DOCSLIB.ORG

Pandax-II ! 2015.4.9 Sino-French PPL, Hefei Pandax Dark Matter Search Program

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Pandax-II ! 2015.4.9 Sino-French PPL, Hefei Pandax Dark Matter Search Program Jinping Mountain WIMPs PandaX Dark Matter Search with Liquid Xenon at Jinping Kaixuan Ni! (on behalf of the PandaX Collaboration)! Shanghai Jiao Tong University! from PandaX-I to PandaX-II ! 2015.4.9 Sino-French PPL, Hefei PandaX dark matter search program ❖ 2009.3 SJTU group visited Jinping for the first time! ❖ 2009.4 Proposals submitted for dark matter search with liquid xenon at Jinping! ❖ 2010.1 PandaX collaboration formed, funding supported by SJTU/MOST/NSFC, started to develop the PandaX-I detector at SJTU! ❖ 2012.8 PandaX-I detector moved to CJPL! ❖ 2012.9-2013.9 Two engineering runs carried out for system integration! ❖ 2014.3 Detector fully functional for data taking! ❖ 2014.8 PandaX-I first results (17 days) published! ❖ 2014.11 Another 63 days dark matter data were collected! ❖ 2015 Upgrading from PandaX-I (125-kg) to PandaX-II (500-kg) PandaX Collaboration for Dark Matter Search Shanghai Jiao Tong University! Shanghai Institute of Applied Physics, CAS! Shandong University! University of Maryland! University of Michigan! Peking University! http://pandax.org/ Yalong River Hydropower Development Co.! China Institute of Atomic Energy (new group joined 2015) Why Liquid Xenon? • Ultra-low background: using self-shielding with 3D fiducialization and ER/NR discrimination • Sensitive to both heavy and light dark matter • Sensitive to both Spin-independent and Spin-dependent (129Xe,131Xe) • Ultra-pure Xe target: xenon gas can be purified with sub-ppb (O2 etc.) and sub-ppt (Kr) impurities • Multi-ton target achievable: with reasonable cost ($1.5M/ton) and relative simple cryogenics (165K) Two-phase xenon for dark matter searches WIMPs/Neutrons. nuclear.recoil. Gammas. electron.recoil. So far the most sensitive dark matter direct detection is from LUX with the two-phase xenon technology.5 1.3 keV 2.6 ee TABLE I. Predicted background rates in the fiducial volume 1.8 (0.9–5.3 keVee) [31]. We show contributions from the γ- 2.4 rays of detector components (including those cosmogenically activated), the time-weighted contribution of activated 2.2 xenon, 222Rn (best estimate 0.2 mDRUee from 222Rn chain measurements) and 85Kr. The errors shown are both 2 3.5 from simulation statistics and those derived from the rate 4.6 1.8 5.9 measurements of time-dependent backgrounds. 1 mDRUee is 7.1 3 /S1) x,y,z corrected 10− events/keVee/kg/day. b 1.6 Source Background rate, mDRUee (S2 10 γ-rays 1.8 0.2stat 0.3sys 1.4 127 ± ± log Xe 0.5 0.02stat 0.1sys 214 ± ± 1.2 Pb 0.11–0.22 (90% C. L.) 6 85 3 6 9 12 15 18 21 24 27 30 keV Kr 0.13 0.07sys nr ± 1 0 10 20 30 40 50 Total predicted 2.6 0.2stat 0.4sys ± ± S1 x,y,z corrected (phe) Total observed 3.6 0.3stat for the WIMP halo, even when using a conservative ± interpretation of the existing low-energy nuclear recoil FIG. 4. The LUX WIMP signal region. Events in the 118 kg fiducial volume during the 85.3 live-day exposure are calibration data for xenon detectors. distribution [31], and the expectations based on the shown.) Lines as shown in Fig. 3, with vertical dashed cyan 48 cm 2 screening results and the independent assay of the lines showing the 2-30 phe range used for the signal estimation LUX will continue operations at SURF during 2014 natural Kr concentration of 3.5 1 ppt (g/g) in the analysis. and 2015. Further engineering and calibration studies ± xenon gas [36] where we assume an isotopic abundance −44 will establish the optimal parameters for detector 85 nat 11 10 of Kr/ Kr 2 10− [31, 34]. Isotopes created ⇠ ⇥ operations, with potential improvements in applied through cosmogenic production were also considered, electric fields, increased calibration statistics, decaying including measured levels of 60Co in Cu components. ratio (PLR) test statistic [37], exploiting the separation 6 8 10 12 backgrounds and an instrumented water tank veto In situ measurements determined additional intrinsic of signal and background distributions in four physical 214 222 further enhancing the sensitivity of the experiment. background levels in xenon from Pb (from the Rn −40 quantities: radius, depth, light10 (S1), and charge (S2). 