Astroparticle and Gravitational Physics - G. Cella - INFN sez. Pisa - Fisica 2011-2020 - Dipartimento di Fisica
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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
20
Unique below 10 eV?
UVHE: Engine? GZK?
Spectrum?
Lower energies:
indirect
Galactic
direct
Isotropic
High flux SMALL DETECTORS
High energies:
Extragalactic
Directional
Low flux BIG DETECTORS
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)
• Charged CR preserve some
directionality only above
4x1019 eV
•
• Directional
• Easy to detect
• Not completely clear origin:
p or e?
A leit-motiv: •
Simultaneous study of • Directional
different channels leads
• Difficult to detect
to a better understanding
• 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
• 30 times more sensitive than
5-10 years lifetime any previous
• Can precisely measure cosmic
e+ and e- spectra up to a TeV
FERMI: some results
ray sky catalog
1400 sources > 100
MeV
Known and
unidentified
New sources
Pulsar catalog
60 gamma PSR
First population
study
Emission far from
surface
Detection of LMC, SNR, starbust galaxies • Very successful experiment
Constraints on Dark Matter models (EGRET • Will last very probably for 10 years
excess excluded)
• Phenomenological and theoretical activities
GRB, flares, transients here in Pisa
………FERMI: some results
ray sky catalog
1400 sources > 100
MeV
Known and
unidentified
New sources
Pulsar catalog
60 gamma PSR
First population
study
Emission far from
surface
Detection of LMC, SNR, starbust galaxies • Very successful experiment
Constraints on Dark Matter models (EGRET • Will last very probably for 10 years
excess excluded)
• Phenomenological and theoretical activities
GRB, flares, transients here in Pisa
………MAGIC: an Imaging Air Cherenkov Technique
telescope
Very high energy gamma
astronomy (10GeV-10TeV)
AGN: production in the jet,
near the BH
Supernova remnants
Lower energy unidentified
few ns flashes of light sources
mirror surface of 240 square metres
GRB
camera with O(100) photomultipliers
Cosmology & fundamental
energy resolution: 30% or better physicsMAGIC: detection principle
Imaging Air Cherenkov Technique
Background rejection
Energy reconstruction
Direction reconstruction
Image reconstruction for
extended sources ( > 0.1 degrees)Results and perspectives
Goals:
lower the threshold to 30GeV (or less)
Increase detection area
New light-to-electron conversion
techniques
Benefits: fundamental & exotic
physics, astrophysics, sinergy with
Four new VHE galactic sources found
satellite detectors, MWL campaigns
First detection of pulsed emission from a
ground based telescope (Crab) Cherenkov Telescope Array
Correlations between gamma and X emissions
(start 2013)?
(MWL campaign)
Extragalactic VHE sources
Suggestions for an higher transparency of
the universe than expected from EBLCALorimetric 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 45°
Search for Dark matter
57
m
Final configuration since 2008KM3NeT: multi-cubic-kilometre Cherenkov
telescope for high energy neutrinos
Deep-sea research infrastructure in the
Mediterranean Sea.
KM3NeT in numbers • multi-km3 Cherenkov telescope for
(full detector) neutrinos with E>100 GeV.
• ~300 DU
• Complementary to ICECUBE
• 20 storey/DU
• ~ 40m storey spacing • Construction can start in 2012, depending
• ~1 km DU height on fundings
• ~180m DU distance Main physics goals
• ~ 5 km3 volume Origin of Cosmic Rays and Astrophysical
sources
Galactic Candidate Sources (SNRs, Fermi Bubbles,
quasar,…)
Extragalactic Candidate Sources (AGN, GRB, …)
Builds on the experience gained with
ANTARES, NEMO and NESTOR
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”Gravitational waves (and other invisible things)
Gravitational waves
Nonlinear equation, difficult to solve in the
general case
Matter tells the spacetime how to curve, and
curved space tells to matter how to move
(J. Wheeler)
Linearized equation: wave equation
From: M. Pössel,
" The wave nature of simple
gravitational waves " in:
Einstein Online Vol. 2
(2006), 1008VIRGO: an interferometric detector of
gravitational waves
Goals:
Challenges:Gravitational wave detectors
networkThe multimessenger approach (II)
Candidates
GW+HEN:
Negligible absorption
travel cosmological
Signatures
distances
No deflection by magnetic fields
tracing back feasible
Weakly interacting
Advantages
Can escape from dense
object
Agreement with ANTARESResults/perspectives
No detections until now
Several interesting upper limits
Advanced detectors in the near
futureTimeline
Gravitation
Lense
Thirring
G-Gran Sasso: design study
Precision tests of
General Relativity
PN effects
Exotic physicsGG: test of equivalence principle
Conclusions AUGER-N 1 ton
ET DM
KM3NET CTA
Astroparticle physics:
1 ton
a rapidly growing field Megaton mass
p Decay +
• 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.Contacts
AMS:
ANTARES: http://www.pi.infn.it/antares/
http://www.pi.infn.it/ams/Group.ht
ml Armando Bigi,Vincenzo Cavasinni, Vincenzo Flaminio,
Stefano Galeotti, Dario Grasso, Mauro
Gabriele Bigongiari, Franco Cervelli, Stefano Morganti, Giuseppe Terreni.
