Pos(ICRC2017)913 , on Behalf of the ANTARES Collab

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PoS(ICRC2017)913 http://pos.sissa.it/ , on behalf of the ANTARES Collab. ∗ [email protected] Speaker. One of the major purposesmatter. of The the ANTARES ANTARES detector neutrino is telescopethe located is southern on French the the coast. indirect bottom search In ofSun, for this the the dark talk Mediterranean Galactic the Sea, Center results 40 and ofpresented. km the the There off Earth search are core, for various advantages dark produced in matter withparing indirect signals searches different to from with analysis other neutrino the methods, experiments. telescopes will whenscattering com- be The cross analysis section between for dark the matter and Suntic hydrogen Center puts and are the good the limits most limits presented stringent for on ofTeV. the the all Galac- indirect spin–dependent detection experiments for WIMP masses above 30 ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 35th International Cosmic Ray Conference —10–20 ICRC2017 July, 2017 Bexco, Busan, Korea IFIC - Instituto de Física Corpuscular, Universitat de València–CSIC, E-46100 Valencia, Spain Department of Physics, Sungkyunkwan University, Seobu 16419, Suwon, South Korea E-mail: Christoph Tönnis Indirect searches for dark matter withneutrino the telescope ANTARES PoS(ICRC2017)913 , 1 1 − s · (1.1) (1.2) ) assuming a SI Christoph Tönnis σ the NFW profile DM and ρ is the WIMP mass and : p SD i χ σ v , σ dl h , m 2 l ∆Ω ) + , θ ν ( dE dN cos ] have been performed using ANTARES. χ 2 2 SC DM 3 , SC ρ m 2 SC π SC ]. ρ 4 2lR 7 R [ SC − 2 3 ∆Ω R − J 2 SC ]. i 5 R v cm 2 · σ q h = 2 DM ν ρ φ dE d max 0 l Z ) = θ ( J are the scaling radius and density. The J-Factor is also needed to relate the SC to the thermally averaged annihilation cross–section ρ ν φ dE d and is the J-Factor integrated over the observation window SC ∆Ω The Sun, however, is sufficiently small to be considered a point–like source, so the source The ANTARES detector, located 40 km off the shore of Toulon in southern France 2500 m One of the main physics goals of neutrino telescopes is the indirect search for dark matter [ The currently most prevalent hypothesis on dark matter is that it is composed of weakly inter- In the search for dark matter in the Milky Way the extension of the source had to be taken is the expected signal neutrino spectrum. For the dark matter halo profile ν ]. The concept behind the search is that dark matter particle accumulate in massive objects either dE dN where R neutrino flux where J was considered with parameters taken from [ extension does not have toare be calculated taken an into equilibrium account.nihilation between When is the limits assumed. accumulation on of dark Thisto dark matter allows spin model matter to dependent parameters in convert and the limits spin Sun independent and and scattering sensitivities their cross–section in an- limits terms ( of neutrino fluxes primordially or via scattering with the matterpairs of the of objects standard and model annihilate inside particles. ofsecondary them, These producing processes. particles then The decay results further, offor producing three neutrinos annihilations of in in these these the searches,proceeding. one Earth Further for and analyses annihilations for one in secluded for the dark annihilations matter Sun, [ one in the Milky Way, are presented in this 2 below the surface ofits the detector Mediterranean medium. sea, is Itin a consists the neutrino of ocean 12, detector, floor 450 which andcontaining m held uses 3 long, up optical the modules. by lines sea An a of water optical buoy.inch electro–optical module as photomultiplier Every is cable, tube a line each (PMT) 17–inch is installed borosilicate of equippedit. sphere the with containing This type 25 a makes Hamamatsu 10– a so–called R7081-20 total storeys, and of each the 900 electronics PMTs in to the control whole detector. acting massive particles (WIMPs) that formfor halos the in WIMP which typically galaxies supersymmetric are particles are embedded. considered. As candidates into account. This extensionJ-Factor. for searches The J-Factor looking is for the annihilationssight. squared is It dark expressed is matter calculated by density by the of so–called the source integrated over the line of Indirect searches for dark matter with the ANTARES neutrino telescope 1. Introduction Maxwellian velocity distribution of theand WIMPs a with local a dark root matter density mean of square 0.3 velocity GeV of 270 km PoS(ICRC2017)913 , µ (1.4) (1.5) (1.6) (1.3) WIMP ¯ is the ν i dE ψ Ch , Det

