Dark Matter II. Marco Cirelli. (CNRS IPhT Saclay) December th TRR Winter School - Passo del Tonale. Reviews on Dark Matter: NewDark
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1 10-14 December th TRR Winter School - Passo del Tonale Dark Matter II Marco Cirelli (CNRS IPhT Saclay) in collaboration with: A.Strumia (Pisa) N.Fornengo (Torino) M.Tamburini (Pisa) R.Franceschini (Pisa) M.Raidal (Tallin) M.Kadastik (Tallin) Gf.Bertone (IAP Paris) M.Taoso (Padova) C.Bräuninger (Saclay) P.Panci (L Aquila + Saclay + CERN) F.Iocco (Saclay + IAP Paris) P.Serpico (CERN) NewDark Reviews on Dark Matter: Jungman, Kamionkowski, Griest, Phys.Rept. 267, , 1996 Bertone, Hooper, Silk, Phys.Rept. 405, , 2005 Einasto, Bergstrom , Cirelli, Strumia arxiv: yymm.nnnn (upcoming)
2 How was Dark Matter produced?
3 Contents 1. Introduction and 'cosmology' - basic properties of - evidences -- galactic rotation curves -- weak lensing [qualitative idea] -- 'precision cosmology' [qualitative] - alternatives (Machos, MOND) - production -- freeze-out & the WIMP miracle -- asymmetric - particle physics candidates 2. Indirect Detection - basics - observables -- charged particle fluxes: production & propagation -- gamma rays: production & propagation -- neutrinos: production & propagation - current status: hints, constraints 3. Direct Detection - basics - observables (recoil spectrum, detection strategies) - current status: hints, constraints 4. Collider Searches - basics - observables (missing energy, monojets) - complementarity
4 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance
5 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance Kolb,Turner, The Early Universe, 1995
6 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance f f Kolb,Turner, The Early Universe, 1995
7 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance f f f f Kolb,Turner, The Early Universe, 1995
8 A thermal relic from the Early Universe Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - symmetric abundance f f f f... Kolb,Turner, The Early Universe, 1995
9 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt cosmology particle physics
10 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) H freeze-out
11 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N tot freeze-out
12 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 rad = 2 30 g T 4 g = X bos g i Ti T X fer g i Ti T 4
13 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g M Pl T 2 f.o. ann
14 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g Tf.o. 2 Define Y X = n X M Pl ann s s = g st 3
15 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = n X ' ann H = r g Y today Y f.o. = r 8 3 G N rad = 1 M Pl T 2 f.o. r g T 2 Define Y X = n X M Pl ann s q g g s M Pl 1 ann T f.o.
16 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g Y today Y f.o. = T 2 f.o. Define Y X = n X M Pl ann s q g g s 1 = M Pl ann T f.o. M Pl ann T f.o. M Pl T f.o. m X /20 g ' g s ' 100 # ann m X
17 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = n X ' ann H = r g Y today Y f.o. = r 8 3 G N rad = 1 M Pl T 2 f.o. r g T 2 Define Y X = n X M Pl ann s q g g s X = X crit = m Xn X crit 1 = M Pl ann T f.o. M Pl ann T f.o. = m XY today s today crit M Pl = m X # ann m X M Pl # ann m X s today crit
18 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = n X ' ann H = r g Y today Y f.o. = r 8 3 G N rad = 1 M Pl T 2 f.o. r g T 2 Define Y X = n X M Pl ann s q g g s X = X crit = m Xn X crit 1 = M Pl ann T f.o. M Pl ann T f.o. = m XY today s today crit M Pl = m X # ann m X M Pl # m X cancels out ann m X s today crit
19 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g Y today Y f.o. = T 2 f.o. Define Y X = n X M Pl ann s q g g s 1 = M Pl ann T f.o. M Pl ann T f.o. M Pl # ann m X X ' 0.2 pb ann
20 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: dn X +3Hn X = h ann vi n 2 X n eq X dt Shortcut (NB: includes cheating) n X = ann H = r 8 3 G N rad = 1 M Pl r g T 2 n X ' r g Y today Y f.o. = T 2 f.o. Define Y X = n X M Pl ann s q g g s 1 = M Pl ann T f.o. M Pl ann T f.o. M Pl # ann m X X ' 0.2 pb ann or Ω X cm 3 s 1 σ ann v
21 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: f f f f... Ω X cm 3 s 1 σ ann v Relic 0.23 for ann v = cm 3 /sec
22 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: f f f f... Ω X cm 3 s 1 σ ann v Relic 0.23 for ann v = cm 3 /sec Weak cross section: g w g w f M f
23 A thermal relic from the Early Universe Boltzmann equation in the Early Universe: f f f f... Ω X cm 3 s 1 σ ann v Relic 0.23 for ann v = cm 3 /sec Weak cross section: g w g w f M f h ann vi (g2 w/4 ) 2 M cm 3 /sec WIMP miracle!
