10-14 December 2012 6 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, 195-373, 1996 Bertone, Hooper, Silk, Phys.Rept. 405, 279-390, 2005 Einasto, 0901.0632 Bergstrom 0903.4849, 1205.48821202.1170 Cirelli, Strumia arxiv: yymm.nnnn (upcoming)
How was Dark Matter produced?
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
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
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
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
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
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
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
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
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
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 8 3 90 g T 2 rad = 2 30 g T 4 g = X bos g i Ti T 4 + 7 8 X fer g i Ti T 4
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 8 3 90 g T 2 n X ' r 8 3 90 g M Pl T 2 f.o. ann
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 8 3 90 g T 2 n X ' r 8 3 90 g Tf.o. 2 Define Y X = n X M Pl ann s s = 2 2 45 g st 3
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 8 3 90 g Y today Y f.o. = r 8 3 G N rad = 1 M Pl T 2 f.o. r 8 3 90 g T 2 Define Y X = n X M Pl ann s q 8 3 90 g 2 2 45 g s M Pl 1 ann T f.o.
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 8 3 90 g T 2 n X ' r 8 3 90 g Y today Y f.o. = T 2 f.o. Define Y X = n X M Pl ann s q 8 3 90 g 2 2 45 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
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 8 3 90 g Y today Y f.o. = r 8 3 G N rad = 1 M Pl T 2 f.o. r 8 3 90 g T 2 Define Y X = n X M Pl ann s q 8 3 90 g 2 2 45 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
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 8 3 90 g Y today Y f.o. = r 8 3 G N rad = 1 M Pl T 2 f.o. r 8 3 90 g T 2 Define Y X = n X M Pl ann s q 8 3 90 g 2 2 45 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
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 8 3 90 g T 2 n X ' r 8 3 90 g Y today Y f.o. = T 2 f.o. Define Y X = n X M Pl ann s q 8 3 90 g 2 2 45 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
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 8 3 90 g T 2 n X ' r 8 3 90 g Y today Y f.o. = T 2 f.o. Define Y X = n X M Pl ann s q 8 3 90 g 2 2 45 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 610 27 cm 3 s 1 σ ann v
A thermal relic from the Early Universe Boltzmann equation in the Early Universe: f f f f... Ω X 610 27 cm 3 s 1 σ ann v Relic 0.23 for ann v =3 10 26 cm 3 /sec
A thermal relic from the Early Universe Boltzmann equation in the Early Universe: f f f f... Ω X 610 27 cm 3 s 1 σ ann v Relic 0.23 for ann v =3 10 26 cm 3 /sec Weak cross section: g w g w f M f
A thermal relic from the Early Universe Boltzmann equation in the Early Universe: f f f f... Ω X 610 27 cm 3 s 1 σ ann v Relic 0.23 for ann v =3 10 26 cm 3 /sec Weak cross section: g w g w f M f h ann vi (g2 w/4 ) 2 M 2 3 10 26 cm 3 /sec WIMP miracle!
Asymmetric : a completely different relic B ' 5 Just coincidence? Or: signal of a link? Possibly a common production mechanism:
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: =6 10 10 = n n n BBN, CMB...? = B B / m B B / m
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: =6 10 10 = n n n BBN, CMB...? = B B / m B B / m m ' 5 GeV Is this the of DAMA, CoGeNT, CRESST?!?
