Recent results status and perspectives from ANTARES and KM3NeT - - PowerPoint PPT Presentation
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
Antonio Capone
10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 1
10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy
Multimessengers astronomy !!
2
Not discussed in this talk
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?
microwave X-rays gamma-rays neutrinos cosmic rays
Multi-wavelength astronomy
Large part of the Universe is
spectrum
If we would "observe" the sky with photons with wavelength < 10-21 m ⟺ energy > 103 TeV we probably would see this map
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This is our region
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Neutrinos from cosmic sources induce 1-100 muon evts/y in a km3 Neutrino Telescope Up-going µ from neutrinos generated in atm. showers S/N ~ 10-4 Down-going µ from atm. showers S/N ~ 10-6 at 3500m w.e. depth
p, nuclei p, nuclei
Search for neutrino induced events, mainly !"# → " %, deep underwater
Picture from ANTARES up-going neutrino µ direction reconstructed from the arrival time of Cherenkov photons on the Optical Modules: needed good measurement of PMT hits, s(t)~1ns, and good knowledge
PMT positions: (s ~10cm) Cherenkov Neutrino Telescope 43°
water/ice rock charge current interactions
§ Search for neutrinos with En>1÷10 TeV
before being stopped
For &! ≥ ( )*+ ,!"~
..0° &! [)*+]
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Gamma ray flux >100 MeV observed by EGRET
It will be important to “observe” the Universe in the whole solid angle From South Pole: ICECUBE From Mediterranean Sea : ANTARES, KM3NeT
Crab VELA GalacFc Centre invisible invisible SS433 Mkn501 Mkn421 Crab VELA GalacFc Centre SS433 Mkn501
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Basic ac've element: Digital Op'cal Module 31 x 3” PMTs
Detection Unit: 18 DOMs/line
ORCA
One block of 115 D.U.
DOMs ∼9 m Volume ≈ 8 Mton
ARCA
TWO blockS of 115 D.U.
Volume ≈ (0.5 x 2) km3 ≈ 1 Gton
ARCA/ORCA = Astroparticle/Oscillation Research with Cosmics in the Abyss Talk by BRUIJN, Ronald in Neutrino #4
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Extragalactic Galactic
Pulsar Wind Nebulae Supernova Remnants RX J1713.73946HESS Microquasars
Their identification requires a detector with accurate angular reconstruction: !(#$) < '. )° +,- .$ > 0123
Experimental signal : staDsDcal evidence of an excess of events coming from the same direcDon
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for a GZK neutrino !"~ 10&'!(
Their iden)fica)on out of the more intense background
high energies (Eµ >> TeV) and requires good energy reconstruc)on.
Search here !!!
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… and also oceanography, biology, seismology, … Earth and Sea sciences
Low Energy !"# < %& < 100 )"#
Medium Energy 10 G"# < %& < 1 :"#
High Energy %& > 1 :"#
mechanism of H.E. Cosmic Rays ANTARES & KM3NeT/ORCA ANTARES & KM3NeT/ARCA ANTARES & KM3NeT/ARCA
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Data sample: 11 years (3136 days of livetime) track and cascade analysis
The most significant cluster
post trial 0.23 (1.2 σ)
15 tracks + 1 shower within 5°
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Data sample: 11 years (3136 days of live6me) track events analysis
Blue dashed lines: arrival time of ANTARES events with Δ"#$%&'()* < 2°
Fermi gamma-ray flux for the BL Lac 3FGL J22551.1+2411
Red dashed lines: arrival time of IceCube EHE IC#3 event (track #3)
The most significant population is the Radio-galaxies
Radio-Galaxy 3C403: α=298.06° δ=+2.5° Blazar MG3J225517+2409 α=343.78° δ=+24.19°
1° 2° 5°
IC EHE #3
FERMI 3FGL J22551.1+2411
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! + # → %& + ' (and also ! + # → %± + ') ↪ %& → # # (and also ↪ %±→ +, -)
expected n flux Then is possible to evaluate the time needed for KM3NeT/ARCA to DISCOVER, with 3s statistical accuracy, the selected sources:
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The IceCube result stated the existence of a diffuse flux of neutrinos in excess to the atmospheric component:
! = #. %& ± (. %&
(! = #. ) ± (. (* or ! = #. * ±+&.*
(.&&)
ANTARES, even with lower statistics can contribute to clarify the issue 11 years data sample (2007-2018):
Observed: 27 tracks + 23 showers = 50 events Expected bkg: 19.9 tracks and 16.2 showers= 36.1±8.7 events
1.8s excess with respect to the atmospheric n flux
, = %. ) ± % - %(+. /01+%23+#4+% ! = #. & ± (. 5
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With the assump,on made for the cosmic diffuse neutrino flux (and for the atmospheric one) it is possible to es,mate the ,me needed to measure it with 5s significance:
~" #$%& '()* " +,-+ ./012 ""3 456 ~7. 9 #$%& '()* )*$ :;// +,-+ <$)$1)0& (>?7 456)
years
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Neutralino annihilation in Sun, Earth, Galactic Center
Neutralino search: cc → n+… not discussed in this talk
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Neutralino search: cc → n+… Distribution of the angular distance between reconstructed the track direction of events and the Sun position for two different track reconstruction algorithms in
to maximize the event reconstruction for single line and multi-lines events. µ
Y
Neutrino spectrum from WIMPSIM (M. Blennow, J. Edsjö, T. Ohlsson, J. Cosmol. Astropart. Phys. 0801 (2008) 021. ) Background estimated from time-scrambled data.
