Cosmic Ray detection with spaceborne detectors M. Casolino Casolino.marco @ gmail.com @casolinomarco INFN University of Rome Tor Vergata RIKEN Tuxla School for astrophysics, 11 2015 15/8/2011
7. Dark and Anti-Matter
Dark Matter Most probably a particle Does not emit or absorb light Does not interact e.m. or strong. Should be transparent matter Interacts gravitationally Most probably interacts weakly
When dark matter? In 1933 Zwicky, observing the movement of galaxies in the Coma cluster understood that their visible mass was not enough to keep them in a bound state. He estimated that not visible mass should have been at least 160 times the galaxies noone listened Immagine a falsi colori: blu visibile (Sloan Digital Sky Survey) Rosso e verde - Infrarosso (NASA's Spitzer Space Telescope)
Fritz Zwicky 14/2/1898, Varna (Bulgaria) 8/2/1974 Pasadena
1959: Louise Volders showed that spiral galaxy M33 does not rotate as expected. Stars in the galactic arms should follow keplerian law, since most of the mass was thought to be concentrated in galactic center Dark matter inside the galaxies
Rotation speed (km/s) Galaxy rotation curve Observed experimentally Predicted by keplerian law Distance from galactic center (kpc)
Doppler shift in the 21 cm (hyperfine line)
Back to cluster of galaxies X-ray emission from Hydrogen gas falling in the gravitational well of galaxy clusters Visible barion fraction: 0.56% f B h 3/2 =0.056 0.014 Matter from Big Bang: 38% W matter h 1/2 =0.38 0.07
Gravitational lensing
Distorsione dello Spazio - Tempo 1 R 8 2 g R G T La massa curva lo spazio. La luce segue il cammino più breve nello spazio.
Una stella
Appare in una posizione diversa
1919 GR predition was more or less verified. Il 29 Maggio, l eclisse di Sole consentì l osservazione dell ammasso globulare delle Iadi, la cui luce era deviata dal campo gravitazionale solare New York Times, November 10, 1919
Twin quasars Q0957+56? 1937 Zwicky again hypotesized the phenomenon of gravitational lensing. The effect was observed in 1979 Identical sources (massa, luce, distanza ecc ) discovered in 1979 Gravitational lenses by a galaxy in front of the quasar
Shape of gravitational lenses Einstein ring
Shape of gravitational lenses Elongated lens: Multiple images
Shape of gravitational lenses Multiple o non uniform lenses give images and multiple arches
Gravitational lens RXJ1131-1231 Visible lens Immagine Quasar B Quasar image D Quasar image A Einstein Ring immagine della galassia del quasar Quasar image C Galassia lente (più vicina)
Gravitational lens: invisible matter
1E 0657-56 - Bullet Cluster Credit X-ray: Chandra NASA/CXC/CfA/M.Markevitch et al.; Optical: NASA/STScI; Magellan/U.Arizona/D.Clowe Lensing Map: NASA/STScI; ESO WFI; Magellan/U.Arizona/D.Clowe et al. Scale Image is 7.5 x 5.4 arcmin Distance Estimate About 3.8 billion light years Red: Xray Blue: Gravitational lens Non visible matter (DM) density M. Casolino, INFN & University Roma Tor Vergata
Set upper limit to DM annihilation σ/m 3 10 3 /GeV 3 Exclude MOND (modified Newtonian Dynamics) Dynamical Simulations Abell 520 1E 0657-56 - Bullet Cluster M. Casolino, INFN & University Roma Tor Vergata
Microlensing Una stella viene illuminata da un buco nero di almeno sei masse solari di passaggio davanti ad essa.