127 nucleon cross section (cm Subsequently, we will complete the ultimate goal of decay chain) [32], and cosmogenically-produced Xe The− fit is made over the parameter of interest plus 129m −45 conducting a blinded 300 live-day WIMP search further (T1/2 = 36.4 days), Xe (T1/2 =8.9 days), and three10 Gaussian-constrained nuisance parameters which 131m 127 −42 127 Xe (T1/2 = 11.9 days). The rate from Xe in the encodeWIMP uncertainty in the rates10 of Xe, γ-rays from improving sensitivity to explore significant new regions WIMP search energy window is estimated to decay from internal components and the combination of 214Pb and of WIMP parameter space. 85 118 kg x 85 days 0.87 mDRUee at the start of the WIMP search dataset Kr. The distributions, in the observed−44 quantities, of 10 This work was partially supported by the U.S. to 0.28 mDRUee at the end, with late-time background the four model1 components2 are as described3 above and 10 10 10 measurements being consistent with those originating do not vary in the fit:m with (GeV/c the non-uniform2) spatial Department of Energy (DOE) under award numbers primarily from the long-lived radioisotopes. distributions of γ-ray backgroundsWIMP and x-ray lines from DE-FG02-08ER41549, DE-FG02-91ER40688, DE-FG02- The neutron background in LUX is predicted from 127Xe obtained from energy-deposition simulations [31]. 95ER40917, DE-FG02-91ER40674, de-na0000979, DE- detailed detector BG simulations to produce 0.06 single FIG.The 5. PLR operates The LUX within 90% the confidence fiducial region limit on but the the spin- FG02-11ER41738, de-sc0006605, DE-AC02-05CH11231, independent elastic WIMP-nucleon cross section (blue), scatters with S1 between 2 and 30 phe in the 85.3 live- spatial background models were validated using data DE-AC52-07NA27344, and DE-FG01-91ER40618; the togetherfrom outside with the the fiducial1σ variation volume. from repeated trials, where day dataset. This was considered too low to include in ± U.S. National Science Foundation under award numbers the PLR. The value was constrained by multiple-scatter trialsThe fluctuating energy spectrum below the of expected WIMP-nucleus number recoils of events is for analysis in the data, with a conservative 90% upper C.L. zeromodeled BG are using forced a standard to 2.3 isothermal (blue shaded). Maxwellian We velocity also show PHYS-0750671, PHY-0801536, PHY-1004661, PHY- 1102470, PHY-1003660, PHY-1312561, PHY-1347449; placed on the number of expected neutron single scatters Edelweissdistribution II [44] [38], (dark with v0 yellow= 220 line), km/s; CDMSvesc = 544 II [45] km/s; (green 3 1 of 0.37 events. line),⇢0 =0 ZEPLIN-III.3 GeV/cm [46]; average (magenta Earth line), velocity CDMSlite of 245 km [47] s− , (dark the Research Corporation grant RA0350; the Center We observed 160 events between 2 and 30 phe (S1) greenand line), Helm XENON10 form factor S2-only [39, [20] 40]. (brown We conservatively line), SIMPLE [48] for Ultra-low Background Experiments in the Dakotas within the fiducial volume in 85.3 live-days of search (lightmodel blue no signalline) and below XENON100 3.0 keVnr (the 100 lowest live-day energy [49] for (orange (CUBED); and the South Dakota School of Mines