Highlights of the ANTARES Neutrino Telescope
Annarita Margiotta Dipartimento di Fisica e Astronomia dell’Università and INFN Bologna on behalf of the ANTARES collaboration
HEP-EPS 2017, 6 Jul 2017 - Venezia ANTARES: the largest neutrino telescope in the Nothern hemisphere HEP-EPS 2017, Venezia 2006 PARTIAL CONFIGURATION 2008 COMPLETED Scien fic goals
• Neutrino astrophysics Highlights of ANTARES - A. Margio a • Mul -messenger studies • Dark ma er searches • Atmospheric neutrinos • Exo c par cles search: nuclearites, monopoles Not discussed • Acous c neutrino detec on today • Earth and Sea sciences
2 How does a ν telescope work? HEP-EPS 2017, Venezia
Highlights of ANTARES - A. Margio a
1.5o θµ −ν = E ν [TeV]
3
€ Event topology background
strongly reduced with geometrical cuts and HEP-EPS 2017, Venezia quality requirements on reconstruc on atmospheric muon μ± μ±
neutrino or
charged lepton Highlights of ANTARES - A. Margio a
ideal tool for astronomy angular resolu on <0.4°
@Eν> 10 TeV; 90% purity
Angular resolu on < 3° (−−) Shower within ≈ 10 m à contained events ν ν energy es mate be er than 10% x
(−−) ν muon neutrino, CC only all neutrino flavours, CC & NC μ (track reconstruc on) (shower reconstruc on) 4
5 HEP-EPS 2017, Venezia Highlights of ANTARES - A. Margio a under s.l. 2500 m m ~ 2500
depth Toulon The ANTARES site
control room
40 km Cable of Electro-op cal La Seyne-sur-Mer The telescope: full configura on since 2008
• 12 lines of 75 PMTs HEP-EPS 2017, Venezia • 1 line for Earth and Marine Storey sciences • 25 storeys / line • 3 PMTs / storey • 885 PMTs ALL-DATA-TO-SHORE: computer farm @ the 14.5 m 350 m shore sta on:
data filtering, Highlights of ANTARES - A. processing and storage.
40 km to Margio a shore
Junc on Box ~70 m Submarine links 4-08-2010 6 7 HEP-EPS 2017, VeneziaHighlights of ANTARES - A. Margio a
neutrinos
) cosmic
sources
energy
extended ridge
of high and single source) fluxes Galac c ANTARES visible sky : for Neutrino astrophysics point-like ( iden fiable : near objects
Search
not Centre and ( sources
flux
AGNs GRBs Galac c Micro-quasars Supernova remnants Magnetars
– – – – – – Diffuse Individual
•
•
Universe
most powerful accelerators in the
Extra-galac c sources
lower luminosity requirements Galac c sources HEP-EPS 2017, Venezia ANTARES search for point-like sources of cosmic νs
Highlights of ANTARES - A. Margio a 9 years of ANTARES data – all neutrino flavours: 7629 track-like + 180 shower-like events 2007-2015 – Total live me = 2423.6 d arXiv:1706.01857
8 Full sky search
Search for an excess of signal events located anywhere in the ANTARES visible sky without HEP-EPS 2017, Venezia any assump on about the source posi on à ANTARES visible sky divided in 1°×1° (r.a x decl.) boxes. à Maximum Likelihood analysis searching for clusters
decl. δ = 23.50, r.a. α = 343.80 = most significant cluster (≈ 1.9 σ )
arXiv:1706.01857 equatorial coordinates 9 Candidate list search HEP-EPS 2017, Venezia
IC HESE – 13 track-like events Red : cascades Blue: tracks candidate sources – 106 known astrophysical sources
Highlights of ANTARES - A. Margio a
GC region arXiv:1706.01857 equatorial coordinates
No significant excess found so far 10 Sensi vity and upper limits HEP-EPS 2017, Venezia
−5 ] 10
-1 ANTARES 2007-15 sensitivity
s ANTARES 2007-15 sensitivity (E < 100 TeV) ν -2 ANTARES 2007-15 limits (candidate list) ANTARES 2007-15 limits (candidate list for HESE events) 90% U.L. ANTARES 2007-15 limits (1 declination bands) −6 °
10 IceCube 7 years sensitivity [ApJ 835(2017)2 151] Highlights of ANTARES - A. Margio a IceCube 3 years MESE sensitivity (E < 100 TeV) [ApJ 824(2016)2 L28] ν [GeV cm IceCube 7 years limits [ApJ 835(2017)2 151]
90%CL −7
Φ 10
2 E
10−8
10−9 PRELIMINARY
10−10 −1 −0.8 −0.6 −0.4 −0.2 0 0.2 0.4 0.6 0.8 1 sinδ arXiv:1706.01857 11 Diffuse flux search HEP-EPS 2017, Venezia νs from unresolved sources, GZK, Z-jets…
