The Golden Age of Astropartic l e Physics in the LHC Era Franco Giovannelli INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma, Italy
Outline • Introduction • How High Energy Astrophysics developed and is developing • What about Astroparticle ? • Some of the most important steps on our Knowledge of the physics of the Universe • Dark Matter • What about Neutrinos ? • Prospects • Conclusions
Introduction
All the cosmic sources emit photons and particles which can be detected on the Earth, or in Space or Underground
Mechanisms of γ -ray production (De Angelis, 2008) JHYHJVJHVHGDHJVJHVJB
γ -ray astronomy GLAST (now Fermi) unexplored MeV 10 GeV 1 GeV 1 TeV 10 TeV 100 GeV Atmospheric EGRET Cherenkov telescopes. Whipple, Veritas, HESS, MAGIC,… (Levinson, 2008)
As of 2010 March 25, there are 98 sources known! 38 extragalactic, 60 galactic (Teshima, Paredes, Boller, http://www.mppmu.mpg.de/~rwagner/sources/ Ubertini, Pittori, (see also http://tevcat.uchicago.edu/) Di Sciascio talks) All the identified source classes also exhibit emission in the radio and/or X-ray regime
Primary particle interaction with atmosphere
Multifrequency Observations (possibly Simultaneous) are Fundamental in Photonic Astrophysics & Particle Astrophysics
T = Thermal component NT = Non-thermal component The multifrequency spectrum from radio to γ -ray for a typical massive early-type star • Thermal radio-IR is the free-free radiation of the hot wind. • Thermal X-ray emission is from shocks in the winds. • Non-thermal radio, IR, X-ray and γ -ray emissions are produced by relativistic particles accelerated by the shocks.
Quasars powerfully radiate energy over a very Quasars powerfully radiate energy over a very wide range of wavelengths, indicating that they wide range of wavelengths, indicating that they contain matter with a wide range of temperatures contain matter with a wide range of temperatures Bryce’s talk
Undoubtedly the advent of spacecrafts gave a strong impulse to astronomy; starting roughly from middle '70ies almost all the electromagnetic spectrum was continuously surveyed by the many space experiments. A large amount of excellent-quality data coming from space experiments rendered the data, acquired during many centuries from the ground, only a small fraction of the Golden Age of M Mu ul lt ti if fr re eq qu ue en nc cy y Astrophysics Astrophysics Golden Age of total now available. The GOLDEN AGE of Multifrequency Astrophysics BEGAN (Giovannelli & Sabau-Graziati: 2004, Space Sci. Rev. 112, 1-443; updated from Lena, 1988)
Cosmic Pie HIC SUNT LEONES (Courtesy of Nino Panagia, 2005)
….The Universe manifests not only through electromagnetic radiation but also through astroparticles
Compact astrophysical sources compact central engine → relativistic outflow → emission can be explosive (e.g., Supernovae, GRBs) AGNs; GRBs; Microquasars accreting black hole → relativistic jets → VHE emission ( γ , CR, ν ) Pulsars; Magnetars relativistic wind magnetized → (stripped) → γ -ray emission neutron vacuum gaps star • sources differ in scales and details, but basic physics is very similar (Amir Levinson, 2008)
Direct measurements Cosmic Ray Multifrequency Spectrometers Measurements ( ∆ A = 1 resolution, Air good E resolution) showers Calorimeters (less good resolution) Air-shower arrays on the ground to overcome low flux. Don’t see primaries directly. (Stanev,Erkykin,Petrera, Pallavicini,Mariazzi, Petrukhin,Nir Shaviv, Jones,Blasi,Codino talks) Gaisser, 2005
How High Energy Astrophysics developed and is developing
EMPIRICAL LAW ON THE EMPIRICAL LAW ON THE DIMENSIONS OF EXPERIMENTS DIMENSIONS OF EXPERIMENTS AT DIFFERENT ENERGIES AT DIFFERENT ENERGIES AGILE MAGI C 1 PeV HESS/ VERI TAS 1 0 -4
Agile 10 -11 Argo Crab Glast Sensitivity [ TeV/cm 2 s ] Hawc 10 -12 Magic2 10% Crab Magic Hess/Veritas 10 -13 1 mCrab C T A Sensitivity 1% Crab 10 -14 10 4 10 5 10 100 1000 E [GeV]
~3000 sources by GLAST, AGILE ~1000 sources by CTA (Bartko, 2007)
LHC can be considered as the eighth-wonder of the world (Arno Straessner’s talk)
LHC Investigation Fields � Dark Energy (Bisnovatyi-Kogan talk) � Dark Matter (Bernabei, Regis, Bruno, Bossi talks) � Extra Dimensions (Auriemma talk) � Higgs � Supersymmetry LHC is the vessel sailing the Dark Energy and Dark Matter unknown oceans
Connecting the LHC and the Universe: towards the origin ATLAS, CMS ALICE, CMS… ALIC 13.8 Billion E,C years MS 23 D. Denegri; Vulcano, May 2006,
LHC is a complementary tool for HE observatories looking directly to the Universe � LHC is probably the highest and ultimately active-physics technological wonder, difficult to be outdated because of dimensions and costs. � Probably in the next decades it will be cheaper to develop more sensitive passive-physics ground-based experiments, and even if space-based or Moon-based.
