Dark Matter - II. Workshop Freudenstadt shedding (Cherenkov) light on dark matter. September 30, 2015
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1 Dark Matter - II GRK 1694: Elementarteilchenphysik bei höchster Energie und höchster Präzision Workshop Freudenstadt 2015 September 30, 2015 Guido Guido Drexlin, Drexlin, Institut Institut für für für Experimentelle Kernphysik shedding (Cherenkov) light on dark matter KIT University of the State of Baden-Württemberg and National Research Center of the Helmholtz Association
2 log cross section (s int /1pb) WIMP WIMP candidates weak interaction s EW < 1 pb ( = cm 2 ) energy-dependent neutrino n neutralino c MSSM Standard Model particles: neutrino cross section: s n,ew = cm 2 = pb supersymmetric particles: neutralino cross section: s c = cm 2 = pb ~ 10-2 s n,ew kev GeV M GUT M Pl suppressed relative to s n,ew due to mixing effects log particle mass (M / 1GeV) 2 Sept. 30, 2015 G. Drexlin DM1
3 log cross section (s int /1pb) WIMP WIMP candidates weak interaction s EW < 1 pb ( = cm 2 ) energy-dependent neutrino n MSSM kev GeV M GUT M Pl log particle mass (M / 1GeV) 3 Sept. 30, 2015 G. Drexlin DM1
4 log cross section (s int /1pb) WIMPzilla WIMP WIMP candidates axion light ( ev) WIMP, produced by non-thermal processes, solves the strong CP-problem (Peccei-Quinn) neutrino n Neutralino c MSSM axino -15 SUSY partner of axion, from decays of SUSY particles gravitino SUSY partner of graviton, only gravitational interaction WIMPzilla extremly massive, non-thermal relics (curvature effects) 4 Sept. 30, 2015 G. Drexlin DM axion axino gravitino kev GeV M GUT M Pl log particle mass (M / 1GeV)
5 outline of today s lecture Dark Matter 2: indirect searches for dark matter - modelling of physics (signal) - modelling of astrophysics (halo, background) - messenger particles: gammas, positrons, anti-protons, neutrinos - FERMI gamma-ray observatory - GC: a model case for signal & background - gammas at the TeV-scale: Atmospheric Cherenkov Telescopes - charged messengers & neutrinos 5 Sept. 30, 2015 G. Drexlin DM2
6 LHC experimental WIMP searches annihilation of neutralinos in CDM halos ~ c 0 c 0 generation of neutralinos at LHC indirect f - f scattering of galactic neutralinos in detector direct 6 Sept. 30, 2015 G. Drexlin DM2
7 indirect detection methods Indirect detection of CDM: observation of secondary particles from WIMP annihilation processes in the local group of galaxies _ - gammas (g), neutrinos (n), antiprotons (p) & positrons (e + ) c 0 c 0 supersymmetric neutralinos quarks u,d leptons e,µ,t gauge bosons W,Z 0 low-energy photons gamma rays gamma rays decay positrons electrons neutrinos antiprotons protons electrons/positrons from: - hadronic decays - pair production - direct production neutrinos from: - hadronic/leptonic decays gammas from: - hadronic decays - bremsstrahlung protons/antiprotons from: - hadronisation & jets - decays of gauge boson 7 Sept. 30, 2015 G. Drexlin DM2
8 WIMP annihilation modelling of signal detection of WIMP annihilation requires precise modelling of a) c 0 -signal: particle physics (decay modes) how: WIMP decays into quarks, leptons, bosons WIMP annihilation 8 Sept. 30, 2015 G. Drexlin DM2
9 Neutralino annihilation processes annihilation into fermion pairs (quarks, Leptons) c c _ f f _ f t-channel c c Z 0 f _ f c c s-channel A f _ f s-channel - Z 0 boson - pseudoscalar Higgs A t-channel - sfermions annihilation into gauge boson pairs W ± Z 0 c c W c c + n c c W c Z 0 W W c W h,h W c t-channel: charginos, neutralinos Z 0 c n Z 0 c h,h c Z 0 Z 0 9 Sept. 30, 2015 G. Drexlin DM2
10 Neutralino annihilation processes an extract of further annihilation channels 10 Sept. 30, 2015 G. Drexlin DM2