Search for excess of HE events over the expected atmospheric background
(so er spectrum ∼ 3.7) Highlights of ANTARES - A. Margio a
12 Diffuse flux search HEP-EPS 2017, Venezia νs from unresolved sources, GZK, Z-jets…
Search for excess of HE events over the expected atmospheric background
(so er spectrum ∼ 3.7) Highlights of ANTARES - A. Margio a
Background of atmospheric ν
13 14 Highlights of ANTARES - A. Margio a ) HEP-EPS 2017, Venezia GeV /
sh
E
( ) evts 10 evts evts : 4 14 4 livedays ± signal
(2450 : 10.5 like Bkg Observed: : cut E
SHOWERS Reconstructed Energy log
Data: 2007-2015 Above IC- .) a.u
Diffuse flux
) evts evts evts : 3 19 livedays Reliable energy es mate required
signal
(2450 : 13.5 ± 4 like Es mator (proxy in Bkg Observed: TRACKS
: cut E
Energy Data: 2007-2015 Above
IC- HEP-PS 2017, Venezia Highlights of ANTARES - A. Margio a 15 Upper limit at 90% C.L. 68% confidence interval for the combined track and shower analysis (systema cs included) -2 E -2.5 E The Galac c ridge - 1
• ν’s and γ-rays produced by CR HEP-EPS 2017, Venezia propaga on o + - pCR + pISM à π π π … πo à γγ (EM cascade) ± π à νµ νe …
Highlights of ANTARES - A.
• Search for νµ , data 2007-2013 • Search region |l|<30° , |b|<4° • Cuts op mized for Γ=2.4-2.5 • Counts in the signal/off zones
• No excess in the HE neutrinos Margio a
• 90% c.l. upper limits: 3 Phys.Le . B 760(2016)143 16 HEP-EPS 2017, Venezia Highlights of ANTARES - A. Margio a 17 events IceCube ANTARES UL 2016 analysis γ new s ν cutoff à δ(R)~1/R and s PeV γ Fermi-LAT new ANTARES UL 2017 50 – 2 ) ridge . 815(2015)L25 LT = 2423.6 d à Le . J . - radially dependent model for γ , ICRC2015:1126,2015 Astroph arxiv:1702.01124 PoS Enhanced produc on of KRA CR transport in the Galaxy : Galac c The Maximum Likelihood analysis Tracks + showers 2007-2015 arXiv:1705.00497 SHOWERS TRACKS Background extracted from data events (5PeV cutoff model) signal for shower and track-like Probability density func on of the Mul messenger program Intense effort in working with other collabora ons HEP-EPS 2017, Venezia • be er understanding of the sources and of the physics mechanisms • increase detector sensi vity (uncorrelated backgrounds) Highlights of ANTARES - A. Margio a Mul wavelength follow-up of neutrinos Radio Visible X-ray GeV-ray TeV-ray GW ν MWA TAROT Swi Fermi-LAT HESS Ligo IC ZADKO HAWC Virgo MASTER Alerts 12/yr 30/yr 6/yr (Offline) (1-10/yr) (Offline) 18 Real- me (follow-up of the selected neutrino events): HEP-EPS 2017, Venezia • op cal telescopes [TAROT, ROTSE, ZADKO, MASTER] • X-ray telescope [Swi /XRT] APP 35 (2012) 530 (method) • GeV-TeV γ-ray telescopes [HESS, HAWC] JCAP02(2016)062 (op cal and X) • radio telescope [MWA] ApJ 820 (2016) L24 (radio) • Online search of fast transient sources [GCN, Parkes] Mul -messenger correla on with: Highlights of ANTARES - A. Margio a • Gravita onal wave [Virgo/Ligo] JCAP 06 (2013) 008; PRD93 (2016), 122010 • UHE events [Auger] ApJ 774(2013) 19 Time-dependent searches: • GRB [Swi , Fermi, IPN] JCAP 1303 (2013) 006; Eur. Phys. J. C 77(2017) 20 • Micro-quasar and X-ray binaries [Fermi/LAT, Swi , RXTE] JCAP 4 (2017) 019 • Gamma-ray binaries [Fermi/LAT, IACT] • Blazars [Fermi/LAT, IACT, TANAMI…] JCAP 1512 (2015), 014; A&A 576 (2015) L8 • Crab [Fermi/LAT] • Fast radio burst [radio telescopes] MNRAS 469 (2017) 4465 19 Real- me follow-up (TAToO) • M. Ageron et al., The ANTARES telescope neutrino alert system, APP 35 (2012) 530 (method) HEP-EPS 2017, Venezia • Adrián-Mar nez et al., Op cal and X-ray early follow-up of ANTARES neutrino alerts, JCAP02(2016)062 External server • Cro et al., Murchison Widefield Array Limits on Radio Emission from ANTARES Neutrino Events, ApJ 820 (2016) L24 (radio) ANTARES trigger Highlights of ANTARES - A. Margio a • single HE ν (~10 TeV) • single