PoS(ICRC2017)1085 http://pos.sissa.it/ ∗† [email protected] Speaker. A footnote may follow. The identification of dark mattervarious experimental particles methods. has Theoretical been studies attempted areas being for dark performed more matter to than propose particle new 30 candidates. particles years of At dark through present, matter particles. we In dothe this not searches brief for have review, I each a will dark clear describe matter the understanding candidate. status about and the persepectives of † ∗ Copyright owned by the author(s) under the terms of the Creative Commons c 35th International Conference 10-20 July, 2017 Bexco, Busan, Korea Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). Yeongduk Kim Overview of DM searches Inst. Basic Science, Korea E-mail: PoS(ICRC2017)1085 ]. 22 6 − , 5 ] and have 7 Yeongduk Kim ] 8 ]. There is compelling 2 , 1 ]. 7 ] are good sources of reviews about dark 9 , 10 , 2 2 ]. WIMPs have been leading candidates [ 8 . The mass of particles ranges from 10 1 Particle candidates for dark matter. The figure is taken from [ Figure 1: eV depending on their nature [ 23 ]. Further observational studies tell us that 26% of the dark component is in the form of 4 , Generally, dark matter particles may interact with or decay into particles be- There is a great puzzle about the universe. Astronomical observations, including the veloci- According to current theoretical research, there are a number of dark matter candidates in 3 matter. evidence that 95% of theble mass [ and energy in the universe is dark in the sense that it is not visi- Many theoretical physicists consider(WIMPs) that are super-symmetric the weakly most probable interactingoccurring particle interactions massive candidates of particles for WIMPs with darklow-background the matter detector nuclei and in of a that normal deep the matter underground extremely environment may [ rarely be measured using a very eV to 10 been searched the most intensively;-like however particles there (ALPs) is are no othersearching clear strong these signal candidates, particles of and are WIMPs recently being several yet. different developed. methods [ of and clumps of dark matter and thedark matter remaining, and 69% the is elucidation homogeneous of its darkin properties contemporary energy. is science The considered because to identification it be of will one affectthe of the the universe basic most and understanding important perhaps of issues provide the insights structure about and origin particle of physics beyond the standard model [ ties of stars and galaxiesuniverse and is gravitational not lensing made measurements, from have the revealed ordinary that matter most of we the are familiar with [ addition to WIMPs as shown in Fig. Overview of DM searches 1. Dark Matter Candidates PoS(ICRC2017)1085 ∼ (2.1) DM Ω ] in 1977. 7 Yeongduk Kim . In addition, we can , which gives 2 ]. We can search for 2 − 11 s 3 cm 26 − 10 1 × − 3 s 3 ∼ i i v cm v 27 ann ann − σ σ h h 10 3 × ], extensive programs are being performed to search 3 12 ∼ 2 h DM Ω Mothods of searching for dark matter particles. Dark matter (DM) particles and standard model WIMPs were first proposed as dark matter particles by B.W. Lee and Weinberg [ The estimated annihilation cross section was Since Goodman and Witten proposed the possibility of searching for WIMPs through direct 22. This consistency with the observed 26% of dark matter contents is referred to as the “miracle.” . The particles considered werelation heavy rate which was interact calculatedremarkable weakly as consistency with with a hadrons, the function current and dark of annihi- matter freezing energy density out in temperature. the universe. The calculation exhibited Figure 2: 2. WIMPs 2.1 WIMP Miracle standard model particles after interactionmatter annihilation with or dark decay matter (indrect search) particles as (direct shown schematically search) in or Fig. from dark (SM) particles can interactdifferent diagram. via three different channels. DM decays can be considered using a slightly Overview of DM searches cause dark matter and visible matter are correlated in the distributionproduce [ and identify dark matter particles throughenergy collisions particle of accelerators. standard model These particles three using strategiesbe high to applied search for for WIMPs dark and mattersterile particles other neutrinos. in dark nature Only matter can the particle direct candidates search such method as has dark been photons, applied for ALPs, axions and until now. scattering of dark matter particles off nuclei [ 0 2.2 Direct Searches PoS(ICRC2017)1085 ]; 13 (2.2) (2.4) (2.3) is the are the are the χ ) 2 ρ q