11 E 2 flux (GeV cm -2 s -1 sr -1 ) Gammas from WIMP annihilations ~ ~ Neutralino annihilation c 0 c 0 qq : fragmentation of quarks leads to ~30-40 gammas (GeV-energies) gamma spectrum depends on annihilation channel ( bb, ZZ) Spektren für _ m(c 0 ) = 100 GeV bb _ M = 100 GeV W + W - t + t - cc _ - decay channels depend on: a) WIMP mass M(c 0 ) b) WIMP flavour composition (bino, wino, higgsino) Z 0 Z g-energy (GeV) - c 0 -decays to light quarks u,d, (and massless g s) are helicity suppressed 11 Sept. 30, 2015 G. Drexlin DM2
12 WIMP annihilation modelling of signal detection of WIMP annihilation requires precise modelling of a) c 0 -signal: particle physics (decay modes) & astrophysics (halo model) where: NFW halo profile (triaxial halo, sub-halos)? 12 Sept. 30, 2015 G. Drexlin DM2
13 DMA-sources & halo profile N Ann ~ ds 2 CDM line of sight number N Ann of WIMP annihilations in DM-halo (per unit time/volume): N Ann ~ ~ s s Ann Ann v v n 2 CDM m 2 CDM 2 CDM CMD v s Ann from NFW profile of the CDM halo WIMP velocity profile in the halo cross section from theoretical calculations WIMP annihilation rate in DM halos: G Ann ~ 2 CDM searching in areas with DM overdensities - galactic centre - sub-halo centres: dwarf galaxies, 13 Sept. 30, 2015 G. Drexlin DM2
14 DM density DM (GeV/cm³) DMA-sources & halo profile WIMP-density profile in inner DM-halo strongly model-dependent! N Ann ~ ds 2 CDM line of sight Moore Einasto NFW isothermal r sun - DMA-signal rates are model-dependent: different parameterisations of the radial WIMP halo profile DM,sun distance r from galactic centre (kpc) 14 Sept. 30, 2015 G. Drexlin DM2
15 WIMP annihilation: line-of-sight energy-dependent flux F AP,i of WIMP annihilation products (g, n) is given by the integration along the line-of-sight: F AP, i 1 dni 2 ( E) ~ s Ann v ds 2 4 m de CDM line of sight dn/de: energy spectrum 1 pb 1 TeV F AP, ( E, ) i 12 cm 2 s 1 : solid angle small flux of particles from DMA 15 Sept. 30, 2015 G. Drexlin DM2
16 integral along line-of-sight WIMP annihilation: line-of-sight energy-dependent flux F AP,i of WIMP annihilation products (g, n) is given by the integration along the line-of-sight: F AP, i 1 dni 2 ( E) ~ s Ann v ds 2 4 m de CDM line of sight dn/de: energy spectrum galactic centre dominant source Andromeda sub-halo dwarf galaxy Virgo galactic centre d = 7.6 kpc angle q Andromeda d = 780 kpc 16 Sept. 30, 2015 G. Drexlin DM2
17 WIMP annihilation modelling of background detection of WIMP annihilation requires precise modelling of b) astrophysical background (sources, background mechanism) how: energy distribution of background, processes? inverse Compton effect low-energy photon gamma high-energy electron e + g where: location of pulsars, SNRs, CR-sources? background: pulsars, SNR 17 Sept. 30, 2015 G. Drexlin DM2
18 WIMP annihilation: gamma background astrophysical background processes for g s - are generated by the production and reactions of the (non-thermal) cosmic radiation - various galactic sources: a) SN-shock waves in SNRs (SuperNova Remnant) b) pulsar winds, ms-pulsars c) processes in the interstellar medium (ISM), - extragalactic a) active galactic nuclei electrons: pulsar wind SN1006 in g-rays (GeV) 18 Sept. 30, 2015 G. Drexlin DM2 protons: SNR
19 WIMP annihilation modelling of transport detection of WIMP annihilation requires precise modelling of c) propagation of (anti-)protons & electron/positrons in galactic B-fields super-bubbles propagation 19 Sept. 30, 2015 G. Drexlin DM2
20 WIMP annihilation modelling of detection detection of WIMP annihilation requires precise modelling of d) efficiency of detectors at GeV-TeV scale super-bubbles propagation Cherenkovshowers TeV-gammas detection telescopes 20 Sept. 30, 2015 G. Drexlin DM2
21 DMA detection: uncertainties systematic effects from astrophysics & particle physics in detecting DMA: ASTRO SUSY DM halo profile (sub-halos?) WIMP-properties: - mass ~ ~ - flavour (B 0, W 0 ) - s Ann v - decay channels - background sources (pulsars, SNR, ) DM propagation (energy losses, B-fields) 21 Sept. 30, 2015 G. Drexlin DM2
