neutrino Astro-particle physics bij Nikhef. Aart Heijboer

Transcriptie

1 neutrino Astro-particle physics bij Nikhef. Aart Heijboer

2 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)

3 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)

4 Buoy 350 m 100 m ~60-75 m Uppsala 2000 Ivo van Vulpen totaal volume ~ 200 x 200 x 300 meter3 Junction box 4

5 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

6 shore station Bucarest 7 countries 29 institutes ~150 scientists+enginers 40 km naar detector

7 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

8

9

10

11

12

13

14 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

15 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

16 Neutrino's! (atmospherisch) up down

17 Neutrino's! (atmospherisch) muon reconstructie software event display eerste neutrino's gevonden

18 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)

19 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.

20 Zoeken naar kosmische bronnen d data e l b 008 m a 2 r sc 7 & 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)

21 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

22 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

23 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

24 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

25 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

26 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

27 V. Bertin - CPPM - Roma The ANTARES Site & Infrastructure Submarine cable

28 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 J SS433 GX339-4 Galactic Centre CRAB VELA

29 The ANTARES Detector 2500m 900 PMTs 12 lines 25 storeys / line 3 PMTs / storey 40 km to shore V. Bertin - CPPM - Roma 450 m Junction Box 70 m Interlink cables

30 autile Building the Detector: Line Connections Line 1, Line 2 Lines 3-5, Lines 6 Victor -10 Robot submarine Lines 11, 12 30

31 Detector status after completion Detector completed 30 may % of modules operational Regular maintenance of in-situ infrastructure foreseen

32 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 Hydrophone: acoustic positioning

33 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

34 In-Situ Calibration with Potassium-40 Gaussian peak on coincidence plot γ Cherenkov e- (β decay) 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

35 Number of Triggers 5 lines (2007) μ 10 or more lines (2008) 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

36 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

37 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.

38 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 )

39 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

40 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 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

41 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

42 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

43 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

44 2008 data: Neutrinos Pr el im in ar y 174 active days 582 upgoing events (multi-line fit)

45 Scrambled Skymap 750 upgoing neutrinos (multi-line) Unblinding once reprocessed with final alignment

46 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

47 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)

48 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 yr 1

49 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 s pointing Magnitude V<17 (10s) V<19 (100s) Operational since May 2009 TAROT La Silla

50 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

51 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

52 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

53 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

54 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

55 Acoustic Detection of Neutrinos neutrino Hydrophone Array Cascade Acoustic Pressure Waves See talk F. Simone, 13/07-15:30 -OG 2.5

56 feb-may

57 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

58 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

59 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