) ( n ) ( ) p q SD Yeongduk Kim ( S ( 2

SI 2 SD F ]. F ) 13 n factors are calculated SD χ 2 σ c is the dark matter – pro- 2 , i 1 ) n i c n 2 0 S , χ h υ ( k / p SD χ + 2 esc 100 keV; thus they can be mea- σ υ p is Avogadro’s number, SD χ − A ∼ are the dark matter – nucleus spin- e σ is the Earth velocity relative to dark N ) 2 − ) i E r p SD 0 ( υ SD S A E ( h SI A / χ ( SI R χ σ E 1 σ 2 c J χ + χ shows the various techniques and experiments − ρ J e M 3 1 4 3 A 4 c A 2 2 h N n A µ µ r 0 0 π 0 υ R E √ 2 = k A SI = χ = 0 σ ) R esc , υ ) R , is the most probable dark matter velocity and energy respectively, q E ( 2 is the dark matter mass, 0 dE υ 2 SI υ ( χ F χ n M SI are the reduced mass of dark matter particle and the nucleus (nucleon). dR χ M 2 1 σ n 2 µ A = 2 2 n A 0 µ µ E and A = µ A and , SI χ 0 σ esc υ dependence (in the case of spin-independent interaction, A is the mass number of the υ 2 target nucleus). Recoil energy spectrum as expected at low energy. Annual modulation due to the annual motion of theDirectional solar asymmetry system. due to the daily rotation of Earth. A and Here, Recoil energies for the direct detection can be as large as The differential elastic recoil event rate as a function of the recoil energy is expressed as [ is the galactic dark matter particle escaping velocity, is the dark matter – nucleon spin-independent cross section, • • • • n SI χ esc min matter distribution, A is thedark mass matter number local of density, target nucleus, of measuring multiple parameters. υ 2.2.1 Direct Detection Techniques sured using conventional detectors.significantly However, the hinder backgrounds the from searches. environmentalbeta radioactivity and As gamma the rays backgrounds with the areclear detectors, recoil mostly techniques (NR) because of signals differentiating of have these beenvarious the backgrounds signals developed. interactions from which Particle nu- of can interactions be in extractedionized detector using charges. material sensors, Multiple generates scintillation parameter lights, detection vibrational techniquessignals phonons, have from been and electron developed recoil to differentiate (ER) NR signals. Figure Overview of DM searches for the WIMPs. Onedirect critical detection question is experiments that ?” “whatinteractions. kind There of are signal four from different WIMPs do signals we expected expect from in WIMP–nucleus independent (SI) and spin-dependent (SD) cross section respectively. from the integration over theυ relative velocity distribution owing to the motion of the Earth over amount of spin carried by theform proton factor and for neutron spin-independent and groups spin-dependent inside interaction the respectively nucleus, [ and σ ton(neutron) spin-dependent cross section, J is the total spin of the target nucleus, PoS(ICRC2017)1085 ], 23 year. · Yeongduk Kim ] experiment, mea- ] detectors measure 14 15 ] experiments. The double phase exper- 21 5 ] experiments detect the total energy deposited inside absorber ], and DarkSide-50 [ 17 25 ] and PICO [ 16 ], XENON1T [ year, among the double phase noble gas experiments. All double phase experiments shows the status of current double phase noble gas detectors, i.e., the LUX [ 24 · 4 Techniques utilized by the direct dark matter search experiments. The three signals from dark Figure In addition, there are single-parameter detectors for direct dark matter detection. NaI(Tl) The DAMIC [ Double phase noble gas detectors are the most interesting developments for direct dark mat- PANDAX-II [ iments confine the fiducial volumematter for detection background is rejection, considerably andobtained smaller the by than fiducial multiplying mass the fiducial used total mass for mass by dark used data for collection the time detectors. in units Exposure of, is for example, kg 2.2.2 Noble Gas Experiments Figure 3: matter interaction, scintillation, ionization, and phonon signalsparameter are measurements measured are in critical various to experiments. differentiate Double nuclear recoil events from electron recoil backgrounds. crystal experiments, i.e., DAMA, COSINE, andwhile ANAIS, measure XMASS and the DEAP scintillation measure lights scintillation in lightsexperiments crystals from measure noble gases. ionization The CDEX only andSuperCDMS for CDMSlite group lower has detection developed thresholds HVionization in sensors detectors to cryogenic with lower detectors. the only threshold. phonon the sensors