The ANTARES The ANTARES Deep-Sea The - Agenda

Transcription

The ANTARES Deep‐
The ANTARES Deep
p‐Sea
Neutrino Telescope
Neutrino Telescope::
Status and First Results
and First Results
Nicolas Picot‐Clémente, CPPM, Marseille
ill
Les Rencontres de Physique de la Vallée d’Aoste
de la Vallée d
Aoste.
28 Feb.‐ 06 March 2010
Multimessenger Astronomy
γ
p
ν
28 Feb.‐ 06 March 2010
Interaction with:
Interstellar medium,
IR, CMB, radio.
Deflected by B fields.
Useful above 1020eV, but eV, but
GZK effect.
Not deflected by B fields,
Not absorbed by dust,
Unambiguous probe of hadronic processes.
Les Rencontres de Physique de la Vallée d’Aoste.
1
The ANTARES Collaboration
NIKHEF, Amsterdam
KVI Groningen
NIOZ Texel

ITEP,Moscow
Lomonosov State University, Moscow

ECAP, Erlangen
Bamberg

IFIC, Valencia
UPV, Valencia
Technical Univ.
Catalonia,, Barcelona
Catalonia

28 Feb.‐ 06 March 2010

CPPM, Marseille
CPPM, Marseille
DSM/IRFU/CEA, DSM/IRFU/CEA, Saclay
Saclay
APC Paris
IPHC (
IPHC (IReS
IReS), ), Strasbourg
Strasbourg
Univ. de H.
Univ. de H.‐‐A., A., Mulhouse
Mulhouse
Clermont
Clermont‐‐Ferrand
IFREMER, IFREMER, Toulon
Toulon/Brest
/Brest
C.O.M. C.O.M. Marseille
Marseille
LAM, LAM, Marseille
Marseille
GeoAzur Villefranche
ISS, Bucarest

University/INFN of Bari
University/INFN
University
University/INFN
/INFN of Bologna
University
University/INFN
/INFN of Catania
LNS – Catania
University
University/INFN
/INFN of Pisa
University
University/INFN
/INFN of Rome
University
University/INFN
/INFN of Genova