and data (shown in Fig. 4), with all observed events being line),which and a direct 225 live-day light yield [50] measurement (red line) results. exists [30, The 41], inset Technology (SDSMT). LIP-Coimbra acknowledges fund- consistent with the predicted background of electron (samewhereas axis indirectunits) also evidence shows the of charge regions yield measured exists from down annual ing from Funda¸c˜aopara a Ciˆencia e Tecnologia (FCT) recoils. The average discrimination (with 50% NR modulationto 1 keVnr in[42]). CoGeNT We do [51] not (light profile red, the shaded), uncertainties along with through the project-grant CERN/FP/123610/2011. Im- acceptance) for S1 from 2-30 phe is 99.6 0.1%, hence exclusionin NR yield, limits assuming from low a model threshold which re-analysis provides excellent of CDMS II perial College and Brown University thank the UK Royal 0.64 0.16 events from ER leakage are expected± below dataagreement [52] (upper with LUX green data line), (Fig. 1 95% and Fig. allowed 6), in addition region from ± the NR mean, for the search dataset. The spatial CDMSto being II silicon conservative detectors compared [53] (green to past shaded) works [23]. and We centroid Society for travel funds under the International Exchange distribution of the events matches that expected from the (greenalso do x), not 90% account allowed for region uncertainties from CRESST in astrophysical II [54] (yellow Scheme (IE120804). The UK groups acknowledge ER backgrounds in full detector simulations. We select shaded)parameters, and DAMA/LIBRA which are beyond allowed the scope region of this [55] work interpreted (but institutional support from Imperial College London, the upper bound of 30 phe (S1) for the signal estimation byare [56] discussed (grey shaded). in [43]). Results Signal sourced models in from S1 DMTools and S2 are [57]. University College London and Edinburgh University, analysis to avoid additional background from the 5 keVee obtained for each WIMP mass from full simulations. and from the Science & Technology Facilities Council for 127 x-ray from Xe. The observed PLR for zero signal is entirely consistent Ph.
Load more

Recommended publications
  • Dark Matter and the Early Universe: a Review Arxiv:2104.11488V1 [Hep-Ph
    Dark matter and the early Universe: a review A. Arbey and F. Mahmoudi Univ Lyon, Univ Claude Bernard Lyon 1, CNRS/IN2P3, Institut de Physique des 2 Infinis de Lyon, UMR 5822, 69622 Villeurbanne, France Theoretical Physics Department, CERN, CH-1211 Geneva 23, Switzerland Institut Universitaire de France, 103 boulevard Saint-Michel, 75005 Paris, France Abstract Dark matter represents currently an outstanding problem in both cosmology and particle physics. In this review we discuss the possible explanations for dark matter and the experimental observables which can eventually lead to the discovery of dark matter and its nature, and demonstrate the close interplay between the cosmological properties of the early Universe and the observables used to constrain dark matter models in the context of new physics beyond the Standard Model. arXiv:2104.11488v1 [hep-ph] 23 Apr 2021 1 Contents 1 Introduction 3 2 Standard Cosmological Model 3 2.1 Friedmann-Lema^ıtre-Robertson-Walker model . 4 2.2 A quick story of the Universe . 5 2.3 Big-Bang nucleosynthesis . 8 3 Dark matter(s) 9 3.1 Observational evidences . 9 3.1.1 Galaxies . 9 3.1.2 Galaxy clusters . 10 3.1.3 Large and cosmological scales . 12 3.2 Generic types of dark matter . 14 4 Beyond the standard cosmological model 16 4.1 Dark energy . 17 4.2 Inflation and reheating . 19 4.3 Other models . 20 4.4 Phase transitions . 21 5 Dark matter in particle physics 21 5.1 Dark matter and new physics . 22 5.1.1 Thermal relics . 22 5.1.2 Non-thermal relics .
