Livetime and sensitivity of the ARIANNA Hexagonal ArrayLivetime and sensitivity of the ARIANNA...

Liveme and sensivity of the ARIANNA Hexagonal Array Background emission Operaons Department of Physics and Astronomy, University of California Irvine, CA, USA Cosmic Rays υ Date, time (UTC) 20-00h 20-12h 21-00h 21-12h 22-00h 22-12h Frequency [GHz] 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 Recorded Amplitude [mV] 10 20 30 40 50 60 70 80 90 Date Dec 18 Jan 01 Jan 15 Jan 29 Feb 12 Feb 26 Mar 11 Mar 25 Apr 08 Apr 22 Fraction of Day 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 Stn Livetime Above 0 Deg Above 2.5 Deg Above 5 Deg Above 7.5 Deg Above 10 Deg Above 12.5 Deg Site B Date Dec 18 Jan 01 Jan 15 Jan 29 Feb 12 Feb 26 Mar 11 Mar 25 Apr 08 Apr 22 Fraction of Day 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 Stn Livetime Above 0 Deg Above 2.5 Deg Above 5 Deg Above 7.5 Deg Above 10 Deg Above 12.5 Deg Site C Strong solar burst of December 2014 visible in ARIANNA antennas Burst caused Aurorae that are also visble Antenna detects different areas of Galacc emission during one day Variaon a result of folding the Galacc emission paern with antenna sensivty Array status and hardware 7 staons with four downward point - ing antennas operaonal since 2014 1 staon with two upward poinng antennas for background studies of lower frequencies (site X) Communicaon via long-range wifi and/or Iridium saelites Next-generaon boards for data-acquision, SST 4 channels of 256 samples 2 Giga-samples per second Band of 0.1 - 1 GHz 32 GB of solid state memory Remotely programmable 12 bits of dynamic range Power consumpon less than 6 Was per staon 1 mV RMS trigger sensivity at > 600 MHz trigger band Power and Communicaon Tower for one ARINNA staon on the Ross Ice-Shelf Ultra-high energy cosmic protons will generate neutrinos in interacon with the Cosmic Microwave Background ARIANNA is designed to detect neutrinos at these energies (> 10 7 GeV) [1,2] ARIANNA is also sensive to radio emission of air showers Important/only background at site on the Ross Ice Shelf Extensive Monte Carlo study underway to determine thresholds for air shower detecon Threshold depends on energy and the distance to the shower maximum Upward facing antennas as addional veto for air showers installed First cosmic ray candidates idenfied CoREAS simulaon Storm at the ARIANNA site Repeated failure to establish wifi communicaon Rare hardware issue inter - rupted running of staons, fixed remotely in February No sunlight aﬅer April 21st Plans for next season Install baeries and newest boards at all staons inside the electronics boxes Run solely on Iridium communicaon to study prospects of low power operaon Improve on cosmic ray idenficaon, study antenna sensivity in ice Explore potenal of lower frequencies (> 50 MHz) Future plans Build the full ARIANNA: extend array to 1000 staons Every staon will be an autonomous and independent neutrino detector [1] S.W. Barwick et al., Astro.Part.Phys. 70 (2015) 12-26 [2] C. Reed for the ARIANNA Collaboraon, PoS(ICRC2015)1149, Board: 279 [3] S.W. Barwick et al., IEEE Trans. on Nucl. Sc. (in press) (2015) [4] S.A. Kleinfelder et al., Proc. IEEE Nucl. Sc. Symp. Seale, WA (2014) Simulaons: CORSIKA 7.4005, QGSJET-II-04, FLUKA ARIANN A Anna Nelles and Chris Persichilli for the ARIANNA Collaboraon E [eV] 17 10 18 10 19 10 20 10 ] 1.7 eV -1 sr -1 s -2 J(E) [m ⋅ 2.7 E 15 10 16 10 17 10 18 10 19 10 20 10 21 10 22 10 23 10 Pierre Auger Coll. (2013) HiRes I (2007) HiRes II (2007) KASCADE Grande (2012) KASCADE (2005) IceTop (2013) TA (2012) Liveme with baery Liveme without baery Liveme > 90%, limited by communicaon windows Enourmous gain in liveme by using a backup baery Details in [3,4] Sunlight at ARIANNA site Downward poinng antennas see no flucaon due to posion and back-lobe suppression

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Transcript of Livetime and sensitivity of the ARIANNA Hexagonal ArrayLivetime and sensitivity of the ARIANNA...

