Moriond09 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 76

77 5 years of GLAST LAT observation, clump at 100 pc, D 0 = cm 2 /s E. A. Baltz, et al., JCAP07(2008)013, arxiv: for a NFW DM distribution with boost factor of 5 and ρ local = 0.4 GeV cm 3 Fermi measurements of the total lepton flux with large statistics will be able to distinguish a gradual change in slope with a sharp cutoff with high confidence ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 77

78 Fermi : Not only γ-rays The Fermi LAT can operate as high energy electron telescope Photon reconstruction works perfectly for electrons, All events above ~20 GeV are downlinked, Rejection power greater than 10 3 demonstrated Advantages: Large collecting area, Continuous (high duty cycle) and long observation No atmospheric correction Can not separate electrons from positrons ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 78

79 What we expect to see Simulation of less than 30 days of on orbit operations The solid line is the primary electron model used in the simulation Spectral index -3.3 above the geomagnetic cutoff We expect to collect >200k events above 100 GeV in 6 months >2.5k events above 500 GeV ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 79

80 Positron ratio Aharonian et al A&A 294 L Profumo, arxiv: Hooper et al., arxiv: Yuksel, Kistler. Stanev, arxiv: cut off : 2 TeV electrons from 300 pc Pre-Fermi era : Vela 500 pc ( 287 pc now ) t=2 10^4 yr ( now ^4 yr) require a very big diffusion coefficent D_10= 2 10^30 cm^/s and energy W=2 10^50 erg in e+e- (difficult) Geminga 100 pc (160 now ) t=3 10^5 yr D_10= ^26 cm^/s W=2 10^47 erg (may be? ) CTA ILIAS k pc 6th (no) Annual Meeting B , February? 16th st, pc (may Dresden be) Aldo Morselli, INFN Roma Tor Vergata 80

81 Millisecond pulsars detected by Fermi Search for pulsations at radio period in first 4 months of Fermi LAT data using radio ephemerides Detection of pulsations from 7 millisecond pulsars - 5 with high significance Confirmation of pulsations from PSR J but with lower significance Alice K. Harding for the Fermi LAT collaboration 7 Jan th AAS Meeting Long Beach, CA. January 2009 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 81

82 The Pulsing Sky Pulses at 1/10 th true rate ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 82

83 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 83

84 Millisecond pulsars Which ones is Fermi detecting? Those with high spin-down flux E! sd / d 2 - The nearby population Spin-down flux (erg/s/kpc 2 ) * Period (s) ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 84

85 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 85

86 New Data is Forthcoming Electron Spectrum: PAMELA & FERMI (GLAST) (taking data in space); ATIC-4 (had successful balloon flight,under analysis); CREST (new balloon payload under development); AMS-02 (launch date TBD); CALET (proposed for ISS); ECAL (proposed balloon experiment). Positron / Electron Separation: PAMELA & AMS-02 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 86

87 The key to understanding the origin of the excess in the ratio is the accurate measurement of positron and electron fluxes separately. To confirm the DM signature, we should look into the signal in HE pbars (PAMELA) and gamma-rays (Fermi (GLAST)). If this is an astrophysical source of positrons, it should be quite close and we should probably be able to see it with Fermi. ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 87

88 Where should we look for WIMPs with FERMI? Galactic center Galactic satellites Galactic halo Extra-galactic ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 88

89 How the FERMI telescope could help to disentangle the Dark Matter puzzle? Search Technique advantages challenges Galactic center Good Statistics Source confusion/diffuse background Satellites, Subhalos, Point Sources Milky Way halo Extragalactic Low background, Good source id Large statistics Large Statistics Low statistics Galactic diffuse background Astrophysics, galactic diffuse background Spectral lines No astrophysical uncertainties, good source id Low statistics ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 89

90 Signal rate from Supersymmetry gamma-ray flux from neutralino annihilation governed by supersymmetric parameters J(ϕ): governed by halo distribution ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 90

91 Main Diagrams for Neutralino Annihilation Light fermion pairs suppressed due to Pauli Principle (neutralinos are Majorana particles and fermions fi Pauli Principle at zero momentum fi p wave fi µ fermion mass!) gauge bosons Low values of tan β (<3.8 excluded by electroweak data (g2, LEP Higgs Limit and BR(bôsγ) At larger values of tan β, bbar dominant final state ( orders of magnitudes for tan β >5 ) fermions ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 91

92 EGRET data & Susy models Annihilation channel W + W - Mχ =80.3 GeV EGRET data N b = N χ = Typical Nχ values: NFW: Nχ = 10 4 Moore: Nχ = Isotermal: Nχ = background model(galprop) WIMP annihilation (DarkSusy) Total Contribution ~2 degrees around the galactic center A.Morselli, A. Lionetto, A. Cesarini, F. Fucito, P. Ullio, astro-ph/ ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 92

