The Golden Age of Astropartic l e Physics in the LHC Era Franco - - PowerPoint PPT Presentation

The Golden Age of Astroparticle 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
• n 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,

• r in Space or

Underground

JHYHJVJHVHGDHJVJHVJB

Mechanisms of γ-ray production

(De Angelis, 2008)

γ-ray astronomy

MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV EGRET GLAST (now Fermi) Atmospheric Cherenkov telescopes. Whipple, Veritas, HESS, MAGIC,… unexplored

(Levinson, 2008)

http://www.mppmu.mpg.de/~rwagner/sources/ (see also http://tevcat.uchicago.edu/)

As of 2010 March 25, there are 98 sources known! 38 extragalactic, 60 galactic

All the identified source classes also exhibit emission in the radio and/or X-ray regime

(Teshima, Paredes, Boller, Ubertini, Pittori, Di Sciascio talks)

Primary particle interaction with atmosphere

Multifrequency Observations

(possibly Simultaneous)

are Fundamental

in

Photonic Astrophysics

&

Particle Astrophysics

The multifrequency spectrum from radio to γ-ray for a typical massive early-type star

T = Thermal component NT = Non-thermal component

• 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 total now available.

The GOLDEN AGE

• f

Multifrequency Astrophysics BEGAN

(Giovannelli & Sabau-Graziati: 2004, Space Sci. Rev. 112, 1-443; updated from Lena, 1988)

Golden Age of Golden Age of M Mu ul lt ti if fr re eq qu ue en nc cy y Astrophysics Astrophysics

Cosmic Pie

(Courtesy of Nino Panagia, 2005)

HIC SUNT LEONES

….The Universe manifests not only through electromagnetic radiation but also through astroparticles

Compact astrophysical sources

AGNs; GRBs; Microquasars accreting black hole → relativistic jets → VHE emission (γ, CR, ν)

compact central engine → relativistic outflow → emission

can be explosive (e.g., Supernovae, GRBs)

• sources differ in scales and details,

but basic physics is very similar

Pulsars; Magnetars relativistic wind (stripped) vacuum gaps magnetized neutron star → γ-ray emission

→

(Amir Levinson, 2008)

Spectrometers (∆A = 1 resolution, good E resolution) Calorimeters (less good resolution)

Direct measurements Air showers

Air-shower arrays

• n the ground to
• vercome low flux.

Don’t see primaries directly.

Gaisser, 2005

Cosmic Ray Multifrequency Measurements

(Stanev,Erkykin,Petrera, Pallavicini,Mariazzi, Petrukhin,Nir Shaviv, Jones,Blasi,Codino talks)

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

1 0 -4

1 PeV MAGI C HESS/ VERI TAS AGILE

10-14 10-13 10-12 10-11 10 100 1000 104 105 E [GeV]

Crab 10% Crab 1% Crab

Glast Magic Magic2

Sensitivity [ TeV/cm2s ]

Agile

C T A

Argo Hawc Hess/Veritas

1 mCrab Sensitivity

~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)

Dark Energy (Bisnovatyi-Kogan talk) Dark Matter (Bernabei, Regis, Bruno, Bossi talks) Extra Dimensions (Auriemma talk) Higgs Supersymmetry

LHC Investigation Fields

LHC is the vessel sailing the Dark Energy and Dark Matter unknown oceans

• D. Denegri; Vulcano, May 2006,

23

Connecting the LHC and the Universe: towards the origin

ALIC E,C MS

ALICE, CMS… ATLAS, CMS

13.8 Billion years

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

• n 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)

The point at z=0 is the result of COBE (TCMBR(0) = 2.726 ! 0.010 K). At z=2.1394 there is an upper limit. At z=2.33771: 6.0 K < TCMBR(2.34) < 14.0 K (vertical bar).

• The dashed line is the prediction from the hot Big Bang:

TCMBR=TCMBR(0)$(1+z) ; [TCMBR(2.34)=9.1 K]

(Srianand, et al.: 2001, Nature 408, 931).

ΩBh2 u 0.023/0.020

(Netterfield et al., 2001)

ΩBh2 u 0.021

(de Bernardis et al., 2000)

BB T = 2.74 K

Energy (eV)

Radio CMB

Visible γ-rays

Flux

IRB

(Ressell & Turner, 1990)

X-rays VHE γ-rays

1TeV

DEBRA

BOOMERanG RESULTS

(de Bernardis et al., 2000)

Schuecker et al. 2003, 2004 REFLEX cosmological constraints (ESO-PR June 2004)

ΩΛ ΩM

Hubble Constant

The “ultimate” Hubble constant

• H0 = 62 ± 1 ± 5 km s-1 Mpc-1

Sandage et al.

