Time-dependent search of neutrino emission from X-ray and gamma-ray binaries with the ANTARES telescope

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1 Time-dependent search of neutrino emission from X-ray and gamma-ray binaries with the ANTARES telescope A. Sánchez-Losa (INFN Sezione di Bari) D. Dornic (CPPM) A. Colerio (IFIC) on the behalf of the ANTARES Collaboration

2 String-based detector; Downward-looking (45 ) PMTs; 2475 m deep; 14.5m ~480 m 40 km cable to shore Junction Box ~70 m 100 m 12 detection lines 25 storeys / line 3 PMTs / storey 885 PMTs 1

3 Introdutcion ANTARES: experiment dominated by the backgrounds: atm muon: 10/s atm neutrino: 4-5/day cosmic neutrino: 1-2/year (?) Backgrounds: atm muons, quite easy to remove: zenith+quality cuts atm neutrinos, irreducible isotropic background, low energy: use of energy estimators 2 types of point-source analysis: All sky search: signif. cluster 8-10 ν per 5σ discovery Candidate list: 50 promising sources => 5-6 ν per 5σ discovery Adding the time information: 2-3 ν per 5σ discovery Increase sensitivity by a factor 2-3 For a very short transient (GRB), only 1 ν per source is sufficient!!! 2

4 X-Ray and γ-ray Binaries Binary systems formed by a compact object (neutron star or black hole) + companion star X-Ray Binary (XRB): Traditionally 2 categories: HMXB and LMXB Few cases with confirmed presence of jets by radio detection γ-ray Binary (γrb): HE emission due to interaction of pulsar wind with the intense stellar wind of the companion massive star. As usual only few indications of hadronic component in XRB, only 2 cases: SS433: S. Migliari et al., Science (2002) 4U : M.D. Trigo et al., Nature (2013) The non-thermal emission of the system is surely dominated by leptonic processes but a hadronic component could also be present (not necessary to have jets) Search for time/space correlations between neutrino and X/γ-ray flares 3

5 Source and flare selection: XRBs Selection of 36 XRBs exhibiting outburst periods from the Swift and MAXI catalogues, extended with RXTE/ASM data when available: Swift/BAT Hard X-ray Transient Monitor: HMXR and LMXB with significant time variabilities (variable/flaring/outburst) preselected Daily LCs characterised with a maximum likelihood block (MLB) procedure Flare significance characterised from baseline and its variability Sources with more than one flare above a 5σ significance selected MAXI Light Curves: Same as with Swift, completes possible missed flares not registered by SWIFT RXTE/ASM Light Curves: Same as with Swift, completes possible missed flares not registered by SWIFT/MAXI Time dependent probability: different flares merging weighted by their relatively intensity P sg (t) sample for GX 1+4, made up with flares registered by SWIFT, Rossi and MAXI MJD 4

6 Four γrbs compatible with ANTARES up-going visibility selected: 1FGL J : M.J. Coe et al., Science (2012) [astro-ph/ ] HESS J : S. Bongiorno et al., ApJL (2011) [astro-ph/ ] LS : J. Casares et al., MNRAS (2005) [astro-ph/ ] PSR B : A. Abramowski et al., A&A (2013) [astro-ph/ ] Flaring periods: ON/OFF periods from its periodic burst emission reported in literature (TeV ones for LS ) Source and flare selection: γrbs Name RA DEC Periastron Period (days) Flaring phase ( ) ( ) (MJD) 1FGL J ± ±0.4 HESS J ± ±0.5 LS ± ±0.05 PSR B ± ±0.5 Additionally, Cyg X 3 XRB has been detected outbursting at gamma-ray energies by Fermi-LAT: A. Bodaghee et al.,apj (2013) [astro-ph/ ] Flaring periods: ON/OFF periods Y+ and Y reported in the reference + #ATel 8591 and 9502 astronomy alerts update ( 5

