neutrino Astro-particle physics bij Nikhef. Aart Heijboer
Waarom Neutrino Astronomie?
We verwachten kosmische neutrino-bronnen: - zeer hoog energetische kosmishe straling - Bronnen van TeV gamma's Detectie van Neutrino's: - ondubbelzinnig bewijs voor hadron-versnelling - astronomie bij >> TeV (gaat niet met's)
on u m neu
Uppsala 2000
o trin
Hoge energie neutrino's cross-sectie ~evenredig met E muon gaat 5 km bij E = 10 TeV Cherenkov straling (35000 photons per meter) → enorm volume met weinig detectoren Ivo van Vulpen
3
helder water → goede hoekresolutie (< 0.5o)
Buoy
350 m
100 m
~60-75 m Uppsala 2000
Ivo van Vulpen
totaal volume ~ 200 x 200 x 300 meter3
Junction box
4
electonica : string power module optische GB link naar de kust (DWDM)
Buoy
350 m
100 m
~60-75 m Uppsala 2000
Ivo van Vulpen
totaal volume ~ 200 x 200 x 300 meter3
Junction box
5
shore station
Bucarest
7 countries 29 institutes ~150 scientists+enginers
40 km naar detector
data aqcuisitie systeem Trigger systeem op de wal (all data to shore) Software om de detector aan te sturen (run-controll)
shore station
Bucarest
7 countries 29 institutes ~150 scientists+enginers
40 km naar detector
Geschiedenis & Huidige Status 2006 : 1 lijn aangesloten : eerste (neergaande muonen) 2007 : 5 lijnen: eerste neutrinos mei 2008: 12 lijn – detector compleet. werkende lijnen,
Huidige status
In totaal 80 miljoen muon triggers
wachten op aansluiting
Geschiedenis & Huidige Status 2006 : 1 lijn aangesloten : eerste (neergaande muonen) 2007 : 5 lijnen: eerste neutrinos mei 2008: 12 lijn – detector compleet.
In totaal 80 miljoen muon triggers
Neutrino's! (atmospherisch)
up
down
Neutrino's! (atmospherisch)
muon reconstructie software event display eerste neutrino's gevonden
Donkere Materie in de Zon? χ
zon
WIMPs ingevangen in de zon
χχ χ χ χ
Aarde
ν
Antares
E ≈ M/3 Zoek naar neutrino's binnen 4 graden van de zon eerste resultaat met 5-lijn detector nog niet gevoelig genoeg, maar ziet er goed uit voor complete detector
Gordon Lim
mSUGRA flux predictions: : > WMAP favoured relic density : within WMAP favoured relic density : < WMAP favoured relic density
focus point region (hard neutrino spectrum)
Zoeken naar kosmische bronnen Eerste resultaat: 5 lijn-detector: Nog geen bron gevonden, limit op de flux voor een groot aantal interesante astronomische objecten meest gevoelige meting voor objecten in the zuidelijke hemel.
Zoeken naar kosmische bronnen d data e l b 008 m a 2 r sc 7 & 0 20
10 x zo veel data al beschikbaar... Nu aan het analyseren: zoeken naar bronnen (Vidi A. Heijboer) ook electron en tau neutrino's neutrinos van gamma ray bursts (Veni M. Bouwhuis) correlaties met hoogste energie Auger events (Veni J. Petrovic)
De Volgende stap. KM3NeT
- plan voor een nog-veel-grotere Detector - minstens 1 km3
- Project in 'Preperatory phase' - Plaats, vorm, etc nog te bepalen - TDR wordt geschreven (eind 2009 klaar) - Nikhef: - mogelijk ontwerp optische modules & detector lijnen. - samenwerking met NIOZ, KVI - subsidie OCW
Conclusie Antares detector voltooid sinds mei 2008 Eerste ronde analyses gebaseerd op 5-line data (2007) Veel meer data nu al beschikbaar – stay tuned. Nikhef speelt grote rol op alle niveaus electronica, DAQ systeem & software, reconstructie data analyse KM3NeT maakt voortgang TDR wordt nu geschreven Beslissing over uiteindelijke
Science with ANTARES SNR
• High energy neutrino astrophysics: galactic: SN, SNRs, µ -quasars... extra-gal: AGNs, GRBs, GZK
GRB
• Search for New Physics: Dark matter (sun, GC), Monopoles.. Binary systems
• Earth-Sea Science: oceanography, sea biology, seismology, environment monitoring...