. Christoph Tönnis µ µ ¯ ¯ tot ν ν N dE dN − ] for the Milky Way. ) s µ 9 n ¯ ν E − ( )) or muon antineutrino energy ¯ eff i ν µ q ν A ν , , i , − p ) , i µ WIMP live th + m ψ is the total live time of the detector. channel is most commonly used as a E ( T µ · Z WIMP , B − ) live − m τ + tot ( τ + µ N ν + τ τ WIMP 90% , , dE ) + µ m i − ¯ ν ( is the supposed number of signal events, q Ch is the energy threshold of the detector and m + , , is assumed. , W s i µ 3 n ν th + p Det Acc ¯ , µ

i Earth W ,E µ µ i , ψ ν ν = are additional event parameters like the reconstruction ¯ ( v b i 1.3 S b A s dE q dN σ n 90% h , ) ( → µ µ ¯ ν ν 10 and + E i µ ( DM ν log eff 1 ¯ + Φ tot = ∑ A i N ] for the Sun and using the code described in [ 8 DM event, p WIMP )) = and a parameter called test statistic is calculated: channel have not been considered for the search for WIMP annihilations th m th s E s n − Z ( µ L ( + is the 90% C.l. sensitivity or limit and T ) = 10 µ is the signal neutrino spectrum at the position of the detector for one particular is the effective area for the muon neutrino energy E Ch ) , log 90% Ch µ , , and ν µ ¯ ν E ¯ Det ν ( +

ν WIMP µ µ eff ν ν ν m ¯ µ ( dE dN For the analyses presented here a maximum likelihood algorithm was used. This algorithm The sensitivities and limits are then converted to neutrino fluxes using a quantity referred to as Pseudo experiments are then used to study the behaviour of the likelihood function. A pseudo For the Earth no equilibrium can be asserted andTo remain instead independent a of particle value dark for matter models, the limits thermally are calculated averaged using so–called an- The is the total number of reconstructed events, , ¯ µ Acc tot ν searches for signals using a likelihood function. For this analysis the likelihood has the form: annihilation channel Ch listed in equation acceptance. The acceptance is defined as: where A E is the WIMP mass.same The number effective of area, events, which issensitivities is calculated on from the the the size fluxes Monte are of then Carlo a calculated simulation. 100%-efficient by: The detector 90% giving C.L. the limits and where experiment is a simulatedgiven event number distribution, of generated fake from signalmised a events. with background regards For to estimate each n including pseudo a experiment the likelihood function is opti- quality or the estimated neutrinoand energy. B S is represents a the function ANTARES that point represents spread the function behaviour (PSF) of the background. annihilation cross section in the Earth, nihilation channels. An annihilation channel islead the assumption to that the all same WIMP pair annihilations of initially standard model particles. There are five channels that were considered: Indirect searches for dark matter with the ANTARES neutrino telescope N angular position of the i in the Sun and thebenchmark Earth for to comparisons simplify between the experiments. analysis.calculated When The for the the expected Sun, the neutrino absorption signalIn of spectra both neutrinos are cases in the neutrino solar oscillations plasmausing were has the accounted to WIMPSIM for be code taken in [ into the account. calculations, which were carried out PoS(ICRC2017)913 . ] 1 12 (1.7) ] and LUX [ 3 the limits on the Christoph Tönnis ] 11 2 2 10 channel) - channel) channel) - - [GeV/c W channel) τ + - W + χ τ + τ + τ m ], PandaX-II [

), the obtained limits are more ux 2014-16 ux 2 L 10 c / . are calculated from the overlap of the ) ) s 90% 0 n ( µ (