on each face and no scintillation lights and phonons instead of ionization. The most recently reported data areposure, from 98 the kg XENON1T experiment and they show the largest ex- material. ter detection. They provide advantagesAmong in detectors, fiducial noble volume gas confinement liquids and suchmatter particle as experiments. liquid identification. Another multi-parameter or detector, liquid i.e., argon the SuperCDMS are [ used the most for dark Overview of DM searches sures ionization and phonons at low temperature conditions. The CRESST [ PoS(ICRC2017)1085 ]. ], 25 19 ], and 25 Yeongduk Kim ], XENON1T [ ], and XENON1T [ 24 23 ], LUX [ 24 ], PANDAX-II [ 23 as shown in the figure. The value of PANDAX-II ] , PANDAX-II [ 6 22 exposure √ / ] , XENON100 [ 21 ]). ], DarkSide-50 [ 21 20 Lowest limits reported in each experiment as a function of the exposure for XENON10 [ Specifications of current double phase noble gas detectors. Exposure and Limit are the values The noble gas double phase experiments reported the lowest limits for the WIMP-nucleon shows the lowest limits reported in all the experiments until now as a function of the maximum PANDAX-I [ DarkSide-50 [ Figure 5: exposure reported by eachzero, experiment. the limits As are proportional the tois backgrounds 1 higher in than expected the limits signal bynot a window clear. factor are of basically approximately two, and the reason for this is currently spin-independent cross section achieved at certain WIMP5 masses in a range of 30 – 50 GeV. Figure Figure 4: reported in the most updated data for each experiments (LUX [ Overview of DM searches reported basically zero background databands. inside the signal gate set by neutron and gamma source PoS(ICRC2017)1085 γ , β Yeongduk Kim ]. The initial data for DEAP- 28 [ ] is the largest scale experiment 2 c 26 / with the expected sensitivity for cross 6 hitting atmospheric backgrounds. 2 cm 49 7 ) using two types of cryogenic detectors (HV and . DARWIN [ − 2 2 c / year is the largest exposure with the fiducial volume cm · 48 − 10GeV ]. ≤ year for only 4.44 days of live time data collection. No candidate 27 Proposed double phase noble gas experiments. · for a WIMP mass of 100GeV 2 cm 44 Figure 6: 10 × 2 . DEAP-3600 is a single-phase liquid argon (LAr) detector with a capacity of 3600kg; it is SuperCDMS SNOLAB is a next-generation experiment aimed at directly detecting low-mass There are two single phase noble gas detectors running at present. The XMASS-I detector As the noble gas double phase detectors are the most successful for high mass WIMP search, backgrounds using only primary scintillationtons light. and The the exposure fiducial is mass 27.0 forsignal kg events the are first observed, analysis which results is incross 2.22 the section upper as limit of 1 the WIMP-nucleon spin-independent installed 2 km underground atthe SNOLAB LAr (Sudbury, scintillation Canada). timing The of substantial NRs difference and between ERs allows for sufficient rejection of the dominant dark matter particles (with masses section limits. The LZ and XENONnTThey experiments could are under reach development to a bewith cross run a around section fiducial 2020. mass of of 10 As 30 DARWIN tons; will it barely can touch reach theliquid 10 neutrino xenon double backgrounds, phase at experiment least should oneWIMPs be approximately performed using whether 30-ton the or LZ scale not or we XENONnT detect detectors. some hints of at the Kamioka laboratory642 consists hexagonal of PMTs mounted 832kg on of anA inner LXe fiducial spherical filled surface volume with as within a angenerated radius a of active in reconstructed approximately scintillation the 40cm. radius target detector of with surface. 20cm is 200 selected kg to reduce the event that is 3600 show potential upgrade to adouble larger phase mass detectors. detector for high mass WIMPs compatible with LXe 2.2.3 Cryogenic Experiments larger scale experiments are proposed, as shown in Fig. Overview of DM searches confinement among noble gas detectors,spectrum and in WIMP the limits fiducial are volume [ provided based on the background PoS(ICRC2017)1085 ]. At 0012 . 0 18 100eV, because ± 2 = c th / ] by CDMS Yeongduk Kim 29 0112 . 5GeV ∼ day data) is shown in · 7 days for 14 years of data ± for a dark matter particle mass of 1 2 eV was reached with the 24 g CaWO4 ) as a light absorber which is referred to ) cm 3 2 . 43 5 10 ± 4mm . × 6 0 . 8 1 × ∼ 190 20 ], CRESST, and CDMS-Si experiments. Howevr, except = ( × th 30 ) as target material, which is referred to as the phonon detector, 250g). 