Il Sistema TOF dell’esperimento AMS-02 Il Sistema TOF dell’esperimento AMS-02 sulla Stazione Spaziale Internazionale: sulla Stazione Spaziale Internazionale:
prestazioni nello spazio e ricerca di materia prestazioni nello spazio e ricerca di materia oscuraoscura
September 2012
Nicolo’ MasiNicolo’ Masi Bologna University and INFN
Contin A.,Laurenti G.,Quadrani L.,Bindi V., Palmonari F.
MatterMatter Anti-MatterAnti-Matter
An Improved Version of AMS-01
An Improved Version of AMS-01
AntimatterAntimatterAstrophysics, Dark Matter
Astrophysics, Dark Matter
StrangeletsStrangelets
Up in the SkyUp in the Sky
TOF consists of 4 plastic scintillator TOF consists of 4 plastic scintillator planes, 2 above and 2 below the planes, 2 above and 2 below the magnet.magnet.The counters of adjacent planes are The counters of adjacent planes are orthogonal.orthogonal.The number of counters per plane has The number of counters per plane has been reduced to 8, 8, 10, 8 counters to been reduced to 8, 8, 10, 8 counters to reduce the weight (34 scintillators). reduce the weight (34 scintillators).
Each TOF counter is composed by: Each TOF counter is composed by: • a plastic scintillator a plastic scintillator 1 cm thick and 1 cm thick and around 120 cm long (Eljen-Technology around 120 cm long (Eljen-Technology type: Ej-200), type: Ej-200), • read at both ends by 2 read at both ends by 2 independently powered independently powered photomultiplier tubes photomultiplier tubes (fine-mesh (fine-mesh Hamamatsu R5946 with max spectral Hamamatsu R5946 with max spectral response at 420 nm),response at 420 nm),• connected with transparent light connected with transparent light guidesguides..
Hamamatsu fine-mesh
R5946
On the ISSOn the ISS
Plateau for the trigger efficiency of one counter
Carbon Beta Resolution: 1.2% -> 48 ps
Longitudinal TOF-Trackercoordinate alignment
And physics beginsAnd physics begins
No Dark Matter Signal!No Dark Matter Signal!Clear Signal!Clear Signal!
….and AMS??….and AMS??
Primary CR Positron from Dark Matter
Primary CR Positron from Dark Matter
Light LZP provides
measurable fluxes for AMS-02
Light LZP provides
measurable fluxes for AMS-02
SUSY Wino, Little Higgs, KK Theory,
PBH, Singlet Scalar, Minimal DM…
SUSY Wino, Little Higgs, KK Theory,
PBH, Singlet Scalar, Minimal DM…
With e+ and low energy antideuteron we can probe
With e+ and low energy antideuteron we can probe
Total Flux High Energy
Antiproton High Energy Signal
from KK particle
Antiproton High Energy Signal
from KK particle
Discrimination parameter I𝜙 for signal and background: the AMSB Wino MSSM
is the most suitable for AMS-02, both in antiproton and positrons channel
Discrimination parameter I𝜙 for signal and background: the AMSB Wino MSSM
is the most suitable for AMS-02, both in antiproton and positrons channelExpected
clear positron signal from heavy Wino
Expected clear positron
signal from heavy Wino
The region above the line can be distinguished from the
background.
The region above the line can be distinguished from the
background.
Wide range of the parameter space, including the region BF = 1Wide range of the parameter space, including the region BF = 1
95% C. L. contour within WMAP constraint for Little Higgs Dark
Matter parameters space
95% C. L. contour within WMAP constraint for Little Higgs Dark
Matter parameters space
e+
Parameters space explorable by AMS-02 in the
antiproton channel
Parameters space explorable by AMS-02 in the
antiproton channel
Goudelis - Antimatter signals of singlet scalar dark matter
Always promising positron search
Always promising positron search
Kinetic Energy (GeV)
The hadronic Low Energy region is realistically obsolete and has been replaced with a High Energy research.
In function of AMS-02 performances, an hadronic research related to very heavy DM particle is ongoing, to restart from PAMELA data. This would be the most significant signal of new particle physics, even cleaner and clearer than the leptonic one.
The positron signal, on the other hand, is of course the fundamental channel for DM study. In terms of intensity of annihilation products fluxes, AMS-02 can see a positron peak for all DM candidates capable of producing e+ beyond 100 GeV.
ConclusionsConclusions
Antiproton & Antideuteron Search :
Dark Matter Parameters Space for a non-
leptophilic candidate:
Just a little patience!