AGN
Microquasars
? ~MeV
GeV-100 GeV
GeV-TeV
TeV-PeV
PeV-EeV
> EeV
Neutrinos and Multi-Messenger Astronomy
Neutrinos • Unambiguous probe of hadronic processes • Not deflected by B fields • Not absorbed by dust • Horizon not limited by interaction with CMB/IR • Detectable over full energy range (GeV->PeV) • Can be correlated with optical signals
Detection principle 3D PMT array
p, α
ν ν
p
µ
Cherenkov light from µ
µ
ν
µ
γ
42°
Sea floor
µ ν
µ
interaction
- Main detection channel: ν also)
µ
- Energy threshold ~ 10 GeV
The reconstruction is based on local coincidences compatible with the Cherenkov light front
interaction giving an ultra-relativistic µ
(ν
e
and ν
τ
NIKHEF, Amsterdam Utrecht KVI Groningen NIOZ Texel
University of Erlangen Bamberg Observatory
ITEP,Moscow Moscow State Univ
ISS, Bucarest
IFIC, Valencia UPV, Valencia UPC, Barcelona
CPPM, Marseille DSM/IRFU/CEA, Saclay APC, Paris LPC, Clermont-Ferrand IPHC (IReS), Strasbourg Univ. de H.-A., Mulhouse IFREMER, Toulon/Brest C.O.M. Marseille LAM, Marseille GeoAzur Villefranche
University/INFN of Bari University/INFN of Bologna University/INFN of Catania LNS – Catania University/INFN of Pisa University/INFN of Rome University/INFN of Genova
26
V. Bertin - CPPM - ARENA'08 @ Roma
The ANTARES Site & Infrastructure
Submarine cable
Region of Sky Observable by Neutrino Telescopes AMANDA/IceCube (South Pole) (Ice: ~2°/0.6°)
ANTARES/KM3 (43° North) (water: ~0.2°/0.1°)
Mkn 421 Mkn 501
Mkn 501 CRAB SS433
RX J1713.7-39 SS433
GX339-4 Galactic Centre
CRAB VELA
The ANTARES Detector 2500m
• • • •
900 PMTs 12 lines 25 storeys / line 3 PMTs / storey
40 km to shore
V. Bertin - CPPM - ARENA'08 @ Roma
450 m
Junction Box 70 m
Interlink cables
autile
Building the Detector: Line Connections • 2006 • 2007 • 2008
Line 1, Line 2 Lines 3 - 5, Lines 6 Victor -10 Robot submarine Lines 11, 12
30
Detector status after completion
• Detector completed 30 may 2008 • 88% of modules operational • Regular maintenance of in-situ infrastructure foreseen
Basic Detector Element: a storey Optical Beacon with blue LEDs: timing calibration
titanium frame: support structure
Optical Module: 10” Hamamatsu PMT in 17” glass sphere (σ TTS ≈ 1.3 ns) photon detection
Local Control Module (in Ti cylinder): Front-end ASIC, DAQ/SC, DWDM, Clock, tilt/compass,
See poster: B. Baret, 13-15/07-OG 2.7 1184
Hydrophone: acoustic positioning
Acoustic Position Alignment
Storey 1 Storey 8 Storey 14 Storey 20 Storey 25
Radial displacement Distances and rotations measured every 2 min
See poster: A. Brown, 13-14/07 - OG 2.7
In-Situ Calibration with Potassium-40
Gaussian peak on coincidence plot
γ Cherenkov
e- (β
decay) 40
40
Ca
Integral under peak
Peak offset
Precision (~5%) monitoring of OM efficiencies
K Cross check of time calibration
See poster: JP. Gomez, 10-11/07 - OG 2.5
Number of Triggers 5 lines (2007) 19.106 μ
10 or more lines (2008) 65.106 μ
CABLE REPAIR
Total : 240 days = 80% of calendar Selected :167d = 70% of total
Total : 243 days = 83% of calendar Selected :173d = 71% of total See poster: M. Bouwhuis, 10-11/07 - OG 2.5
Track Reconstruction Online Algorithm
Offline Algorithm
• Triplets as single points • Find clusters of floors allowing one skipped floor • Only lines with at least one such cluster • Add compatible single hits • Chi square fit
• Uses final alignment • Loose selection • Full likelihood fit • Multiple starting points • not immediately available • excellent angular resolution
• Immediately available • non-optimal angular resolution
See talk: A. Heijboer, 13/07 - 15:30 - OG 2.5
Expected Performance (full detector) Neutrino effective area
Angular resolution
Ndet =Aeff × Time × Flux
• For Eν <10 PeV, Aeff grows with energy due to the increase of the interaction cross section and the muon range. • For Eν >10 PeV the Earth becomes opaque to neutrinos.