    [Show full text]
  • Letter of Interest Cosmic Probes of Ultra-Light Axion Dark Matter
    Snowmass2021 - Letter of Interest Cosmic probes of ultra-light axion dark matter Thematic Areas: (check all that apply /) (CF1) Dark Matter: Particle Like (CF2) Dark Matter: Wavelike (CF3) Dark Matter: Cosmic Probes (CF4) Dark Energy and Cosmic Acceleration: The Modern Universe (CF5) Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before (CF6) Dark Energy and Cosmic Acceleration: Complementarity of Probes and New Facilities (CF7) Cosmic Probes of Fundamental Physics (TF09) Astro-particle physics and cosmology Contact Information: Name (Institution) [email]: Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Institute, University of Toronto) [ [email protected]] Authors: Simeon Bird (UC Riverside), Simon Birrer (Stanford University), Djuna Croon (TRIUMF), Alex Drlica-Wagner (Fermilab, University of Chicago), Jeff A. Dror (UC Berkeley, Lawrence Berkeley National Laboratory), Daniel Grin (Haverford College), David J. E. Marsh (Georg-August University Goettingen), Philip Mocz (Princeton), Ethan Nadler (Stanford), Chanda Prescod-Weinstein (University of New Hamp- shire), Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Insti- tute, University of Toronto), Katelin Schutz (MIT), Neelima Sehgal (Stony Brook University), Yu-Dai Tsai (Fermilab), Tien-Tien Yu (University of Oregon), Yimin Zhong (University of Chicago). Abstract: Ultra-light axions are a compelling dark matter candidate, motivated by the string axiverse, the strong CP problem in QCD, and possible tensions in the CDM model. They are hard to probe experimentally, and so cosmological/astrophysical observations are very sensitive to the distinctive gravitational phenomena of ULA dark matter. There is the prospect of probing fifteen orders of magnitude in mass, often down to sub-percent contributions to the DM in the next ten to twenty years.
    [Show full text]
  • Supersymmetric Dark Matter Candidates in Light of Constraints from Collider and Astroparticle Observables
    THESE` Pour obtenir le grade de DOCTEUR DE L’UNIVERSITE´ DE GRENOBLE Specialit´ e´ : Physique Theorique´ Arretˆ e´ ministeriel´ : 7 aoutˆ 2006 Present´ ee´ par Jonathan DA SILVA These` dirigee´ par Genevieve` BELANGER´ prepar´ ee´ au sein du Laboratoire d’Annecy-le-Vieux de Physique Theorique´ (LAPTh) et de l’Ecole´ Doctorale de Physique de Grenoble Supersymmetric Dark Matter candidates in light of constraints from collider and astroparticle observables These` soutenue publiquement le 3 juillet 2013, devant le jury compose´ de : arXiv:1312.0257v1 [hep-ph] 1 Dec 2013 Dr. Rohini GODBOLE Professeur, CHEP Bangalore, Inde, Presidente´ Dr. Farvah Nazila MAHMOUDI Maˆıtre de Conferences,´ LPC Clermont, Rapporteur Dr. Ulrich ELLWANGER Professeur, LPT Orsay, Rapporteur Dr. Celine´ BŒHM Charge´ de recherche, Durham University, Royaume-Uni, Examinatrice Dr. Anupam MAZUMDAR Professeur, Lancaster University, Royaume-Uni, Examinateur Dr. Genevieve` BELANGER´ Directeur de Recherche, LAPTh, Directeur de these` A meus av´os. Contents Acknowledgements - Remerciements vii List of Figures xi List of Tables xvii List of Abbreviations xix List of Publications xxiii Introduction1 I Status of particle physics and cosmology ... and beyond5 1 From the infinitely small : the Standard Model of particle physics ...7 1.1 Building of the model : gauge sector . .8 1.2 Matter sector . 10 1.2.1 Leptons . 10 1.2.2 Quarks . 12 1.3 The Higgs mechanism . 13 1.4 Full standard picture . 16 1.5 Successes of the SM . 18 1.6 SM issues . 19 1.6.1 Theoretical problems . 19 1.6.2 Experimental discrepancies . 20 1.6.3 Cosmological connexion . 22 2 ... To the infinitely large : the Lambda Cold Dark Matter model 23 2.1 Theoretical framework .
