Eleonora Presani Antares Collaboration Nikhef Amsterdam Concept of

Eleonora Presani Antares Collaboration – Nikhef – Amsterdam

Concept of Neutrino detector • blue light produced by charged particles with v>c/n • optical sensors detect the time and charge produced by light 12/13/2021 Natural radiator is low cost and allows huge instrumented regions Has very little light scattering. Eleonora Presani - NOW 2008 2

The ANTARES neutrino telescope 500 m 15 m 40 km 900 PMTs 12 lines 25 storeys/line 3 PMTs/storey 60 m 12/13/2021 -2475 m Eleonora Presani - NOW 2008 3

June 1889: L’Institut Michel Pacha Status until 2006 (40 km) Oct. ’ 01: MEO Cable Dec. ’ 02: Junction Box Dec. ’ 06: Line 3 Mar. ’ 06: Line 1 12/13/2021 Mar. ’ 05: MILOM Eleonora Presani - NOW 2008 Sept. ’ 06: Line 2 4

Status during 2007 Jan ’ 07: Lines 4 & 5, Line connection Mar. ’ 07: Line 6 Apr. ’ 07: Line 7 Apr. /July ’ 07: MILOM -> IL 07 July ’ 07: Lines 8 & 9 Nov. ’ 07: Line 10 Dec. ’ 07: Line connection 12/13/2021 Eleonora Presani - NOW 2008 5

Detector Completed! March-May 2008: Lines 11 & 12, connection 2008 – 2 xxx: Lots of physics data! 12/13/2021 Eleonora Presani - NOW 2008 6

Software Trigger Full sky trigger: All data sent to shore through Gb links and filtered looking for directions for light signals compatible with a muon track Other available triggers: -1 D Trigger following the Galactic Center - GRB Trigger with GRB stellite alert - Monopole trigger -. . . Trigger rate: 2 -3 Hz (10 Lines) All muons!!! 12/13/2021 Eleonora Presani - NOW 2008 7

Proportion of time < rate Background light rate 12/13/2021 Median counting rate in 10” PMT in Line 1 March 2006 – May 2008 Eleonora Presani - NOW 2008 8

Effective area & angular resolution ANTARES 12 lines 12/13/2021 Eleonora Presani - NOW 2008 9

Time resolution RMS <1 ns On shore laser system Laser In sea LED beacon system 12/13/2021 Optical fibres RMS <1 ns LED beacon Eleonora Presani - NOW 2008 10

Reconstruction of a muon track Online Data filter : • Look for local coincidences (trigger hits) within 20 ns • Ask for ≥ 5 trigger hits μ 12/13/2021 Hit altitude (relative to mid detector) [m] Reconstruction with Line 1: Algorithm minimizes χ2 of PMT hit time vs. altitude to find zenith angle of m track Run 21240 Event 13212 Antares preliminary Zenith θ = 147 o + Eleonora Presani - NOW 2008 Triggered hits Hits used in fit Snapshot hits Hit time [ns] 11

Data taking with the 12 lines detector Detector footprint from atmospheric muons Bright muon bundle event ! Neutrino candidate 12/13/2021 Eleonora Presani - NOW 2008 12

Event Display 12/13/2021 Eleonora Presani - NOW 2008 13

Methods for the search of point -like sources • Different methods has been developed within ANTARES collaboration for the search for point-like sources: EM algorithm ML Ratio Grid/Cluster Unbinned techniques Signal-like 12/13/2021 Background-like Binned techniques Signal-like Eleonora Presani - NOW 2008 Background-like 14

Expected Limits for point sources ANTARES 1 yr 12/13/2021 Eleonora Presani - NOW 2008 15

rate [Hz] Neutrinos? q neutrinos! muon d(q ) Earth cos q

What to do with them? • Dark Matter • Monopoles Solar system Life History of Universe χ decoupling of cosmic micro-wave background 15 billion years Today T = 2. 7 K -ν Galaxy formation ν 400, 000 years T = 3000 K Matter recombination Indirect detection of WIMPs using neutrino telescopes: Ø Ø Ø 1 s Nucleosynthesis Relic WIMPs from the Big Bang traversing the universe undergo 1 multiple γc Me. V elastic interactions with inside a massive celestial object (e. g. the Sun), lose kinetic 10 -6 s µ energy and become gravitationally boundneutrons to the object. quark-hadron transition protons, 1 Ge. V Over time, the WIMP density in the core of the object increases. This enhances the WIMP annihilation rate significantly, resulting in a neutrino 10 flux-11 with s energies Electro-weak phase transition θc = 42º Separation of EM and weak forces up to 400 Ge. V that will reach the Earth. 103 Ge. V light elements These neutrinos can interact through a CC interaction in the vicinity of a neutrino telescope, producing an energetic muon. When traversing the transparent Super-symmetry? medium of the telescope, the muon will emit Cherenkov light. By measuring the time & position of the photons using a 3 D grid of PMTs, the neutrino 10 -35 track s can be. Grand Baryogenesis reconstructed. 15 10 12/13/2021 Ge. V νμ Unification transition 10 -43 s Big Bang Quantum gravity barrier Eleonora Presani NOW 2008 1019 -Ge. V 17

Gamma-Ray Burst What to do with them? Tau Neutrino Name Baloon • Gamma Ray Bursts n t Lollipop • Tau Neutrinos t detector t 1 01 11 01 alert nt x 2– 10 t m Volume Sugardaddy nt 10 Inverted Lollipop (T. De. Young - location of GRB Ice. Cube) Double Bang 12/13/2021 All data nt save t analysis Eleonora Presani - NOW 2008 All data before, during and after GRB 18

Conclusions • ANTARES is completed! • First data are being analyzed and neutrinos are extracted from atmospheric muon background • Calibrations ensure an angular resolution at the level of 0. 2 degrees > 10 Te. V of neutrino energy • The systematic errors are already under study • Astronomy is a reality in ANTARES!! 12/13/2021 Eleonora Presani - NOW 2008 19

Backup slides 12/13/2021 Eleonora Presani - NOW 2008 20

Cable Fix 12/13/2021 Eleonora Presani - NOW 2008 21

Outlook • • The ANTARES collaboration Detector COMPLETED! Performances of Antares Calibration Trigger and reconstruction First results! Expected limits Conclusions 12/13/2021 Eleonora Presani - NOW 2008 22

Amplitude Calibration Example 1: Threshold value in photo electron equivalent units Example 2: Counting rate on single photomultiplier Before calibration 12/13/2021 After calibration Eleonora Presani - NOW 2008 23

Detector understanding Water absorption length OM angular acceptance ± 10% variation 12/13/2021 Eleonora Presani - NOW 2008 Different parameterisations 24

Project history 1996 - 2000 Measurements with autonomous lines 1) Optical background study: 2) Biofouling-sedimentation study: 3) Optical properties study: 15 deployments 4 deployments 28 deployments 45 km long EOC developed in 2001 The Junction box, the heart of the array for data and HV distribution, installed in Dec 2002 works perfectly 12/13/2021 Eleonora Presani - NOW 2008 25

The angular distribution Multi line fit Single line fit 36 neutrinos 78 neutrinos Data Atmospheric Neutrino Monte Carlo Atmospheric Muon Monte Carlo 12/13/2021 Eleonora Presani - NOW 2008 26

GRB Trigger In some cases, data are recorded even before the alert Out of 198 GCN triggers 176 have been handled by Antares DAQ 12/13/2021 Eleonora Presani - NOW 2008 27