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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
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