    [Show full text]
  • Light Dark Matter
    Light dark matter Maxim Pospelov Perimeter Institute, Waterloo/University of Victoria, Victoria CERN-Korea Theory Institute, 2016 1 Light dark matter § What does ”light DM” mean ? Gravity does not care whether these are 10-30, 1 or 1030 kg objects as long as they have same velocity distribution. 2 Light dark matter § What does ”light DM” mean ? Gravity does not care whether these are 10-30, 1 or 1030 kg objects as long as they have same velocity distribution. § Working definition: light dark matter is some form of particle dark matter with mass lighter than the range where most search efforts and $ are currently being spent. 3 Big Questions in Physics “Missing mass” – what is it? New particle, new force, …? Both? How to find out? Challenges ?? Too many options for DM. In “direct detection” or collider experiments there is an extrapolations from ~ kpc scale (~ 1021 cm) down to 102 cm scale. Outline of the talk 1. Introduction. Types of dark matter. Weakly interacting massive particles (WIMPs). 2. Light dark matter and light mediators. Examples of models that pass current experimental constraints. 3. Searches at short baseline neutrino experiments and missing energy searches. Searches of mediators. 4. Ways to improve sensitivity: SHiP, electron beam experiments, underground experiments. 5. Direct detection of light dark matter using the electron recoil – bridge to detecting super-weakly interacting DM. 6. Conclusions. 5 DM classification At some early cosmological epoch of hot Universe, with temperature T >> DM mass, the abundance of these particles relative to a species of SM (e.g. photons) was Normal: Sizable interaction rates ensure thermal equilibrium, NDM/Ng =1.
    [Show full text]
  • Asymmetric Dark Matter and Dark Radiation
    Prepared for submission to JCAP CERN-PH-TH/2012-070; MPP-2012-56 Asymmetric Dark Matter and Dark Radiation Mattias Blennowa Enrique Fernandez Martinezb Olga Menac Javier Redondod Paolo Serrae aMax-Planck-Institut f¨urKernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany bCERN Physics Department, Theory Division, CH-1211 Geneva 23, Switzerland cInstituto de F´ısicaCorpuscular, CSIC-Universitat de Val`encia, 22085, E-46071 Valencia, Spain dMax-Planck-Institut f¨urPhysik F¨ohringerRing 6, D-80805 M¨unchen, Germany dInstitut d'Astrophysique Spatiale, UMR8617, Universite Paris-Sud & CNRS, Bat. 121, Orsay F-91405, France E-mail: [email protected], [email protected], omena@ific.uv.es, [email protected], [email protected] Abstract. Asymmetric Dark Matter (ADM) models invoke a particle-antiparticle asymme- try, similar to the one observed in the Baryon sector, to account for the Dark Matter (DM) abundance. Both asymmetries are usually generated by the same mechanism and generally related, thus predicting DM masses around 5 GeV in order to obtain the correct density. The main challenge for successful models is to ensure efficient annihilation of the thermally produced symmetric component of such a light DM candidate without violating constraints from collider or direct searches. A common way to overcome this involves a light mediator, into which DM can efficiently annihilate and which subsequently decays into Standard Model particles. Here we explore the scenario where the light mediator decays instead into lighter degrees of freedom in the dark sector that act as radiation in the early Universe. While this assumption makes indirect DM searches challenging, it leads to signals of extra radiation at arXiv:1203.5803v2 [hep-ph] 19 Jun 2012 BBN and CMB.