Anche per i pianeti extrasolari Microlenti planetarie: Amplificano la luce delle stelle attorno a cui orbitano quando passano di fronte ad esse Dal numero di eventi di microlenti si deduce che pianeti isolati o stelle spente non possono costituire la materia oscura. Anche particelle massive Machos non possono essere candidati plausibili
M. Casolino, INFN & University Roma Tor Vergata
W 1 Visible luminous matter (stars): 0.2% - 0.6% W Barions (H, He, n): 1.6% - 2.4% W Neutrinos: ~ 0.3 10% W Rest of cosmic rays (photons, e - ) ~5% W Dark matter in Galactic Halo: ~10% W Dark Matter in the galaxies: ~30% W
Different approaches to search for Dark Matter PAMELA LHC FERMI Jem-Euso M. Casolino, INFN & University Roma Tor Vergata UNDERGROUND
Underground search
LHC production
Indirect search electron positron
Indirect search proton antiproton
Indirect search gamma gamma
Dark Matter Searches Cosmology Detection, not identification LHC Search Supersymmetry, not necessarily DM 1E 0657-56 - Bullet Cluster Direct Detection Local structure and nature DAMA Indirect Detection Various galactic scales M. Casolino, INFN & University Roma Tor Vergata g: Galactic centre Antiprotons: Galactic average positrons: Local galactic 1kpc
M. Casolino, INFN & University Roma Tor Vergata From Serfass TevPa 2015
Indirect Dark matter search in space
Apj 795 91 2013 ApjL 799 4 2015 2008AdSpR..41..168C 2008AdSpR..41.2037D 2008AdSpR..41.2043C Physics Reports 544, 4, 323-370 Apj 770 2 2013 Science 2011 arxiv:1103.4055 Apj 791 2 2014 Nature, Astrop. Phys ApJ 457, L 103 1996 ApJ 532, 653, 2000 arxiv:0810.4994, PRL, NJP11,105023 Prl 111 1102 203 PrL 106 1101 2011 PrL105 121101 2010 --
Annihilation signal
Discovery of antiprotons in cr, 1979 p/p ratio 6 x 10-4 2-5 GeV From Robert E. Streitmatter Bogomolov, E.A. et al. 1979, Proc. 16th ICRC, Kyoto, 1, 330, A Stratospheric Magnetic Spectrometer Investigation of the Singly Charged Component Spectra and Composition of the Primary and Secondary Cosmic Radiation
Also Golden, 1979 Robert L. Golden
Antimatter Search Wizard Collaboration MASS 1,2 (89,91) TrampSI (93) CAPRICE (94, 97, 98) BESS (93, 95, 97, 98, 2000) Heat (94, 95, 2000) IMAX (96) AMS-01 (1998)
CAPRICE HEAT
1991 astromag on the alpha space station
The PAMELA apparatus Spatial Resolution 2.8 μm bending view 13.1 μm non-bending view MDR from test beam data 1 TV Calorimeter Performances: p/e + selection eff. 90% p rejection factor 10 5 e - rejection factor 10 4 ND p/e separation capabilities >10 above 10 GeV/c, increasing with energy GF ~20.5 cm 2 sr Mass: 470 kg Size: 120x40x45 cm 3 Power Budget: 360 W
AMS
Cosmic ray science in the Hillas Plot Direct e + / e - P / P - Jem-Euso g
Cosmic rays on Galactic scale: Nuclei, protons, antiprotons, isotopes
Antiprotons Secondary production, kinematics well understood Probe for extra sources Galactic scale
Antiproton/proton ratio Low Energy Confirms charge dependent solar modulation High Energy Consistent with models (Galprop, Donato ) Simon et al. (ApJ 499 (1998) 250) Ptuskin et al. ApJ 642 2006 902 Donato et al. (PRL 102 (2009) 071301) PRL. 105, 121101, 2010 PRL 102:051101,2009
Antiproton absolute flux Apparently no extra sources Rule out and strongly constrain many models of DM S M. Asano, et al, Phys. Lett. B 709 (2012) 128. R. Kappl et al, PRD 85 (2012) 123522 M. Garnyet al, JCAP 1204 (2012) 033 D. G. Cerdeno, et al, Nucl. Phys. B 854 (2012) 738
Synchrotron Radiation and Inverse Compton Limit propagation to 1-2 kpc Galactic neighborhood: e+, e- (1-2 kpc)
Pamela positron fraction Charge dependent solar modulation increase over background Nature 458, 607-609 ( 2009) M. Casolino, INFN & University Roma Tor Vergata
Pamela positron fraction: comparison with other data M. Casolino, INFN & University Roma Tor Vergata Nature 458, 607-609 (2 April 2009)
Charge dependent solar modulation L. Maccione, PRL 110 (2013) 081101 AMS & FERMI confirm PAMELA data Anomalous source at high energy Charge dependet Solar modulation at low energy Need 3D model of heliosphere.
Absolute positron spectrum Propagation Charge dependent solar modulation PRL111, 081102 (2013) PRL 111 2013
PRL111, 081102 (2013) Solid - Galprop ApJ M&S 1998 Dot - second. Delahaye, AA 2010 Dash Dot second + astrophys Delahaye, AA 2010 Dash DMatterAnnFinkbeiner JCAP 2011
Secondary production Dark Matter Annihilation Astrophysical sources, SNR M. Casolino, INFN & University Roma Tor Vergata
Electron spectrum GALPROP e- only e - - e+ + e- e + + e - - From E. Mocchiutti
M. Casolino, INFN & University Roma Tor Vergata