10-14 December 2012 6 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, 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)
10-14 December 2012 6 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, 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)
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
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
Executive summary
Executive summary DM exists
Executive summary DM exists it s a new, unknown particle no SM particle can fulfil dilutes as 1/a 3 with universe expansion
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 =0.1126 ± 0.0036 (notice error!)
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 =0.1126 ± 0.0036 (notice error!)
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 =0.1126 ± 0.0036 (notice error!) cold or not too warm p/m <<1 at CMB formation
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 =0.1126 ± 0.0036 (notice error!) cold or not too warm very feebly interacting p/m <<1 at CMB formation -with itself -with ordinary matter ( collisionless )
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 =0.1126 ± 0.0036 (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 10 17 sec
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 =0.1126 ± 0.0036 (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 10 17 sec
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 =0.1126 ± 0.0036 (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 10 17 sec
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 =0.1126 ± 0.0036 (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 10 17 sec DM Direct Detection DM
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 =0.1126 ± 0.0036 (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 10 17 sec DM Direct Detection DM DM Indirect Detection SM
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 =0.1126 ± 0.0036 (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 10 17 sec DM Direct Detection DM DM Indirect Detection SM SM Collider DM
The cosmic inventory Most of the Universe is Dark Ω lum 0.01 72% 1% 4% Ω b 0.040 ± 0.005 -BBN -CMB 23% DM 0.23 de 0.72 - 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?
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)
The cosmic inventory Most of the Universe is Dark Ω lum 0.01 72% 23% 1% 4% Ω b 0.040 ± 0.005 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?
The cosmic inventory neutrinos 10% 15% radiation 12% baryons 63% Dark Matter At the time of CMB formation (380 Ky)
How do we know that Dark Matter is out there?
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
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
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
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 bullet cluster - NASA astro-ph/0608247 [further developments]
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 chandra.harvard.edu
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 bullet cluster - NASA astro-ph/0608247 [further developments]
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 bullet cluster - NASA astro-ph/0608247 [further developments]
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 bullet cluster - NASA astro-ph/0608247 [further developments]
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 bullet cluster - NASA astro-ph/0608247 [further developments]
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 bullet cluster - NASA astro-ph/0608247 [further developments]
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 bullet cluster - NASA astro-ph/0608247 [further developments]
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 ring of Dark Matter (2007)
The Evidence for DM 1) galaxy rotation curves Ω M 0.1 2) clusters of galaxies - rotation curves - gravitational lensing Ω M 0.2 0.4 ring of Dark Matter (2007)
The Evidence for DM 1) galaxy rotation curves ΩM! 0.1 2) clusters of galaxies ΩM 0.2 0.4 3) CMB+LSS(+SNIa:) WMAP Millennium M.Cirelli and A.Strumia, astro-ph/0607086
DM N-body simulations 2 10 6 CDM particles, 43 Mpc cubic box Andrey Kravtsov, cosmicweb.uchicago.edu [back]
DM N-body simulations 2 10 6 CDM particles, 43 Mpc cubic box Andrey Kravtsov, cosmicweb.uchicago.edu [back]
DM N-body simulations Aquarius project of the VIRGO coll.: 1.5 10 9 CDM particles, single galactic halo VIRGO coll., Aquarius project, www.mpa-garching.mpg.de/aquarius/ [back]
DM N-body simulations 2dF: 2.2 10 5 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: 10 10 particles, 500 h -1 Mpc [back]
CMB CMB & Large Scale Structure LSS LSS matter power spectrum
CMB CMB & Large Scale Structure LSS LSS matter power spectrum
CMB CMB & Large Scale Structure T = 2.725 K T 5 10 T CMB spectrum cold spots LSS hot spots 1 LSS matter power spectrum
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 2000 0 0 500 1000 1500 2000 Multipole { (in particular: no DM => no 3rd peak!) Dodelson, Liguori 2006 6000 CAMB online {H{+1L C{ ê2p in mk2 8000 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
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 =1.2 10 10 m/s 2 Sanders, McGaugh, Ann. Rev. AA, 2002 can fit (bullet) cluster if adding 2 ev neutrinos... Angus et al., astro-ph/0609125
CMB The Evidence for DM LSS The Tensor-Vector-Scalar and its cosmology The Tensor-Vector-Scalar theory and theory its cosmology 19 19 How would the power spectra be in MOND/TeVeS, without DM? C.Skordis, Review, 0903.3602 C.Skordis, Review, 0903.3602 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
The Evidence for DM 1) galaxy rotation curves ΩM! 0.1 2) clusters of galaxies ΩM 0.2 0.4 3) CMB+LSS(+SNIa:) WMAP-3yr ACbar CBI Boomerang DASI VSA WMAP Millennium SDSS, 2dFRGS LyA Forest Croft LyA Forest SDSS M 0.275 ± 0.02 (spectra w/o DM) M.Cirelli and A.Strumia, astro-ph/0607086
The Evidence for DM 1) galaxy rotation curves 2) clusters of galaxies 3) CMB+LSS(+SNIa:) ΩM! 0.1 ΩM 0.2 0.4 M 0.275 ± 0.02 What is the DM?? It consists of a particle. Permeates galactic haloes.
What do we know of the particle physics properties of Dark Matter?
DM can NOT be:
an astro je ne sais pas quoi: DM can NOT be:
DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas - Black Holes - brown dwarves
DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas - Black Holes - brown dwarves
DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas - Black Holes - brown dwarves
DM can NOT be: an astro je ne sais pas quoi: - neutrons - gas - Black Holes - brown dwarves strong lensing
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, 2000 95% excl OGLE-3 2011 EROS coll., 2006 95% excl. 95% excluded 10-7 10-6 10-5 10-4 10-3 10-2 10-1 1 10 MACHO mass M in solar masses
DM can NOT be: an astro je ne sais pas quoi: a baryon of the SM: - neutrons - gas - Black Holes - brown dwarves strong lensing
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
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, 2000 95% excl OGLE-3 2011 EROS coll., 2006 95% excl. 95% excluded 10-7 10-6 10-5 10-4 10-3 10-2 10-1 1 10 MACHO mass M in solar masses
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:
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
(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
(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
Recap: DM factsheet
Recap: DM factsheet DM exists
Recap: DM factsheet DM exists
Recap: DM factsheet DM exists
Recap: DM factsheet DM exists
Recap: DM factsheet DM exists
Recap: DM factsheet DM exists
Recap: DM factsheet DM exists
Recap: DM factsheet DM exists How heavy? DM 10-1000 GeV proton 1 GeV
DM exists Recap: DM factsheet How heavy? How dense? DM 10-1000 GeV proton 1 GeV 10 GeV 100 GeV
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 10-1000 GeV proton 1 GeV 10 GeV 100 GeV
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 10-1000 GeV proton 1 GeV 10 GeV 100 GeV They interact a little little bit...
How was Dark Matter produced?