Dark Matter. 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 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 10-14 December th TRR Winter School - Passo del Tonale Dark Matter 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)
3 Contents 1. Introduction and 'cosmology' - basic properties of DM - evidences -- galactic rotation curves -- weak lensing [qualitative idea] -- 'precision cosmology' [qualitative] - alternatives (Machos, MOND) - DM production -- freeze-out & the WIMP miracle -- asymmetric DM - 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 Contents 1. Introduction and 'cosmology' - basic properties of DM - evidences -- galactic rotation curves -- weak lensing [qualitative idea] -- 'precision cosmology' [qualitative] - alternatives (Machos, MOND) - DM production -- freeze-out & the WIMP miracle -- asymmetric DM - particle physics candidates lecture I lecture II 2. Indirect Detection - basics - observables -- charged particle fluxes: production & propagation -- gamma rays: production & propagation -- neutrinos: production & propagation - current status: hints, constraints lecture III lecture IV 3. Direct Detection - basics - observables (recoil spectrum, detection strategies) - current status: hints, constraints 4. Collider Searches - basics - observables (missing energy, monojets) - complementarity lecture V
5 Executive summary
6 Executive summary DM exists
7 Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion
8 Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter DM h 2 = ± (notice error!)
9 Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter neutral particle dark... DM h 2 = ± (notice error!)
10 Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter neutral particle dark... DM h 2 = ± (notice error!) cold or not too warm p/m <<1 at CMB formation
11 Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter neutral particle dark... DM h 2 = ± (notice error!) cold or not too warm very feebly interacting p/m <<1 at CMB formation -with itself -with ordinary matter ( collisionless )
12 Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter neutral particle dark... DM h 2 = ± (notice error!) cold or not too warm very feebly interacting p/m <<1 at CMB formation -with itself -with ordinary matter ( collisionless ) stable or very long lived DM sec
13 Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter neutral particle dark... DM h 2 = ± (notice error!) cold or not too warm very feebly interacting p/m <<1 at CMB formation -with itself -with ordinary matter ( collisionless ) stable or very long lived possibly a relic from the EU DM sec
14 Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter neutral particle dark... DM h 2 = ± (notice error!) cold or not too warm very feebly interacting p/m <<1 at CMB formation -with itself -with ordinary matter ( collisionless ) stable or very long lived possibly a relic from the EU searched for by DM sec
15 SM SM Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter neutral particle dark... DM h 2 = ± (notice error!) cold or not too warm very feebly interacting p/m <<1 at CMB formation -with itself -with ordinary matter ( collisionless ) stable or very long lived possibly a relic from the EU searched for by DM sec DM Direct Detection DM
16 SM SM DM SM Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter neutral particle dark... DM h 2 = ± (notice error!) cold or not too warm very feebly interacting p/m <<1 at CMB formation -with itself -with ordinary matter ( collisionless ) stable or very long lived possibly a relic from the EU searched for by DM sec DM Direct Detection DM DM Indirect Detection SM
17 SM SM DM SM SM DM Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion makes up 23% of total energy 80% of total matter neutral particle dark... DM h 2 = ± (notice error!) cold or not too warm very feebly interacting p/m <<1 at CMB formation -with itself -with ordinary matter ( collisionless ) stable or very long lived possibly a relic from the EU searched for by DM sec DM Direct Detection DM DM Indirect Detection SM SM Collider DM
18 The cosmic inventory Most of the Universe is Dark Ω lum % 1% 4% Ω b ± BBN -CMB 23% DM 0.23 de CMB + SNIa - CMB - DM - acoustic peak in baryons x = x c ; CMB first peak tot = 1 (flat); HST h =0.71 ± 0.07 what s the difference between DM and DE?
19 The cosmic inventory Most of the Universe is Dark 72% FAvgQ: what s the difference between DM and DE? 23% 1% 4% DM behaves like matter - overall it dilutes as volume expands - clusters gravitationally on small scales - (NR matter) w = P/ =0 (radiation has w = 1/3 ) [back] DE behaves like a constant - it does not dilute - does not cluster, it is prob homogeneous - w = P/ 1 - pulls the acceleration, FRW eq. ä a = 4 G N 3 (1 3w)
20 The cosmic inventory Most of the Universe is Dark Ω lum % 23% 1% 4% Ω b ± DM 0.23 de 0.72 particle physics -BBN -CMB cosmology - CMB + SNIa - CMB - DM - acoustic peak in baryons x = x c ; CMB first peak tot = 1 (flat); HST h =0.71 ± 0.07 what s the difference between DM and DE?