L PandaX-II (2016) PandaX-II L 2 ANTARES 2007-2012 bb channel) (Earth, ANTARES 2007-2012 (Earth, ANTARES 2007-2012 W (Earth, ANTARES channel) 2007-2012 bb (Sun, ANTARES 2007-2012 (Sun, ANTARES 2007-2012 W (Sun, ANTARES 4 10 10 log = . Results from IceCube-79 [ 1 − TS s 3 cm 26 − 10 · 3 = IceCube 2011-2012 Earth i v -1 -2 -9 -7 -8 -3 -6 -5 -4 A -10 σ

h 10 10 10 10 10 10 10 10 10 SI scattering cross section [pb] section cross scattering SI 10 Limits on the spin–independent WIMP–nucleon scattering cross–section as a function of WIMP The indirect search for dark matter in the Sun was performed using a dataset that was collected For the search for Dark matter annihilations in the Earth data recorded from 2007 to 2012 spin dependent scattering cross–section are compared to the results from other experiments. At low 3. Search in the Sun between 2007 and 2012. In thatspin dataset dependent no and spin signiﬁcant independent excess scattering was cross–section found were and set. therefore In limits Figure on the mass assuming are shown as well. Figure 1: Indirect searches for dark matter with the ANTARES neutrino telescope The sensitivities in terms of detected signal events For masses of the WIMP closestringent to than the mass those of obtained iron by nuclei other (50GeV indirect searches. have been used. Upper limits atindependent 90% scattering C.L. cross-section on of the WIMPs WIMPchannels. to annihilation A nucleons rate comparison were in of the calculated these Earth for limits and three to the annihilation the spin results of other experiments is presented in Figure distribution of TS values for differentnumber numbers of of signal inserted events fake are signaldistributions then of events. pseudo calculated Upper experiments. comparing limits the on the TS value of the actual2. data to Search in the the TS Earth PoS(ICRC2017)913 • W + Christoph Tönnis 4 IceCube W 10 they can usually not [GeV] p SD • τ

σ + τ WIMP M IceCube ]. 3 10 18 XENON100 (this work) b 2 b (this work) • ], XENON100 [ 5 (this work) ANTARES b • W 10 τ +

+ 17 τ is much more favourable since the limits shown there • τ IceCube b 3

ANTARES W + τ ANTARES . Direct detection experiments, being designed for a high 2 ], SuperK [ channels. Limits given by other experiments are also shown: Ice- SuperK 16 10 − W PICO•60 + W PICO•2L and ], PICO-2L [ − 15 τ ], which did not include limits on the spin independent cross–section. + 1 1 τ 5 2 3 4 1 − the spin independent scattering cross section limit is shown in comparison to other − − − − 13

SD 10 ¯

[pb] 10 10 10 10 b 3 σ p b Limits on the spin–dependent WIMP–nucleon scattering cross–section as a function of WIMP ], PICO-60 [ 13 The comparison to IceCube in figure Since direct detection experiments are not designed to be sensitive to In figure did only use muon tracks andtype a of smaller search data [ sample as the most recent IceCube publication for this mass for the Figure 2: Cube [ sensitivity to spin independent scattering,neutrino provide experiments. much lower limits in comparison to those from experiments. The spin independent scattering iswhilst dependent the on spin the dependent abundance scattering of depends heliumless on in the prevalent the abundance than Sun, of hydrogen hydrogen. in Sincestringent helium the than is Sun those much the shown spin in independent figure cross–section limits are much less Indirect searches for dark matter with the ANTARES neutrino telescope WIMP masses the SuperKamiokandewith experiment the provides limits the from neutrino most telescopesthe stringent at lowest 100 limits limits. GeV. Above intersecting However that the the comparisonthe IceCube to experiment enormous the generates ANTARES difference limits in is extremely sizebetter close angular between considering resolution the of experiments. ANTARES dueto to This ice. the is smaller possible amount of because scattering of in the water much compared compete with neutrino experiments for thiscan parameter. Only provide the limits bubble chamber in experimentdensity a PICO of similar unpaired order spin. of magnitude because it uses a target material with a high PoS(ICRC2017)913 ], 14 • W . For all WIMP Christoph Tönnis + 4 4 10 IceCube W [GeV] WIMP M b 3 IceCube b 10 (this work) • W + (this work) b (this work) • ANTARES W τ

