PoS(NOW2018)099 https://pos.sissa.it/ [email protected] [email protected] This manuscript presents a summaryNeutrino of Oscillation the Workshop – parallel NOW session 2018. Vtion The "Particles of topics in new covered the theoretical by Cosmos" the approaches sessionupcoming of and projects. are the ideas a and combina- a selection of recent experimental results and 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). Neutrino Oscillation Workshop (NOW2018) 9 - 16 September, 2018 Rosa Marina (Ostuni, Brindisi, Italy) Karoline Schaeffner GSSI - Gran Sasso Science Institute,E-mail: L’Aquila, 67100, Italy Basudeb Dasgupta Tata Institute of Fundamental Research, HomiE-mail: Bhabha Road, Mumbai 400005, India Particle Physics in the Cosmos: Session Summary PoS(NOW2018)099 and the lightest π CDM cosmology. Λ 75 . 0 − < δ < π 90 . ]. 0 2 − eV [ ) 004 . 0 1 − ]. 1 002 . 0 ( ∼ 1 m discussed that, among the different realizations, the Akhmedov-Rubakov- discussed an extension of the Standard Model with three heavy right-handed CDM standard model of cosmology, a flat Universe dominated by a cosmological con- Λ The Stefano Morisi Session V was devoted to the role of “Particle Physics in the Cosmos.” In the following The generation of the dark matter relic density and the baryon asymmetry of the Universe are Giorgio Arcadi 2.2 Beyond the Standard Model of Cosmology? stant and cold dark matter, isparadigm found is to mostly tested be by in observations excellentmodel at agreement faces very with large problems observations. scales. that However, On have this theWhile even scales been it of dubbed is dwarf as galaxies, possible, the the andobservational small-scale probably crisis explanations, even of it likely, is that these interestingparticle tensions physics. to have wonder A mundane if simple astrophysical model andMeV-scale or that mediator. how does they This the can leads job be to introduces addressed a dark new matter by gauge self-interactions new interaction solving through the an cusp-core, too big to neutrinos. In the proposed mechanism, activeand neutrinos baryon get asymmetry a is mass generated through throughhierarchical the leptogenesis. structure seesaw for Moreover, mechanism they the considered Dirac a neutrinoUnder mass reasonable such matrix, a similar conditions to a the relevant up-typeDirac connection quark between mass neutrino the matrix. CP high scale phase CPneutrino emerges. violation mass and spectrum, Further, low which energy leptogenesis in requires turnIn implies a particular, a the compact relation Dirac between heavy CP low right-handed phase energy is neutrino restricted parameters. in the range active neutrino mass in the range we will give aThe brief topics summary cover, of on the the oneStandard contributions hand, Model to theories of explaining this Cosmology, and the session theoretical baryonthe of asymmetry, frameworks other physics for the hand, beyond new a NOW the dark selection 2018 mattera of workshop. candidates, new latest experimental to results approach on from in WIMPscattering. the and recently WIMP-like very dark active field matter of searches coherent and elastic neutrino-nucleus 2. Theorists’ Perspective 2.1 Explaining the Baryon Asymmetry among the major puzzles ofpuzzle modern is physics. represented by The the probably leptogenesis mechanisms. most popular solution for the second Particle Physics in the Cosmos 1. Introduction Smirnov mechanism ensures a successful baryogenesisModel via with leptogenesis degenerate by right-handed/sterile extending neutrino the with Standard This mass scale high not mass exceeding the degeneracy GeVmasses, is scale. the related, linear in and somenically the scenarios natural. inverse for see-saw, The to the results a generationshowing that of tiny of successful a violation the leptogenesis occurs thorough of SM in numerical the regionsat neutrino of analysis lepton present the and of number, parameter future being these space experimental which scenarios tech- facilities can [ were be probed presented, PoS(NOW2018)099 all . Be- ) 2 ν T ]. New in- ∼ 7 ( ]. The dynamics that 8 ]. As the new interaction ]. 6 9 , which correspond to small ) ` ( interaction can mimic blue primordial ν CDM. A primordial tensor spectrum with pos- ]. interaction is also constrained from CMB scalar 5 Λ , 2 scattering cross-section was either independent of ν 4 , ν 3 0. Therefore DM- ∼ T n 0, i.e., a blue spectrum, also enhances the CMB-B modes at high or proportional to the square of neutrino temperature > ) T 0 ν n CDM cosmology [ T Λ ∼ ( discussed the effects of such non-standard neutrino interactions on primordial discussed a tempting possibility: identifying the new light particle with the discussed the possibility that our Universe is filled with dark radiation, such as focussed on neutrino oscillations in dark backgrounds [ CDM for which Λ interaction can have a larger effect on CMB-B modes. ν Luca Vecchi Josef Pradler Joern Kersten Subhajit Ghosh compared to scale modes of PGW, get enhanceditive compared tensor to spectral index ` tensor