24 Asymmetric : a completely different relic B ' 5 Just coincidence? Or: signal of a link? Possibly a common production mechanism:
25 Asymmetric : a completely different relic B ' 5 Just coincidence? Or: signal of a link? Possibly a common production mechanism: Baryogenesis: B = n B n n B Darko genesis: = = n n n BBN, CMB...? = B B / m B B / m
26 Asymmetric : a completely different relic B ' 5 Just coincidence? Or: signal of a link? Possibly a common production mechanism: Baryogenesis: B = n B n n B Darko genesis: = = n n n BBN, CMB...? = B B / m B B / m m ' 5 GeV Is this the of DAMA, CoGeNT, CRESST?!?
27 Asymmetric : a completely different relic B ' 5 Just coincidence? Or: signal of a link? Possibly a common production mechanism: Baryogenesis: B = n B n n B Darko genesis: = = n n n BBN, CMB...? = B A variety of specific models/ideas: transferring or co-genesis cfr J. March-Russell via leptogenesis stores the anti-b number connection to neutrino masses
28 Asymmetric : a completely different relic Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - Asymmetric abundance - large annihilation cross sec Comoving density Y x f f! f f? Y Y x m T Y pb m 4.5 GeV density Y x Y Y no osc pb m 1000 GeV m 10 4 ev 2
29 Asymmetric : a completely different relic Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - Asymmetric abundance - large annihilation cross sec Comoving density Y x f f! f f? Y Y x m T Y pb m 4.5 GeV density Y x Y Y no osc pb m 1000 GeV m 10 4 ev 2
30 Asymmetric : a completely different relic Consider a particle χ:!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - Asymmetric abundance - large annihilation cross sec Comoving density Y x f f! f f? Y Y x m T Y pb m 4.5 GeV density Y x Y Y no osc pb m 1000 GeV m 10 4 ev 2
31 Asymmetric : a completely different relic Consider a particle χ: X ' m X s crit 0!... - subject to - heavy (e.g. 100 GeV) - stable - in an expanding Universe - Asymmetric abundance - large annihilation cross sec Comoving density Y x density Y x f f! f f? Y Y Y Y x m T no osc Y pb m 4.5 GeV m 25 pb m 1000 X GeV m 10 4 ev The relic abundance is determined by and. 0 2
32 Particle Physics candidates for Dark Matter
33 Contents 1. Introduction and 'cosmology' - basic properties of - evidences -- galactic rotation curves -- weak lensing [qualitative idea] -- 'precision cosmology' [qualitative] - alternatives (Machos, MOND) - production -- freeze-out & the WIMP miracle -- asymmetric - particle physics candidates 2. Indirect Detection - basics - observables -- charged particle fluxes: production & propagation -- gamma rays: production & propagation -- neutrinos: production & propagation - current status: hints, constraints 3. Direct Detection - basics - observables (recoil spectrum, detection strategies) - current status: hints, constraints 4. Collider Searches - basics - observables (missing energy, monojets) - complementarity