3 , while iZIPs provide better sensitivity above ∼ 2 c / 10mm × ]. The mass of the CRESST-III detector module is significantly lower than 5GeV ]. Therefore, at present, there is no strong indication for low mass WIMPs 20 18 ≤ 30 × . 7 and with a capacity to continue exploration of smaller masses and better sensitivities. crystal (20 2 4 . The solid lines represent experimental data and the dashed lines represent the expected . c 7 7 / DAMA/LIBRA data clearly show annual modulation with an amplitude of 0 Two detector designs, denoted by HV and iZIP, have common physical dimensions (100 mm in A prototype CRESST-III module has successfully been tested in a cryogenic setup above The plot of spin-indendent WIMP-nucleon cross sections versus WIMP mass is shown in The CRESST group is updating their low mass search experiment with scintillating crystals counts/keV/kg/day (differential rate unit, dru) and a phase of 144 except the annual modulation data reported by the DAMA/LIBRA experiment. 2.2.5 DAMA Experiment crystal. This is the lowestdemonstrates threshold that reported the for main direct design goal dark of mattershould CRESST-III phase search be 1, easily experiments. namely, a achieved The threshold when result of the E detectorspresent, are 10 operated CRESST-III detector in the modules low-noise are CRESSTGran assembled setup Sasso and [ laboratory. mounted The in expected the sensitivity CRESSTFig. for setup CRESST at (with the 1000 kg group. The SuperCDMS and CRESSTbelow experiments are 10 leading GeV; the however, searches for approximatelybackgrounds. low There three mass were WIMPs orders several claims of thatcluding magnitudes low the mass are DAMA/LIBRA, CoGENT WIMP left [ signals may over have solar been detected, neutrino in- limits of future experiments. The plot is produced using the WIMP limit plotter [ diameter and 33.3 mm thick) and areEach fabricated Ge(Si) from the crystal same has materials a using masssensitivity the same for of techniques. mass 1.39(0.61) kg. The HV detectors are designed to provide better that of the CRESST-II crystals ( ground. An NR energy threshold of E 2.2.4 Current Limits Fig. GeV of their capability to discriminatephonon sensors between on ER each and face with NRbetter no interactions. phonon ionization collection sensors. HV and The thus detectors phonon-only better sensorrecoil consist phonon layout energies of energy allows compared resolution for six to and a detector sensitivityis similar at shown iZIP lower in detector. Fig. The expected sensitivity for the Ge HV setup and a silicon-on-sapphire (SOS) discas (20 the light detector [ DAMA/LIBRA, CRESST and CDMS groups confirmed thatdata, there is and no the signal CoGENT persistent with experimentground more reported estimation lower [ significance owing to the uncertainty in back- connected to transition-edge-sensors (TES).CaWO The CRESST-III detector module consists of a 24g Overview of DM searches iZIP) and two target materialsan (germanium initial and sensitivity silicon). to NR The cross experiment sections is of being designed with PoS(ICRC2017)1085 ]. 34 Yeongduk Kim 9 ], and the neutrons from deep underground cosmic 35 ]. 37 , 36 ]. 29 ]. In addition, the modulation phase of DAMA/LIBRA is faster by a 33 , 37 ] provided an upper limit of 0.0119 dru with 90% confidence for the same 38 The spin-indendent WIMP-nucleon cross sections versus WIMP mass. The solid lines are ]. As and the neutrons induced by underground muons modulate in phases similar 32 The analysis for potential annual modulation signals from several experiments has been re- There was theoretical speculation that the phase difference between flux modulation and , 31 ported. KIMS-CsI [ As the phase ofminor the contribution modulations of the of neutrons solar fromof neutrinos solar the neutrino is DAMA interactions detector opposite with could to the shiftwith surrounding the that the materials phase of more by quantitative atmospheric a simulations month. muons,the with However, neutrino a this realistic interactions argument experimental are is conditions. extremely not few consistent The [ neutrons from the DAMA modulation is owing to the contribution on the neutron flux from solar neutrinos [ experimental data and dashed linesWIMP are limit expected plotter limits by CDMS for group future [ experiments. The plot is produced using [ to the DAMA/LIBRA data, itbe is due natural to to the speculatethat cosmic that the muons. the flux origin of However, neutrons of detailedmodulation at DAMA/LIBRA simulation amplitude the data [ with DAMA may underground detector muon locationmonth is flux compared to too shows the low phases to of explain thelaboratory. modulation the by DAMA/LIBRA neutrons or muons measured at the Gran Sasso Figure 7: muons are not sufficiently abundant [ Overview of DM searches PoS(ICRC2017)1085 . σ . In addi- ) ]. Yeongduk Kim day ], and COSINE · 44 , 48 ] provided a mod- kg · 43 39 , nr 42 ] with an upper limit of keV 41 ( / ], PICO-LON [ 47 compared to the expected amplitude of ) day · ], ANAIS [ ton 46 10 · , which is contradictory DAMA data with 5.7 ) keV day ( · / . Even though most direct dark matter experiments are con- ee ton · keV / keV ( 73 events ]. . kg / 0 / 29 ± day / 67 events . syst 7 . events 3 0 ] experiment provided an upper limit of 0.06 events 10 ± 40 × The spin-dendent WIMP-proton cross sections versus WIMP mass. The solid lines are experi- stat ) 2 7 . . 1 3 ± The following four experimental groups are attempting to directly (de)confirm directly DAMA/LIBRA While liquid xenon detectors are being rapidly developed and the upper limits on the WIMP- ∼ ] experiments. Saint-Gobain Crystals, which developed and produced the DAMA/LIBRA crys- 2 7 . . 1 45 The CDMS [ tradictory to the modulation amplitude measured bythat the attempt DAMA group, to there explain are the theoreticalmultaneously DAMA models through modulation WIMP signals interaction and in null the results DAMA/LIBRA detectors from [ other experiments si- data using the same NaI(Tl) crystals; SABRE [ ulation amplitude of 1 ( 12 tals, no longer producesshould the perform ultra-low R&D backgrond from NaI(Tl) theNaI(Tl) crystals. beginning crystals. with It other Therefore, would companies require newthe several to experiments years DAMA/LIBRA develop to crystals. ultra-low develop background crystals The with ANAISof a and approximately quality COSINE 2-5 similar experiments dru to achieved below that the awith of 6 background 112 keV level kg energy crystals region. in Thein the ANAIS the summer group Fall of began of 2017 an 2016. and experiment Thenew COSINE Hamamatsu DAMA group group PMTs began has and 110 collected will kg approximately releaseDAMA/LIBRA crystal 6 the data experiment more data and years in the of the data data near from using future. the the COSINE It and is ANAIS interesting experiments. 2.2.6 to compare New the Techniques mental data and dashed lineslimit are plotter expected by limits CDMS for group future [ experiments. The plot is produced using WIMP energy window of 2–6 keV as DAMA data. The XENON100 experiment [ tion, the XMASS experiment provided results on annual modulation [ [ Figure 8: Overview of DM searches PoS(ICRC2017)1085 (2.5) ].” is the product 54 Yeongduk Kim ]. Another pro- 2 50 2 ]) ]. Ω , 49 s [ ] r 2 ~ ( ]. Inside liquid helium, elementary ? ρ , ds . However, recent measurements could 51 . s s . / o 3 is a good miraculous benchmark value as . l 3 Z cm × 26 cm − ]. This could be because approximately 35GeV 26 SM − 11 10 55 dE ]. The next generation of gram-scale calorimeters dN 10 × 53 7 × × [ . 1 i 3 2 χ 2 c rel ∼ ∼ m / v i is the annihilation cross section of dark matter particles. For i π cleus experiment may extend the reach of dark matter particle σ 8 i h rel is the number of dark matter particles in the solid angle of line rel v − v rel χ 2 = v σ ν is the differential number of standard model particles from each σ I, we can observe scintillation in addition to the bubbles from NR h m h 3 σ / h SM 2 dE ϕ dE ]) d dN Ω d . Ω ) , s 2 [ 9 eV. This low threshold allows to probe elastic scattering of dark matter c . r / ~ 0 ( ρ ± 7 ]. ds . . s . 52 10MeV o [ . ( l 2 R c / The flux of standard model particles from WIMP annhilation, as shown in Fig. Several ideas about new detectors particularly for low mass dark matter particles were pro- Target nuclei should be light to be sensitive to low mass WIMPs below 10 GeV. Helium is one Here, One of the main challenges that are encountered when searching for signatures from dark There were several claims about an excess of gamma rays approximately 1 GeV from the A prototype 0.5g sapphire detector developed by CRESST group has achieved an energy 2.3 Indirect Searches of sight of measurement, described in section 2.1 and it does not depend on WIMP mass [ WIMPs annihilated at a rate of posed in a recent workshop, “US Cosmic Visions : New Ideas in Dark Matter 2017 [ dark matter annihilation, and the annihilation cross section, of the best candidates, and the double phase liquid helium detector is interesting [ matter annihilation in the cosmicand gamma-ray