spectrum which is amodification UV are characteristic different, of therefore, PGW. However, high thedifferentiate precision shapes between CMB these of B-mode two these scenarios. experiments two shouldmodes, types DM- be of but able these to boundsonly can a be fraction weakened of significantly theDM- in total multicomponent DM DM interacts scenario with where neutrinos. Therefore in a multicomponent model, SM neutrinos or newlogically physics long states, lifetime. that For are neutrinounderground sourced dark rare radiation by event he searches. the discussed decay Forfor the 21cm new of experimental astronomy physics detectability dark and dark in offered matter radiation an with explanation he of cosmo- highlighted the the EDGES implications result [ cause of the new interaction, CMB B-modes at large multipoles completes the Standard Model mustcase be its either effects very decouple heavy from orfar. experiments, very thus weakly-coupled It explaining to the was us: absence arguedbetween in of that the either any Standard neutrino direct Model oscillation evidence and so dark experimentsprobe sectors, of are as light sensitive long new physics to as sectors these very coupled are feeble to very us light. interactions via This the offers neutrino a portal. unique neutrino temperature sterile neutrino associated with the LSND and MiniBooNE anomaly [ gravitational waves which source polarization anisotropies in the CMB as B-modes [ Particle Physics in the Cosmos fail, and diversity problems. In addition,by a the new new light interaction, particle which species keepsfrom interacts the chemical with dark the equilibrium. matter dark in As matter kineticsolves equilibrium a the long result, missing after structure satellites its formation freeze-out problem. issmall-scale Thus, problems suppressed a of at simple small particle scales, physics model which is able to address also suppresses sterile neutrino productionthe by cosmological oscillations neutrino in mass the bound early canthat universe, be this there avoided. is is However, the not hope most possible that recentparticles because studies have of conclude to sterile be neutrino generic productionneutrinos. dark at fermions later that times. mix In at this most case, very the weakly with new the Standard Model teractions of neutrinos can stopstress them responsible from for free damping streaming, GWs,realization, suppressing and neutrinos the thus enhance growth were of PGW coupled and anisotropic In with CMB the dark B-modes. parameter matter space In of maintaining the the electroweak specific model, gauge the invariance. DM- PoS(NOW2018)099 ]. ]. The mass range between 11 10 eV [ µ 3 and masses up to 3 1 − GeV 11 − discussed the possibility of majorons as dark matter. Majorons are the Gold- proposed a new way to most efficiently search for axion-like particles. The dis- Ranjan Laha Julian Heeck Still today the nature of dark matter remains an unsolved puzzle. It was back in the 1970s The most popular dark matter candidate through the past decades is the so-called WIMP covery of high-energy astrophysical neutrinos motivate thephotons presence up of to sources an which can energyabsorbed produce of and a thus can few be PeV. used Gamma-raynear to photons search the at for source axion-like these magnetic particles. energies field, Photon arethe and - Milky most these ALP Way conversion efficiently ALPs magnetic happens can field. back Usinglike convert this HAWC, into technique, CTA, high-energy existing and gamma-rays and LHAASO in upcoming cansensitive gamma-ray to probe detectors, couplings new above parts 10 of the parameter space. LHAASO can be keV and MeV can onlymajorons be can probed be indirectly warm with or the cold dark majoron matter decay depending into on two the photons; underlying keV-scale freeze-in mechanism. stone bosons of spontaneously broken leptonneutrino number masses. and hence Since intimately all connected majoroninteresting to couplings Majorana candidates are heavily for suppressed long-lived byneutrinos dark the seesaw matter. is scale potentially they The are detectable signaturecomplementary with decay to neutrino into the detectors two loop-induced for mono-energetic decays majoron into visible masses particles above [ MeV and when astronomers started to buildvides a overwhelming evidence model for which, the based existenceprecision on level. of a The dark observations matter variety include in of temperatureground, our observations anisotropies baryonic Universe today of at acoustic the pro- a oscillations, cosmic unprecedented type microwave back- and 1a rotation supernovae curves as of well galaxies as .a gravitational However, particle the lensing candidate Standard studies that Model could of explain particle theseter physics observations. requires does Consequently, not physics the provide beyond existence of the dark Standardvery mat- Model, attractive making and this explaining the specific huge fieldto interest in resolve and astroparticle effort physics this taken long-standing incovering