Recent results status and perspectives from ANTARES and KM3NeT Mediterranean Neutrino Telescopes Antonio Capone on behalf of ANTARES and KM3NeT Collaborations 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 1
Ta Talk outline Motivation for High Energy Astrophysical neutrino detection • Optical photons, Gamma ray, Cosmic Rays, … GW: messengers from the H.E. sources in the Universe • Multimessengers astronomy !! H.E. astrophysical Neutrino detection can complete the observation: ANTARES, KM3NeT • • ANTARES and KM3NeT main physics goal: search for astrophysical neutrinos Search for a diffuse flux • • Search for point-like sources Indirect search for Dark Matter: from the SUN, the Galactic Plane, the Earth • n oscillations and properties • Not discussed in this talk searches for monopoles/nuclearites • • . . . • Transient/multi-messenger studies Search for GRB • • Search for transient high intensity gamma sources Search for common CR+neutrino, GW+neutrino, … point like sources • Perspectives for the future • • Conclusions & Summary 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 2
Mult lti-Messe ssenger Astronomy Multi-wavelength astronomy X-rays gamma-rays neutrinos cosmic rays microwave optical ? Large part of the Universe is opaque to the EM If we would "observe" the spectrum sky with photons with wavelength < 10 -21 m ⟺ energy > 10 3 TeV we probably would see this map 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 3
Ne Neut utrino no fl flux uxes: wha hat do do we kno know/expe pect ? This is our region of interest 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 4
Cherenkov n Te Ch Telescope: Detection principle - Atmospheric neutrino flux ~ E n -3 � E n -3.7 Search for neutrino induced events, - Neutrino flux from cosmic sources ~ E n -2 mainly ! " # → " % , deep underwater § Search for neutrinos with E n >1 ÷ 10 TeV Down-going µ from atm. showers S/N ~ 10 -6 at 3500m w.e. depth - ~TeV muons propagate in water for several km before being stopped p, nuclei • go deep to reduce down-going atmospheric µ backg. • long µ tracks allow good angular reconstruction ..0° For & ! ≥ ( )*+ , !" ~ & ! [)*+] µ direction reconstructed from the arrival time of Cherenkov photons on Cherenkov the Optical Modules: needed good Neutrino Neutrinos from cosmic sources measurement of PMT hits, s (t)~1ns, Telescope induce 1-100 muon evts/y and good knowledge of PMT in a km 3 Neutrino Telescope positions: ( s ~10cm) p, nuclei Up-going µ from neutrinos generated in atm. showers S/N ~ 10 -4 43° charge current interactions water/ice rock up-going neutrino Picture from ANTARES 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 5
Ho How many Neutrino Telescopes ?? It will be important to “observe” the Universe in the whole solid angle Gamma ray flux >100 MeV observed by EGRET Mkn421 Mkn501 Mkn501 SS433 invisible Crab SS433 Crab invisible VELA VELA GalacFc GalacFc Centre Centre From South Pole: ICECUBE From Mediterranean Sea : ANTARES, KM3NeT 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 6
AN ANTAR ARES : : A st stronomy with N eu o T el e and A by . RE RES ea eutr trino elesc escop ope a byss en envi viron onm. earch 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 7
Th The KM KM3N 3NeT T neutri rino o Telescop opes: same me technol ology ogy, 2 2 detector ors Basic ac've element: Digital Op'cal Module 31 x 3” PMTs Talk by BRUIJN, Ronald in Neutrino #4 ORCA ARCA Depth ∼ 2500 m • Depth ∼ 3500 m • One block of 115 D.U. TWO blockS of 115 D.U. Average distance between D.U. ∼ 20 m • Average distance between D.U. ∼ 90 m • Average vertical distance between • Vertical distance between DOMs ∼ 36 m • DOMs ∼ 9 m Volume ≈ (0.5 x 2) km 3 ≈ 1 Gton Volume ≈ 8 Mton Detection Unit: 18 DOMs/line ARCA/ORCA = Astroparticle/Oscillation Research with Cosmics in the Abyss 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 8