2
ANTARES science goals
Understanding production mechanisms of HE cosmic rays
Understanding production mechanisms of HE cosmic rays.
SNR
Study very energetic objects:
Study
very energetic objects:
_ Galactic: SN, SNR, Microquasars, …
_ Extra‐Galactic: AGN, GRB, …
Search for new physics: Dark matter (Sun, GC), Monopoles, Nuclearites, …
AGN
Multidisciplinary science: Oceanography, Sea biology, Seismology, Environment
Oceanography, Sea
biology, Seismology, Environment monitoring, … monitoring, …
28 Feb.‐ 06 March 2010
3
Detection Principle
μ−
νμ
W‐
u
μ+
νμ
W+
d
d
u
Detector
Cherenkov emission
θc=43°
μ
ν
Time‐position correlation muon direction.
MC TeV muon traversing the apparatus
28 Feb.‐ 06 March 2010
4
The ANTARES The ANTARES telescope
telescope
350 m
• 12 lines
Calibration systems:
• 25 storeys
25 storeys / line
/ line
• Acoustic positioning
• 3 PMTs / storey
• Optical beacons
• 900 PMTs
14.5 m
Cable to
shore (40km)
shore (40km)
2500m depth
100 m
100 m
Junction
Box
~70 m
Anchor/line socket
Link cable
5
The ANTARES site
Toulon
La Seyne sur mer
Shore Station
28 Feb.‐ 06 March 2010
6
Sky coverage
AMANDA/IceCube (South Pole)
(
(resolution in ice: ~2°/0.8°)
l ti i i ~2°/0 8°)
28 Feb.‐ 06 March 2010
ANTARES (43° North)
(
(resolution in water: 0.3°)
l ti i
t 0 3°)
7
Line connections
• 2006 Lines 1, Line 2 • 2007
Lines 3 ‐ 5, Lines 6 ‐10 • 2008 Lines 11‐12
2008
Li
11 12
Manned submarine Nautile
28 Feb.‐ 06 March 2010
Robot submarine Victor
9
storey
Detector status
Detector status after completion
Detector completed 30 May 2008.
Regular
g
maintenance of the infrastructure foreseen
infrastructure foreseen.
Line 12: Successful
Successful
recuperation++repair
recuperation
repair, and , and then
then
redeployment in in November 2009.
in November
2009
Line 6: Currently in reparation
in reparation..
Line 9: Planned to be
to be recovered
this week.
week.
line
28 Feb.‐ 06 March 2010
10
Optical Background
B t from
Bursts
f
macroorganisms
(strongly affected
by sea currents
by sea
by currents))
Baseline
~ 60kHz from K40 + microorganisms.
γ Cherenkov
γ
Cherenkov
e‐ (β decay)
40K
40Ca
28 Feb.‐ 06 March 2010
11
(m)
Position Alignment
Position Alignment
Line 4
Distances and rotations
Distances
and rotations
measured every 2 min.
28 Feb.‐ 06 March 2010
Radial displacement (2 months 2007)
Position resolution better than ~ 10 cm.
12
In situ Calibration
Computation of time differences
between pairs of OMs.
pairs of OMs
Time resolution of Time resolution
Time of ~ 0.5 ns.
0.5 ns
0 5 ns.
Detector efficiency:
Absorption length
Absorption length at ANTARES site.
LED beacon
28 Feb.‐ 06 March 2010
13
In situ Calibration In situ Calibration with
with K40
40K coincidence rate
t i 2
tuning 2
tuning 1
tuning 1
on average
~35 photons
Time offsets for all OMs
Time offsets for all OMs
Crosscheck
C
h k of f
time calibrations.
K40 decay
28 Feb.‐ 06 March 2010
tuning 3
14
Event display: Event display: Atmospheric
Atmospheric muon
Example of a reconstructed down‐
Example of a reconstructed down‐
going muon, detected in all 12 going muon
going muon, detected in all 12 detected in all 12
detector lines.
height
time
28 Feb.‐ 06 March 2010
15
Event display: Neutrino
Event display: Neutrino‐‐induced muon
Example of a reconstructed up
Example
of a reconstructed up‐
up‐going going
muon (i.e. a neutrino candidate) detected in 6 detector lines.
h i ht
height
time
28 Feb.‐ 06 March 2010
16
Atmospheric Background
Atmospheric μ ~ 107 per year
Atmospheric ν ~ 103 per year
upgoing
pg g
28 Feb.‐ 06 March 2010
downgoing
g g
17
Atmospheric Background
Atmospheric μ ~ 107 per year
Atmospheric ν ~ 103 per year
upgoing
pg g
downgoing
g g
~90
90 days
days with the 5‐line detector
the 5 line detector
Main sources of simulation uncertainties:
• Angular dependance of OM efficiency
of OM efficiency..
• Absorption Absorption length of
Absorption length
of light in sea
of light in light in sea water.
water
Measurements agree with MC within
MC within
systematics, and systematics
, and cannot
and cannot distinguish
between this various models
models..
28 Feb.‐ 06 March 2010
17
Muon depth‐‐intensity relation Muon depth
from coincidence rates
