Recent Results from ANTARES and prospects for KM3NeT. Aart Heijboer. Nikhef, Amsterdam On behalf of the ANTARES and KM3NeT collaborations

Transcription

1 Recent Results from ANTARES and prospects for KM3NeT Aart Heijboer Nikhef, Amsterdam On behalf of the ANTARES and KM3NeT collaborations

2 European Neutrino Telescopes 2 * and ANTARES ANTARES KM3NeT * * Münster Moscow * + Since April 2017: CIRA Perth Australia as observer Marrakech ** Rabat Granada * * * Saclay Strasbourg Nantes Mulhouse * Clermont * * Deployment sites * ANTARES ORCA * * * * * * * * * * ARCA * 2

3 European Neutrino Telescopes 3 ARCA building block ORCA Operating for 10 years now Producing key science results thanks to angular resolution and view of Galactic center with up-going muons - Under construction - Two sub-arrays with same technology: ARCA: 2 sparse building blocks, Italy, 2022, Gton, cosmic neutrinos ANTARES: 22 contributions KM3NeT: 13 contributions ORCA: 1 dense building block, France, 8 Mton, 2020, oscillations, mass hierarchy. 3

4 European Neutrino Telescopes 4 ARCA building block ORCA Operating for 10 years now Producing key science results thanks to angular resolution and view of Galactic center with up-going muons - Under construction - Two sub-arrays with same technology: ARCA: 2 sparse building blocks, Italy, 2022, Gton, cosmic neutrinos ANTARES: 22 contributions KM3NeT: 13 contributions ORCA: 1 dense building block, France, 8 Mton, 2020, oscillations, mass hierarchy. 4

5 Sea Water as a detection Medium 5 ANTARES Tracks Cherenkov light arrives on-time Upgoing tracks (n μ CC) Angular resolution <0.4 for E n >10 TeV PoS ICRC2015 (2016) 1078 ANTARES Cascades Upgoing cascades(n e/ n t CC, NC) Angular resolution < 3 Energy resolution for n e : 5%

6 Sea Water as a detection Medium 6 ANTARES ANTARES Absolute pointing ANTARES verified by detecting (3.5σ) Moon shadow in down-going muons. ANTARES Poster M. Sanguinetti, PoS (ICRC) 1053

7 Sea Water as a detection Medium 7 ANTARES Tracks Cherenkov light arrives on-time Cascades ANTARES (n e ) Track s (n μ CC) Angular resolution <0.1 for Eν>100 TeV Cascade events (n e/ n t CC, NC) Angular resolution < 1.5 Energy resolution for n e ~5% Talk K Melis, PoS (ICRC) 950

8 Sea Water as a detection Medium From E. Resconi, 6 year HESE data E > 60 TeV ϴ<20 o Points : 3FHL, HBL Resolution for ν e ANTARES KM3NeT Resolution for ν μ ANTARES. KM3NeT. Resolution of key importance for catalogue searchers 8

9 KM3NeT first detection lines 9 Timing check with LED flashers Poster 1059 Time after flash (ns) Deployed May 2016 Deployed Dec 2015 In the water for >1 year Valuable validation of technology Next step: 2 ORCA lines (September 2017) Posters on technology: - Reliability Studies, - Front end electronics - Software Defined Networks - Acoustic positioning - In situ calibration 1059

10 KM3NeT first detection lines 10 If more than 7 PMTs fire -> remove all optical background at DOM-level. Count muons vs depth. Test of in-situ per-pmt efficiency measurement Talk M. Jongen 1018

11 KM3NeT Supernova sensitivity Excess of modules where 6-10 PMTs fire simultaneously Number of firing PMTs Can use same idea to measure O(10 MeV) neutrinos from Galactic core- collapse supernova! Poster D. Colomer PoS (ICRC2017) 14 >80% of all Galactic SN with a single detector/block! 11