• H0 = 72 ± 3 ± 7 km s-1 Mpc-1

Freedman et al.

• H0 = 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

EGRET Image + ROSAT-HRI contour

A 1758A

(Colafrancesco: 2002, A&A 396, 31)

F (E > 100 MeV) } [S(1.4 GHz)]0.19 ! 0.09 Lγ } LX

0.19 ! 0.09

Peterson et al. 03 XMM

Metallicities in the ICM

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

(Schindler, 2005)

Galactic Winds

(Schindler, 2005)

SUBARU Telescope, NAO, Japan

UNIFIED MODEL FOR COMPACT SOURCES

• 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.

AGNs & GALACTIC COLLAPSED OBJECTS: AGNs & GALACTIC COLLAPSED OBJECTS: UNIFIED SCHEME UNIFIED SCHEME

• THE EMISSION OF EXTRAGALACTIC X-RAY SOURCES IS:

LTOT = LNUC + LHGC LNUC = TOTAL NUCLEAR LUMINOSITY LHGC = HOST GALAXY COMPONENT (from discrete sources)

z = 6.1

10 m Keck image of QSO J 1148+5251

109 yr after Big Bang

Giovannelli & Polcaro, 1986, MNRAS 222, 619-627

QSO J 1148+5251

Expected (2 KeV) Lx ~ 7 x 1047 erg s-1

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

1.5 2.0 2.5 3.0 3.5 4.0 4.5 0.1 0.2 0.3 0.4

Redshift Parameter z

Spectral Index

PKS2005 PG1553

Jets

• Multifrequency Coordinated

Observations allow to solve:

• Morphology of the jet.
• The physical processes occurring inside.

(Chechetkin, Kundt talks)

X-Ray Jet in the Radio Galaxy Pictor A

Crab Nebula (Chandra) Vela Pulsar (Chandra) Cygnus A (Chandra) Cen A (Chandra) HH (Chandra)

(Levinson, 2008)

Proton Jet Reactions

(Andreas M (Andreas Mü üller, 2002) ller, 2002)

(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 previous missions 〈z 〉 = 2.8 vs 〈z 〉 =1.6 GRBs are thus ideal probes of the high- redshift Universe

Courtest of Malesani

(Malesani, 2009)

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.

SN

(Credit: Dai Zigao, Nanjing University)

BeppoSAX GRB X-ray Afterglow

• f the GRB 970228 (Costa et al., 1999)

Optical light curve

log (T) log (F) 10-100 s 0.01 d 2d 10d 100d

Prompt emission Afterglow Jet break (Afterglow) Supernovae appearance Host galaxy (Pozanenko, 2009)

Chronicle of the Galaxy

The first H-R diagram constructed with measured distances (HIPPARCOS)

Nuclear Astrophysics

(Giora Shaviv, Gustavino talks)

Laboratory Underground Nuclear Astrophysics

Measurements of nuclear cross sections of interest in BBN with the LUNA experiment

Carlo Gustavino (2006)

For the LUNA collaboration

• BBN and the “Precision Cosmology” Epoch
• The LUNA experiment
• P(D,γ)3He
• 3He(D,p)4He
• 3He(4He,γ)7Be In progress!!
• D(4He,γ)6Li
• Conclusions

50 kV accelerator 400 kV accelerator

σ(E)=S(E)/E e–2πη

2πη = 31.29 Ζ1Ζ2 √µ/Εcm µ = m1m2 / (m1+m2)

Astrophysical Factor Gamow Factor

• Very low cross sections because of the coulomb barrier

UG experiments to reduce the background due to cosmic ray

N.B. differently from stars, in BBN we don’t have a fixed T (Gamow peak), although there is a kinetic equilibrium

Why underground Measurements?

S(0) = 5.32 MeV barn

σmin= 0.02 pb 2 events/month !

• J. Bachall: “Historical breakthrough”

Magnetars

(von Kienlin, Kanbach talks)

AXP Discovery P[s] B[1014 G]

Persistent 1E2259+586 (SNR) 1981 6.98 0.6 1E1048.1-594 1985 6.45 5.0 4U 0142+61 1993 8.69 1.3 1RXS J1708-4009 1997 11.00 4.6 1E1841-045 (SNR) 1997 11.77 7.1 CXOU J0110-721 (SMC) 2002 8.02 3.9 CXOU J164710.2-455216 2005 10.61 < 3.0 (Westerlund 1) Transient AX J1845-026 (?) 1998 6.97 ? XTE J1810-197 2003 5.54 2.6

Durant et al. 2 0 0 6

(Kuiper, 2007)

10 m: acceleration zone 1015 Gauss

Quark Stars ?