22 WIMP annihilation: modelling of signal modelling of different contributions to DMA signal galactic centre WIMP halo sub-halos sum 22 Sept. 30, 2015 G. Drexlin VL11
23 DMA: antiprotons, positrons Satellit: Fermi c c g, p, e n,,... DM annihilation in galactic centre, in CDM sub-halos ISS: AMS-02 e + _ p antiprotons, positrons: - deflection in galactic B-field - energy losses (e + : local origin only) - rather small backgroud (antiprotons) & well-defined (e/m) signal - atmosphere shields p and e + : satellites with strong B-field (GeV) 23 Sept. 30, 2015 G. Drexlin DM2
24 DMA: Gammas g c c g, p, e n,,... DM annihilation in galactic centre, in CDM sub-halos Gamma-rays: - point back to their region of origin (source) - no energy losses (no inelastic scattering) - no deflection in galactic B-fields - gamma energies extend up to m(c) - but: atmosphere shields GeV-TeV g s: satellites (GeV) & Cherenkov-telescopes (TeV) g upper atmosphere 24 Sept. 30, 2015 G. Drexlin DM2
25 DMA: Gammas extra-galactic: good statistics diffuse background galactic centre: very good statistics many bright sources galactic halo: good statistics diffuse background 25 Sept. 30, 2015 G. Drexlin DM2
26 DMA: gammas E > 10 GeV ~500 sources DMA? Geminga Vela Crab galaxis: 38 g/cm 2 atmosphere: 1000 g/cm 2 GeV 3C454 3 TeV 26 Sept. 30, 2015 G. Drexlin DM2
27 Fermi-Gamma-Observatory Fermi-g-Observatory - principle: pair conversion - successor of Compton-GRO with major improvements: - larger effective area - better angular resolution - higher g energies Fermi key parameters data taking since mid-2008 altitude 560 km dimensions 2.8 m(h) 2.5 m(ø) weight 4.3 t g-energy interval 20 MeV 300 GeV effective area 1 m 2 angular resolution ~ 1 LAT 27 Sept. 30, 2015 G. Drexlin DM2
28 Fermi Large Area Telescope LAT LAT: large area covered solid angle d ~ 20% (at any time) - 4 coverage every 3 hours - 16 single towers single tower g g-conversion (16 W-foils) Si-strips (tracker) gamma-direction e - e + calorimeter (8.6 L 0 ) CsJ-crystals Gamma energy anti-coincidence 28 Sept. 30, 2015 G. Drexlin DM2
29 FERMI results after 3 years 3-year data taking with FERMI galactic chart in multi-gev gammas energy spectrum shows no clear hints for DM annihilation PSR J DMA? Geminga Geminga Vela Vela Crab Crab 3C C454 3 E > 10 GeV - ms Pulsare - g-pulsare ~500 sources 29 Sept. 30, 2015 G. Drexlin DM2
30 events / 1 1 Fermi results after 3.7 years Data taking from 8/2008 4/2012: gamma map from GeV - more than 500 point sources eliminated from dat definition of ROIs around galactic centre R3-3 / R16-6 / R Likelihood analyses to search for line sources 30 Sept. 30, 2015 G. Drexlin DM2
31 95%CL limit flux F g (cm -2 s -1 ) Fermi results after 3.7 years Data taking from 8/2008 4/2012: gamma map from GeV - no significant g-line in overall dat-set observed expected limit 68% CL 95% CL 133 GeV? R16-results (3.7 Jahre) E g (GeV) - weak hints for g-line at E g = 133 GeV (most prominent in R3) - signal also observed (but weaker) in direction of earth horizon! - actual significance s (depends on interval & model) 31 Sept. 30, 2015 G. Drexlin DM2
32 Fermi 2014 update on results excess of g-events in energy range 1-3 GeV, extending up to 1.5 kpc from GC - interpreted as decay of WIMP with M = GeV bb quarks (the hooperon : lead author Dan Hooper, Fermilab) 32 Sept. 30, 2015 G. Drexlin DM2
33 E 2 g dn g /de g (GeV) Fermi 2014 update on results _ modelling of gamma spectra from 30 GeV WIMP-decays: bb-channel? M c = 30 GeV E g (GeV) 33 Sept. 30, 2015 G. Drexlin DM2
34 E 2 g dn g /de g (10-6 GeV/cm²/s/sr) Fermi 2014 update on results Fit to FERMI data by Hooper et al. for galactic NFW profile: a hooperon? 3 M c = GeV 2 _ bb 1 s v = cm³/s for local = 0.3 GeV/cm³ E g (GeV) 34 Sept. 30, 2015 G. Drexlin DM2