12 Antares point source search Days of live-time 7629 tracks, 180 Cascades Arxiv: Submitted PRD Talk G. Illuminati PoS (ICRC2017) 986 Limits for 103 source candidates and sources 13 HESE tracks X Track Cascade Source candidate HESE track

13 Antares point source search Most significant cluster p = 6% In full (1.9 sky sigma) p = 6% (1.9 sigma) Most significant candidate source HESSJ p = 13% Exclude point source near galactic center Depending on assumed spectrum, exclude point source that could Produce 3-10 IC events anywhere Near GC. Also: time correlation with IC events (poster G. Illuminati, 987) Most significant HESE track p = 20% 13

14 Antares point source search days of live-time Antares preliminary 7629 tracks, 180 cascades Limits for 103 candidate sources and 13 HESE tracks No significant excess Best limits for part Southern Hemisphere E n <100 TeV Relevant energy range for Galactic Results to be combined with latest IC search

15 15 KM3NeT point source sensitivity Poster A. Trovato PoS (ICRC) 999 Muon neutrinos still dominant in analysis More than order of magnitude improvement in Southern hemisphere good acceptance in few-tev range : Directly constrain (or discover) hadronic scenario in galactic TeV gamma sources

16 16 Search for high-energy excess (aka diffuse flux ) ANTARES data Talk T. Eberl PoS (ICRC2017) 993 Tracks Cascades Neural network energy estimator for tracks, fitted E for cascades 33 observed, 24 +/- 7 expected from background, ~8 expected from IceCube flux P-value = 0.15, based on counting.

17 17 Search for High-energy excess (aka diffuse flux ) - Neural network energy estimator for tracks, fitted E for cascades - 33 observed, 24 +/- 7 expected from background, NNN expected from IceCube flux - P-value = 0.15.

18 18 Search for High-energy excess (aka diffuse flux ) for an E -2.5 spectrum Excess is not (very) significant, but compatible with IceCube flux, as illustrated by 68% confidence interval.

19 19 Search for High-energy excess (aka diffuse flux ) KM3NeT: Confirm IceCube flux within one year. Talk R. Conoglione PoS(ICRC2017)998 Then: high resolution follow-up and e.g. Flavour composition poster T. Heid PoS(ICRC2017)1006

20 20 ANTARES Multi-messenger Talk D. Dornic PoS (ICRC2017) 985 Send real-time alerts (5 s delay) of neutrinos pairs And very high energy neutrinos. Typically 30/yr. E -2.5 spectrum assumed.

21 Multi-messenger studies Maxi Ligo Milagro Virgo Fermi HAWK TA Parkes Auger Utmost IceCube 21

22 Multi-messenger/time correlation studies 22 Object Messenger Telescope ICRC Flaring Blazars Gamma FERMI/LAT Poster A. Sanchez-Loza Maxi 971 Flaring X-ray binaries X & gamma-ray Swift, MAXI Milagro RXTE/ASM, Fermi/LAT Ligo Flares from Mrk 421 and Mrk 501 Auger Talks A. Sanchez-Losa 970 Fermi Gamma HAWK Poster M. Organokov 946 Gamma Ray Bursts Gamma Swift, GCN Talk S. Celli 988 IceCube Events Neutrino IceCube Poster G. Illuminati 987 UHECR CR Auger,TA Poster I. Di Palma 990 Galactic plane Model fit Fermi, Milagro Talk B. Baret 942 Fast Radio Bursts Radio SUPERB@Parkes, UTMOST, ASKAP Parkes Talk M. Sanguineti 1053 Fermi Bubbles Gamma Fermi Poster S. Hallmann 1001 BH/NS mergers Gravitational waves Ligo/Virgo (+Icecube) Talk T. Pradier 947

23 Galactic Ridge 23 Guaranteed galactic neutrinos from CR interactions with matter Does it contribute to IC flux? KRAγ model spectrum and morphology reproduce Fermi & Milagro data. [D. Gaggero, et al Ast.. J. Lett., 815:L25, 2015.] Analysis uses full model morphology and spectrum ANTARES Limit is a factor 1.3 above the KRAγ model. KM3NeT s