    [Show full text]
  • Possibilities of Detecting Light Dark Matter Produced Via Drell-Yan Channel in a Fixed Target Experiment
    universe Article Possibilities of Detecting Light Dark Matter Produced via Drell-Yan Channel in a Fixed Target Experiment Eduard Ursov 1,2,* , Anna Anokhina 1,2 , Emil Khalikov 2, Ivan Vidulin 1 and Tatiana Roganova 2 1 Department of Physics, Federal State Budget Educational Institution of Higher Education, M.V. Lomonosov Moscow State University, 1(2), Leninskie gory, GSP-1, 119991 Moscow, Russia; [email protected] (A.A.); [email protected] (I.V.) 2 Skobeltsyn Institute of Nuclear Physics (SINP MSU), Federal State Budget Educational Institution of Higher Education, M.V. Lomonosov Moscow State University, 1(2), Leninskie gory, GSP-1, 119991 Moscow, Russia; [email protected] (E.K.); [email protected] (T.R.) * Correspondence: [email protected] Abstract: This work presents the complete modeling scheme of production and detection of two types of light dark matter (LDM) — Dirac fermionic and scalar particles — in a fixed target experiment using SHiP experiment as an example. The Drell-Yan process was chosen as a channel of LDM production; the deep inelastic scattering on lead nuclei was simulated and analyzed in the detector; the production of secondary particles was modeled with the aid of PYTHIA6 toolkit. Obtained observable parameters of secondary particles produced in events associated with LDM were compared with the background neutrino events that were simulated using GENIE toolkit. The yield of LDM events was calculated with various model parameter values. Using machine learning methods, a classifier that is able to distinguish LDM events from neutrino background events based on the observed parameters with high precision has been developed.
    [Show full text]
  • Superfluid Quantum Space and Evolution of the Universe
    Chapter 5 Superfluid Quantum Space and Evolution of the Universe Valeriy I. Sbitnev and Marco Fedi Additional information is available at the end of the chapter http://dx.doi.org/10.5772/68113 Abstract We assume that dark energy and dark matter filling up the whole cosmic space behave as a special superfluid, here named “superfluid quantum space.” We analyze the relationship between intrinsic pressure of SQS (dark energy's repulsive force) and gravity, described as an inflow of dark energy into massive particles, causing a nega- tive pressure gradient around massive bodies. Since no superfluid has exact zero viscosity, we analyze the consequences of SQS’s viscosity on light propagation, and we show that a static Universe could be possible, by solving a modified Navier-Stokes equation. Indeed, Hubble’s law may actually refer to tired light, though described as energy loss due to SQS’s nonzero viscosity instead of Compton scattering, bypassing known historical problems concerning tired light. We see that SQS’sviscositymayalso account for the Pioneer anomaly. Our evaluation gives a magnitude of the anomalous À À À10 À2 acceleration aP = HΛc = 8.785 10 ms . Here, HΛ is the Hubble parameter loaded by the cosmological constant Λ. Furthermore, the vorticity equation stemming from the modified Navier-Stokes equation gives a solution for flat profile of the orbital speed of spiral galaxies and discloses what one might call a breathing of galaxies due to energy exchange between the galactic vortex and dark energy. Keywords: gravity, dark energy, Hubble’s law, tired light, Pioneer anomaly, flat profile 1.
