Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
1
Exotic Physics searches in ANTARES
Ersilio CastorinaPisa University and INFN
on behalf of the ANTARES Collaboration
Workshop on Exotic Physics with Neutrino Telescopes
Uppsala September 20-22 2006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
2
bull Current status of ANTARESbull MC simulation of χ Dark Matter
from the Sunbull Ongoing studies (preliminary only)
ndash early results for χ from the Earthndash first estimate of ldquoslowrdquo Magnetic
Monopoles
Outline
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
3
ANTARES
Astronomy with a Neutrino Telescope and Abyss environmental RESearch
httpantaresin2p3fr
Project to build an undersea neutrino telescopein the Mediterranean Sea
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
4
ANTARES collaboration
IFREMER BrestDAPNIA SaclayIReS StrasbourgMulhouseCPPM MarseilleIFREMERToulonCOM MarseilleOCA Nice
ITEPMoscow
IFICValencia
NIKHEFAmsterdam
Groningen
GenovaBari
CataniaRoma
Erlangen
LNS
PisaBologna
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
5
ANTARES Site
Submarine CableThe detector will be located at 2400 m depth 40 km off the Toulon (France) coast (42ordm50rsquoN 6ordm10rsquoE)
Institute Michel Pacha (La Seyne sur Mer)
The shore station is at La Seyne sur Mer 40 km NW of the
ANTARES site
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
6
Detector Design and Construction Status
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
7
Detector Geometry
70 m
12 lines (900 PMTs) 25 storeys line 3 PMTsstorey
350 m
100 m
145 m
Junctionbox
Interconnections
40 km toshore
Depth2400 m
storey
Horizontal layout
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
8
č
43deg2400 mdepth
Cherenkov light from induced by interaction detected by 3D PMT array Time amp position of hits allow the reconstruction of the (~ ) trajectoryCC
interaction
Neutrino Detection
N X
W
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
9
Local Control Moduleelectronics boards for readout of PMT signal and data acquisition (plus calibration equipment)
Optical Beaconfor timing calibration
Optical Module17rdquo glass sphere10rdquo PMT Ham R7081-20in a cage for magneticshielding
Hydrophone RXfor acoustic positioning
Basic Dector Element the storey
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
2
bull Current status of ANTARESbull MC simulation of χ Dark Matter
from the Sunbull Ongoing studies (preliminary only)
ndash early results for χ from the Earthndash first estimate of ldquoslowrdquo Magnetic
Monopoles
Outline
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
3
ANTARES
Astronomy with a Neutrino Telescope and Abyss environmental RESearch
httpantaresin2p3fr
Project to build an undersea neutrino telescopein the Mediterranean Sea
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
4
ANTARES collaboration
IFREMER BrestDAPNIA SaclayIReS StrasbourgMulhouseCPPM MarseilleIFREMERToulonCOM MarseilleOCA Nice
ITEPMoscow
IFICValencia
NIKHEFAmsterdam
Groningen
GenovaBari
CataniaRoma
Erlangen
LNS
PisaBologna
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
5
ANTARES Site
Submarine CableThe detector will be located at 2400 m depth 40 km off the Toulon (France) coast (42ordm50rsquoN 6ordm10rsquoE)
Institute Michel Pacha (La Seyne sur Mer)
The shore station is at La Seyne sur Mer 40 km NW of the
ANTARES site
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
6
Detector Design and Construction Status
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
7
Detector Geometry
70 m
12 lines (900 PMTs) 25 storeys line 3 PMTsstorey
350 m
100 m
145 m
Junctionbox
Interconnections
40 km toshore
Depth2400 m
storey
Horizontal layout
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
8
č
43deg2400 mdepth
Cherenkov light from induced by interaction detected by 3D PMT array Time amp position of hits allow the reconstruction of the (~ ) trajectoryCC
interaction
Neutrino Detection
N X
W
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
9
Local Control Moduleelectronics boards for readout of PMT signal and data acquisition (plus calibration equipment)
Optical Beaconfor timing calibration
Optical Module17rdquo glass sphere10rdquo PMT Ham R7081-20in a cage for magneticshielding
Hydrophone RXfor acoustic positioning
Basic Dector Element the storey
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
3
ANTARES
Astronomy with a Neutrino Telescope and Abyss environmental RESearch
httpantaresin2p3fr
Project to build an undersea neutrino telescopein the Mediterranean Sea
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
4
ANTARES collaboration
IFREMER BrestDAPNIA SaclayIReS StrasbourgMulhouseCPPM MarseilleIFREMERToulonCOM MarseilleOCA Nice
ITEPMoscow
IFICValencia
NIKHEFAmsterdam
Groningen
GenovaBari
CataniaRoma
Erlangen
LNS
PisaBologna
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
5
ANTARES Site
Submarine CableThe detector will be located at 2400 m depth 40 km off the Toulon (France) coast (42ordm50rsquoN 6ordm10rsquoE)
Institute Michel Pacha (La Seyne sur Mer)
The shore station is at La Seyne sur Mer 40 km NW of the
ANTARES site
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
6
Detector Design and Construction Status
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