34 Candidates A matter of perspective:
35 Candidates A matter of perspective: SuSy Non SuSy
36 Candidates A matter of perspective: SuSy Non SuSy?
37 Candidates A matter of perspective: SuSy neutralino other exotic candidates
38 SuSy in 2 minutes h
39 SuSy in 2 minutes h m h ' 125 GeV
40 SuSy in 2 minutes h m h ' 125 GeV h t h m h GeV
41 SuSy in 2 minutes ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ h h2 h1 ~ h2 ~ m h ' 125 GeV h t h m h GeV h ~t h m h GeV
42 SuSy in 2 minutes 200 GeV ~ ~ ~ ~ ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ h1 ~ h2 ~ m h ' 125 GeV h t h m h GeV h ~t h m h GeV
43 SuSy in 2 minutes 200 GeV ~ ~ ~ ~ ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ R = +1 h1 ~ h2 ~ m h ' 125 GeV R = 1 h t h m h GeV h ~t h m h GeV
44 SuSy in 2 minutes 200 GeV ~ ~ ~ ~ ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ R = +1 h1 ~ h2 ~ m h ' 125 GeV R = 1 h t h m h GeV h ~t h m h GeV
45 SuSy in 2 minutes 2 TeV ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ R = +1 ~ ~ ~ ~ m h ' 125 GeV R = 1 h1 ~ h2 ~ h t h m h GeV h ~t h m h GeV
46 Candidates A matter of perspective: SuSy neutralino other exotic candidates
47 Candidates A matter of perspective: SuSy neutralino
48 Candidates A matter of perspective: SuSy neutralino
49 Candidates A matter of perspective: SuSy neutralino SuSy e.g. RH sneutrino
50 Candidates A matter of perspective: SuSy neutralino SuSy Weak e.g. RH sneutrino WIMP
51 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV e.g. RH sneutrino WIMP TC some KK
52 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle e.g. RH sneutrino WIMP TC some KK
53 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK
54 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK gravitino?
55 Candidates A matter of perspective: SuSy neutralino SuSy gravitino? e.g. RH sneutrino Weak WIMP TeV particle sub-gev axion TC some KK
56 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP gravitino? axion TC some KK
57 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK axino? gravitino?
58 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK axino? gravitino?
59 Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK axino? gravitino?
60 Candidates A matter of perspective: Caveat: no categorization is perfect.
61 Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: em weak strong-ish other none (other than gravity)
62 Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: em weak strong-ish other none (other than gravity)
63 Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: em weak strong-ish neutralino etc Little Higgs KK Inert Doublet Minimal TC mirror } a other none (other than gravity) secluded WIMPless singlet scalar sterile neutrino gravitino axion
64 Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: naturalness-inspired em weak strong-ish neutralino etc Little Higgs KK Inert Doublet Minimal TC mirror } a other none (other than gravity) secluded WIMPless singlet scalar sterile neutrino gravitino axion
65 Candidates A matter of perspective: Interactions: em weak strong-ish naturalness-inspired neutralino etc Little Higgs KK Inert Doublet Minimal TC mirror } a Caveat: no categorization is perfect. Production mechanism? thermal freeze out thermal freeze out thermal freeze out thermal freeze out thermal freeze out exhaustion Stability? R parity T parity K parity Z2 symmetry gauge sym Tbaryon # Z2 symmetry other secluded WIMPless sort of freeze out sort of freeze out some symmetry some symmetry singlet scalar thermal freeze out Z2 symmetry none (other than gravity) sterile neutrino gravitino mixing thermal or decay just long lived R parity or just long lived axion misalignment? just long lived
66 Candidates A matter of perspective: plausible mass ranges (1 TeV) ev
67 Candidates A matter of perspective: plausible mass ranges only 90 orders of magnitude!
68 How do we search for Dark Matter?
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