the flux astrophysical is background. the discrimination between a possible signal 2.3.1 Diffuse Gamma-ray Excess galactic center of our , the Milky Way [ posals using liquid helium for WIMP search are appeared [ which will be developed for the masses of O of three factors, i.e.standard model the particles number per of annihilation.WIMP annhilation WIMPs, The can the be differential expressed annihilation standard as model cross ; particle section, flux and from the the number of threshold of 19 particles down to masses of 140MeV Overview of DM searches nucleon cross section in theefforts higher toward WIMP further mass investigation of region low areheated mass material being WIMP rather reduced, search. than there If CF areevents. we considerable The use Scintillating liquid Bubble xenon Chamber as has a been super- demonstrated [ excitations (phonons or rotons) are producedwhich owing have to an the energy WIMP-nucleus interaction. greaterevaporation of Excitations than helium the atoms. binding energy Itelectric was field. of proposed Because helium the to to binding detect the energyscheme these of surface opens atoms helium up can to by new surfaces result ionizing possibilities can them in for beto in below the the 1MeV 1 a detection meV, of this strong detection dark matter particles in a mass range down PoS(ICRC2017)1085 , X Z γ γ , (2.6) → ]. Refer γγ 59 χχ Yeongduk Kim ] . The expected 55 pair measurements, ]. The Icecube and − 59 e ] However, recent data + e 61 , 60  2 X 2 X m m 4 − 1 ) and a second particle (X); for example, 12 γ  X ] for the expected sensitivity of CTA experiment. m 58 = ]. Therefore, a dark matter interpretation of the galactic γ E 56 ] show no enhancements in the energy region of 130 GeV. 63 ]. 58 ] and Fermi-LAT [ shows the 90% confidence limits for the annihilation rate obtained through vari- 62 9 WIMP annihilation rate limits from indirect search experiments reproduced from ref. [ ] for the details of each experiment and [ Another channel that has been studied for dark matter annihilation is neutrinos. Neutrinos from WIMP pairs can annihilate into a photon ( Detections of a linelike feature at 130 GeV have been reported in literature. This feature is Figure H. As dark matter is electrically neutral and has no direct coupling to photons, the 59 γ or process is suppressed. Photons are monochromatic with an energy of Earth, the Sun, and galactic and extra-galactic sources are measured to find excesses in the energy to [ 2.3.3 Decaying Heavy DM search 2.3.2 Line Gammas Figure 9: reported to be strongly correlated with the Galactic center region [ ANTARES data are from neutrino measurements, theand AMS Planck data are is from the cosmic microwavethe background 10-1000 measurement. GeV Generally, mass the region neurino are channelslation less in reported sensitive from to Fermi-LAT other data channels. is The representedsensitivity by indication of the of the region WIMP Cherenkov circled annihi- Telescope in Array red (CTA)shown [ experiment with is a added dashed to line the [ original figure and from HESS [ ous indirect search experiments, reproduced from a reference by Conrad [ center excess cannot be robustly claimed and upper limits are provided. Overview of DM searches not confirm the excess gammacenter rays gamma-ray as excess is due present to overpulsars the estimated can backgrounds, WIMP other annihilations. produce sources similar such Even as excess though milisecond [ the galactic PoS(ICRC2017)1085 ]. for 66 ]. In (3.2) (3.1) 77 , MeV 1 76 ≤ Yeongduk Kim a eV [ m 21 ≤ ]. A recent ovewview eV ] in this conference. 12 74 ] − , 75 67 73  eV a 5 − m a GeV f 7 10 ) 10  GeV ]. / eV 6 15 79 . 13 − 0 10 ∼ × a 3 . f 2 QCD 1 Λ ( ]. However, there are also multiple theoretical explanations ∼ ∼ γ a 72 a , m g 71 eV can be measured, and the direction appeared to be isotropic [ ]. The ICE-CUBE and ANTARES detectors discovered that ultra-high 16 64 ], there have been numerous theoretical models that explain the data based ]. 