Some of the most important steps on our Knowledge of the physics of the Universe (biased by my knowledge and feelings)
Cosmology and Background in the Universe (Colafrancesco, Panagia, Della Valle, Sanchez talks)
Ω B h 2 u 0.023/0.020 (Netterfield et al., 2001) Ω B h 2 u 0.021 (de Bernardis et al., 2000) BB T = 2.74 K (Srianand, et al.: 2001, Nature 408, 931). The point at z=0 is the result of COBE (T CMBR (0) = 2.726 ! 0.010 K). At z=2.1394 there is an upper limit. At z=2.33771: 6.0 K < T CMBR (2.34) < 14.0 K (vertical bar). • The dashed line is the prediction from the hot Big Bang: T CMBR =T CMBR (0) $ (1+z) ; [T CMBR (2.34)=9.1 K]
1TeV VHE γ -rays Energy (eV) γ -rays (Ressell & Turner, 1990) X-rays Visible IRB DEBRA CMB Radio Flux
BOOMERanG RESULTS (de Bernardis et al., 2000)
Schuecker et al. 2003, 2004 REFLEX cosmological constraints (ESO-PR June 2004) Ω Λ Ω M
Hubble Constant
The “ultimate” Hubble constant • H 0 = 62 ± 1 ± 5 km s -1 Mpc -1 Sandage et al. • H 0 = 72 ± 3 ± 7 km s -1 Mpc -1 Freedman et al. • H 0 = 64 ± 1 ± 5 km s -1 Mpc -1 is a compromise that the Universe could take! Could you? (Courtesy of Nino Panagia)
Clusters of Galaxies
HARD X-RAY EXCESS IN COMA CLUSTER (BeppoSAX Measurements) (Fusco Femiano et al.: 1999, Ap.J. Letters 513 , L21)
3EG J1337+5029/Abell 1758A F (E > 100 MeV) } [S (1.4 GHz) ] 0.19 ! 0.09 A 1758A L γ } L X 0.19 ! 0.09 EGRET Image + ROSAT-HRI contour ( Colafrancesco : 2002, A&A 396 , 31)
(Schindler, 2005) Metallicities in the ICM Peterson et al. 03 XMM The amount of metals in the ICM is at least as high as the sum of the metals in all galaxies a lot of gas must have been transported from galaxies into the ICM
Galactic Winds SUBARU Telescope, NAO, Japan (Schindler, 2005)
UNIFIED MODEL FOR COMPACT SOURCES
AGNs & GALACTIC COLLAPSED OBJECTS: AGNs & GALACTIC COLLAPSED OBJECTS: UNIFIED SCHEME UNIFIED SCHEME • THE MAIN IDEA (now very popular): ENGINE PRODUCING HIGH ENERGY RADIATION IS OF THE SAME KIND FOR ALL EXTRAGALACTIC EMITTERS (Giovannelli & Polcaro, 1986). • DIFFERENCES IN MASS AND MASS ACCRETION RATES u ANALOGY CAN BE EXTENDED UNTIL GALACTIC BLACK HOLES. THE EMISSION OF EXTRAGALACTIC X-RAY SOURCES IS: • L TOT = L NUC + L HGC L NUC = TOTAL NUCLEAR LUMINOSITY L HGC = HOST GALAXY COMPONENT (from discrete sources)
z = 6.1 10 9 yr after Big Bang 10 m Keck image of QSO J 1148+5251
QSO J 1148+5251 Expected (2 KeV) L x ~ 7 x 10 47 erg s -1 Giovannelli & Polcaro, 1986, MNRAS 222, 619-627
Absorption of γ -ray in the Universe (De Lotto talk)
Absorption of γ -Rays in the Universe Pair creation: γ＋γ � e + + e - BL Lac objects 4.5 PKS2005 PG1553 4.0 Spectral Index 3.5 3.0 2.5 2.0 1.5 0 0.1 0.2 0.3 0.4 Redshift Parameter z
Jets • Multifrequency Coordinated Observations allow to solve: • Morphology of the jet. • The physical processes occurring inside. (Chechetkin, Kundt talks)
Crab Nebula (Chandra ) X-Ray Jet in the Radio Galaxy Pictor A Vela Pulsar (Chandra ) Cygnus A (Chandra) HH (Chandra) Cen A (Chandra)
(Levinson, 2008)
Proton Jet Reactions (Andreas Mü üller, 2002) ller, 2002) (Andreas M
(Bednarek, Giovannelli, Karakula & Tkaczyk, 1990, A&A 236 , 268)
GAMMA-RAY BURSTS (Hurley, Connaughton, Amati, Makoto, Saavedra talks)
The (long) GRB redshift distribution Swift afterglows are faint Significantly larger redshift than Courtest of Malesani previous missions 〈 z 〉 = 2.8 vs 〈 z 〉 = 1.6 GRBs are thus ideal probes of the high- redshift Universe (Malesani, 2009)
SN GRBs are believed to be detectable out to very high redshifts up to z ~ 25 (the first stars: Lamb & Reichart 2000; Ciardi & Loeb 2000; Bromm & Loeb 2002). SNe Ia are detected only at redshifts of z ~ 1.7. (Credit: Dai Zigao, Nanjing University )
BeppoSAX GRB X-ray Afterglow of the GRB 970228 (Costa et al., 1999)
Recommend
More recommend