24 24 Search for neutrinos + gravitational waves Neutrino follow up relevant in case of baryonic ejecta Coincident neutrino signal would allow pinpointing the source (< 1 deg) PRD 93, arxiv: GW Current GW detections: - Combined analysis Ligo/Virgo, IceCube and ANTARES (dominates for E ν <100 TeV) - No counterpart observed limit on energy radiated in neutrinos : 10% - Now, real-time follow-up science run

25 Indirect dark matter detection 25 Relic WIMPs gravitationally bound / elastic collisions (Sun, Earth, Galactic Center) n <E n > ~ M /3 Earth ANTARES Talk C. Tonnis 913 PHys Dark Univ., PLB 769 (2017) 249 JCAP 10 (2015) 068 Sun spin dependent cross section Phys.Lett. B759 (2016) Nb: latest Pico result not in this plot Galactic Center Phys. Let. B 769 (2017) M WIMP (GeV) M WIMP (GeV) M WIMP (GeV)

26 Indirect dark matter detection 26 Relic WIMPs gravitationally bound / elastic Ideas collisions for combining with IceCube (Sun, Earth, Galactic Center) See poster Earth J.A. Aguilar, C Tonnis P.Hys Dark Univ., n 16 (2017) PLB 769 (2017) 249 <E n > ~ M /3 Sun JCAP 10 (2015) 068 ANTARES Phys.Lett. B759 (2016) Talk C. Tonnis 913 Sun spin dependent cross section Nb: latest Pico result not in this plot Galactic Center Phys. Let. B 769 (2017) estimated ORCA sensitivity promising M WIMP (GeV) M WIMP (GeV) M WIMP (GeV)

27 Oscillations New work-in-progress in ANTARES Sensitivity estimate Talk I. Salvadori PoS (ICRC2017) P(νμ νμ) for θ=130º IH NH 0.5 νμ 0 νe Eν [GeV] To resolve Mass Hierarchy, need Sensitivity in 5-10 GeV range => KM3NeT ORCA 27

28 28 KM3NeT/ORCA Unique facility to study atmospheric neutrinos in 5-50 GeV region Flagship measurement: neutrino mass hierarchy 3 σ in 4 years, or better Talk A. Kouchner PoS (ICRC2017) 1027 But also: Dark matter Non-standard interactions Sterile neutrinos Tau appearance [Talk S. Hallman 1025] Earth Tomography [poster S. Bouret 1020] Sensitivity to θ 23, Δm 2 comparable to Nova Systematics included

29 Conclusions 29 ANTARES : 10 years of continuous data taking Point source results strongest limits for Galactic sources Southern Hemisphere, energy < 100 TeV Cascade events routinely used in analyses, with up to 3 o resolution At high energy: weak excess, of magnitude expected from cosmic flux Many multi-messenger studies, looking for transients (X-ray, TeV-gamma, GW) KM3NeT Under construction! First two ARCA lines operated for 1 year -> verify timing and performance ARCA : high-resolution follow up of IceCube flux (5σ within 1 yr) ORCA : Measure neutrino mass hierarchy (3σ in 4 years) ESFRI roadmap 2016, New funds for both ORCA and ARCA => beyond phase 1 Letter of Intent for KM3NeT 2.0 available

30 Backup 30

31 KM3NeT first detection lines First line deployed Dec

32 32 Search for High-energy excess (aka diffuse flux ) - Neural network energy estimator for tracks, fitted E for cascades - 33 observed, 24 +/- 7 expected from background, NNN expected from IceCube flux - P-value = 0.15.

33 Fermi bubbles & Fast radio bursts 33

34 Sea Water as a detection Medium Resolution for ν e ANTARES KM3NeT 34

35 Probing neutrinos from the Fermi Bubbles New analysis only tracks - energy threshold - no significant excess - ongoing work to include cascades To be ICRC17 Visibility signal and off-zones