70 ]. Axions are light, and axion mass is given as , 85 79 69 , 68 is the axion decay constant, and axion mass ranges from 10 a remains unidentified. As decaying heavy dark matter particles are predicted in several f σ Axions are frequently considered as an alternative to WIMPs and have recently received con- Since the Alpha Magnetic Spectrometer (AMS) group first announced their positron and an- Cosmic rays and their secondary backgrounds are highly energetic up to 10 Axions are hypothetical particles associated with the spontaneous breaking of the Peccei- Here, to be between 100 GeV and the Planck scale [ a f models, the observation of high-energy neutrinosat enables one the to corresponding probe mass heavy decaying scales.pothesis dark is matter Fits the are atmospheric performed flux onallows and experimental for diffuse flux data. from astrophysical decaying The flux; dark backgrounddark the matter. matter hy- signal Even lifetime, though hypothesis they the additionally are fits consistent in with the background analyses fluctuations converge [ to a finite siderable experimental attention. Axions candecay of be axions searched in experimentally astrophysical objects, by (2) (1)through-wall” producing searching and experiments), detecting for axions (3) the in detecting laboratories (“shine- searching galactic for axions axions produced using in the theDark Sun microwave or matter cavities, nuclear axions reactors, and can which (4) are be(Primakoff strong searched effect) gamma-ray [ using sources. axion–photon conversion in the presence of EM fields The origin of this high energy neutrinoat flux over with purely 5 atmospheric contribution being disfavoured based on astrophysical sources such as nearby supernovas and pulsars [ on dark matter annihilations[ energy neutrinos up to 10 tiproton data [ Quinn symmetry [ Overview of DM searches region of the detectors [ 2.3.4 Charged Particles of AMS data and theoretical interpretations is presented by A, Kounine [ addition, their rates are several orderssimilar higher energy than region. the Furthermore, expected dark theis matter origin indirect not of signals clearly the for cosmic-ray understood the particlethe yet. acceleration backgrounds mechanism for Therefore, indirect large darkflux matter uncertainties of signals. typically antiparticles, more To exist improve precise in the estimationrequired. of certainty the The the about estimation estimation backgrounds the of with of origin systematic more of uncertainties detailed is the simulations critical is to extract small potential signals. 3. Axions and Axion-Like Particles PoS(ICRC2017)1085 . 13 10 (3.3) = a), axio- ae is axion– g ), where A + a ae ) and axion– A g Yeongduk Kim + ae g e → ] and DFSZ (non- + e 81 , → 80 e + , e is the fine structure constant, ! 3 / α 2 3 a β ), axion–electron ( γ a − g 1

2 e a ), axio-deexcitation (A m ] with an axion–electron coupling of 2 a + E 84 A πα 3 16 . → 14 a 2 ae A β g ) Energy (keV) + a E ( pe σ a), and electron-electron collision ( ) = + is the photoelectric cross section for target nuclei, a E A ( pe 0 2 4 6 8 10 12 1 3 2 0 4 + σ

ae

3.5 2.5 1.5 0.5

e σ

) m year keV (10 Flux

•2 •1 •1 20 → is the axion velocity over the speed of light, A a ] β + 89 a), axio-recombination (e ] models. The strengths of axion–photon ( + 83 ]. The total axion flux produced on Earth from the Sun was recently estimated in ref. e , ) couplings are different for both models. In particular, the axion-electron coupling Flux of solar axions due to Compton scattering, axio-recombination, axio-deexcitation, axio- 89 82 aN → is axion energy, g e a is electron mass. + e γ The cross section for the axio-electric effect is given by The interaction strength of axions is determined by their mass, as mentioned above; however There are two well-known axion models, i.e. the KSVZ (hadronic) [ ], which includes processes with axion-electron and axion-photon couplings, as shown in Fig. . 84 where E electron coupling, Figure 10: bremsstrahlung and electron-electron collisions on Earth [ The figure is from [ and m [ 10 ALPs can have independent coupling and mass. 3.1 Solar Axion Searches with Dark Matter Detectors Overview of DM searches hadronic) [ nucleon ( in the DFSZ model occursis at the strongly tree suppressed level while owingmodel, the to the axion-electron axion-electron coupling processes in coupling related the to ataxion-photon KSVZ coupling axion-electron the model as coupling loop an prevail axion level. overing production the ( mechanism Primakoff Thus, in process, in stars with and the the DFSZ Sun: Compton scatter- is an atom [ bremsstrahlung (e PoS(ICRC2017)1085 ] 92 ]). The 5neV at ]. There- 90 ≤ 96 , Yeongduk Kim eV [ ALP 95 µ m ≤ ≤ 5 . ALP parameter between solar axions ae g -ray spectrum of NGC 1275, which is ]. In addition, ICECUBE and MINOS γ (yellow band). 94 for ALP masses of 0 σ 2 U[ 1 ± 235 GeV ]) show no indication of eV scale sterile neutrinos. 15 12 93 10 × . 11 (green band), and σ 1 ± ] indicated eV scale sterile neutrinos, and the reactor neutrino anomaly [ ] as shown in Fig. eV parameter region of LSND data as neutrino oscillations [ ]. 