93 Fermi Expectation & Susy models ~2 degrees around the galactic center, 2 years data Annihilation channel W + W - Mχ =80 GeV N b = N χ = Typical Nχ values: NFW: Nχ = 10 4 Moore: Nχ = Isotermal: Nχ = (Galprop) (one example from DarkSusy) astro-ph/ A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, , June 2004 [astro-ph/ ] ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 93

94 Differential yield for each annihilation channel WIMP mass=200gev A.Cesarini, ILIAS F.Fucito, 6th Annual A.Lionetto, Meeting A.Morselli,, February 16th P.Ullio, - 19st, Astroparticle 2009 Dresden Physics, 21, Aldo 267, Morselli, 2004 [astro-ph/ ] INFN Roma Tor Vergata 94

95 Differential yield for b bar neutralino mass A.Cesarini, ILIAS F.Fucito, 6th Annual A.Lionetto, Meeting A.Morselli,, February 16th P.Ullio, - 19st, Astroparticle 2009 Dresden Physics, 21, Aldo , Morselli, 2004 INFN [astro-ph/ ] Roma Tor Vergata 95

96 Model independent results for the GC 5 years of operations, truncated NFW Baltz et. al, JCAP07(2008)013 arxiv: ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 96

97 Model independent results for the GC after the Fermi Galactic Diffuse Emission data 5 years of operations, truncated NFW ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 97

98 Model independent results for the Sagittarius Baltz et. al, JCAP07(2008)013 ILIAS 6th Annual arxiv: Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 98

99 after the Fermi Galactic Diffuse Emission data < σ v > ( cm 3 s -1 ) Model independent results for the Sagittarius Dwarft above EGRET observation detectable detectable by GLAST by Fermi ( conventional and optimized GALPROP models assumptions) Not detectable by Fermi channel bb at 3 σ, Moore profile m Wimp (GeV/c 2 ) ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 99

100 Fermi and LHC WIMP Detection Sensitivity arxiv: Fermi Fermi sensitivity in five years for a Navarro Frank and White (NFW) halo profile ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 100

101 Fermi PAMELA and LHC WIMP Detection Sensitivity Fermi sensitivity in five years for a Navarro Frank and White (NFW) halo profile arxiv: ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 101

102 Optimized diffuse background and a 5 line signal at 200 GeV 5σ signal at 200 GeV Optimized diffuse background ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 102

103 5 sensitivity contours to line signal (5 years) arxiv: con: conventional Galactic background model opt: Optimized Galactic background model ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 103

104 z = 0.1 A galactic dark matter halo 1.1 billion particles inside r vir run Springel, Wang, Volgensberger, Ludlow, Jenkins, Helmi, Navarro, Frenk & White 08 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 104

105 Substructures within substructures There are substructures embedded within other structures The hierarchy is cleary NOT self-similar and is heavily dependent on the degree of tidal stripping of the subhalo Most of the substructure mass is in the few most massive halos ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 105

106 Milky Way halo seen in DM annihilation radiation Aquarius simulation: N 200 = 1.1 x 10 9 ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 106

107 Mare Nostrum simulation (with baryons) ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 107

108 Gustavo Yepes ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 108

109 Mare Nostrum simulation (without baryons) preliminary ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 109

110 Mare Nostrum simulation (with baryons) preliminary ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 110

111 Conclusion: Astrophysics of cosmic rays and related topics is a very dynamic field: expect many breakthroughs and discoveries soon! Intermediate latitude -ray spectra can be explained by cosmic-ray propagation models based on local cosmic-ray nuclei and electron spectra. The EGRET GeV excess is not seen in this region of the sky with the Fermi LAT. Work to analyse and understand diffuse emission over the entire sky is in progress. Fermi has started to probe interesting regions of the supersymmetric parameter space. More statistics and the high energy all -electron spectra will expand these regions. ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 111

112 to learn more the book of the Course on Astroparticle and gamma-ray physics in Space Pre-launch estimates for GLAST sensitivity to Dark Matter annihilation signals GLAST sensitivity to Point Sources of Dark Matter Annihilation The Galactic Center as a Dark Matter Gamma-Ray Source Tools for analysis in Astroparticle and Particle Physics ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 112

113 Ricap 09 Roma International Conference on Astro-Particle physics at University of Roma Tor Vergata - May 13-15, you are all invited more results from PAMELA and FERMI will be presented thank you! ILIAS 6th Annual Meeting, February 16th - 19st, 2009 Dresden Aldo Morselli, INFN Roma Tor Vergata 113