Dark Matter Searches. Christian Spiering DESY, Zeuthen
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1 Dark Matter Searches Christian Spiering DESY, Zeuthen Bad Honnef,
2 Outline CDM candidates WIMPs: direct and indirect detection Indirect detection with neutrino telescopes Search for Q-balls and other super-heavy exotics with neutrino telescopes
3 Dark Matter Candidates
4 Dark Matter Candidates
5
6 Detection methods DIRECT DETECTION SEARCHES NEUTRINO INDIRECT SEARCHES Observe scattering of χ s off nuclei in low-background environments Search for neutrinos produced in χχ annihilations in the core of gravitational dips, e.g.the center of Sun or Earth, where χ s get trapped μ ANTIMATTER INDIRECT SEARCHES Disentangle antimatter produced in χχ annihilations in the galactic halo from standard antimatter Sources. GAMMA RAY INDIRECT SEARCHES Observe gamma rays produced by χχ annihilations regions of high DM density.
7 Detection methods DIRECT DETECTION SEARCHES NEUTRINO INDIRECT SEARCHES Observe scattering of χ s off nuclei in low-background environments Search for neutrinos produced in χχ annihilations in the core of gravitational dips, e.g.the center of Sun or Earth, where χ s get trapped μ ANTIMATTER INDIRECT SEARCHES Disentangle antimatter produced in χχ annihilations in the galactic halo from standard antimatter Sources. GAMMA RAY INDIRECT SEARCHES Observe gamma rays produced by χχ annihilations regions of high DM density.
8 Direct detection WIMP + nucleus WIMP + nucleus Measure recoil energy Suppress background enough to be sensitive to a signal (if possible zero) Smoking gun signatures due to motion of Earth through halo: Search for annual modulation of rate Search for directional signature
9 Direct detection: experiments Noble liquids TPC Ionization DRIFT MIMA C EDELWEISS, CDMS bolometric Ge, Si Superheated liquids ZEPLIN, XENON, LUX (Xe) WARP, ArDM (Ar) WIMP Heat SIMPLE, PICASSO, COUPP Noble liquids XMASS, DEAP, CLEAN, DAMA/LXe Scintillation DAMA, ANAIS, KIMS crystals NaI, CsI CRESST bolometric CaWO 4
10 Direct detection: experiments Noble liquids TPC Ionization DRIFT MIMA C EDELWEISS, CDMS bolometric Ge, Si Superheated liquids ZEPLIN, XENON, LUX (Xe) WARP, ArDM (Ar) WIMP Heat SIMPLE, PICASSO, COUPP Noble liquids XMASS, DEAP, CLEAN, DAMA/LXe Scintillation DAMA, ANAIS, KIMS crystals NaI, CsI CRESST bolometric CaWO 4
11 Limits vs. MSSM Model 2007 Spin-independent scattering cross section (pb) XENON 2007 Neutralino mass (GeV)
12 Limits vs. constrained MSSM Model 2007 Spin-independent scattering cross section (pb) XENON 2007 Neutralino mass (GeV)
13 From infancy to technological maturity Cross section (pb) Stage 1: Field in Infancy Stage 2: Prepare the instruments Stage 3: Maturity. Rapid progress Stage 4: - Understand remaining background.100 kg scale - Determine best method for ton-scale detectors results of LHC may modify this picture! LHC Stage 5: Build and operate ton-scale detectors
14 From infancy to technological maturity 10-4 Cross section (pb) Background - Funding / Infrastructure
15 WG requests for European Dark Matter projects Investment - Total ASPERA ArDM CYGNUS DAMA1ton ELIXIR EURECA SIMPLE Ulisse ULTIMA ZEPLIN Underground Infrastructure k DAMA-1ton ELIXIR (liquid Xe) EURECA (bolometric)
16 WG recommendations for European Dark Matter projects Underground Infrastructure k ELIXIR (liquid Xe) EURECA (bolometric)
17 Detection methods DIRECT DETECTION SEARCHES NEUTRINO INDIRECT SEARCHES Observe scattering of χ s off nuclei in low-background environments Search for neutrinos produced in χχ annihilations in the core of gravitational dips, e.g.the center of Sun or Earth, where χ s get trapped μ ANTIMATTER INDIRECT SEARCHES Disentangle antimatter produced in χχ annihilations in the galactic halo from standard antimatter Sources. GAMMA RAY INDIRECT SEARCHES Observe gamma rays produced by χχ annihilations regions of high DM density.
18 Annihilation in the halo Charged annihilation products Diffusion of charged particles. Looking for excess of antiparticles. Best current detector is Pamela. Next big step would be AMS.
19 Example: the HEAT Positron Excess Better data mandatory. Wait first PAMELA data. Then AMS!!
20 Detection methods DIRECT DETECTION SEARCHES NEUTRINO INDIRECT SEARCHES Observe scattering of χ s off nuclei in low-background environments Search for neutrinos produced in χχ annihilations in the core of gravitational dips, e.g.the center of Sun or Earth, where χ s get trapped μ ANTIMATTER INDIRECT SEARCHES Disentangle antimatter produced in χχ annihilations in the galactic halo from standard antimatter Sources. GAMMA RAY INDIRECT SEARCHES Observe gamma rays produced by χχ annihilations regions of high DM density.