21 The cosmic inventory neutrinos 10% 15% radiation 12% baryons 63% Dark Matter At the time of CMB formation (380 Ky)
22 How do we know that Dark Matter is out there?
23 Contents 1. Introduction and 'cosmology' - basic properties of DM - evidences -- galactic rotation curves -- weak lensing [qualitative idea] -- 'precision cosmology' [qualitative] - alternatives (Machos, MOND) - DM production -- freeze-out & the WIMP miracle -- asymmetric DM - 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
24 The Evidence for DM 1) galaxy rotation curves m v2 c (r) r centrifugal = G NmM(r) r 2 centripetal r GN M(r) v c (r) = Z r with M(r) =4 (r) r 2 dr v c (r) const ρ M (r) 1 r 2 Begeman et al., MNRAS 249 (1991) Ω M 0.1
25 The Evidence for DM 1) galaxy rotation curves m v2 c (r) r centrifugal = G NmM(r) r 2 centripetal r GN M(r) v c (r) = Z r with M(r) =4 (r) r 2 dr v c (r) const ρ M (r) 1 r 2 Begeman et al., MNRAS 249 (1991) Ω M 0.1
26 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M bullet cluster - NASA astro-ph/ [further developments]
27 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M chandra.harvard.edu
28 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M bullet cluster - NASA astro-ph/ [further developments]
29 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M bullet cluster - NASA astro-ph/ [further developments]
30 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M bullet cluster - NASA astro-ph/ [further developments]
31 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M bullet cluster - NASA astro-ph/ [further developments]
32 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M bullet cluster - NASA astro-ph/ [further developments]
33 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M bullet cluster - NASA astro-ph/ [further developments]
34 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M ring of Dark Matter (2007)
35 The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M ring of Dark Matter (2007)
36 The Evidence for DM 1) galaxy rotation curves ΩM! 0.1 2) clusters of galaxies ΩM ) CMB+LSS(+SNIa:) WMAP Millennium M.Cirelli and A.Strumia, astro-ph/
37 DM N-body simulations CDM particles, 43 Mpc cubic box Andrey Kravtsov, cosmicweb.uchicago.edu [back]
38 DM N-body simulations CDM particles, 43 Mpc cubic box Andrey Kravtsov, cosmicweb.uchicago.edu [back]
39 DM N-body simulations Aquarius project of the VIRGO coll.: CDM particles, single galactic halo VIRGO coll., Aquarius project, [back]
40 DM N-body simulations 2dF: galaxies SDSS: 10 6 galaxies, 2 billion lyr Of course, you have to infer galaxies within the DM simulation Springel, Frenk, White, Nature 440 (2006) Millennium: particles, 500 h -1 Mpc [back]
41 CMB CMB & Large Scale Structure LSS LSS matter power spectrum
42 CMB CMB & Large Scale Structure LSS LSS matter power spectrum
43 CMB CMB & Large Scale Structure T = K T 5 10 T CMB spectrum cold spots LSS hot spots 1 LSS matter power spectrum
44 CMB The Evidence for DM LSS How would the power spectra be without DM? (and no other extra ingredient) no DM data no DM 4000 data Multipole { (in particular: no DM => no 3rd peak!) Dodelson, Liguori CAMB online {H{+1L C{ ê2p in mk need DM oftomatter gravitationally FIG. 1:(you Power spectrum fluctuations in a the catalyse structure formation) ory without dark matter as compared to observations of the
45
46 MOND? TeVeS? Instead of adding matter, modify Newton or GR. F = ma F = ma µ(a) with F = m a2 = GMm a 0 r 2 a = force balance p GMa0 ) = v2 ) r tangential acceleration fits rotation curves very well r µ(a) = ( v =(GMa 0 ) 1/4 = const 1 a>a 0 a/a 0 a a 0 a 0 = m/s 2 Sanders, McGaugh, Ann. Rev. AA, 2002 can fit (bullet) cluster if adding 2 ev neutrinos... Angus et al., astro-ph/
47 CMB The Evidence for DM LSS The Tensor-Vector-Scalar and its cosmology The Tensor-Vector-Scalar theory and theory its cosmology How would the power spectra be in MOND/TeVeS, without DM? C.Skordis, Review, C.Skordis, Review, CDM TeVeS CDM TeVeS (in particular: no DM => no 3rd peak!) (here you can make it) Figure 3. LEFT : The Cosmic Microwave Background angular power spectrum
48
49 The Evidence for DM 1) galaxy rotation curves ΩM! 0.1 2) clusters of galaxies ΩM ) CMB+LSS(+SNIa:) WMAP-3yr ACbar CBI Boomerang DASI VSA WMAP Millennium SDSS, 2dFRGS LyA Forest Croft LyA Forest SDSS M ± 0.02 (spectra w/o DM) M.Cirelli and A.Strumia, astro-ph/
50 The Evidence for DM 1) galaxy rotation curves 2) clusters of galaxies 3) CMB+LSS(+SNIa:) ΩM! 0.1 ΩM M ± 0.02 What is the DM?? It consists of a particle. Permeates galactic haloes.