+ τ 2 ANTARES b 6 10 • τ ANTARES

+ LUX τ ]. SuperK 20 10 XENON100 are compared to those from other experiments in ﬁgure i v ], XENON100 [ σ h 19 1 3 4 5 6 7 8 9 2 10 − − − − − − − − −

10 10 10 10 10 10 10 10

SI 10 [pb] σ ], LUX [ Limits on the spin–independent WIMP–nucleon scattering cross–section as a function of WIMP ]. 17 4 , 3 Gamma ray experiments provide the most stringent limits for WIMP masses lower than 30 Despite the much smaller size of ANTARES in comparison to similar experiments competitive For the search in the Galactic Centre a larger dataset, containing events from 2007The limits to on 2015, TeV. Above that the limits from ANTARESthe are caveat that the the most limits stringent. from HESS Thisprofile use has used the to for Einasto be the halo considered profile, ANTARES limit. which with is less cuspy than the NFW 5. Conclusions limits for the spin dependent scatteringthe cross–section very could strong be constrains provided. thatare were Especially the set positive on currently were the best thermally limitsexperiments. averaged of annihilation all cross–section, neutrino Further that telescopes analyses andwell for even [ supersede the limits Earth from and gamma secluded ray dark matter have been performed as masses above 100 GeV the limits fromorder ANTARES supersede of those magnitude. from IceCube This by comparison morethe is than Galactic favourable one since Centre, ANTARES whilst has IceCube areduces needs good the to visibility effective use towards area a of veto IceCube, to particularly at exclude high atmospheric energies. muons. This veto has been used. Just ashas in been the found case and of limits the on Sun the no thermally significant averaged annihilation excess cross–section above the were set. expected background Figure 3: mass for the different channels considered.SuperK Limits [ given by other experiments are also shown: IceCube [ 4. Search in the Galactic Centre Indirect searches for dark matter with the ANTARES neutrino telescope PoS(ICRC2017)913 , Phys. Christoph Tönnis , MNRAS 414 , as a function of i ]. The results from 5 v 25 σ 10 h , 24 , 23 , , Progress in Particle and ,JCAP 07 016 (2013) 22 WIMP Mass [GeV/c²] WIMP , 21 4 10 A search for Secluded Dark Matter in the Sun 7 3 10 Search for dark matter annihilation in the earth using the - τ + τ - τ , JCAP 05 016 (2016) , JCAP 0801 021 (2008) + - τ τ - Neutrinos from WIMP Annihilations obtained using a Full + τ τ + τ Particle Dark Matter: Evidence, Candidates and Constraints , Phys. of the Dark Univ. 16 41 (2017) Indirect and direct search for dark matter 2 10 Limits on the WIMP-nucleon scattering cross-section from neutrino IceCube GC ANTARES GC ANTARES GC IceCube GC + cascade FERMI dSphs b b b FERMI + MAGIC dSphs b HESS GC Einasto The Dark Matter Halo of the Milky Way, AD 2013 The mass distribution and gravitational potential of the Milky Way PPPC 4 DM ID: A Poor Particle Physicist Cookbook for Dark Matter Indirect , JCAP 0904 009 (2009) , JCAP 1103 051 (2011) 21 27 22 23 24 25 26 20 − − − − − − − − 90% C.L. limits on the thermally averaged annihilation cross–section,

10 10 10 10 10 10 10 10 v> [cm v> < s ]

