Astroparticle and Gravitational

Physics

G. Cella – INFN sez. Pisa

Fisica 2011-2020 Congressino di Dipartimento

Lunedì 11 aprile 2011

An interdisciplinary field…

Astroparticle Physics - Science

• High Energy Rays

• Neutrino Mass

• High Energy Cosmic Rays

• High Energy Cosmic Neutrinos

• Dark Matter direct detection

• Gravitational Waves

• Low Energy Neutrinos & Proton decay

Cosmic rays

(and other exuberant

things)

Cosmic rays Protons, light nuclei

Astrophysical origin

Acceleration mechanisms

Unique below 1020 eV?

UVHE: Engine? GZK?

Spectrum?

Lower energies:

Galactic

Isotropic

High flux SMALL DETECTORS

High energies:

Extragalactic

Directional

Low flux BIG DETECTORS

direct

indirect

AMS: the Alpha Magnetic Spectrometer at ISS

Ams: perspectives

cosmic rays spectroscopy

antimatter search

dark matter indirect search

PAMELA e+ excess

gamma astrophysics

Will operate until 2020 and beyond (with

permanent magnet):

Precise & simultaneous measurement

of rates and spectra of the different

components of CR in GeV-TeV range

Main step forward in the tuning of

models for CR propagation

The multi-messenger approach (I)

A leit-motiv:

Simultaneous study of different channels leads to a better understanding

• Charged CR preserve some directionality only above 4x1019 eV

•

• Directional

• Easy to detect

• Not completely clear origin: p or e?

•

• Directional

• Difficult to detect

• Origin: p

FERMI: a -ray space telescope

LAT: 20MeV-300GeV

GBM: 8KeV-40MeV (12 NaI + 2

BGO detectors)

Huge field of view:

30' every direction

full sky in 3 hours

5-10 years lifetime • 30 times more sensitive than

any previous

• Can precisely measure cosmic e+ and e- spectra up to a TeV

FERMI: some results

Detection of LMC, SNR, starbust galaxies

Constraints on Dark Matter models (EGRET excess excluded)

GRB, flares, transients

………

ray sky catalog

1400 sources > 100 MeV

Known and unidentified

New sources

Pulsar catalog

60 gamma PSR

First population study

Emission far from surface

• Very successful experiment

• Will last very probably for 10 years

• Phenomenological and theoretical activities here in Pisa

FERMI: some results

Detection of LMC, SNR, starbust galaxies

Constraints on Dark Matter models (EGRET excess excluded)

GRB, flares, transients

………

ray sky catalog

1400 sources > 100 MeV

Known and unidentified

New sources

Pulsar catalog

60 gamma PSR

First population study

Emission far from surface

• Very successful experiment

• Will last very probably for 10 years

• Phenomenological and theoretical activities here in Pisa

MAGIC: an Imaging Air Cherenkov Technique

telescope

few ns flashes of light

mirror surface of 240 square metres

camera with O(100) photomultipliers

energy resolution: 30% or better

Very high energy gamma

astronomy (10GeV-10TeV)

AGN: production in the jet,

near the BH

Supernova remnants

Lower energy unidentified

sources

GRB

Cosmology & fundamental

physics

MAGIC: detection principle

Imaging Air Cherenkov Technique

Background rejection

Energy reconstruction

Direction reconstruction

Image reconstruction for

extended sources ( > 0.1 degrees)

Results and perspectives

Four new VHE galactic sources found

First detection of pulsed emission from a

ground based telescope (Crab)

Correlations between gamma and X emissions

(MWL campaign)

Extragalactic VHE sources

Suggestions for an higher transparency of

the universe than expected from EBL

Goals:

lower the threshold to 30GeV (or less)

Increase detection area

New light-to-electron conversion

techniques

Benefits: fundamental & exotic

physics, astrophysics, sinergy with

satellite detectors, MWL campaigns

Cherenkov Telescope Array

(start 2013)?

CALorimetric Electron Telescope (CALET)

Fill the gap between satellite/balloon & ground experiments

Launch foreseen 2013, 5 year mission

Neutrinos

(and other shy things)

ANTARES: a deep sea neutrino telescope Scientific goals:

Disentangle Synchrotron-Inverse Compton from Hadronic production in SNRs

Study Binary systems, µQuasars

Investigate the very high energy processes occurring in GRBs

Search for Dark matter

57

m

45°

Final configuration since 2008

KM3NeT: multi-cubic-kilometre Cherenkov

telescope for high energy neutrinos Deep-sea research infrastructure in the

Mediterranean Sea.

• multi-km3 Cherenkov telescope for neutrinos with E>100 GeV.