mystery. the a particle mass physics The range community list fromblack of ultralight holes. bosons possible (so-called The dark fuzzy latter matter dark gainedfrom candidates matter) particular the to interest is merger massive after of very primordial black the long, holes first by observations the of experiments gravitational LIGO waves and Virgo. (Weakly Interacting Massive Particle). Assuming WIMPUniverse particles and thermally weak-scale produced in interactions the interestinglyThis early is leads often to referred the to correctunlikely. as The relic the WIMP dark WIMP miracle matter miracle, maydetect density. as be interactions hitting considered of dark as the matter the weak particles in starting scalelished earth-bound point by detectors. a of so-called Thereby, chance the a standard seems community global scenario, estab- highly effort whereand to dark coherently directly matter off particles are atomic expected nuclei. to scatter elastically Apart from direct searches dark matter particles can also be Particle Physics in the Cosmos 2.3 Other Dark Matter Candidates 3. Experimentalists’ Perspective 3.1 The Search for WIMP and Light Dark Matter PoS(NOW2018)099 the crystals as target material op- 4 reported on an excess of events Luca Pattavina 4 from the XENON1T collaboration explained is to cryogenic detectors are a cutting edge technology in particu- ]. Furthermore Marco Selvi 13 yr exposure. The experiment obtained a record for their ultra-low · ]. The next phase of the experiment, XENONnT, is already in preparation in the WIMP dark matter community but we should keep in mind that . However, given that with next generation of such experiments most of 2 12 [ Luca Pattavina 2 mass range. CRESST-III employs scintillating CaWO 2 feeling of doom , 24 g) of 26 eV and thus setting a new benchmark in this field which is expected to open 4 Liquid nobel gas searches like XENON1T, LUX, PandaX, DarkSide and their successors (e.g. As reported by Despite enormous efforts within the last decade that extremely pushed the sensitivity to unex- The strategy for the future as erated at mK temperature. Thankslight, to with the a simultaneous separate read-out cryogenic ofsuppressed. light heat, In detector, in 2018, the the the background main first in absorber, stageing and of the CRESST-III region an data of taking unprecedented was interest successfully energy is completed,CaWO strongly threshold achiev- for nuclear recoilsnew frontiers with in their the near best futurewhich detector [ they observe (detector in A, theirnew CRESST-III experimental detectors run in with improved the and low modified energy detectorsclarifications already on regime started this close and observation. is to subject threshold. to further A lar for the investigations of light(Cryogenic dark Rare matter Event thanks to Searchhigh their with sensitivity low the Superconducting energy parameter thresholds. space Thermometers) of The low experimentsub-GeV/c mass CRESST explores dark matter with candidates, being the pathfinder in the for 2019. They aim forachieve an an improvement increase in in sensitivity target by mass a by factor 10 a in factor five three years. XENONnt, and LZ, a DarkSide-20k) reduced are background, the to leadingabove technology about in 10 the GeV/c field ofthe classical parameter WIMP space searches for thebelow classical the WIMP WIMP scale will started be to be ruledasymmetric of dark out interest matter in recently models the also are community. considered low-mass Indark a the dark fruitful matter context matter option of problem, as light they, also dark apart matter connect frombeyond a its the solution generation WIMP-age to of to the trying the toavailable baryon technologies expand asymmetry. and the facilities. search This in reflects different the directions idea and making use of all ampled high level, in particularhit of the direct neutrino detection floor), experiments no (nextconvincingly particle generation detected other experiments at than will the a weak Standard-Model-compatibledark scale. Higgs matter boson The candidates has absence like been of WIMP/WIMP-likecreate a particles a positive or detection axions of and the sterile most neutrinos popular started to Particle Physics in the Cosmos searched for at colliders (missingucts). mass) and in indirect detection experiments (annihilation prod- evening crowns the day. push the sensitivity and fully exploit theto potential further of increase present the and sensitivity near-future toto experimental eventually detect facilities reach WIMPs the using a neutrino double-phase floor. xenonin The time the XENON projection INFN project chamber, Laboratori operated aims Nazionali deep del underground with Gran the Sasso. current They detector, presented XENON1T, the withdays, most a recent corresponding fiducial results to mass obtained of a 1.3 1.0background t, t and a set data the taking strongest campaign upperlarger of than limit 279 6 on GeV/c the WIMP-nucleon cross section for WIMP mass PoS(NOW2018)099 mass 2 ]. The project 15 d) they will