7 Analysis method Unbinned method: minimization of a likelihood ratio Applied to a subsample data in (~2412 days live time) All flavour neutrino: tracks + showers Event selection optimized for the best 3σ model discovery potential Likelihood: max Test statistic: Q = ln L sg+bk ln L sg+bk = σ ch σ i ln n ch sg P ch sg + n ch bk P ch bk n ch sg = n sg A ch cc δ S A TOTAL cc δ S tr sh n sg/bk = n sg/bk +n sg/bk ln L bk MC (ν) Signal: P sg ch α, δ, E, t = PSF ch α, δ P sg ch E P sg t + lag Noise: P ch bk α, δ, E, t = X/γ-ray LCs ANGULAR ENERGY TIME P bk δ P bk E P bk t n sg + n bk PSF tr PSF sh P tr sg E P sg sh E DATA P tr bk δ P sh bk δ P bk t 6

8 Preliminary sensitivities Preliminary sensitivities for the track channel only have been computed Improvement w.r.t. previous analysis: A. Albert et al. JCAP (2017) [astro-ph/ ] Doubled the livetime Extended flaring periods Sensitivities ~4 better than previous U.L. Shower inclusion will improve more dn/de = Φ 90% 0 (E/GeV) -2 E 95%E F 90% = Δt න dn/de de E5% Name RA DEC Φ 90% 0 F 90% ( ) ( ) 10-8 GeV -1 cm -2 s -1 GeV cm -2 1FGL J HESS J LS PSR B Cyg X Name RA DEC Satellite Φ 90% 0 F 90% ( ) ( ) (#flares days) 10-8 GeV -1 cm -2 s -1 GeV cm -2 1A S(#11 417)+M(#2 30) A S(#1 141) A S(#1 3)+M(#5 284) U S(#6 437)+M(#3 278) Aql X S(#7 460)+M(#10 95) AX J S(#1 85) Cir X S(#10 205)+M(#18 478) Cyg X S(#9 1965) EXO S(#3 191)+M(#4 237) GRO J S(#12 614) GRS S(#1 143)+M(#2 264) GS S(#1 1427)+M(#2 13) GS S(#1 136)+M(#3 16) GX S(#9 661)+M(#2 58)+R(#1 93) GX S(#16 579)+M(#1 10) GX S(#5 525)+M(#5 121) H S(#1 107) H S(#7 967)+M(#12 384) H S(#12 772)+M(#3 33) IGR J S(#1 9)+R(#1 61) KS S(#4 324)+M(#10 242) MAXI J M(#2 475) MAXI J M(#3 131) MAXI J S(#2 125)+R(#2 96) MAXI J S(#1 83)+M(#2 18) MXB S(#1 37)+M(#1 2)+R(#1 4) SAX J M(#6 382) SMC X S(#1 90)+M(#1 3) SWIFT J S(#1 46) SWIFT J S(#1 198) SWIFT J S(#1 133)+R(#1 356) SWIFT J S(#2 52)+M(#2 14) V404 Cyg S(#2 89)+M(#1 28)+R(#4 19) XTE J S(#2 210)+M(#12 229) XTE J M(#2 277) XTE J S(#1 61)+M(#1 12)

9 Preliminary sensitivities SENSITIVITY L.A. Anchordoqui et al. ApJ (2003) 8

10 Preliminary sensitivities SENSITIVITY F.L. Vieyro et al. A&A (2012) 9

11 Preliminary sensitivities SENSITIVITY J.F. Zhang et al. MNRAS (2010) 10

12 ANTARES: Most sensitive neutrino telescope in the TeV-PeV range Seeing the southern sky Conclusions Transient searches offer the most sensitive method to look for a neutrino source since backgrounds are significantly suppressed by the time correlation cuts X/γ-ray binaries: promising neutrino sources Search for 36 binaries flaring in X-rays + 4 binaries flaring in gamma-rays Promising preliminary sensitivities for the track only channel 11

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