21 Annihilation in the halo or certain regions Gamma rays can be searched for with Imaging Air Cherenkov Telescopes (IACTs) or GLAST. Signal depends strongly on the halo profile or local cluster factors
22 EGRET data Mannheim & Elsässer Subtract galactic/halo component Extragalactic origin 520 GeV De Boer halo origin 65 GeV Now: Agile Wait for GLAST!
23 Extragalactic gamma background D. Elsässer & K. Mannheim, Phys.Rev.Lett. 94:171302, 2005
24 H.E.S.S. Galactic Center & Dark Matter Annihilation From D.Horns et al. Energy spectrum not well described by neutralino- or KK-annihilation (Mx =14 TeV, MKK=5TeV) Sagittarus Dwarf Galaxy: astrophysical component small set interesting limits on cross section (private comm. G. Heinzelmann)
25 M87 spectrum for WIMP annihilation From D. Elsässer
26 CTA Cherenkov Telescope Array > 1 km Large ~50 dish IACT array of 2-3 different sizes
27 CTA
28 Detection methods DIRECT DETECTION SEARCHES NEUTRINO INDIRECT SEARCHES Observe scattering of χ s off nuclei in low-background environments Search for neutrinos produced in χχ annihilations in the core of gravitational dips, e.g.the center of Sun or Earth, where χ s get trapped μ ANTIMATTER INDIRECT SEARCHES Disentangle antimatter produced in χχ annihilations in the galactic halo from standard antimatter Sources. GAMMA RAY INDIRECT SEARCHES Observe gamma rays produced by χχ annihilations regions of high DM density.
29 standard detection scheme detector muon nuclear reaction neutrino
30 AMANDA 677 optical modules at 19 strings Installation
31 AMANDA Neutrino Skymap 75 o Amanda (green) & Baikal (blue) Galactic coordinates 60 o 45 o o o h 0h AMANDA-II: (1001 live days) 4282 ν from Northern hemisphere No significant excess found
32 A curious coincidence WHIPPLE Arrival time of neutrinos from the direction of the AGN ES Flux of TeV photons (arb. units) 3 2 ν ν 1 0 May June July Year
33 IceCube IceTop Air shower detector 80 pairs of ice Cherenkov tanks Threshold ~ 300 TeV : 13 strings deployed Current configuration - 22 strings - 52 surface tanks : 8 strings InIce Goal of 80 strings of 60 optical modules each 17 m between modules 125 m string separation 1450m 2450m : 1 string AMANDA-II 19 strings 677 modules 2007/08: add 14 to 18 strings and tank stations Completion by 2011.
34 IceCube IceTop IceCube 1450m AMANDA-II 19 strings 677 modules 2450m
35 IceCube IceTop : 13 strings deployed Current configuration - 22 strings - 52 surface tanks : 8 strings IceCube 1450m 2450m AMANDA-II 19 strings 677 modules AMANDA now AMANDA operating now as part operating of IceCube as part of IceCube
36 Advantage for WIMP detection AMANDA as low energy subdetector of IceCube IceCube threshold 100 GeV IceCube with Amanda 30 GeV Amanda without IceCube 50 GeV
37 Effect on 22-string detector 8200 incl. AMANDA 30 GeV! Preliminary Atmos. ν μ per 200 days (trigger level, IC22+AMANDA) 5400 IceCube only Gross, Tluczykont, Ha, Rott, DeYoung, Resconi, & Wikström, ICRC 2007
38 A new low energy subdetector 6 strings each with 40 PM, spaced by 10 m better veto from top located in best ice (below 2100 m exceptionally clear) uses IceCube technology for IceCube? AMANDA new core? considerably better performance at low energy Scatt. Coeff. Physics targets Solar WIMPs Look upward (contained events)
39 now High Energy Neutrino Telescopes operation AMANDA oonstruction + operation operation IceCube operation NT200, NT200+ design study construction + operation? GVD operat construction c + o operation ANTARES R&D KM3 NESTOR, NEMO FP6 Design Study construction + operation KM3NeT operat
40 Neutralino Capture in the Sun Sun Earth Detector
41 Neutralino Capture in the Earth χ ν Look for neutrinos from the center of the Earth. χ + χ b + b C + μ + ν μ
42 Capture by Sun and Earth Capture in Sun Mostly on Hydrogen Both spin-independent and spin- dependent scattering Figure from Jungman, Kamionkowski and Griest Capture in Earth Mostly on Iron Essentially only spinindependent scattering Resonant scattering when mass matches element in Earth
43 Amanda Analysis: Earth WIMPs 1999 as example Background rejection optimization = f (mass, decay mode) Angular distribution 1,1 10 1,1 10 1,1 10 1, Start with 1,1 10 events at trigger level in 99 data 1, ,1 10 1, A eff LIMIT 1,1 10 1,1 10 1,1 2 1
44 Muon flux limits compared to MSSM predictions Situation 2004 but
45 Lundberg & Edsjö, 2004: When the halo WIMPs have reached the Earth, they have gained speed 2005 by the Sun s attraction. Hence, capture is very inefficient. But: Halo WIMPs diffuse in the solar system by action of the other planets.