(Courtesy of Todor Stanev)

(Giovannelli & Sabau (Giovannelli & Sabau-

• Graziati, 2007)

Graziati, 2007)

Cataclysmic Variables

Gravitational Radiation Magnetic Braking Polars Intermediate Polars SW Sextantis Systems

ORBITAL PERIOD DISTRIBUTION

• f Cataclysmic Variables

(Rodriguez-Gil, P.: 2003, Ph.D. Thesis, La Laguna University, Spain)

CVs falled into oblivion CVs falled into oblivion ….But… at beginning of 1990-ies TeV TeV emissions emissions have been detected from the Intermediate Intermediate Polar AE Polar AE Aqr Aqr and the Polar AM Her

(These measurements were never confirmed...but then they triggered the new interest for CVs)

It is impressive how many (magnetic or not) CVs are detected by INTEGRAL (see also Barlow et al. 2006 Barlow et al. 2006):

• 23

23 (out of ~300 objects, i.e. ~8%) in the 3rd IBIS survey;

• ~

~12% 12% of optical identifications (9 out of 78 cases).

(Masetti, 2007)

(Tsuru, 2008)

AE Aqr AE Aqr SUZAKU also has measured emission from AE Aqr

X-Ray Pulsars

(Zdziarski, Ziolkowski talks)

A powerful application of the multifrequency approach: the study of the X-ray/Be systems

(started with long term monitoring of A0535+26/HDE245770 (Flavia’ star)

X-ray Flux Intensity (Crab Unit)

0.001 0.01 1 28 Apr-1 May 1975 7-11Nov 1975 24 May 1977 3 Dec 1977 0.1 1 Jun1975 1 Jul 1977 9 Jan 1978 10-15 Dec 1977

Detected X-ray Outburst 8 Dec 1977 - 3 Jan 1978

X-ray measurements Predicted measurements

Upper limits

A0535+26/HDE 245770

How the optical counterpart was discovered

Time Optical Measurements (Giovannelli, 2005)

Narrow absorption components at ∼ -350 km/s indicate “puffs” of material expelled by the star.

C IV (1548 Å) C IV (1548 Å) C IV (1548 Å) C IV (1548 Å)

HDE 245770: IUE High Resolution Short Wavelengths Spectra

(Guarnieri et al.: 1985, in Multifrequency Behaviour of Galactic Accreting Sources,

• F. Giovannelli (ed.), p. 318-325

05 Dec 1981 = JD 2444944 is 13 orbital cycles after 20 Dec 1977 = JD 2443498

A telegram to HAKUCHO- Team triggered the X-ray measurements with the detection of the 13 Dec X-ray short outburst

(Nagase, F. et al.: 1982, ApJ 263, 814). 4522 1.5 Crab 4537 big outb.

September 1983 – April 1984 X-ray – UBVRIH Campaign

(Giovannelli F. et al.: 1984, in X-ray Astronomy ’84, ISAS, Meguro-ku, Tokyo, Japan, p. 205) & (Giovannelli F. & Sabau-Graziati L.: 1992, Space Sci. Rev. 59, 1-81)

T = 1 Orbital Period Toutb-opt = 3 Oct 1983 = JD 2445611 6 Orbits after 5 Dec 1981 Outburst Toutb-X = 1 – 18 Oct 1983 Ix max ∼ 8 days delay with respect to max optical outburst

HeI (5875 Å) Hβ HeI (5015 Å) Hγ 19 March 2010 (MJD 2455275)

87.18 cycles after 3 Oct 1983 opt. outb. 93.19 cycles after 5 Dec 1981 opt. Outb. 114.93 cycles after 1 May 1975 X-ray

• utburst. Supposing opt. outburst 8 days

before, we obtain 115.00 cycles!!!

(Giovannelli, F., Gualandi, R., & Sabau-Graziati, L.: 2010, ATel # 2497)

Strong optical activity

EXTREMELY IMPORTANT

• On the basis of such a strong optical

activity – especially Hγ in emission – we PREDICTED (Giovannelli, Gualandi &

Sabau-Graziati: 2010, ATel # 2497) the

incoming X-ray outburst, which actually occurred (Caballero, I. et al.:

2010, ATel # 2541). The intensity

reached 1.18 Crab on April 3, 2010 in the range 15–50 keV of BAT/SWIFT

55253.6

93 Porb after 5 Dec ‘81 optical outburst

5275.29 = 19 March 2010, 19 UT Strong Optical Activity: Hγ in emission

(Giovannelli, F., Gualandi, R., & Sabau-Graziati, L.: 2010, ATel # 2497)

No Optical Data

i) Normal outburst Be: “quiet” Periastron Passage ~ 0.1-0.5 Crab ii) Noisy (Anomalous)

• utburst

Be: “puffs” ~ 0.5- á 1 Crab iii) Casual outburst > 1 Crab Be: “shell”

A0535+26 - e = 0.47

Dark Matter

Covering the whole e.m. spectrum

Synchrotron S Z E f f e c t I C S Brem.+ICS+π0 Brem.+ICS ICS

χχ

annihilation products

(courtesy of Sergio Colafrancesco, 2006)

Galactic Center Galactic Center

Distance (7.5 kpc) GC best candidate for indirect DM searches ?