Neutrino fluxes from !"#$ + !"#$ → '( ', !*!+, ,*,+ evaluated for 50 GeV/c2 < MWIMP < 5 TeV/c2 à limits to n fluxes and to WIMP-nucleon cross sections
(
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Limits on a neutrino flux coming from the Sun as a function of the WIMP masses for the different channels considered.
Limits on the spin-dependent WIMP-nucleon sca<ering cross-sec=on as a func=on of WIMP mass for the bb ̄, τ+τ− and W+W− channels. Limits on the spin-independent WIMP-nucleon scattering cross-section as a function of WIMP mass for the different channels considered.
No excess observed over the expected background: evaluate 90% C.L. upper limits for expected signal
Physics Le<ers B 759 (2016) 69–74
6 years of ANTARES data: 2007-2012
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11 years of ANTARES data: 2007-2018 - ANTARES ”observes” the G.C > 66% time. Search performed for:
', !*!+, ,*,+, -*-+, .( .
Distribution of measured angles between reconstructed tracks and the Galactic Centre (crosses). The red line describes what is expected from background event.
µ
Y
Parameter NFW Burkert McMillan rs [kpc] 16.1+17.0
−7.89.26+5.6
−4.217.6 ± 7.5
ρlocal [GeV/cm3]
0.471+0.048
−0.0610.487+0.075
−0.0880.390 ± 0.034
The integrated J-Factor, Jint , for a cone-shaped region centred on the G.C. with an opening angle Y
Jint() =
DM · dl · d
The expected n flux depends on the DM distribu\on around the GC. 3 halo models have been considered
No excess found over the expected backg. à limits to < 01 >
dνµ+¯
νµ
dEνµ+ ¯
νµ
= ⟨σ v⟩
8πM2
WIMP
·
dNνµ+¯
νµ
dEνµ+¯
νµ
· Jint(),
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11 years of ANTARES data: 2007-2018 - ANTARES ”observes” the G.C > 66% Bme. Search performed for:
', !*!+, ,*,+, -*-+, .( .
dνµ+¯
νµ
dEνµ+ ¯
νµ
= ⟨σ v⟩
8πM2
WIMP
·
dNνµ+¯
νµ
dEνµ+¯
νµ
· Jint(),
Sensitivity for KM3NeT/ARCA-24 DUs, 1 year comparable: with 11 years of ANTARES
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Limits on the WIMP-WIMP annihilaOon rate in the Earth Limits on the spin independent WIMP-nucleon cross-secOon
ANTARES, Physics of the Dark Universe 16 (2017) 41–48
10/09/2019 Antonio Capone - University La Sapienza and INFN - Roma - Italy 23 90% C.L. upper limits on σpSI as a function of ⟨σAn⟩Earth for mWIMP =52.5 GeV 90% C.L. upper limits on ΓA as a func8on of the WIMP mass.
90% C.L. upper limits on σpSI as a func8on of the WIMP mass for ANTARES 2007–2012 (Earth) and ANTARES 2007–2012 (Sun), assuming ⟨σA#⟩Earth = 3·10−26 cm3 s−1 and WIMP pair annihila8on to 100% into either t+ t- (blue), W+ W- (green) or $% $ (purple).
ANTARES, Physics of the Dark Universe 16 (2017) 41–48
25 Gev/c2 < MWIMP < 1 Tev/c2
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Real-&me (follow-up of the selected neutrino events):
Mul&-messenger correla&on with:
understand the “acceleraDon mechanisms”, the physics inside the source
Time-dependent searches:
Swift, RXTE]
A long list of ac&vi&es:
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ANTARES generate alerts:
AQer On-line reconstrucNon (<delay>: ∼6 s, s(q) ∼0.4°-0.5°) send alerts as Gamma-ray Coordinates Network circular In 10 years 311 alerts set to robo=c telescopes
NO TRANSIENT SOURCE ASSOCIATED SO FAR TO ANTARES ALERTS ANTARES receives a GCN alert:
Follow-up of
Fermi GRBs.) NO NEUTRINO ASSOCIATED TO EXTERNAL ALERTS SO FAR
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12 Lines, 885 OM
3 Building Blocks on 2 Sites 3*115 lines, ~6210 OMs, ~ 192510 PMTs Basic acFve element: Digital OpFcal Module 31 x 3” PMTs 18 OMs/line
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KM3NeT Collabora-on comprises 53 ins-tutes and groups in 44 ci-es in 17 countries on 4 con-nents.
The Detector is in the construc-on phase:
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Optical background (40K) and down-going atmospheric muons can be easily selected/rejected looking at PMT's multiplicity.
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h"ps://arxiv.org/pdf/1906.02704.pdf
Data collected with ARCA (3500m depth) and ORCA (2500m depth)
PMT efficiencies can be equalized using 40K single photon signals Atmospheric muons rate as a function of depth measured by ARCA/ORCA well agree with model
Model by Bugaev et al,
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Selected up-going muon tracks : atmospheric neutrino candidates.
ARCA $%& ~ 100 *+, ORCA $%& ~ .+/ *+, ARCA detected μatm ∼0.2 Hz - natm ∼1/day ORCA detected μatm ∼2 Hz - natm ∼10/day Sel Selec ected ed ∼6 6 neut neutrino nos with h cos(θre
rec)<
)<-0. 0.8 8 MC MC: μatm ∼0. - natm ∼3.3 Sel Selec ected ed ∼77 77 neut neutrino nos MC MC: μatm ∼4. - natm ∼67.5
Very good Data-MC agreement
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