• Complementary to ICECUBE

• Construction can start in 2012, depending on fundings

KM3NeT in numbers

(full detector)

• ~300 DU

• 20 storey/DU

• ~ 40m storey spacing

• ~1 km DU height

• ~180m DU distance

• ~ 5 km3 volume

Main physics goals

Origin of Cosmic Rays and Astrophysical sources

Galactic Candidate Sources (SNRs, Fermi Bubbles, quasar,…)

Extragalactic Candidate Sources (AGN, GRB, …)

Telescope optimisation: “point sources” energy range 1 TeV-1 PeV

Implementation requirements

Construction time ≤5 years

Operation over at least 10 years without “major maintenance”

Builds on the experience gained with ANTARES, NEMO and NESTOR

Gravitational waves

(and other invisible things)

Linearized equation: wave equation

Matter tells the spacetime how to curve, and curved space tells to matter how to move

(J. Wheeler)

Nonlinear equation, difficult to solve in the general case

Gravitational waves

From: M. Pössel, " The wave nature of simple gravitational waves " in: Einstein Online Vol. 2 (2006), 1008

VIRGO: an interferometric detector of

gravitational waves

Goals:

Challenges:

Gravitational wave detectors network

The multimessenger approach (II) Candidates

Signatures

Advantages

GW+HEN:

Negligible absorption

travel cosmological

distances

No deflection by magnetic fields

tracing back feasible

Weakly interacting

Can escape from dense

object

Agreement with ANTARES

Results/perspectives

No detections until now

Several interesting upper limits

Advanced detectors in the near

future

Timeline

Gravitation

Precision tests of General Relativity

PN effects

Exotic physics

Lense

Thirring

G-Gran Sasso: design study

GG: test of equivalence principle <10-17

• Violation signal is modulated

• Satellite in rotation (T=1s)

• Thermal effects reduced

Orbit as low as possible: h=600km

Laser readout

Conclusions

Astroparticle physics:

a rapidly growing field

• Dramatically increasing sensitivities

• Very probably at the threshold for new discoveries

• International collaborations required

Interdisciplinary field

• Technological aspects

• Numerical computations

• Experimental techniques

European community recommendation encourage developements.

Funding agencies add a question mark.

KM3NET CTA

AUGER-N

ET

1 ton mass Megaton

p Decay +

1 ton DM

Contacts AMS:

http://www.pi.infn.it/ams/Group.html

Gabriele Bigongiari, Franco Cervelli, Stefano Di Falco , Giovanni Gallucci, Marco Incagli, Federico Pilo, Valerio Vagelli.

FERMI/GLAST: http://glast.pi.infn.it/

Luca Baldini, Ronaldo Bellazzini, Johan Bregeon, Alessandro Brez, Marco Ceccanti, Michael Kuss, Luca Latronico, Marco Maria Massai, Massimo Minuti, Nicola Omodei, Melissa Pesce-Rollins, Michele Pinchera, Massimiliano Razzano, Carmelo Sgrò, Gloria Spandre.

MAGIC: http://www.pi.infn.it/magic/

Pedro Antoranz, Massimilano Bitossi, Roberto Cecchi, Paolo Da Vela, Elvira Leonardo, Mario Meucci, Vincenzo Millucci, Jose Miguel Miranda, Ricardo Padrino, Riccardo Paoletti, Serena Partini, Pier Giorgio Prada Moroni, Steve N. Shore, Antonio Stamerra, Diego Tescaro

CALET:

Pier Simone Marrocchesi

ANTARES: http://www.pi.infn.it/antares/

Armando Bigi,Vincenzo Cavasinni, Vincenzo Flaminio, Stefano Galeotti, Dario Grasso, Mauro Morganti, Giuseppe Terreni.

KM3NET: http://www.km3net.org/home.php

Bachir Bouhadef, Vincenzo Flaminio, Enrico Maccioni, Antonio Marinelli, Mauro Morganti, Fabio Stefani

VIRGO: http://www.ego-gw.it/

Balestri G., Basti A., Bitossi M., Boschi V., Bradaschia C., Cella G., Di Lieto A., Di Virgilio A., Ferrante I., Fidecaro F., Frasconi F., Gennai A., Giazotto A., Magazzu’ C., Mantovani M., Paoletti F., Paoletti R., Passaquieti R., Passuello D., Poggiani R., Toncelli A., Tonelli M., Torre O., Vajente G.

GG: http://eotvos.dm.unipi.it/

M. L. Chiolafo, F. Maccarrone , G. Mengali, A.M. Nobili, P. Paolicchi, R. Pegna , E. Polacco,T.R. Saravanan, F. Pegoraro.