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: =6 10 10 = 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
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 10 8 10 9 10 10 10 11 10 12 f f! f f? 9... 0 0 Y Y 20 40 60 80 100 x m T Y 0 0 0 1.02 10 10 0 7 pb m 4.5 GeV density Y x 10 7 10 8 10 9 0 Y Y no osc 0 1.02 10 10 0 25 pb m 1000 GeV m 10 4 ev 2
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 10 8 10 9 10 10 10 11 10 12 f f! f f? 9... 0 0 Y Y 20 40 60 80 100 x m T Y 0 0 0 1.02 10 10 0 7 pb m 4.5 GeV density Y x 10 7 10 8 10 9 0 Y Y no osc 0 1.02 10 10 0 25 pb m 1000 GeV m 10 4 ev 2
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 10 8 10 9 10 10 10 11 10 12 f f! f f? 9... 0 0 Y Y 20 40 60 80 100 x m T Y 0 0 0 1.02 10 10 0 7 pb m 4.5 GeV density Y x 10 7 10 8 10 9 0 Y Y no osc 0 1.02 10 10 0 25 pb m 1000 GeV m 10 4 ev 2
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 10 8 10 9 10 10 10 11 10 12 f f! f f? 9... 10 7 10 8 10 9 0 0 0 Y Y 20 40 60 80 100 Y Y x m T no osc Y 0 0 0 1.02 10 10 0 7 pb m 4.5 GeV 0 1.02 10 10 0 m 25 pb m 1000 X GeV m 10 4 ev The relic abundance is determined by and. 0 2
Particle Physics candidates for Dark Matter
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
Candidates A matter of perspective:
Candidates A matter of perspective: SuSy Non SuSy
Candidates A matter of perspective: SuSy Non SuSy?
Candidates A matter of perspective: SuSy neutralino other exotic candidates
SuSy in 2 minutes h
SuSy in 2 minutes h m h ' 125 GeV
SuSy in 2 minutes h m h ' 125 GeV h t h m h 10 19 GeV
SuSy in 2 minutes ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ h h2 h1 ~ h2 ~ m h ' 125 GeV h t h m h 10 19 GeV h ~t h m h 10 19 GeV
SuSy in 2 minutes 200 GeV ~ ~ ~ ~ ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ h1 ~ h2 ~ m h ' 125 GeV h t h m h 10 19 GeV h ~t h m h 10 19 GeV
SuSy in 2 minutes 200 GeV ~ ~ ~ ~ ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ R = +1 h1 ~ h2 ~ m h ' 125 GeV R = 1 h t h m h 10 19 GeV h ~t h m h 10 19 GeV
SuSy in 2 minutes 200 GeV ~ ~ ~ ~ ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ R = +1 h1 ~ h2 ~ m h ' 125 GeV R = 1 h t h m h 10 19 GeV h ~t h m h 10 19 GeV
SuSy in 2 minutes 2 TeV ~ ~ ~ ~ h h2 ~ ~ ~ ~ ~ ~ ~ ~ R = +1 ~ ~ ~ ~ m h ' 125 GeV R = 1 h1 ~ h2 ~ h t h m h 10 19 GeV h ~t h m h 10 19 GeV
Candidates A matter of perspective: SuSy neutralino other exotic candidates
Candidates A matter of perspective: SuSy neutralino
Candidates A matter of perspective: SuSy neutralino
Candidates A matter of perspective: SuSy neutralino SuSy e.g. RH sneutrino
Candidates A matter of perspective: SuSy neutralino SuSy Weak e.g. RH sneutrino WIMP
Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV e.g. RH sneutrino WIMP TC some KK
Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle e.g. RH sneutrino WIMP TC some KK
Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK
Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK gravitino?
Candidates A matter of perspective: SuSy neutralino SuSy gravitino? e.g. RH sneutrino Weak WIMP TeV particle sub-gev axion TC some KK
Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP gravitino? axion TC some KK
Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK axino? gravitino?
Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK axino? gravitino?
Candidates A matter of perspective: SuSy neutralino SuSy Weak TeV particle sub-gev e.g. RH sneutrino WIMP axion TC some KK axino? gravitino?
Candidates A matter of perspective: Caveat: no categorization is perfect.
Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: em weak strong-ish other none (other than gravity)
Candidates A matter of perspective: Caveat: no categorization is perfect. Interactions: em weak strong-ish other none (other than gravity)
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
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
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
Candidates A matter of perspective: plausible mass ranges (1 TeV) ev
Candidates A matter of perspective: plausible mass ranges only 90 orders of magnitude!
How do we search for Dark Matter?