51 What do we know of the particle physics properties of Dark Matter?
52
53 DM can NOT be:
54 an astro je ne sais pas quoi: DM can NOT be:
55 DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas - Black Holes - brown dwarves
56 DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas - Black Holes - brown dwarves
57 DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas - Black Holes - brown dwarves
58 DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas - Black Holes - brown dwarves strong lensing
59 MACHOs or PBHs as DM fraction f of halo mass consisting of MACHOs 60% 50% 40% 30% 20% 10% 0% MACHO EROS-1 + MACHO, 1998 coll, % excl OGLE EROS coll., % excl. 95% excluded MACHO mass M in solar masses
60 DM can NOT be: an astro je ne sais pas quoi: a baryon of the SM: - neutrons - gas - Black Holes - brown dwarves strong lensing
61 DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas a baryon of the SM: - BBN computes the abundance of He in terms of primordial baryons: too much baryons => Universe full of Helium - CMB says baryons are 4% max - Black Holes - brown dwarves strong lensing
62 MACHOs or PBHs as DM fraction f of halo mass consisting of MACHOs 60% 50% 40% 30% 20% 10% 0% MACHO EROS-1 + MACHO, 1998 coll, % excl OGLE EROS coll., % excl. 95% excluded MACHO mass M in solar masses
63 DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas a baryon of the SM: - BBN computes the abundance of He in terms of primordial baryons: too much baryons => Universe full of Helium - CMB says baryons are 4% max - Black Holes - brown dwarves strong lensing neutrinos:
64 DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas a baryon of the SM: - BBN computes the abundance of He in terms of primordial baryons: too much baryons => Universe full of Helium - CMB says baryons are 4% max - Black Holes - brown dwarves strong lensing neutrinos: too light! m 1 ev do not have enough mass to act as gravitational attractors in galaxy collapse
65 (Neutrino) HDM in LSS no HDM some HDM m =0 m = 6.9 ev CDM - Gadget2-768 Mpc 3 T.Haugboelle, S.Hannestad, Aarhus University
66 (Neutrino) HDM in LSS no HDM some HDM m =0 m = 6.9 ev CDM - Gadget2-768 Mpc 3 T.Haugboelle, S.Hannestad, Aarhus University
67 Recap: DM factsheet
68 Recap: DM factsheet DM exists
69 Recap: DM factsheet DM exists
70 Recap: DM factsheet DM exists
71 Recap: DM factsheet DM exists
72 Recap: DM factsheet DM exists
73 Recap: DM factsheet DM exists
74 Recap: DM factsheet DM exists
75 Recap: DM factsheet DM exists How heavy? DM GeV proton 1 GeV
76 DM exists Recap: DM factsheet How heavy? How dense? DM GeV proton 1 GeV 10 GeV 100 GeV
77 DM exists Recap: DM factsheet They do not interact with normal matter nor with themselves, they fly freely thru matter How heavy? How dense? DM GeV proton 1 GeV 10 GeV 100 GeV
78 DM exists Recap: DM factsheet They do not interact with normal matter nor with themselves, they fly freely thru matter How heavy? How dense? DM GeV proton 1 GeV 10 GeV 100 GeV They interact a little little bit...
79 How was Dark Matter produced?
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