Whither WIMP Dark Matter Search? Pijushpani Bhattacharjee AstroParticle Physics & Cosmology Division Saha Institute of Nuclear Physics Kolkata
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1 Whither WIMP Dark Matter Search? AstroParticle Physics & Cosmology Division Saha Institute of Nuclear Physics Kolkata 1/51
2 2/51
3 Planck 2015 Parameters of the Universe 3/51
4 Discovery of Dark Matter Fritz Zwicky (1933) F. Zwicky, "Die Rotverschiebung von extragalaktischen Nebeln", Helvetica Physica Acta 6: (1933) F. Zwicky, "On the Masses of Nebulae and of Clusters of Nebulae", Astrophysical Fritz Zwicky ( ) Journal 86: 217 (1937) 4/51
5 Also, earlier Oort (1932) Jan Hendrik Oort ( ) To explain kinematics of vertical motion of the disk stars, Oort needed invisible mass of density ~ 2 GeV / cm^3 at the solar neighborhood. Modern value ~ 0.3 Gev / cm^3 5/51
6 6/51
7 7/51
8 Paolo Gondolo, AAPCOS 2015 SINP 8/51
9 Colliding Galaxy Clusters Bullet Cluster 9/51
10 Colliding Galaxy Clusters (95% C.L.) DM self-interaction can solve some problems of CDM Harvey et al, Science (27 March 2015) 10/51
11 Dark Matter in the Galaxy 11/51
12 Dark Matter Density near the Solar System 12/51
13 Candidates of DM: No lack of options! 13/51
14 Scattering Cross Sections 14/51
15 The WIMP `Miracle' DM must be non-baryonic, and can have only very weak interaction with SM particles Clustering on (sub)galactic scales => 'cold', i.e., massive, and hence non-relativistic Weakly Interacting Massive Particles (WIMPs) In the sufficiently early universe, WIMPs would be in thermal equilibrium due to thermal production by collision of, and annihilation into, SM particles: In thermal equilibrium, If thermal equilibrium prevailed till today, present-day abundance would be negligible! But,... 15/51
16 The WIMP Miracle Annihilation rate since But expansion rate So, at some T=T_f, at which The species freezes out or decouples and leaves the exponentially falling abundance curve Present -day abundance: 16/51
17 The WIMP Miracle 17/51
18 Some numbers More than 10 million DM particles in this room Typical speed ~ 300 km/s. Thus, about 10 trillion DM particles will have passed through your body during this presentation! Can't we detect them? 18/51
19 Direct Detection of WIMPs : Drukier & Stodilsky (1984); Goodman & Witten (1985); Primack, Seckel, Sadulet (1988) 19/51
20 20/51
21 21/51
22 WIMP-Nucleus (Effective) Interaction The effective WIMP-Nucleus X-section can be obtained from fundamental WIMP-quark/gluon x-section: Spin-independent (SI) interaction: V= WIMP-nucleus relative velocity Form factor: Coherence loss of coherence WIMP-nucleon x-section WIMP-nucleon reduced mass = nucleon mass for m_wimp>>m_n Spin-dependent (SD) Interaction 22/51
23 23/51
24 Detection Strategies The energy deposited by WIMP-induced nuclear recoil in the detector medium manifests as light (scintillation), sound (acoustic waves/phonons) and charge (ionization) 24/51
25 Go Underground to reduce Cosmic Ray Background J. Formaggio and C. Martoff, Ann. Rev. Nucl. Part. Sci. 54 (2004) /51
26 From: Dan Bauer, /51
27 27/51
28 Annual Modulation:DAMA Expt. 28/51
29 Exclusion Curves (spin-independent interaction) Column 1 Column 2 Column Row 1 Row 2 Row 3 Row 4 P. Cushman et al, arxiv: /51
30 Exclusion Curves: Spin-dependent interactions Aprile et al (XENON100) 2013 Amole et al (PICO) PRL 2015 (SINP) 30/51
31 Viktor Zacek (AAPCOS-2015, SINP) 31/51
32 Superheated Liquid as a threshold detector for WIMPs Works at room temperature! 32/51
33 Viktor Zacek 33/51
34 Fluorine good for spin-dependent WIMP search Courtesy: Tony Noble 34/51
35 35/51
36 36/51
37 Viktor Zacek (PICASSO/PICO) 37/51
38 Viktor Zacek 38/51
39 Viktor Zacek 39/51
40 Courtesy: Viktor Zacek (PICASSO/PICO) 40/51
41 Largest ever Bubble Chamber for DM search 36.8 kg (18.4 Litre) of CF3I 3415 kg-days of exposure (between June'13 and May'14 No DM candidates after cuts! 41/51
42 PICO-60 (CF3I) Bubble PICO collaboration (arxiv: v2) 42/51
43 Looking Ahead on Bubble Chambers DM Detection 43/51
44 Ultimate Background: The Neutrino Floor Cushman et al, arxiv: DM detectors will start detecting astrophysical neutrinos through Coherent Neutrino-Nucleus Elastic Scattering (SM process)! 44/51
45 Detecting SN neutrino with DM detectors 45/51
46 INDIRECT DETECTION AMS-02: Positron excess in Galactic CR FERMI-LAT: Gamma rays from WIMP annihilation in dwarf Spheroidal satellites of Milky Way Super-K, ICECUBE: Neutrinos from WIMP annihilation in Sun 46/51
47 47/51
48 Milky Way's dwsphs 48/51
49 Constraints on WIMP annihilation from gamma rays from Milky Way's dsphs Fermi-LAT collaboration (Dec 2015) 49/51
50 Wither WIMP Direct Detection? Courtesy: Viktor Zacek (adapted from R. Gaitskell) 50/51
51 THANK YOU! 51/51
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