Di Falco , Giovanni Gallucci, Marco
KM3NET: http://www.km3net.org/home.php
Incagli, Federico Pilo, Valerio Vagelli.
Bachir Bouhadef, Vincenzo Flaminio, Enrico
FERMI/GLAST: http://glast.pi.infn.it/ Maccioni, Antonio Marinelli, Mauro Morganti,
Fabio Stefani
Luca Baldini, Ronaldo Bellazzini, Johan
Bregeon, Alessandro Brez, Marco VIRGO: http://www.ego-gw.it/
Ceccanti, Michael Kuss, Luca Latronico,
Marco Maria Massai, Massimo Minuti, Balestri G., Basti A., Bitossi M., Boschi V., Bradaschia
Nicola Omodei, Melissa Pesce-Rollins, C., Cella G., Di Lieto A., Di Virgilio A., Ferrante
I., Fidecaro F., Frasconi F., Gennai A., Giazotto
Michele Pinchera, Massimiliano Razzano, A., Magazzu’ C., Mantovani M., Paoletti F.,
Carmelo Sgrò, Gloria Spandre. Paoletti R., Passaquieti R., Passuello D., Poggiani
R., Toncelli A., Tonelli M., Torre O., Vajente G.
MAGIC: http://www.pi.infn.it/magic/
GG: http://eotvos.dm.unipi.it/
Pedro Antoranz, Massimilano Bitossi, Roberto
Cecchi, Paolo Da Vela, Elvira Leonardo, M. L. Chiolafo, F. Maccarrone , G. Mengali, A.M.
Nobili, P. Paolicchi, R. Pegna , E. Polacco,T.R.
Mario Meucci, Vincenzo Millucci, Jose Saravanan, F. Pegoraro.
Miguel Miranda, Ricardo Padrino,
Riccardo Paoletti, Serena Partini, Pier G-Gran Sasso DS:
Giorgio Prada Moroni, Steve N. Shore, http://www.df.unipi.it/~carelli/ricerca/giro.html
Antonio Stamerra, Diego Tescaro
Maria Allegrini, Filippo Bosi, Jacopo Belfi, Niccolò
CALET: Beverini, Giorgio Carelli, Giancarlo Cella ,
Angela Di Virgilio, Isidoro Ferrante, Enrico
Maccioni, Flavio Stefani
Pier Simone MarrocchesiExtra slides
AMS: the Alpha Magnetic Spectrometer on the
ISS
e/p separation
TRD 3D tracking
charged particles trigger
time direction
TOF beta measurement
Z measurement (dE/dx)
MG B=0.86 dipolar field
TR rigidity up to 2-3 TeV
ACC 3D tracking
AST Z separation (dE/dx)
veto eff. > 99.99%.
TOF
beta measurement
Z separation
upgoing particle rejection
RICH
Isotopes separation (with TR)
energy measurement
EMC e/h separation
e.m. Showers trigger
3D imagingCR factories
Max Energy:
Magnetic field
LHC
intensity
Size of accelerating
regionGZK limit Scattering on cosmological photons
D. Grasso (Pisa); D. Gaggero (Pisa, Ph.D. stud.); L. Maccione (DESY); G. Di
Bernardo (Goteborg); C. Evoli (SISSA)
PAMELA e+ excessFERMI: detection principle
LAT: pair conversion telescope
4x4 array
precision converter/tracker
16 tungsten foils
16 X-Y alternated silicon
strips detectors
Calorimeter (caesium iodide)
measure shower energy &
GBM: burst monitor shower profile
Scintillators:
plastic segmented anti-coincidence
• 12 NaI (8kEV-1MeV)
detector
• 2 Bismuth-Germanate
(150keV-30MeV) DAQRecent 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.34:274-283,2010Work in progress & future plans
We are using DRAGON to derive new Markov chain MC comparison of
constraints on DM and astrophysical astrophysical/DM models and AMS-02
models on the basis of PAMELA antiproton multichannel data. Study the implications
data and estimate the projected AMS-02 for the fundamental physics accounting also
sensitivity (in collaboration with SISSA for LHC results.
DM group).
Consistent modeling of the diffuse γ-ray
We are studying the PAMELA and Fermi- (Fermi-LAT) and the synchrotron (PLANCK)
LAT new measurements in the lepton emission of the Galaxy. Features in their
sector and estimate the expected AMS-02 spectral and angular distributions may
capability to discriminate different confirm the presence of new CR components
interpretations of those results. This is and help identifying their sources. This is
also relevant for the CALET project. also useful to model the CMB foreground.
We are modeling the diffuse γ-ray Use PLANCK results and CR electron models to
emission of the Galaxy consistently with CR improve our knowledge of the Galactic
data and propose a new interpretation of magnetic field. It will help modeling UHECR
the puzzling longitude profile of the γ-ray deflections which is crucial to better
emissivity of the Galaxy observed by identify UHECR sources and composition
Fermi-LAT (gradient problem). (relevant for AUGER).ANTARES: detection principle
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
Basic idea:
select
secondary
generated
inside the
earthResults and perspectives
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,
ANTARES infrastructure completed:
GW)
Largest neutrino telescope in the Northern hemisphere
Operating smoothly, maintenance capability proven
Understanding of detector and data analysis progressingKM3NET: sensitivity window
100 %
0%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,
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