Search for supersymmetric Dark Matter with GLAST!!

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1 Search for supersymmetric Dark Matter with GLAST!! Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata ICCRC2003 The 28th International Cosmic Ray Conference Tsukuba, Japan, July 31- August 7, 2003 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 1

2 What is the Universe made of? Bright stars: 0.5% Baryons (total): 4.4% ± 0.4% Matter: 27% ± 4% Cold Dark Matter: 22.6% ± 4% Neutrinos: < 0.15% Dark Energy: 73% ± 6% h= Cold Dark Matter CDM Baryons astro-ph WMAP+SN+HST astro-ph/ Dark Energy Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 2

3 Neutralino WIMPs Assume c present in the galactic halo c 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 (c c annihilation) is an interesting signature ie: c c --> p + X Produced from (e. g.) c c --> q / g / gauge boson / Higgs boson and subsequent decay and/ or hadronisation. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 3

4 PAMELA POSITRONS expectation for 3 years of operation Secondary production Secondary production Moskalenko & Strong model without reacceleration Total Primary production from c c annihilation (m(c) = 336 GeV) Primary production P. Picozza and A. Morselli, astro-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 4

5 PAMELA ANTIPROTONS expectation Secondary production (upper and lower limits) Simon et al. Primary production from c c annihilation (m(c) = 964 GeV) Secondary production Primary production AMS98 P. Picozza and A. Morselli, astro-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 5

6 PAMELA status: OG 1.5 Status of the PAMELA Experiment On-Board of the Resurs DK-1 Spacecraft OG 1.5 The Time-of-Flight System of the PAMELA Experiment OG 1.5 A Second Level Trigger for PAMELA OG 1.5 The Time-of-Flight System of the PAMELA Experiment OG 1.5 PAMELA Space Mission: The Transition Radiation Detector OG 1.5 The Anticounter System of the PAMELA Space Experiment OG 1.5 Performance Studies of the Anticounter System of the PAMELA Space Experiment SH 1.5 Solar Particle Events Observation Capabilities of PAMELA Experiment PAMELA Launch : Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 6

7 Indirect Detection through Cosmic Rays We compute (using Darksusy) the expected continuum gamma ray flux from a small region around the galactic centre (~ 2 degrees) due to neutralinoneutralino annihilations. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 7

8 Differential yield for each annihilation channel total yields yields not due to p 0 decay WIMP mass=200gev Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 8

9 Differential yield for b bar neutralino mass Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 9

10 EGRET data & Susy models A.Morselli, A.Lionetto, A.Cesarini, F.Fucito, P.Ullio, 2003 EGRET data Annihilation channel b-bbar Mc =50 GeV background model(galprop) WIMP annihilation (DarkSusy) Total Contribution ~2 degrees around the galactic center Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 10

11 GLAST Performance Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 11

12 effective area distribution of observing time with inclination angle for the declination of the Galactic center. This is for a sky survey with +/-35 deg rocking and with the inclusion of the loss of exposure due to SAA (South Atlantic Anomaly) passages. The target direction was considered to be viewable if its zenith angle was no more than 105 deg. The fractions are for one precession period of the orbit (54.9 days). The main numbers are : Fraction of time in SAA: Fraction of non-saa time that source is not occulted: Net fraction of time that source can be observed: The figure divides this fraction into inclination angle ranges, the sum of all values is 1 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 12

13 GLAST Expectation & Susy models ~2 degrees around the galactic center, 2 years data (Galprop) (one example from DarkSusy) astro-ph/ A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, astro-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 13

14 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 five parameters are fixed: M 1/2 the mass parameter of supersymmetric partners of gauge fields (gauginos) the higgs mixing parameters m that appears in the neutralino and chargino mass matrices m 0, the common mass for scalar fermions at the GUT scale A, the trilinear coupling in the Higgs sector the ratio between the two vacuum expectation values of the Higgs fields defined as: tang b = v 2 / v 1 = <H 2 > / <H 1 > (3 S ) Experimental lower limit on the mass of the lightest neutralino assuming MSSM (Minimal Standard Supersymmetric Model) M c > 50 GeV ( Lep, s = 189 GeV ) hep-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 14