G-Gran Sasso DS: http://www.df.unipi.it/~carelli/ricerca/giro.html

Maria Allegrini, Filippo Bosi, Jacopo Belfi, Niccolò Beverini, Giorgio Carelli, Giancarlo Cella , Angela Di Virgilio, Isidoro Ferrante, Enrico Maccioni, Flavio Stefani

Extra slides

AMS: the Alpha Magnetic Spectrometer on the

ISS

TRD

TOF

TOF

MG TR

ACC AST

RICH

EMC

e/p separation 3D tracking

charged particles trigger time direction beta measurement Z measurement (dE/dx)

B=0.86 dipolar field rigidity up to 2-3 TeV 3D tracking Z separation (dE/dx) veto eff. > 99.99%.

beta measurement Z separation upgoing particle rejection Isotopes separation (with TR)

energy measurement e/h separation e.m. Showers trigger 3D imaging

CR factories

Max Energy:

Magnetic field

intensity

Size of accelerating

region

LHC

GZK limit Scattering on cosmological photons

PAMELA e+ excess

D. Grasso (Pisa); D. Gaggero (Pisa, Ph.D. stud.); L. Maccione (DESY); G. Di Bernardo (Goteborg); C. Evoli (SISSA)

FERMI: detection principle

LAT: pair conversion telescope

precision converter/tracker

16 tungsten foils

16 X-Y alternated silicon

strips detectors

Calorimeter (caesium iodide)

measure shower energy &

shower profile

plastic segmented anti-coincidence

detector

DAQ

4x4 array

GBM: burst monitor

Scintillators:

• 12 NaI (8kEV-1MeV)

• 2 Bismuth-Germanate

(150keV-30MeV)

Recent works on CR physics D. Grasso (Pisa); D. Gaggero (Pisa, Ph.D. stud.); L. Maccione (DESY); G. Di Bernardo (Goteborg); C. Evoli (SISSA)

Provided the first combined interpretations of the Fermi-LAT

electron spectrum and the positron fraction measured by PAMELA

in terms of pulsar or DM annihilation.

Astropart.Phys.32:140-151,2009; Phys.Rev.D82:092004,2010;

Astropart.Phys.34:528-538,2011

Developed and tested a new CR propagation package (DRAGON),

alternative to GALPROP, and interfaced it with DARKSUSY so to

treat the prop. of DM annihilation/decay products consistently.

DRAGON is built to consistently model also the γ-ray and neutrino

diffuse emission. JCAP 0810:018,2008; http://www.desy.de/~maccione/DRAGON/

Improved the constraints on CR propagation models by using CREAM

light nuclei and PAMELA antiproton data (first combined analysis). Astropart.Phys.34:274-283,2010

Work in progress & future plans

We are using DRAGON to derive new

constraints on DM and astrophysical

models on the basis of PAMELA antiproton

data and estimate the projected AMS-02

sensitivity (in collaboration with SISSA

DM group).

We are studying the PAMELA and Fermi-

LAT new measurements in the lepton

sector and estimate the expected AMS-02

capability to discriminate different

interpretations of those results. This is

also relevant for the CALET project.

We are modeling the diffuse γ-ray

emission of the Galaxy consistently with CR

data and propose a new interpretation of

the puzzling longitude profile of the γ-ray

emissivity of the Galaxy observed by

Fermi-LAT (gradient problem).

Markov chain MC comparison of

astrophysical/DM models and AMS-02

multichannel data. Study the implications

for the fundamental physics accounting also

for LHC results.

Consistent modeling of the diffuse γ-ray

(Fermi-LAT) and the synchrotron (PLANCK)

emission of the Galaxy. Features in their

spectral and angular distributions may

confirm the presence of new CR components

and help identifying their sources. This is

also useful to model the CMB foreground.

Use PLANCK results and CR electron models to

improve our knowledge of the Galactic

magnetic field. It will help modeling UHECR

deflections which is crucial to better

identify UHECR sources and composition

(relevant for AUGER).

ANTARES: detection principle

Basic idea: select

secondary

generated

inside the

earth

Detector:

12 detection lines

75 10'' PMTs/line

V separation: 14.5m (upper PMT depth 100m)

H separation: 60-70m

Data transfer: optical fibers

LED beacons for calibration

Environmental monitoring: T,P,salinity, light attenuation, speed of sound

Results and perspectives

ANTARES infrastructure completed:

Largest neutrino telescope in the Northern hemisphere

Operating smoothly, maintenance capability proven

Understanding of detector and data analysis progressing

Exciting physics program in

progress….

Unexplored regions of

sensitivity in southern

hemisphere

Steady/transient sources,

monopoles, DM, oscillations ……

2009-2010 data coming soon

Multi-messenger programs

established (optical, satellite,

GW)

KM3NET: sensitivity window

0%

100 %

VIRGO: detection principle

Michelson interferometer

Resonant cavities

along the arms

Power recycling

Seismic attenuation

system for suspended

mirrors

Noises:

Seismic

Thermal (suspensions/mirrors)

Optical (shot noise)

“Next generation” noises:

Thermal, Quantum,

Newtonian