Livetime and sensitivity of the ARIANNA Hexagonal Array

Background emission

Operations

Department of Physics and Astronomy, University of California Irvine, CA, USA

Cosmic Rays

Date, time (UTC)20-00h 20-12h 21-00h 21-12h 22-00h 22-12h

Freq

uenc

y [G

Hz]

00.10.20.30.40.50.60.70.80.9

Reco

rded

plitu

de [m

102030405060708090

DateDec 18 Jan 01 Jan 15 Jan 29 Feb 12 Feb 26 Mar 11 Mar 25 Apr 08 Apr 22

Frac

tion

of D

00.10.20.30.40.50.60.70.80.9

Stn Livetime

Above 0 Deg

Above 2.5 Deg

Above 5 Deg

Above 7.5 Deg

Above 10 Deg

Above 12.5 Deg

Site B

DateDec 18 Jan 01 Jan 15 Jan 29 Feb 12 Feb 26 Mar 11 Mar 25 Apr 08 Apr 22

Frac

tion

of D

00.10.20.30.40.50.60.70.80.9

Stn Livetime

Above 0 Deg

Above 2.5 Deg

Above 5 Deg

Above 7.5 Deg

Above 10 Deg

Above 12.5 Deg

Site C

Strong solar burst of December 2014 visible in ARIANNA antennas

Burst caused Aurorae that are also visble

Antenna detects different areas of Galactic emission during one day

Variation a result of folding the Galactic emission pattern with antenna sensitivty

Array status and hardware

7 stations with four downward point-ing antennas operational since 2014

1 station with two upward pointing antennas for background studies of lower frequencies (site X)

Communication via long-range wifi and/or Iridium sattelites

Next-generation boards for data-acquisition, SST

4 channels of 256 samples2 Giga-samples per secondBand of 0.1 - 1 GHz 32 GB of solid state memoryRemotely programmable 12 bits of dynamic rangePower consumption less than 6 Watts per station1 mV RMS trigger sensitivity at > 600 MHz trigger band

Power and Communication Tower for one ARINNA station on the Ross

Ice-Shelf

Ultra-high energy cosmic protons will generate neutrinos in interaction with the Cosmic Microwave Background

ARIANNA is designed to detect neutrinos at these energies (> 107 GeV) [1,2]

ARIANNA is also sensitive to radio emis-sion of air showers

Important/only background at site on the Ross Ice Shelf

Extensive Monte Carlo study underway to determine thresholds for air shower detection

Threshold depends on energy and the distance to the shower maximum

Upward facing antennas as additional veto for air showers installed

First cosmic ray candidates identified

CoREAS simulation

Storm at the ARIANNA siteRepeated failure to establish wifi communication

Rare hardware issue inter-rupted running of stations, fixed remotely in February No sunlight after

April 21st

Plans for next seasonInstall batteries and newest boards at all stations inside the electronics boxesRun solely on Iridium communication to study prospects of low power operationImprove on cosmic ray identification, study antenna sensitivity in iceExplore potential of lower frequencies (> 50 MHz)

Future plansBuild the full ARIANNA: extend array to 1000 stationsEvery station will be an autonomous and independent neutrino detector

[1] S.W. Barwick et al., Astro.Part.Phys. 70 (2015) 12-26[2] C. Reed for the ARIANNA Collaboration, PoS(ICRC2015)1149, Board: 279[3] S.W. Barwick et al., IEEE Trans. on Nucl. Sc. (in press) (2015)[4] S.A. Kleinfelder et al., Proc. IEEE Nucl. Sc. Symp. Seattle, WA (2014)

Simulations:CORSIKA 7.4005, QGSJET-II-04, FLUKA

ARIANN

AAnna Nelles and Chris Persichilli for the ARIANNA Collaboration

E [eV]1710 1810 1910 2010

]1.

7 e

V-1

-1 s

-2 J

(E) [

m⋅

2.7