15 Signal rate from Supersymmetry gamma-ray flux from neutralino annihilation governed by supersymmetric parameters governed by halo distribution Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 15

16 Estimated reaches with GLAST Minimal Supersymmetric Standard Model with: A 0 = 0 m > 0 m t =174 GeV region where 0.1 < W CDM. h 2 < 1 region where 0.1 < W CDM. h 2 < 0.12 if GLAST do not see Supersymmetry this region is excluded for a NFW halo tan b = 50 GLAST sensitivity (5 s) for a neutralino density Nc of 10 4 in a DW=10-5 sr region around the galactic center Typical Nc values: NFW: Nc = 10 4 Moore: Nc = Isotermal: Nc = Excluded by LEP A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, astro-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 16

17 Estimated reaches with GLAST Minimal Supersymmetric Standard Model with: A 0 = 0 m > 0 m t =174 GeV tan b = 10 region where 0.1 < W CDM. h 2 < 1 GLAST sensitivity for a neutralino density Nc of 10 6 in a DW=10-5 sr region around the galactic center Typical Nc values: NFW: Nc = 10 4 Moore: Nc = Isotermal: Nc = Excluded by LEP A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, astro-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 17

18 Mixed Anomaly mediated -gauge mediated model: Test with GLAST AMSB-GMSB model six free parameters region where 0.1 < W CDM. h 2 < 0.3 GLAST sensitivity for a neutralino density Nc of 10 4 in a DW=10-5 sr region around the galactic center Typical Nc values: NFW: Nc = 10 4 Moore: Nc = Isotermal: Nc = Excluded by LEP Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 18

19 Gamma-Ray GLAST Large Area Space Telescope GLAST Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 19

20 Transition from design to flight hardware fabrication Engineering Models constructed for each hardware subsystem under test and evaluation have carried out subsystem Peer Design Reviews of each subsystem; Jan - March 2003 Production readiness reviews long-lead parts ordered and long-lead fabrication initiated finalizing flight instrument design details: comprehensive review at LAT Critical Design Review (CDR) CD-3; May 12-16, 2003 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 20

21 LAT Schedule highlights Calendar Years Balloon Flight PDR Critical Design Review TKR & CAL FM A/B Begin LAT I&T Scheduled Completion Schedule Float Scheduled LAT Delivery Launch Ops. Prelim. & Sys. Design Final Design Engr g Models Build & Test Flight Units LAT I&T Observatory I&T FABRICATION PHASE COMMISSIONING PHASE GLAST scheduled for launch in September 2006 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 21

22 Sensitivity of g-ray detectors All sensitivities are at 5s. 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, AMS) are for 1 year of observation. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 22

23 Energy versus time for X and Gamma ray detectors AMS GLAST AGILE MEGA SuperAGILE Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 23

24 Conclusions Neutralinos are a promising candidate for WIMP dark matter Neutralinos can annihilate in the galactic halo... this could give rise to high energy (> 10GeV) antiproton signature and/or gamma-ray signature. Pamela experiment is designed to measure antiproton spectrum from 80MeV to 190GeV. >3 year mission large event samples Combination of TRD + Si tracker + imaging Si- W calo + TOF (trigger) and anticoincidence can isolate a pure sample of antiprotons. Engineering model currently under construction. Flight model due ~ Dec Launch: From March 2006 GLAST will search for gamma-ray signature Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 24

25 2 nd Conclusions GLAST will explore a good portion of the supersymmetric parameter space and this is only additional an item for GLAST! Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 25

26 3 rd Conclusions Í GLAST will be an important step in gamma ray astronomy ( ~ sources compared to ~ 200 of EGRET) Í A partnership between High Energy Physics and g Astrophysics Í Beam test and software development well on the way Í Wide range of possible answers/discoveries Í Gold era for multiwavelenght studies Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 26

27 Gamma-Ray Astronomy Long Term Plan Ultimate Objective: To image the particle accelerator near the event cm -2 s -1 Sensitivity cm -2 s arc sec Angular resolution cm -2 s -1 GLAST 10 arc sec 1%? Energy resolution 5 arc min 5 % Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 27

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