7
Detector Geometry
70 m
12 lines (900 PMTs) 25 storeys line 3 PMTsstorey
350 m
100 m
145 m
Junctionbox
Interconnections
40 km toshore
Depth2400 m
storey
Horizontal layout
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
8
č
43deg2400 mdepth
Cherenkov light from induced by interaction detected by 3D PMT array Time amp position of hits allow the reconstruction of the (~ ) trajectoryCC
interaction
Neutrino Detection
N X
W
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
9
Local Control Moduleelectronics boards for readout of PMT signal and data acquisition (plus calibration equipment)
Optical Beaconfor timing calibration
Optical Module17rdquo glass sphere10rdquo PMT Ham R7081-20in a cage for magneticshielding
Hydrophone RXfor acoustic positioning
Basic Dector Element the storey
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
4
ANTARES collaboration
IFREMER BrestDAPNIA SaclayIReS StrasbourgMulhouseCPPM MarseilleIFREMERToulonCOM MarseilleOCA Nice
ITEPMoscow
IFICValencia
NIKHEFAmsterdam
Groningen
GenovaBari
CataniaRoma
Erlangen
LNS
PisaBologna
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
5
ANTARES Site
Submarine CableThe detector will be located at 2400 m depth 40 km off the Toulon (France) coast (42ordm50rsquoN 6ordm10rsquoE)
Institute Michel Pacha (La Seyne sur Mer)
The shore station is at La Seyne sur Mer 40 km NW of the
ANTARES site
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
6
Detector Design and Construction Status
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
7
Detector Geometry
70 m
12 lines (900 PMTs) 25 storeys line 3 PMTsstorey
350 m
100 m
145 m
Junctionbox
Interconnections
40 km toshore
Depth2400 m
storey
Horizontal layout
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
8
č
43deg2400 mdepth
Cherenkov light from induced by interaction detected by 3D PMT array Time amp position of hits allow the reconstruction of the (~ ) trajectoryCC
interaction
Neutrino Detection
N X
W
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
9
Local Control Moduleelectronics boards for readout of PMT signal and data acquisition (plus calibration equipment)
Optical Beaconfor timing calibration
Optical Module17rdquo glass sphere10rdquo PMT Ham R7081-20in a cage for magneticshielding
Hydrophone RXfor acoustic positioning
Basic Dector Element the storey
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
5
ANTARES Site
Submarine CableThe detector will be located at 2400 m depth 40 km off the Toulon (France) coast (42ordm50rsquoN 6ordm10rsquoE)
Institute Michel Pacha (La Seyne sur Mer)
The shore station is at La Seyne sur Mer 40 km NW of the
ANTARES site
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
6
Detector Design and Construction Status
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
7
Detector Geometry
70 m
12 lines (900 PMTs) 25 storeys line 3 PMTsstorey
350 m
100 m
145 m
Junctionbox
Interconnections
40 km toshore
Depth2400 m
storey
Horizontal layout
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
8
č
43deg2400 mdepth
Cherenkov light from induced by interaction detected by 3D PMT array Time amp position of hits allow the reconstruction of the (~ ) trajectoryCC
interaction
Neutrino Detection
N X
W
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
9
Local Control Moduleelectronics boards for readout of PMT signal and data acquisition (plus calibration equipment)
Optical Beaconfor timing calibration
Optical Module17rdquo glass sphere10rdquo PMT Ham R7081-20in a cage for magneticshielding
Hydrophone RXfor acoustic positioning
Basic Dector Element the storey
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
6
Detector Design and Construction Status
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
7
Detector Geometry
70 m
12 lines (900 PMTs) 25 storeys line 3 PMTsstorey
350 m
100 m
145 m
Junctionbox
Interconnections
40 km toshore
Depth2400 m
storey
Horizontal layout
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
8
č
43deg2400 mdepth
Cherenkov light from induced by interaction detected by 3D PMT array Time amp position of hits allow the reconstruction of the (~ ) trajectoryCC
interaction
Neutrino Detection
N X
W
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
9
Local Control Moduleelectronics boards for readout of PMT signal and data acquisition (plus calibration equipment)
Optical Beaconfor timing calibration
Optical Module17rdquo glass sphere10rdquo PMT Ham R7081-20in a cage for magneticshielding
Hydrophone RXfor acoustic positioning
Basic Dector Element the storey
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
7
Detector Geometry
70 m
12 lines (900 PMTs) 25 storeys line 3 PMTsstorey
350 m
100 m
145 m
Junctionbox
Interconnections
40 km toshore
Depth2400 m
storey
Horizontal layout
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
8
č
43deg2400 mdepth
Cherenkov light from induced by interaction detected by 3D PMT array Time amp position of hits allow the reconstruction of the (~ ) trajectoryCC
interaction
Neutrino Detection
N X
W
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
9
Local Control Moduleelectronics boards for readout of PMT signal and data acquisition (plus calibration equipment)
Optical Beaconfor timing calibration
