1 Astroparticle Physics (2/3) Nathalie PALANQUE-DELABROUILLE CEA-Saclay CERN Summer Student Lectures, August )What is Astroparticle Physics ? Big Bang Nucleosynthesis Cosmic Microwave Background 2)Dark matter, dark energy Evidence for dark matter Candidates and experimental status Supernovae and dark energy 3)High energy astrophysics

2 Dark matter in clusters Amas de Coma Zwicky, 1933 Mass of luminous matter = 10% Gravitational mass Zwicky

3 Rotation curves (planets) Rotation of planets Associated rotation curve Earth : 1 yr (at km)v=30 km/s Saturn :30 yrs (at 1, km)v=10 km/s  m = v = G M c / r v2rv2r G m M c r 2

4 Rotation curve of spiral galaxies Doppler distortion across galaxy  velocity distribution  Flat rotation curve ! 90% of gravitational mass is invisible (DARK HALOs) NGC 3198

5 Gravitational lensing Luminous mass ~ 1% Gravitational mass  HST Einstein ring

6 Summary of evidence Dark Energy (~70%) Stars (~2%) Baryonic DM (~3%) Non baryonic DM (~25%)  =  /  c  = 1 for k = 0

7 Lecture outline 1)What is Astroparticle Physics ? Big Bang Nucleosynthesis Cosmic Microwave Background 2)Dark matter, dark energy Evidence for dark matter Candidates and experimental status Baryonic (EROS, MACHO) Exotic (Edelweiss, DAMA, Antares) Supernovae and dark energy 3)High energy astrophysics

8 Dark matter candidates Baryonic (astrophysical candidates) Non baryonic (particle candidates) Molecular clouds Compact objects Planets Brown dwarfs Red dwarfs Black holes … White dwarfs Neutron stars low mass objects stellar residues Neutrinos WIMPS Axions

9 Dark matter candidates Baryonic (astrophysical candidates) Non baryonic (particle candidates) Molecular clouds Compact objects Neutrinos WIMPS Microlensing Accelerators Direct search (10 -7 M sun  ~10 M sun ) Mass? telescopes Axions Mass?

10 Principles of microlensing Angular separation of images ~ rad  Only 1 (combined) image, amplified Motion of deflector (220 km/s)  Duration t E ~ 90  M/M sun days

11 Microlensing light curve Luminosity Impact parameter Achromatic (Red & Blue) Symmetric To discriminate against variable stars :

12 Targets (EROS, MACHO) Event rate : ~ 1 per year per 20 million stars monitored LCM SCM Magellanic clouds : ly away (edge of halo?) (Milky Way ~ ly in diameter) Magellanic Clouds Halo Milky Way Earth (not to scale) ~30 million stars monitored: - > variable stars - >100 SN - Microlensing events ?   

13 Initial results Candidates (microlensing technique validated), t E ~ 30 days Over half of the dark halo in the form of dark objects of ~ 0.5 solar mass ! LCM, 1993 t E ~ 30 days SMC, 1998 t E ~ 120 days

14 Final results

15 White dwarfs White dwarf = final state of low mass star 38 white dwarfs found in old plates - moving fast  belongs to halo (vs. disk) - old (i.e. cold)  1st population of stars in our Galaxy White dwarfs (~1 M sun ) may compose 3 to 35% of the halo

16 Conclusions on baryonic DM Favored candidates (compact astrophysical objects) rejected on all mass range (only small window remaining at ~ M sun ) Gas Cold molecular clouds …

17 Non baryonic DM > 80% of DM is non baryonic Hot DM ?Cold DM ? Axions (invoked to solve strong CP violation pb in SM) Significant if < m a < eV WIMPS

18 Structure formation HDM wipes out structure on small scales Simulations of DM density maps CDM creates too many sub-structures? Hubble Deep Field

19 Neutrinos as HDM - exist as relic from Big Bang (~ 300 cm -3 ) - (now) known to have mass: neutrino oscillations Solar Atm masses (eV) from oscillations (most likely solution) contribution to matter density:  v ~  m / 46 eV m ~ 0.05 eV   v ~ 0.003

20 Weakly Interacting Massive Particles If SUSY exists - production of sparticles in early universe - all decay except LSP (conservation of R-parity)  relic from Big Bang - m  ~ 30 GeV (accelerator) - annihilate through  X X - relic density   ~ 0.3 for typical weak annihilation rates actual abundance equilibrium abundance Increasing Freeze out N eq  e -m  /T X = m  /T (time  )