ν correlated to local galaxies for SNe (~1 TeV) • doublet of ν’s Performances: • Time to send an alert: ~ 5 s • Median angular resolu on: 0.3o - 0.4o • First image of the follow-up: <20 s • Dedicated op cal image analysis 20 GW observa on neutrino follow-up joint analyses ANTARES/IceCube/LigoSC/Virgo HEP-EPS 2017, Venezia GW150914 GW151226 LVT151012 Highlights of ANTARES - A. Margio a • No ANTARES events in ±500 s around event me • ANTARES limits dominates for Eν < 100 TeV • Size of GW150914 : 590 deg2 • ANTARES resolu on: <0.5 deg2 • < 10% GW total energy radiated in ν Phys.Rev. D93 (2016), 122010 + arxiv:1703.06298 (accepted on PRD) 21 νµ associated with GeV and TeV γ-ray flaring blazars and X-ray binaries HEP-EPS 2017, Venezia • Search for ν’s (2008-2012) correlated with high ac vity state • Blazars monitored by FERMI-LAT and IACTs (JCAP 1512 (2015), 014) • 40 blazars + 33 X-ray binaries during flares observed by Swi -BAT, RXTE- ASM and MAXI. Transi on states from telegram alerts • No significant excess Highlights of ANTARES - A. Margio a • Upper limits on ν fluence and model parameters constrain JCAP04(2017)019 22 HEP-EPS 2017, Venezia Highlights of ANTARES - A. Margio a 23 Dark Ma er from the Sun the Earth and the Galac c Centre HEP-EPS 2017, Venezia Highlights of ANTARES - A. • Gravita onal trapping and accumula on of DM par cles in the centre of astrophysical objects like the Sun, the Galac c centre and also the Earth • DM annihila on would produce eventually a HE neutrino flux with no significant astrophysical backgrounds Margio a • ν spectrum àWIMPSIM [Blennow,Edsjö,Ohlsson,arXiv:0709.3898] μ • Bkg es mated from me scrambled data. No excess observed 24 JCAP, 10 (2015) 068 Phys.Le . B 769 (2017) 249 The Galac c Center − + − + − + HEP-EPS 2017, Venezia 5 annihila on channels XWIMP XWIMP →νν, bb, W W , τ τ , µ µ 3 DM halo models in the Milky Way good visibility of the GC effect on the thermally averaged cross sec on only muon like events considered è angular resolu on <0.4° Highlights of ANTARES - A. Margio a 2 J-factor à ρ DM integrated over a line of sight at an angular separation Ψ from the center of the source, depends on the halo model 25 Dark Ma er annihila on in the Earth and the Sun HEP-EPS 2017, Venezia data collected between 2007-2012 3 channels: τ+ τ-, W+ W-, bb Limits on the SI WIMP-nucleon Limits on the SD WIMP-nucleon sca ering cross sec on sca ering cross-sec on Physics of the Dark Universe, 16 (2017) 41 Phys.Le . B 759 (2016) 69 Highlights of ANTARES - A. -1 1 10 ANTARES 2007-2012 (Earth, bb channel) + - ANTARES 2007-2012 (Earth, channel) [pb] ANTARES 2007-2012 (Earth, W+W- channel) IceCube b b Sun -2 p SD 10 ANTARES 2007-2012 (Sun, bb channel) + - IceCube 2011-2012 ANTARES 2007-2012 (Sun, channel) + - -3 ANTARES 2007-2012 (Sun, W W channel) 10 1 10 ANTARES b b (this work) -4 XENON100 10 PICO-60 2 Margio a -5 10 10 IceCube W+ W - + - ANTARES W W (this work) -6 10 PICO-2L 10 3 10-7 Earth SuperK + - -8 SI scattering cross section [pb] section cross scattering SI 10 Sun 10 4 -9 + - + - IceCube 10 PandaX-II (2016) ANTARES (this work) Lux 2014-16 -10 10 3 5 2 10 3 10 10 1 10 102 10 104 m [GeV/c2] M [GeV] WIMP 26 Summary • ANTARESà the largest underwater neutrino telescope HEP-EPS 2017, Venezia • Search for a neutrino flux from the Southern sky • Huge mul messenger effort – EM radia on: radio (MWA), op cal, X-ray, γ-rays (LAT,IACTs) – Gravita onal Wave observatories and IceCube • Important contribu on to the indirect searches for Dark Ma er Highlights of ANTARES - A. Margio a • compe ve sensi vi es and excellent angular resolu on in both track and cascade events because of – OPTICAL PROPERTIES OF THE SEAWATER – LOCATION à Northern Hemisphere Mediterranean Sea – DEPTH • main limita on è reduced size The future: KM3NeT/ARCA (talk C. Distefano, on Sat morning) 27