Optical Module17rdquo glass sphere10rdquo PMT Ham R7081-20in a cage for magneticshielding
Hydrophone RXfor acoustic positioning
Basic Dector Element the storey
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
8
č
43deg2400 mdepth
Cherenkov light from induced by interaction detected by 3D PMT array Time amp position of hits allow the reconstruction of the (~ ) trajectoryCC
interaction
Neutrino Detection
N X
W
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
9
Local Control Moduleelectronics boards for readout of PMT signal and data acquisition (plus calibration equipment)
Optical Beaconfor timing calibration
Optical Module17rdquo glass sphere10rdquo PMT Ham R7081-20in a cage for magneticshielding
Hydrophone RXfor acoustic positioning
Basic Dector Element the storey
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
9
Local Control Moduleelectronics boards for readout of PMT signal and data acquisition (plus calibration equipment)
Optical Beaconfor timing calibration
Optical Module17rdquo glass sphere10rdquo PMT Ham R7081-20in a cage for magneticshielding
Hydrophone RXfor acoustic positioning
Basic Dector Element the storey
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
10
Apr 2005 Mini Instrumentation Line with OMs (MILOM) Mar 2006 Line 1 first complete detector line 2006 Line 2 deployed in July to be connected TODAY
2006 - 2007 installation of remaining 10 lines 2008+ Physics with full detector
Construction Status
MILOM2005
Line 12006
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
11
A Selection of Results Time CalibrationThe timing calibration systems of
ANTARES allowbull ~100 ns in absolute timing bull le 1 ns in relative timing (between
OMs)
Light source
T between hits on2 OMs in the same storey
= 07 nsHorizontal
Diagonallarger distance
less intensity
light scattering
= 26 ns
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
12
A Selection of Results a downgoing
H
it a
ltit
ud
e (
rela
tive t
o m
id d
ete
cto
r)
[m]
ANTARES preliminary
Hit time [ns]
Triggered hits
Hits used in fit
Snapshot hits = 172o
P(2ndf) = 094+
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
13
Searches for Neutralino DMin ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
14
ANTARES Science goals
bull Neutrinos from point-like amp diffuse flux sourcesndash Pulsarsndash Young SN Remnants (up to 100
evyearkm2 ) ndash Microquasars (SS433 up to 250
evyearkm2)ndash AGN (steady)ndash Gamma Ray Bursts (transient 1-100
s)bull Exotic Physicsndash Neutrinos from annihilation in the
Sun the Earth and the Galactic Centre
ndash Magnetic monopoles
+ oceanography biology seismology hellip
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
15
From down to
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
18
mSUGRA Predictions amp Sensitivity
Less constrained models are currently under investigation
Improvements of low E reco will
affect (ie lower) the sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
19
Annihilation in the Earth work in progressmSUGRA flux predictions are extremely low
Evaluate just the sensitivity (a general MSSM model could perhaps produce much more neutrinos)
The signal is expected within a cone of a few degrees (max ~10 ) depending on m
Less restrictive cuts on events direction
Different atmosphericbackground
Different Sensitivity
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
20
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
21
Searches for Magnetic Monopoles
in ANTARES
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
22
Detection of Magnetic Monopoles
Monopoles are predicted by Grand Unified TheoriesThey can be studied through their interaction with matter
bull Ionization energy lossbull Radiative energy lossbull Catalysis of proton decay
Exp Upper Limits on the average monopole flux
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
23
Detection of Magnetic Monopoles
MM produce direct and -ray induced Cherenkov light
(a tiny but easily detectable fraction of the ionization energy loss) Direct Cherenkov emission (th=074 in sea water)
A monopole with gD and =1 emits about 3106 photons
between 300 and 600 nm per cm path length
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
24
Detection of Magnetic Monopoles
-ray emission
Kinetic Energy spectrum of -raysCherenkov
Threshold for e-
in water Tth= 025 MeV
Direct -ray Cherenkov radiation
(PhD Thesis by B van Rens NIKHEF)
-ray
Direct
emitted photonscm path lenght
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
25
ANTARES 1-year
MACRO
Upper limit on Monopole flux
below the Cherenkov limit
Simulation+
dedicated Trigger amp Analysis
(PhD Thesis by B van Rens NIKHEF)
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
Ersilio Castorina - Exotic Phys with nu Telescopes Uppsala Sept 2006
26
Conclusions amp Outlook
Most promising sources SunGalactic Centre (though modelling still under debate)Earth (though expected fluxes are low)
Itrsquos indeed possible to detect DM signal (though indirectly)
ANTARES has started data acquisition with the first full line
Complete detector by the end of 2007
Itrsquos even easier to detect Monopole signal (if they exist)Through Cherenkov light
direct-ray induced
Thanks andhelliphellipstay tuned
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