• For Eν <10 TeV, the angular resolution is dominated by the ν -µ angle. • For Eν >10 TeV, the resolution is limited by track reconstruction uncertainities.
Data-MC Comparison: Downgoing Muons (5-lines)
data CORSIKA QGSJET +NSU
MC uncertainty
• No quality cuts applied MUPAGE data CORSIKA QGSJET +NSU CORSIKA QGSJET+Horandel
• Agreement within (substantial) theoretical + MC uncertainty • Main experimental errors stem from OM efficiency and acceptance and optical water properties (λ abs λscatt )
5 lines (2007): Depth vs. Intensity
in ar y
y ar in im el Pr
Pr el im
2,5km 6km
See talk: M. Bazzotti, 8/7/09, HE340
Work on reducing systematics is ongoing
Search for Large-Scale Asymmetry Pr el im in in Down-going Muons ar y 5 line data (2007)
Elevation >10 degrees At least 2 lines >20 hits 660000 downgoing muons Ang Resolution <5 degrees 10*10 degree bins No asymmetry observed with current statistics See talk S. Mangano, 8/7/09, HE1131 See poster G. Guillard, Antares as a gamma telescope
5 line data (2007): NEUTRINOS
p, α
ν
ν
µ
µ
p
Pr el im
γ
in ar y
168 active days 168 upward events (multi-line fit) down up
horizontal
All-Sky Point Search Results BIC distribution of only background
Pr el im
• Stringent cuts to ensure low background and good angular resolution.
in ar y
• Expectation-MaxImisation algorithm Pr el im
in a
ry
BICobs In our sample : BICobs = 1.4 (highest value) p-value = 0.3 (1σ excess) (δ = -63.7º RA =243.9º)
See talk S. Toscano, 13/7/09, OG2.5
No significant excess found
Source Candidate List Search applied to 25 selected sources
φ
90
(10-9 TeV cm-2 s-1 ) Pr el im
• The lowest value corresponds to a
p-value pre-trial of 3σ • Expected in 10% of the experiments when looking at 25 sources (post-trial probability)
Competitive limits in southern sky
in ar y
2008 data: Neutrinos
Pr el im
in ar y
174 active days 582 upgoing events (multi-line fit)
Scrambled 2007+2008 Skymap
750 upgoing neutrinos (multi-line) Unblinding once reprocessed with final alignment
Transients with ANTARES Triggered search
Rolling search
Requires Satellite trigger
Full sky search
Low backgrounds due to direction and time coincidences
24hr/24hr
Dump all L0 data in 2min window around trigger (i.e. no trigger losses) Special track reconstruction using known direction See poster M. Bouwhuis, 341, OG2.4
Sliding time window around events Fast online reconstruction ⇒ optical follow up to identify source Also sensitive to dark bursts See talk D. Dornic, 13/7/09, OG2.5
Triggered Search: Time Delays GRB alerts from three satellites
INTEGRAL
Swift
Fermi
Response time = time delay – buffering time
Swift
INTEGRAL
24 alerts from INTEGRAL
241 alerts from Swift
Fermi
198 alerts from Fermi
(From February 2007 to May 2009)
Rolling Search Triggers - Multiplet of neutrino events
- Single High Energy Neutrino
From the same direction and within a short time window
Above ~20 - 50 TeV, the background rate begins to be negligible
R2
atm
(
∆ Ω atm ≈ 2 ∆t R1 2π
)
2
Application to ANTARES: Cuts tuned to give 1-2 triggers per month
R atm ≈1000 yr −1 1
ΔΩ = 3° x 3° Δt = 15 min
R
2 atm
≈ 0.005 yr −1
Optical Follow-Up TAROT (Télescope à Action Rapide pour les Objets Transitoires) Two robotic 25 cm diameter telescopes -TAROT Calern, France -TAROT La Silla, Chile