be able to give · : a lower energy threshold for NS) was predicted for the first time al- ν Natalia di Marco 5 reported the excellent results obtained with the SEDINE dark matter particle. An upgraded version is presently under 2 presented a novel cryogenic neutrino experiment with the name Phillippe Gros and a comparatively little exposure of O(100kg for a 0.5 GeV/c π 2 Johannes Rothe cm 37 − ]. NEWS-G uses light noble gases to search for dark matter in the sub-GeV/c 10 · 14 NS become a very active and dynamic field of interest since it opens up new opportunities to Coherent Elastic Neutrino-Nucleus Scattering (CE The majority of experiments in the field of direct detection do not find a hint for the detection This is exactly what the COSINUS project (Cryogenic Observatory for SIgnals seen in Next- An alternative to cryogenic detectors but with sensitivity for low mass dark matter is NEWS- ν most 40 years ago andCE in 2017 finally discoveredprobe by physics the beyond COHERENT the collaboration. Standardsterile Model Since neutrinos. such then as the search for a neutrino magnetic moment or region. The NEWS-G projecttector, builds a on 60 the cm experience SPCModane. gathered which The with has goal the been is so-called to operating SEDINEoperate build for now de- it several a at years 140 SNOLAB. cm at diameter theprototype SPC Laboratoire with using Souterrain Ne even higher de as purity targetabove materials, 4.4 nuclei, and which exclude at 90% confidence level (C.L.) cross-sections nuclear recoils and background suppression byNaI-based particle searches. identification, a While completely the new first feature generationenergy for of threshold the cryogenic of NaI about prototype 6 detectors keVgoal arrive thus at of an 1 ask keV, for the still sensitivity of somerecently the improvements light received to detectors funding achieve already to the meets move experimental the fromphase, requirements an [ COSINUS-1 R&D to ainsight physics whether experiment. DAMA Already sees a within nuclear its recoil first signal, or not. 3.2 Coherent Elastic Neutrino-Nucleus Scattering of dark matter yet. Remarkablyyears though, an annual the modulation DAMA/LIBRA signal experiments which observesthe matches since galatic the halo, about expected but signal 20 is from inconsistent darkSince matter with different particles null experiments in results use of diverse numerous target materials, otherpossible a direct if direct dark comparison matter taking of searches. their intobetween results account is dark only certain matter assumptions, and ordinary inclarification matter. of particular the The on DAMA/LIBRA only the claim wayexperiment. is interaction of the providing mechanism use a of fully the model-independent same target material, butgeneration in Underground a Searches) different aims foriodide by as employing in target their material, experimentcurrently just crystals under as of way DAMA/LIBRA. sodium to Yet, testCOSINUS different the will DAMA/LIBRA from not signal other operate (COSINE-100, the experiments ANAIS, NaIscintillation SABRE, that crystals light Pico-lon) as are signal pure created scintillation by detectors adetection which particle solely approach interaction. acquire based the Instead, on COSINUS the makesscintillating use detectors CRESST at of technology: milli-Kelvin a temperatures novel NaI measure two crystalsinteraction, independent signals operated the from as a heat particle low-temperature signaldetection and has the two simultaneously distinctive advantages emitted explained scintillation light. This dual channel construction with a deployment at SNOLAB planned for spring 2019. G (New Experiments With(SPCs) Spheres-Gas), [ an experiment using Spherical Proportional Counters Particle Physics in the Cosmos PoS(NOW2018)099 , (2017) 96 (2017) 102 , (2012) 231301 1705 (2018) no.3, 031103 , Phys. Rev. Lett. 109 121 , Phys. Rev. D NS cross-section within ν , already allow to explore new NS with miniaturized gram-scale ν (2018) no.10, 817 ]. For the full-optimized version they report Johannes Rothe 78 (2017) no.12, 024 16 6 (2018) no.5-6, 1174. 1712 193 CDM cosmology?,” Phys. Rev. Lett. 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Schäffner et al., “A NaI-Based Cryogenic Scintillating Calorimeter: Results from[16] a COSINUS R. Strauss et al., that an energy threshold of belowtarget 10 array eV of is feasible. 10 g For the only, they first aim step NU-CLEUS-10g, for operating a a O(10%) measurement of the CE Particle Physics in the Cosmos NU-CLEUS (ERC grant by R.power Strauss) reactor which and will will allow be fordetectors. operated precision The at measurements detector of moderate concept CE distance relies on toWith cryogenic a calorimeters a based nuclear recent on the NU-CLEUS CRESST demonstrator technology. they operated achieved above an ground ultra-low using threshold sapphire of crystals 19.7 as eV target [ one year of data taking. Thisphysics should, at as explained the by low-energy neutrino frontier which so far was notReferences accessible by other experiments.