Ersilio Castorina - Exotic Phys. with nu Telescopes, Uppsala Sept. 2006 1 Exotic Physics searches in...

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


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


3

ANTARES

Astronomy with a Neutrino Telescope and Abyss environmental RESearch

httpantaresin2p3fr

Project to build an undersea neutrino telescopein the Mediterranean Sea


4

ANTARES collaboration

IFREMER BrestDAPNIA SaclayIReS StrasbourgMulhouseCPPM MarseilleIFREMERToulonCOM MarseilleOCA Nice

ITEPMoscow

IFICValencia

NIKHEFAmsterdam

Groningen

GenovaBari

CataniaRoma

Erlangen

LNS

PisaBologna


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


6

Detector Design and Construction Status


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


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


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


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


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


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+


13

Searches for Neutralino DMin ANTARES


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


15

From down to


18

mSUGRA Predictions amp Sensitivity

Less constrained models are currently under investigation

Improvements of low E reco will

affect (ie lower) the sensitivity


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


20


21

Searches for Magnetic Monopoles

in ANTARES


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


23


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


24


-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


25

ANTARES 1-year

MACRO

Upper limit on Monopole flux

below the Cherenkov limit

Simulation+

dedicated Trigger amp Analysis



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

Slide 1

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Slide 24

Slide 25

Slide 26


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


3

ANTARES


httpantaresin2p3fr



4



ITEPMoscow

IFICValencia

NIKHEFAmsterdam

Groningen

GenovaBari

CataniaRoma

Erlangen

LNS

PisaBologna


5

ANTARES Site




ANTARES site


6



7

Detector Geometry

70 m


350 m

100 m

145 m

Junctionbox

Interconnections

40 km toshore

Depth2400 m

storey

Horizontal layout


8

č

43deg2400 mdepth


interaction

Neutrino Detection

N X

W


9







10



Construction Status

MILOM2005

Line 12006


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

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Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

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Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


3

ANTARES


httpantaresin2p3fr



4



ITEPMoscow

IFICValencia

NIKHEFAmsterdam

Groningen

GenovaBari

CataniaRoma

Erlangen

LNS

PisaBologna


5

ANTARES Site




ANTARES site


6



7

Detector Geometry

70 m


350 m

100 m

145 m

Junctionbox

Interconnections

40 km toshore

Depth2400 m

storey

Horizontal layout


8

č

43deg2400 mdepth


interaction

Neutrino Detection

N X

W


9







10



Construction Status

MILOM2005

Line 12006


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

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Slide 9

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Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


4



ITEPMoscow

IFICValencia

NIKHEFAmsterdam

Groningen

GenovaBari

CataniaRoma

Erlangen

LNS

PisaBologna


5

ANTARES Site




ANTARES site


6



7

Detector Geometry

70 m


350 m

100 m

145 m

Junctionbox

Interconnections

40 km toshore

Depth2400 m

storey

Horizontal layout


8

č

43deg2400 mdepth


interaction

Neutrino Detection

N X

W


9







10



Construction Status

MILOM2005

Line 12006


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

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Slide 7

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Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


5

ANTARES Site




ANTARES site


6



7

Detector Geometry

70 m


350 m

100 m

145 m

Junctionbox

Interconnections

40 km toshore

Depth2400 m

storey

Horizontal layout


8

č

43deg2400 mdepth


interaction

Neutrino Detection

N X

W


9







10



Construction Status

MILOM2005

Line 12006


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


6



7

Detector Geometry

70 m


350 m

100 m

145 m

Junctionbox

Interconnections

40 km toshore

Depth2400 m

storey

Horizontal layout


8

č

43deg2400 mdepth


interaction

Neutrino Detection

N X

W


9







10



Construction Status

MILOM2005

Line 12006


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


7

Detector Geometry

70 m


350 m

100 m

145 m

Junctionbox

Interconnections

40 km toshore

Depth2400 m

storey

Horizontal layout


8

č

43deg2400 mdepth


interaction

Neutrino Detection

N X

W


9







10



Construction Status

MILOM2005

Line 12006


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


8

č

43deg2400 mdepth


interaction

Neutrino Detection

N X

W


9







10



Construction Status

MILOM2005

Line 12006


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


9







10



Construction Status

MILOM2005

Line 12006


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


10



Construction Status

MILOM2005

Line 12006


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


11



OMs)

Light source


= 07 nsHorizontal


less intensity

light scattering

= 26 ns


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


12


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


P(2ndf) = 094+


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

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Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


13



14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


14










15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

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Slide 26


15

From down to


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

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Slide 25

Slide 26


18






19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

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Slide 8

Slide 9

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Slide 11

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Slide 26


19








20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

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20


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

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Slide 19

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Slide 24

Slide 25

Slide 26


21


in ANTARES


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

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Slide 14

Slide 15

Slide 18

Slide 19

Slide 20

Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


22






23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

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Slide 15

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Slide 19

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Slide 21

Slide 22

Slide 23

Slide 24

Slide 25

Slide 26


23







24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

Slide 2

Slide 3

Slide 4

Slide 5

Slide 6

Slide 7

Slide 8

Slide 9

Slide 10

Slide 11

Slide 12

Slide 13

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Slide 25

Slide 26


24


-ray emission


Threshold for e-




-ray

Direct



25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


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25

ANTARES 1-year

MACRO



Simulation+




26







direct-ray induced


Slide 1

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26







direct-ray induced


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Ersilio Castorina - Exotic Phys. with nu Telescopes, Uppsala Sept. 2006 1 Exotic Physics searches in...

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Transcript of Ersilio Castorina - Exotic Phys. with nu Telescopes, Uppsala Sept. 2006 1 Exotic Physics searches in...