    [Show full text]
  • (Light) Dark Matter Detection
    Recent Ideas for (Light) Dark Matter Detection Yonit Hochberg YH @ DESY Theory Forum, 2020 The Universe is Dark Dark energy Dark matter Atoms u c t g ?? What is it? d s b γ ?? How does it interact? H e µ τ W ?? ν ν# ν $ " Z YH @ DESY Theory Forum, 2020 Past 40 years YH @ DESY Theory Forum, 2020 WIMP, glorious WIMP* *Also axions, of course also axions :-) YH @ DESY Theory Forum, 2020 The WIMP Correct thermal relic abundance: For weak coupling, weak scale emerges. The dominant paradigm for ~40 years. DM SM DM SM annihilation YH @ DESY Theory Forum, 2020 Searching for WIMPs Direct production Direct detection Indirect detection Experiments getting increasingly sensitive Haven’t yet detected dark matter YH @ DESY Theory Forum, 2020 Great opportunity for new ideas! YH @ DESY Theory Forum, 2020 Beyond the WIMP Dark matter mass [GeV] Hitoshi @ BCTP, Tahoe 2015 YH @ DESY Theory Forum, 2020 Beyond the WIMP Dark matter mass [GeV] Lots of activity inHitoshi recent @ BCTP, years: Tahoe 2015 Theory & Experiment YH @ DESY Theory Forum, 2020 New Theory Ideas • …… • Weakly coupled WIMPs [Pospelov, Ritz, Voloshin 2007; Feng, Kumar 2008] • Asymmetric dark matter [Kaplan, Luty, Zurek, 2009] • Freeze-in dark matter [Hall, Jedamzik, March-Russell, West, 2009] • SIMPs [YH, Kuflik, Volansky, Wacker, 2014; YH, Kuflik, Murayama, Volansky, Wacker, 2015] • ELDERs [Kuflik, Perelstein, Rey-Le Lorier, Tsai, 2016 & 2017] • Forbidden dark matter [Griest, Seckall, 1991; D’Agnolo, Ruderman, 2015] • Co-decaying dark matter [Dror, Kuflik, Ng, 2016] • Co-scattering dark matter
    [Show full text]
  • Constraining Light Dark Matter with Diffuse X-Ray and Gamma-Ray
    FERMILAB-PUB-13-377-A-T YITP-SB-29-13, MCTP-13-27 Constraining Light Dark Matter with Diffuse X-Ray and Gamma-Ray Observations Rouven Essig,1 Eric Kuflik,2 Samuel D. McDermott,3, 4 Tomer Volansky,2 and Kathryn M. Zurek3 1C.N. Yang Institute for Theoretical Physics, Stony Brook University, Stony Brook, NY 11794, USA 2Raymond and Beverly Sackler School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel 3Michigan Center for Theoretical Physics, University of Michigan, Ann Arbor, MI 48105, USA 4Theoretical Astrophysics Department Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA Abstract We present constraints on decaying and annihilating dark matter (DM) in the 4 keV to 10 GeV mass range, using published results from the satellites HEAO-1, INTEGRAL, COMPTEL, EGRET, and the Fermi Gamma-ray Space Telescope. We derive analytic expressions for the gamma-ray spectra from various DM decay modes, and find lifetime constraints in the range 1024 1028 sec, depending − on the DM mass and decay mode. We map these constraints onto the parameter space for a variety of models, including a hidden photino that is part of a kinetically mixed hidden sector, a gravitino with R-parity violating decays, a sterile neutrino, DM with a dipole moment, and a dark pion. The indirect constraints on sterile-neutrino and hidden-photino DM are found to be more powerful than other experimental or astrophysical probes. While our focus is on decaying DM, we also present constraints on DM annihilation to electron-positron pairs. We find that if the annihilation is p-wave suppressed, the galactic diffuse constraints are, depending on the DM velocity at recombination, more powerful in some cases than the constraints from the Cosmic Microwave Background.
    [Show full text]
  • Asymmetric Dark Matter
    Asymmetric Dark Matter Joshua Berger We present notes on asymmetric dark matter (ADM), with a particular focus on elaborating on the points made in [1]. We focus undestanding how to derive cosmological properties of general models of dark matter, as well as particle physics and cosmological considerations that must be taken into account when working with models of ADM. We also summarize some possible signatures of models of ADM and mention some follow up work on the subject. 2 Component Ω Cosmological Constant/Dark Energy 0.742 Dark Matter 0.214 Baryonic Matter 0.0441 TABLE I. Energy distributions of the major components of the universe relative to the critical density ρcrit ∼ 1. I. MOTIVATION Recent results from cosmological observations have led to several new puzzles. It is possible that some of these puzzles are connected to the major puzzles of particle physics at the weak scale. One such puzzle that may be plausibly connected to the weak scale relates to the abundances of particles in the universe. Using data from astrophysical observations from several sources, including the CMB specturm, structure on super-galactic scales, and redshifts of distant luminous sources, the relative energy density distributions of the major components of the present-day universe have been determined accurately[2], as shown in Table I. Note that three components of the universe that we might think are unrelated all have contributions within an order of magnitude of each other. The order 1 contribution of the cosmological constant could plausibly be a coincidence, albeit a very striking one, since its contribution was small in the early universe and only relatively recently on cosmological scales became important.