Ne Neut utrino no Telescope pe ph physic’s goals: 1 1 - se search ch for poin int-lik like cosm smic ic Neut Ne utrino no Sour urces Extragalactic Pulsar Wind Nebulae Galactic Supernova Remnants Microquasars RX J1713.73946HESS Their identification requires a detector with accurate angular reconstruction: !(# $ ) < '. )° +,- . $ > 0123 Experimental signal : staDsDcal evidence of an excess of events coming from the same direcDon 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 9
Ne Neut utrino no Telescope pe ph physic’s goals: 2 2 - se search ch for Di Diffu fuse fl flux of of Cos osmic Ne Neutrinos os • Neutrinos from: • Unresolved AGN • "Z-bursts" Search • "GZK like" proton-CMB interactions here !!! • Top-Down models Neutrinos • …. Their iden)fica)on out of the more intense background of atmospheric neutrinos (and µ ) is possible at very high energies (E µ >> TeV) and requires good energy reconstruc)on. • Strong correlation with High Energy C.R. studies: for a GZK neutrino ! " ~ 10 &' ! ( 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 10
Ri Rich program m of physics in a large e Ener ergy Ra Range ANTARES & KM3NeT/ORCA ANTARES & KM3NeT/ARCA ANTARES & KM3NeT/ARCA Low Energy Medium Energy High Energy !"# < % & < 100 )"# 10 G "# < % & < 1 :"# % & > 1 :"# * +,-.//01.+2, Indirect search for Dark Ma2er * 53+6 "<1301"33",13.0/ ,+83-", • • • * .213.2,.- 43+4"31.", Search for Monopoles, nuclearites Origin and production • • • mechanism of H.E. Cosmic Rays * 53+6 784"32+90" • … and also oceanography, biology, seismology, … Earth and Sea sciences 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 11
Se Search chin ing for sin single le poin int t lik like so source ces, s, la latest t resu sults lts Data sample: 11 years (3136 days of livetime) track and cascade analysis Full sky search upper limits and sensitivities The most significant cluster • α=343.7° δ=+23.6° • p-value: pre-trial 1.5 10 -6 (4.8 σ) post trial 0.23 (1.2 σ) • 3 track events within 1° 15 tracks + 1 shower within 5° G. Illuminati, S. Navas – PoS(ICRC2019)920 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 12
ANTARES: S: se search chin ing for exce cess ss of events s stack ckin ing se several l so source ces Data sample: 11 years (3136 days of live6me) track events analysis Blazar MG3J225517+2409 α=343.78° δ=+24.19 ° FERMI 3FGL 5° J. Aublin – PoS(ICRC2019)840 J22551.1+2411 2° 1° IC EHE #3 The most significant population is the Radio-galaxies Red dashed lines: arrival time of IceCube EHE IC#3 event (track #3) Blue dashed lines: arrival time of ANTARES events with Δ" #$%&'()* < 2° Fermi gamma-ray flux for the BL Lac 3FGL J22551.1+2411 Radio-Galaxy 3C403: α=298.06° δ=+2.5° 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 13
or n fr KM KM3NeT eT/AR ARCA: CA: sen ensi0v 0vity for from g galac0c s sour urces Select sources with observed intense g fluxes - Assume: g originated in hadronic processes - ! + # → % & + ' (and also ! + # → % ± + ') ↪ % & → # # (and also ↪ % ± → + , - ) Assume the source transparent (to g ) - From the observed g spectra/flux evaluate the - expected n flux R. Coniglione – PoS(ICRC2019)006 Then is possible to evaluate the time needed for KM3NeT/ARCA to DISCOVER, with 3 s statistical accuracy, the selected sources: ∼ 5 years for the SNR RXJ1713 • ∼ 3 years stacking RXJ1713 & Vela Jr • 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 14
ANTARES: S: se search chin ing for Dif iffuse se flu lux x of Cosm smic ic Neutrin inos The IceCube result stated the existence of a diffuse flux of neutrinos in 11 years data sample (2007-2018): excess to the atmospheric component: Observed: 27 tracks + 23 showers = 50 events - no known point-like sourc e has been associated to this flux Expected bkg: 19.9 tracks and 16.2 showers= 36.1±8.7 events - events collected as - "up-going" (muon tracks) agree with a energy spectrum index 1.8 s excess with respect to the atmospheric n flux ! = #. %& ± (. %& - "all sky events" , mainly cascade, agree with a "softer spectrum" , = %. ) ± % - %( +. /01 +% 23 +# 4 +% (.&& ) ( ! = #. ) ± (. (* or ! = #. * ± +&.* ! = #. & ± (. 5 ANTARES, even with lower statistics can contribute to clarify the issue L. Fusco - PoS(ICRC2019)891 10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 15
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