• other γ-ray sources in the FOV, i.e. SNR Sgr A East
• competing plausible scenarios

BUT:

• halo core radius: extended vs point-like

Highest DM density candidate Close by Not extended

Targets for DM search

H.E.S.S.

(Dogiel, Aschenbach talks)

What about neutrinos ?

(Grieder, Montaruli, Aguilar-Sanchez, Jollet-Meregaglia, Katz, Sisti, Yusuke, Fargion, Ludhova, Vissani talks)

Conditions required for production of high energy neutrinos in astrophysical sources:

• Acceleration of charged particles

(protons or nuclei) to high energies E > 1015 eV

• Accelerated particles should lose

energy through pion production or neutron decay Obey gamma-ray and neutrino flux limits

1 > ⋅ ⋅

pB B

n R σ

(Semikoz, 2004) (Semikoz, 2004)

Neutrinos from pion production

µ µ

ν ν µ ν µ π + + ⇒ + ⇒

± ± ± ± e

e

...

'

+ ⇒ + + ⇒ +

∑ ∑

i b i b

P P N N π π γ

p n

γ π 2

0 ⇒

e

e p n ν + + ⇒

−

Conclusion: photon and neutrino fluxes are connected in well- defined way. If we know one of them we can predict other:

tot tot

E E

ν γ

~

(Semikoz, 2004) (Semikoz, 2004)

• Diffuse fluxes

– Neutrinos from UHECR – Neutrinos from AGN

• Most probable point-like neutrino sources

– AGN – Galaxy center – Microquasars – SuperNova high energy E > TeV neutrinos – GRB

Sources of Neutrinos

The Neutrino Telescope World Map

ANTARES + NEMO + NESTOR join their efforts to prepare a km3-scale neutrino telescope in the Mediterranean KM3NeT Design Study

• Neutrinos would (and will) provide very valuable

astrophysical information, complementary to photons and charged cosmic rays

• Exploiting the potential of neutrino astronomy

requires cubic-kilometre scale neutrino telescopes providing full sky coverage

• The KM3NeT detector in the Mediterranean

Sea will complement IceCube in its field of view and exceed its sensitivity by a substantial factor

• They are working towards a start of

construction by 2011

Photonic Astrophysics Particle Astrophysics

Astroparticle Physics

Neutrino Astrophysics

PROSPECTS

Energy versus time for X and Gamma ray detectors

Fermi Fermi

GeV | TeV | PeV | EeV | ZeV |

Direct detection Balloons & Satellites Indirect detection (EAS) [arrays & florescence] High Z [ENTICE, ECCO] Antiparticles and Antinuclei [BESS,PAMELA,AMS Elemental Composition [CREAM, ATIC, BEAR, ACCESS?, NUCLEON?, INCA?, PROTON-5? Extreme Energy CR [AUGER, EUSO, TUS, KLYPVE?, OWL??] Light elements and Isotopes [ACE] (Spillantini, 2008)

(Santangelo talk)

OPERA: OPERA: O Oscillation scillation P Project roject with with E Emulsion mulsion t tR Racking acking A Apparatus pparatus

732 km

ν

OPERA Detector

As of October 3, 2008 OPERA registered 728 candidate interactions in the brick (basic unite of experiment)

Waiting for τ registration…

The OPERA experiment aims at the direct observation of νµ → ντ oscillations in the CNGS (CERN Neutrinos to Gran Sasso) neutrino beam produced at CERN. Since the νe contamination in the CNGS beam is low, OPERA is also able to study the sub-dominant oscillation channel νµ → νe

(Chukanov, 2008)

We can affirm that since roughly 1990-ies we entered in

The GOLDEN AGE of ASTROPARTICLE PHYSICS

To which we directly contributed with

• ur Workshops in Vulcano, since 1984:

Frascati Workshops Multifrequency Behaviour of High Energy Cosmic Sources Vulcano Workshops Frontier Objects in Astrophysics and Particle Physics

Many Thanks for Your Attention