Field of view of 1.86° x 1.86° 10s pointing Magnitude V<17 (10s) V<19 (100s)
Operational since May 2009
TAROT La Silla
Gravitational Waves and Neutrinos
Common sky coverage for VIRGO+LIGO+ANTARES In geocentric coordinates (assumes ANTARES has 100% visibility in its antipodal hemisphere and 0% elsewhere) Drafting of MOU in progress See poster V. Van Elewyck, 1196, OG2.5
Indirect Search for Dark Matter dark matter annihilations in the sun
χ
Sun
WIMPs gravitational trapped via elastic collisions in the sun
χ χ χ χ χ
Earth
ν
Antares <Eν > ~ Mχ /3 χ
χ
→
WW, ff W, f →
ν
X
Dark matter search: Neutrino limits Pr el im
in ar y
5-line data, 68.4 days
No excess observed (90% C.L. limits) à la Feldman-Cousins
mSugra model predictions
Фνμ+νμ from the Sun
green : WMAP favoured relic density red : > WMAP favoured relic density blue : < WMAP favoured relic density
See talk: G. Lim, 10-11/07 - OG 2.5
Dark matter search: muon LIMITS
Preliminary
12 lines, 5 years, ν flux Most of focus point region excluded for m<180GeV
mSUGRA flux predictions: : : :
> WMAP favoured relic density within WMAP favoured relic density < WMAP favoured relic density
Search for Monopoles & Nuclearites Pr el im
in ar y
Search for monopoles
Search for nuclearites
• Extremely high energy deposition • Direct Cherenkov light for β > 0.74 • δ-rays for β > 0.51
• Very characteristic signature:an extended source of photons “heated wire” • 84 days of 5-line data
(strangelets, quark nuggets, Q-balls).
See talk: G. Pavalas, 9/7/09, HE695
Acoustic Detection of Neutrinos
neutrino
Hydrophone Array Cascade Acoustic Pressure Waves
See talk F. Simone, 13/07-15:30 -OG 2.5
feb-may 2008
56
Dark Matter: Search for Neutralino Annihilation in the Sun
mSUGRA flux predictions: : > WMAP favoured relic density : within WMAP favoured relic density : < WMAP favoured relic density
Antares limits: Not yet competitive with other experiments, but promising limit based on data taken within 1/2 year with only 5/12 of the detector operational
Gordon Lim
KM3NET – Design Study and Preparatory Phase • • • •
Consortium ANTARES/NEMO/NESTOR Partially funded by FP6 & FP7 ASPERA/ApPEC roadmaps ESFRI ‘list of opportunities’
– Maximise physics potential • Instrumented volume >1km3 • Angular resolution ~0.1 degrees (E>10 TeV) • Substantial improvement over ICECUBE
– Build in a reasonable time ∼ 4 years • Multi-line deployment techniques • Speed-up integration time • Sub contract part of the production
– At a reduced cost • Factor 2 reduction cf ANTARES • Simplified architecture • Reduced maintenance
See talk J-P. Ernenwein, 14/7/09, OG 2.7
Summary ANTARES infrastructure completed since May 29th 2008 • Detector operation and its calibration understood • Largest neutrino telescope in the northern hemisphere • Observe galactic sources with unprecedented resolution
Exciting physics program ahead… • • • •
Over a thousand neutrinos already reconstructed Muons, neutrinos, dark matter, monopoles, …… Best limits for point sources in the southern sky Multi-messenger approach strongly pursued
Real-time readout and in-situ power capabilities facilitates
a large program of synergetic multi-disciplinary activities: acoustics, biology, oceanography, seismology…… Major step towards the KM3NeT multi-disciplinary deep-sea research infrastructure