35 Fermi 2014 update on results Fit to FERMI data by Hooper et al. for galactic NFW profile: centered on GC 35 Sept. 30, 2015 G. Drexlin DM2
36 s v (10-26 cm³/s) Fermi 2014 update on results Fit to FERMI data by Hooper et al. for galactic NFW profile: the parameters m c (GeV) 36 Sept. 30, 2015 G. Drexlin DM2
37 Fermi 2014/15 update on results excess of g-events in energy range 1-3 GeV, extending up to 1.5 kpc from GC - could also stem from much more massive (200 GeV) neutralinos in MSSM - annihilation cross section s v = ( ) cm³ s -1 - conventional scenario based on unresolved population of ms-pulsars (Weniger et al, arxiv: ) ms-pulsars emit g s with E g ~ 2 GeV, distinct sources give a better fit DMA of hooperon ms-pulsars 2 GeV g 37 Sept. 30, 2015 G. Drexlin DM2
38 Fermi 2015 results from KIT excess of g-events in energy range 1-3 GeV disappears by proper modelling - g-excess in galactic plane correlates with regions of Al-26 production (SNR) - scenario: excess due to old CRs in dense environment of GMCs - hard component with E -2.1 slope from fresh CRs shows same morphology - conclusion by de Boer / Gebauer: excess at GC disappears when GMC with high column density are correctly described arxiv: ( ) DMA of hooperon no excess in de Boer et al. 38 Sept. 30, 2015 G. Drexlin DM2 Al-26
39 gamma flux (TeV -1 cm -2 s -1 ) WIMP annihilation: IACTs & satellites IACT sensitivity is ideal for high g-energies in the multi-tev-region MeV/GeV: satellites TeV: IACTs Fermi gamma energy (TeV) 39 Sept. 30, 2015 G. Drexlin DM2
40 atmospheric Cherenkov telescopes ground-based gamma astronomy at TeV-scale with IACTs: Imaging Atmospheric Cherenkov Telescope search for TeV-gammas from DMA at galactic centre (GC) - range of TeV-g s: ~ 100 Mpc - 1Gpc (o.k. for c 0 -annihilation) - telescope operation: only in clear moonless nights (~ 1000 h / year) GC 40 Sept. 30, 2015 G. Drexlin DM2
41 atmospheric Cherenkov telescopes Ground-based gamma astronomy at TeV-scale with IACTs: - TeV gammas initiate airshower cascades & generate charged particles - cascade process: g e + e - (pair production) g (bremsstrahlung) - relativistic e + e - emit Cherenkov-photons into a narrow cone (~1 ) TeV-gamma ray TeV-g air shower air shower ~10 km photons m -2 GeV -1 reflector area ~ 100 m 2 41 Sept. 30, 2015 G. Drexlin DM2
42 TeV Gamma-observatories Veritas MAGIC Milagro H.E.S.S. CANGAROO III 42 Sept. 30, 2015 G. Drexlin DM2
43 H.E.S.S. galactic centre in TeV gammas HESS observes a clear TeV g signal from the galactic centre Sgr A* after subtraction of this source extended regions of TeV-g-emission are visible: interactions of CR protons with giant molecular clouds 43 Sept. 30, 2015 G. Drexlin DM2
44 H.E.S.S. galactic centre in TeV light search for mono-energetic DMA-line from TeV in central 1 around galactic centre (avoiding galactic plane) over t = 112 h in inner increased g-rate due to HE cosmic rays supernova explosions activity of central SMBH phenomenological description G(x), P(x) of g-energy spectrum no signal 44 Sept. 30, 2015 G. Drexlin DM2 total background G(x) MC for 2 TeV g-line DMA P(x) 1 10 gamma energy (TeV)
45 CTA observatory CTA : world-wide flagship project of TeV gamma astronomy Cherenkov Telescope Array CTA: (10 GeV 100 TeV) - new observatory: 1 southern, 1 northern hemisphere - more than 100 Cherenkov telescopes of different size - commissioning and first data-taking ~ 2020, will look for DMA 45 Sept. 30, 2015 G. Drexlin DM2
46 CTA observatory search for DMA in specific target regions: - galactic centre - galactic halo - dwarf spheroidal galaxies - diffuse emission focus on high energies ~ 1-10 TeV 46 Sept. 30, 2015 G. Drexlin DM2
47 CTA observatory search for DMA in specific target regions: - galactic centre - galactic halo - dwarf spheroidal galaxies - diffuse emission 47 Sept. 30, 2015 G. Drexlin DM2
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