46 Neutrino-induced muon fluxes from the Earth center Usual Gaussian New estimate including approximation solar capture Maxwell-Boltzmann velocity distribution assumed.
47 Neutrino-induced muon fluxes from the Sun Compared to the Earth, much better complementarity due to spindependent capture in the Sun.
48 Comparing direct vs. indirect searches: a word of caution indirect searches ~ density squared Density integrated over cosmological times Low-velocity region direct searches ~ density actual density High-velocity region Branching ratios!
49 Sun Neutrino-induced fluxes and future direct detection limits Earth Future direct detection sensitivity is assumed to be 10-9 pb.
50
51 Magnetic Monopoles Dirac 1931 Typical signature when crossing a superconducting coil (Cabrera) Strong Ionization: ~ (g/e) 2 with g/e = 137/2 Astrophysical Parker Bound: ~ cm -2 s -1 sr -1 GUT Monopoles may catalyze proton decay MACRO at Gran Sasso: most prominent monopole detector (closed in 2000, ionization &ToF)
52 Flux upper limits for GUT Magnetic Monopoles Direct detection via Ionization: MACRO -4
53 GUT Magnetic Monopoles Mass GeV/c² Velocity β ~ 10-4 M + p M + e + + π 0 May catalyze proton decay with σ σ 0 / β 2 bright track from Cherenkov radiation from proton decay products in water detectors
54 Flux upper limits for GUT Magnetic Monopoles IMB Kamiokande 1985 σ 0 = cm 2 σ 0 = cm 2 Baikal Direct detection via Ionization: MACRO -4 including limits from p-decay catalysis assumption
55 Intermediate mass Magnetic Monopoles Mass GeV Produced in the Early Universe in later phase transitions Can be accelerated in the galactic B field to relativistic. velocities W = g D B L ~ 6 x ev (B/3x10-6 G) (L/300pc) Galaxy W ev Neutron stars W ev AGN W ev Connection to highest energy cosmic ray E > ev?
56 Detection via Cherenkov light Cherenkov Light n 2 (g/e) 2 n = 1.33 (g/e) = 137 /
57 Amanda 2000 blue: background MC dots: exp. data a. u monopole with β = 1.0, 0.9, 0.8, NCH (fiber OMs)
58 upper limit (cm -2 s -1 sr -1 ) Soudan KGF MACRO Orito δ electrons IceCube Amanda 0.75 β = v/c Baikal 1.00 Relativistic Magnetic Monopoles Cherenkov-Light n 2 (g/e) 2 n = 1.33 (g/e) = 137 /
59 Flux upper limits for Magnetic Monopoles IMB Kamiokande 1985 Baikal σ 0 = cm 2 σ0 = cm MACRO AMANDA 1997 Baikal AMANDA 2000
60 Flux upper limits for Magnetic Monopoles IMB Kamiokande 1985 Baikal σ 0 = cm 2 σ0 = cm 2 MACRO, σ 0 = cm MACRO AMANDA 1997 Baikal AMANDA 2000
61 NUCLEARITES (Strange Quark Matter+electrons) Aggregates of u, d, s quarks + electrons Stable for baryon number 300 < A < ρ N g cm -3 (ρ nuclei g cm -3 ) Produced in Early Universe, candidates for sub-dominant dark matter May be produced also in neutron stars Light generation via Planck radiation Virial velocities Supersymmetric Q-balls Coherent states of squarks, sleptons and Higgs fields 10 8 < M Q GeV Produced in Early Universe, candidates for (sub-dominant) dark matter Light generation via ionization (SECS) or catalysis of proton decay (SENS) Virial velocities
62 Slow Particles in AMANDA / IceCube particle with β = 10-2 β (AMANDA) β : 10-4 (IceCube): elongated events 2-muon event IceCube trigger under design.
63 Slow Particles in AMANDA / IceCube β ~ increased counting rates of individual PMs (msec windows, Supernova Trigger ) or several sequential events aligned along a straight path
64 Fluxes above this line excluded by Galactic dark matter limit Nuclearites IceCube after 1 yr ancient mica Macro IceCube after 5 yr Herrin and Teplitz 6-ton event following Buford Price
65 Neutral Q-Balls Q Dark Matter Flux Limit Baikal limit (Girlyanda 86) Macro Q-balls stable 5 yr IceCube sensitivity following Buford Price
66 Conclusions Neutralino is favored DM SUSY candidate. To confirm, one needs: Neutralino is LSP of SUSY. Confirmation from LHC Direct detection Different nuclei Annual modulation (possibly directional signature) Indirect detection Gammas: GLAST, CTA; charged CRs: AMS Neutrinos: Earth disfavoured, Neutrino flux from Sun complementary to direct searches due to spin-dependent capture in Sun Highest discovery potential with direct methods if they reach a sensitivity below pb. Next 5 years: IceCube well competes with direct 10-9 pb searches. Exotic superheavy particles (Q-balls, monopoles,..): sensitivity will improve by 1-2 orders in the next years.
67 End
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