21 Direct detection of WIMPS If halo DM made of WIMPS ~ 500 WIMPS/m 3 with v ~ 220 km/s  > WIMPs/cm 2 /s on Earth (from -v sun ) Requirement :High mass detectors Low radioactive background (discrimination) Experimental signature : nuclear recoil (vs. electronic “recoil”) e-e-  e - n WIMP Main source of background (radioactivity) n WIMP

22 Background rejection Scintillation Ionisation Heat DAMA, ZEPLIN I, UKDMC,… HDMS,… CRESST, CUORE, ROSEBUD CRESST, ROSEBUD ZEPLIN II EDELWEISS, CDMS Diodes Scintillators Bolometers - Deep underground - Event by event discrimination of nuclear vs. electronic recoil

23 Annual modulation Motion of Earth in the  wind v sun = 220 km/s  = 30 o v Earth = 30 km/s Modulation of annual rate  7% Max in June DAMA NaI-1 DAMA NaI-2 DAMA NaI-3 DAMA NaI-4 Seen by DAMA? m  ~ GeV BUT 1 signature only Not confirmed independantly

24 Edelweiss: detector Dilution cryostat low background (temperature ~15mK) Archeological lead shielding In Modane underground laboratory Negligible neutron background (~ 0,01 evt/kg/day) Detectors 3 x 320g bolometers

25 Edelweiss: analysis Electronic recoil (  90% 99.9% Nuclear recoil (WIMP, n) 90% Heat + Ionisation Background free analysis No event in signal region Recoil energy (keV) Ionisation / recoil

26 Conclusions on direct detection Regions of WIMPs models Regions above the curves excluded by experiments

27 Indirect detection of WIMPs Energy loss by elastic scattering with massive bodies (halos, Earth, Sun, galactic center) Gravitational capture + annihilation Earth, Sun, GC telescopes   X SuperK, Baksan, IMB, MACRO AMANDA, ANTARES, Baïkal… Halo High energy astronomy    AMS, GLAST, VERITAS, BESS, CELESTE, CAPRICE, MILAGRO…  Lecture 3

28 Lecture outline 1)What is Astroparticle Physics ? Big Bang Nucleosynthesis Cosmic Microwave Background 2)Dark matter, dark energy Evidence for dark matter Candidates and experimental status Baryonic (EROS, MACHO) Exotic (Edelweiss, DAMA, Antares) Supernovae and dark energy 3)High energy astrophysics

29 Geometry of the Universe 1 =  k (t) + ∑  x (t) +   (t) Curvature Energy density of components (matter, radiation)   ~ 2.47 x Density of dark energy Expansion vs geometry: q O =  m / 2 -  

30 Closed Universe Flat Universe Open Universe Measurement of the geometry AT A GIVEN DISTANCE Known physical sizeangle depends on geometry Known luminosity flux depends on geometry CMB SN Ia

31 Life of a small star (<8 M sun )

32 White dwarfs in binary systems SN Ia Very luminous (L ~ L sun ), out to high z Standard candles (1.4 M sun ) ~ 1 to 2 / century / galaxy

33 Light curves Unique parameter (strech factor)

34 SuperNova Legacy Survey 3 steps - discovery (differential photometry) 4 deg 2 monitored from CFHT (Hawaii) - identification (spectrum) - photometric follow-up  light curve (SNLS : same images as discovery)

35 CCD detectors at CFHT RCA CCD, 320 x 512 champ 2’ x 3.5’ RCA CCD, 640 x 1024 champ 2’ x 3.5’ SAIC CCD, 1K x 1K champ 4.2’ x 4.2’ Lick CCD, 2K x 2K champ 7’ x 7’ MOCAM CCDs, 4K x 4K champ 14’ x 14’ UH8K CCDs, 8K x 8K champ 28’ x 28’ CFH12K CCDs, 12K x 8K champ 42’ x 28’ MegaCam CCDs, 20K x 18K champ 1° x 1°

36 Hubble diagram Redshift z m = log F + cst = 5 log (H 0 D L ) + M - 5 log H H 0 D L cz z  0 mesure de H 0 z grand : mesure de  m,   Magnitude m older fainter 1+z = a(t obs )/a(t em ) At a given z Calan Tololo Hamuy et al., A.J.1996 Supernova Cosmology Project Accelerated expansion = smaller rate in the past = more time to reach a given z = larger distance of propagation of the photons = smaller flux 

37 Initial constraints (1998) 42 supernovae q 0 =  M /2 -   < 0 : Accelerating Universe If flat (  tot = 1) :  M = 0.28   = 0.72

38 Concordance CMB LSS Expected precision with JDEM (>2010)