Low‐energy threshold compared to full reconstruction.
Low‐
Muon flux attenuation with depth directly measured.
Paper
Paper accepted for publication in Astroparticle
Paper accepted for publication in accepted for publication in Astroparticle Physics.
Physics
(Astroparticle Physics 33 (2010) pp. 86
Physics 33 (2010) pp. 86‐‐90)
28 Feb.‐ 06 March 2010
18
Depth‐intensity relation for Depth‐
atmospheric muons
Angular dependance of the muon flux at 2000m.
~ 90 days with the 5‐line detector
MC MUPAGE
MC MUPAGE
Data
Cos(zenith)
2,5km
6km
Submitted to Astroparticle
Submitted to Astroparticle Physics
Physics..
28 Feb.‐ 06 March 2010
19
Neutrinos
2007+ 2008 fit events (341 days of effective livetime)
2007+ 2008 fit events (341
days of effective livetime)
28 Feb.‐ 06 March 2010
20
Neutrinos
1062 events
1062 events
Neutrino‐‐induced muon purity
Neutrino
muon purity of ~ 96%
of ~ 96%
2007+ 2008 fit events (341 days of effective livetime)
2007+ 2008 fit events (341
days of effective livetime)
28 Feb.‐ 06 March 2010
20
Scrambled neutrino neutrino sky
sky map
2007‐‐2008
2007
750 upgoing neutrinos (multi‐
neutrinos (multi‐line) in line) in 341 days 341 days of effective of effective livetime
livetime..
Real sky map will be shown next summer conferences.
28 Feb.‐ 06 March 2010
21
Point Source Search
Point Source Search
•Definition
Definition of a list
of a list of potential
of potential sources sources
(SNR, BL Lac objects, etc …)
•Analysis based on simulations, following a blinding procedure.
Expected sensitivity competitive with
previous multi‐
multi‐year experiments
experiments..
Analysis for 2007 and 2008 data period
for 2007 and 2008 data period
presented soon.
soon.
28 Feb.‐ 06 March 2010
Declination (°)
22
Magnetic monopole search
monopole search
1931: Dirac 1931: Dirac introduced
introduced::
1974: ’t Hooft and Polyakov
1974: ’t Hooft and Polyakov::
Magnetic field:
Magnetic field:
Any unified gauge theory in which U(1)
Any
unified gauge theory in which U(1)E.M. is is
embedded in a spontaneously broken semi‐simple gauge group necessarily contains M.Ms.
Magnetic charge:
Number of emitted photons in sea water
Signal in sea
Signal in g
sea water:
•Direct Cherenkov emission βMM > 0.74:
Direct Cherenkov
γ from a MM with g from
MM
g=gD.
x 8500
Cherenkov γ from
delta-rays.
Number of photons emitted by a MM with the minimal charge gD ~ 68.5 e, is ~ 8500 times more than that of a muon.
g
from
d-rays
Cherenkov
γ from
g froma μ.
m
•Indirect Cherenkov emission βMM > 0.51:
The energy transferred to electrons allows to pull out electrons (δ rays) which can emit Cherenkov light
(δ‐rays), which can emit Cherenkov light.
28 Feb.‐ 06 March 2010
23
monopole search
E t
Extremly
l high
hi h energy deposition
d
deposition.
iti .
Analysis using the large number
of hits in ANTARES OMs.
U
Upgoing
i magnetic
ti monopole monopole event
l eventt with
ith β ~ 0.99.
~ 0 99
28 Feb.‐ 06 March 2010
24
monopole search
Expected sensitivity 90% C.L. after one year of data taking with the 12-line detector.
~1.1 expected
~1.1 expected background background events
events after one one year
year of 12
of 12‐‐line ANTARES data taking
line ANTARES data taking..
28 Feb.‐ 06 March 2010
25
Conclusion and Outlook
ANTARES is the largest neutrino telescope in the g
p
northern hemisphere.
First neutrino telescope under sea completed and First
neutrino telescope under sea completed and
taking data.
Mediterranean site complementary to South Pole.
Physics analysis are on the track.
M ltidi li
Multidisplinary platform.
l tf
First step towards a km3 scale detector.
28 Feb.‐ 06 March 2010
26
BACKUP
Search for Large for Large Scale
Scale Asymetry
in Downgoing
in Downgoing Muons
5 line data (2007)
Selection:
Elevation >10
Elevation >10°°.
At least 2 lines
At least 2 lines..
>20 hits.
>20 hits.
>20 hits
660000 downgoing muons.
muons.
Ang. Resolution < 5
Ang. Resolution < 5
Ang. Resolution < 5°
5°.
10*10 degree bins.
No asymmetry observed with current statistics.
No asymmetry observed with current statistics.
28 Feb.‐ 06 March 2010
EM showers
EM showers from atm
atm. muons
. muons
Link to the cosmic ray composition.
(5.6 days)
(5.6 days)