-1 3 Nuclear Physics 85 1 (2015) Rep. 405 279 (2005) with the ANTARES neutrino telescope ANTARES neutrino telescope 2446 (2015) telescopes Three-Flavor Monte Carlo Approach Detection [2] G. Bertone, D. Hooper, J. Silk, [3] ANTARES Collaboration, S. Adrian-Martinez et al., [4] ANTARES Collaboration, A. Albert et al., [5] F. Nesti, P. Salucci, [6] Paul J. McMillan, [7] G. Wikström, J. Edsjö, [1] M. Klasen, M. Pohl, G. Sigl, [8] M. Blennow, J. Edsjo, T. Ohlsson, [9] M. Cirelli et al., the WIMP mass in comparison to the limits from other experiments [ Figure 4: IceCube and ANTARES were obtained with the NFW proﬁle. References Indirect searches for dark matter with the ANTARES neutrino telescope PoS(ICRC2017)913 , Christoph Tönnis , Phys. Rev. Lett. , JCAP 1604 022 (2016) , Phys. Rev. PRL 114 141301 , Phys. Rev. Lett. 117 11 111301 (2016) , EPJC 76 531 (2016) Search for Neutrinos from Annihilation of Captured Searching for Dark Matter Annihilation from Milky 8 First search for dark matter annihilations in the Earth Improved limits on dark matter annihilation in the Sun Search for dark matter annihilations in the Sun with the Search for Dark Matter Annihilation in the Galactic All-ﬂavour Search for Neutrinos from Dark Matter Limits on spin-dependent WIMP-nucleon cross sections Dark Matter Search Results from 225 Live Days of , Phys. Rev. D 93 6 062004 (2016) Dark Matter Results from First 98.7 Days of Data from the Search for dark matter annihilations towards the inner Results from a search for dark matter in the complete LUX First results from the LUX dark matter experiment at the , Phys. Rev. Lett. 112 091303 (2014) , Phys. Rev. Lett. 111 021301 (2013) Dark Matter Search Results from the PICO-60 CF3I Bubble Improved Dark Matter Search Results from PICO-2L Run-2 , Phys. Rev. Lett., 110 131302 (2013) , EPJ C77 82 (2017) , EPJC 75492 (2015) , Phys. Rev. Lett. 117 121303 (2016) , Phys. Rev. Lett. 109 181301 (2012) , Phys. Rev. D 93 052014 (2016) , Phys. Rev. Lett. 118 021303 (2017) Search for Gamma-ray Emission from Dark Matter Annihilation in the Small Magellanic Cloud with the Fermi Large Area Telescope with the IceCube Detector with the 79-string IceCube detector and implications for supersymmetry 79-string IceCube detector Chamber Phys. Rev. D 93 061101 (2016) Low-Mass Dark Matter Particles in the(2015) Sun by Super-Kamiokande Center with IceCube-79 Annihilations in the Milky Way with IceCube/DeepCore 115 231301 (2015) Wood, Galactic halo from 10 years of observations with H.E.S.S PandaX-II Experiment exposure from 225 live days of XENON100 data Sanford Underground Research Facility XENON100 Data Way Dwarf Spheroidal Galaxies with Six Years of Fermi Large Area Telescope Data [15] PICO Collaboration, C. Amole et al., [16] PICO Collaboration, C. Amole et al., [22] M. G. Aartsen et al., IceCube Collaboration, [17] Super-Kamiokande Collaboration, K. Choi et al., [18] XENON100 Collaboration, E. Aprile et al., [24] R. Caputo, M. R. Buckley, P. Martin, E. Charles, A. M. Brooks, A. Drlica-Wagner, J. M. Gaskins, M. Indirect searches for dark matter with the ANTARES neutrino telescope [10] IceCube Collaboration, M. G. Aartsen et al., [11] PandaX-II Collaboration, Andi Tan et al., [12] LUX Collaboration, D. S. Akerib et al,. [14] IceCube Collaboration, M. G. Aartsen et al., [19] LUX Collaboration, D. S. Akerib et al., [20] XENON100 Collaboration, E. Aprile et al., [23] M. Ackermann et al., Fermi-LAT Collaboration, [25] H. Abdallah et al., HESS Collaboration, [21] M. G. Aartsen et al., IceCube Collaboration, [13] IceCube Collaboration, M. G. Aartsen et al.,