91 89 90 ∼ , 88 , -ray spectra, provided that ALP mass is sufficiently small (m γ Red curve: LUX 2013 data; 90% C.L. limit on the coupling between solar axions and electrons. 87 , 86 Sterile neutrinos are good candidates for if their mass is at the keV scale. The If ALPs constitute a significant fraction of , then they could be detected Using the measured background specrum for dark matter experiments, one can deduce the Fermi-LAT group searched for spectral irregularities inthe the central galaxy of the Perseusfor cluster. ALPs Using 6 and years excluded of couplings Fermi-LAT data, above they 5 found no evidence was also interpreted owing to theline eV neutrino scale oscillation sterile experiments neutrinos. (NEOS However, [ recentFurthermore results Daya for Bay short data base- indicate thatthe the reactor theoretical neutrino estimation anomaly of is antineutrino due fluxdata to from the exclude uncertainties the in LSND experiment [ 4. Sterile Neutrinos Figure 11: 95% confidence [ Blue curve: 90% C.L. sensitivity, through their coupling toimprint photons on in magnetic fields. Photon–ALP interactions could leave an 3.2 Axion-Like Particle Searches upper limits for the cross section of each energy bin and for the Overview of DM searches and electrons. The LUX, XMASS,limits XENON100, [ KIMS-CsI experiments have provided the upper PoS(ICRC2017)1085 ∼ Yeongduk Kim ), then the energy opacity is shown in γ + 4 ray - a

0 QCD axion QCD ν − 1 IAXOIAXO ALPS IIALPS II ]. This can be interpreted γ eV, including fuzzy dark → 25 97 rm s Globular clusters ν 5 - 10 0

1

∼ ADMX eV 6 - 22 0 − 1 ]. Unfortunately, the Hitomi spacecraft ) 98 ]. V e CTA opacity ( 98

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γ a − m ) V e G ( g 1 = γ E Comparison of Fermi-LAT limits with other works. Other limits are shown in red, expected ] Dark matter candidates become more diverse from 10 If sterile neutrinos decay to active neutrinos with a long halflife ( 90 5keV emission line reported in several low-resolution studies of various massive systems such . of gammas are Newton observatory shows enhancement in the 3.5 keV energy region [ as the decay of 7 keV sterileX-ray neutrinos, spectroscopy which can with form Hitomi the warm was3 dark expected matter to halo. resolve High-resolution theas origin of and the clusters, faint includinglost unidentified the its E Perseus ground cluster contact [ ondiscontinued. 26 March Even 2016, though and data the wereand recovery collected data operation were for by inconsistent a JAXA with was short XMM-Newton subsequently period, data no [ 3.5 keV peak was observed 5. Summary fore, the eV scale sterileinvestigations are neutrino required. indications are becoming weaker; however more experimental sensitivities in green. The parameterblue. space The where QCD ALPs axion could is explainin shown a [ as low a gray shaded band and solid black line. The figure is taken from Fig. 2 matter, , asymmetric darksearch matter, for and dark strongly interacting matterWIMPs, dark more the matter broadly high etc. mass becauseapproximately We region there must 50 will is tons. be no The searchedniques lower preferable with are mass candidate larger being region developed. LXe at requires The or a present. DAMAsearches lower LAr conumdrum will threshold, be should detectors, further For be and developed at solved several for in a new higher the mass tech- scale near WIMPs future. of and improved Indirect sensitivity. Further back- Figure 12: Overview of DM searches PoS(ICRC2017)1085 Yeongduk Kim CDM paradigm should be Λ ].” The backgrounds in direct and indirect dark 99 17 At present, the standard model works extremely well with almost no anomaly. There appear matter searches are obstacles for thepotential searches; new anomaly. however they are also a playground searching for a to be several anomalies; howeverinconsistent they with should all be interpretations confirmedthrough from as rigorous the facts verification and existing processes. should paradigm.and Exploring be experiments more proved should An parameter to be anomaly spaces be pursuedfollowing: can using until be new “Anomaly real appears techniques produced anomalies only are againstprecise confirmed. the and background Thomas far-reaching provided Kuhn that by stated paradigmand the the is, hence paradigm. the of an more The occasion sensitive more for an paradigm indicator change it [ provides of anomaly Overview of DM searches ground understanding is critical ! 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