Compatible Compatible with
p
with a mixed composition a mixed composition (
p
(Horandel model))
28 Feb.‐ 06 March 2010
Mechanisms
L t i
Leptonic process: Hadronic process: 28 Feb.‐ 06 March 2010
HE l t
HE electron
HE electron
HE electron
LE γ
S h t
Synchrotron radiation di ti
followed by inverse by inverse Compton scattering
Compton scattering..
LE γ
LE γ
Synchrotron radiation followed by π
by π° photo
photo‐‐
production..
production
Mechanisms
L t i
Leptonic process: Hadronic process: 28 Feb.‐ 06 March 2010
HE l t
HE electron
HE electron
HE electron
LE γ
S h t
Synchrotron radiation di ti
followed by inverse by inverse Compton scattering
Compton scattering..
LE γ
LE γ
Synchrotron radiation photo‐‐
followed by π
by π ± photo
production..
production
Detector present
Detector present status
Line 6: Recovered in October 2009.
Line 9: Planned to be recovered this week.
Line 12: First Line 12: First example
example of of successfull
successfull
recuperation++repair
recuperation
repair++redeployment
redeployment..
28 Feb.‐ 06 March 2010
Expected performances
Neutrino effective area
Ndet=Aeff × Time × Flux
FFor EEν<100 TeV, A
<100 T V Aeff grows with energy due ith
d
to the increase of the interaction cross section and the muon range.
For Eν>100 TeV the Earth becomes opaque to neutrinos.
28 Feb.‐ 06 March 2010
FFor EEν<10 TeV, the angular resolution is 10 T V th
l
l ti i
dominated by the ν−μ angle.
For EEν>10 TeV, the resolution is limited by For
>10 TeV, the resolution is limited by
track reconstruction uncertainties.
Introduction of magnetic monopoles
Initially introduced by Dirac
y
y
in 1931: Make symmetric Maxwell’s equations.
eImply the quantization of the electric charge.
M.M.
Magnetic charge is given by .
The smallest magnetic charge is the Dirac charge gD, where k=1.
28 Feb.‐ 06 March 2010
Introduction of magnetic monopoles
’t Hooft and Polyakov
y
in 1974:
Any unified gauge theory in which U(1)E.M. is embedded in a spontaneously
broken semi-simple gauge group necessarily contains M.Ms.
Transition example with the minimal GUT group:
MM appear with charge g=gD at the first transition.
In this typical case the monopole mass is about ~ 10
In
this typical case the monopole mass is about ~ 1016 GeV with a radius of the order ~ 10
with a radius of the order ~ 10‐28 cm.
cm
Predicted magnetic monopole’s masses : 108 to 1017 GeV (depending on the unified gauge group).
28 Feb.‐ 06 March 2010
Acceleration of magnetic monopoles in the
Universe
E
Energy
gain
i in
i a magnetic
ti coherent
h
t field:
fi ld
Magnetic monopoles with masses below 1014 GeV could be relativistic
( i h extragalactic
(with
l i sheets
h
expecting
i to dominate
d i
the
h spectrum).
)
Estimated energy loss when crossing the Earth is ~ 1011 GeV.
M.M.
28 Feb.‐ 06 March 2010
M.M. with masses up to about 1014 GeV are expected
to cross the Earth and be relativistic.
relativistic
Magnetic monopole’s signal in ANTARES
Direct Cherenkov emission β > 0.74
0 74 :
nsea water ~ 1.35
Direct Cherenkov γ
g from MM
from a MM with
g=gD.
x 8500
Number of photons emitted by a MM with the
minimal charge gD ~ 68.5 e, compared to a muon of
same velocity is about ~ 8500 more!
Cherenkov γ from
d lt
delta-rays.
g from
d-rays
Indirect Cherenkov emission β > 0.51 :
The energy transferred to electrons allows
to pull out electrons (δ-rays), which can
emit Cherenkov light.
28 Feb.‐ 06 March 2010
Cherenkov γ
from a μ.
g from m
KM3NeT
12 lines, 900 PMTs
– Design Design Study
Study and Preparatory
and Preparatory Phase
• Consortium ANTARES/NEMO/NESTOR
– Maximise Maximise physics
physics potential
• Instrumented
d volume >1km
l
k 3
• Angular resolution ~0.1 ~0.1 degrees
degrees (E>10 (E>10 TeV
TeV))
– Build in a reasonable
in a reasonable time ∼4 years
∼4 years
• Multi‐line deployment techniques
• Speed‐up integration time
• Sub contract part of the production
– At a reduced
a reduced cost
• Factor 2 reduction
Factor 2 reduction cf ANTARES
• Simplified
Si lifi d architecture
hi
• Reduced maintenance
28 Feb.‐ 06 March 2010
Dark matter search: Neutrino limits
Фνμ+νμ from the Sun
y
5-line data, 68.4 days
y
No excess observed (90% C.L. limits)