    [Show full text]
  • Search for Light Dark Matter–Electron Scattering in the Pandax-II Experiment
    PHYSICAL REVIEW LETTERS 126, 211803 (2021) Search for Light Dark Matter–Electron Scattering in the PandaX-II Experiment Chen Cheng,2 Pengwei Xie,3 Abdusalam Abdukerim,1 Wei Chen,1 Xun Chen,1,4 Yunhua Chen,5 Xiangyi Cui,3 Yingjie Fan,6 Deqing Fang,7 Changbo Fu,7 Mengting Fu,8 Lisheng Geng,9,10 Karl Giboni,1 Linhui Gu,1 Xuyuan Guo,5 Ke Han,1 Changda He,1 Shengming He,5 Di Huang,1 Yan Huang,5 Yanlin Huang,11 † Zhou Huang,1 Xiangdong Ji,12 Yonglin Ju,13 Shuaijie Li,3 Qing Lin,14,15 Huaxuan Liu,13 Jianglai Liu,1,3,4, Liqiang Liu,5 Xiaoying Lu,16,17 Wenbo Ma,1 Yugang Ma,7 Yajun Mao,8 Yue Meng ,1,4,* Parinya Namwongsa,1 Kaixiang Ni,1 Jinhua Ning,5 Xuyang Ning,1 Xiangxiang Ren,16,17 Nasir Shaheed,16,17 Changsong Shang,5 Guofang Shen,9 Lin Si,1 Andi Tan,12 Anqing Wang,16,17 Hongwei Wang,18 Meng Wang,16,17 Qiuhong Wang,7 Siguang Wang,8 Wei Wang,2 Xiuli Wang,13 Zhou Wang,1,4 Mengmeng Wu,2 Shiyong Wu,5 Weihao Wu,1 Jingkai Xia,1 Mengjiao Xiao,12 Xiang Xiao,2 Binbin Yan,1 Jijun Yang,1 Yong Yang,1 Chunxu Yu,6 Jumin Yuan,16,17 Ying Yuan,1 Xinning Zeng,1 Dan Zhang,12 Tao Zhang,1 Li Zhao,1 Qibin Zheng,11 Jifang Zhou,5 Ning Zhou,1 and Xiaopeng Zhou9 (PandaX-II Collaboration) 1School of Physics and Astronomy, Shanghai Jiao Tong University, Key Laboratory for Particle Astrophysics and Cosmology (MOE), Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai 200240, China 2School of Physics, Sun Yat-Sen University, Guangzhou 510275, China 3Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai 200240, China 4Shanghai Jiao Tong University
    [Show full text]
  • Dark Matter= Modified Gravity? Scrutinising the Spacetime-Matter
    Dark Matter = Modified Gravity? Scrutinising the spacetime–matter distinction through the modified gravity/ dark matter lens Niels C.M. Martens1,2,3 and Dennis Lehmkuhl1,2 1DFG Research Unit “The Epistemology of the Large Hadron Collider” (grant FOR 2063) [email protected] , [email protected] 2Lichtenberg Group for History and Philosophy of Physics, University of Bonn 3Institute for Theoretical Particle Physics and Cosmology, RWTH Aachen University This is a postprint (i.e. post-peer-review but pre-copyedit) version of an article accepted for publication in Studies in History and Philosophy of Modern Physics. The final authenticated version is/will be available online (open access) at: www.sciencedirect.com/science/article/abs/pii/S135521982030109X. September 10, 2020 Abstract This paper scrutinises the tenability of a strict conceptual distinction be- tween space(time) and matter via the lens of the debate between modified gravity and dark matter. In particular, we consider Berezhiani and Khoury’s novel ‘superfluid dark matter theory’ (SFDM) as a case study. Two families of criteria for being matter and being spacetime, respectively, are extracted from the literature. Evaluation of the new scalar field postulated by SFDM according to these criteria reveals that it is as much (dark) matter as anything could possibly be, but also—below the critical temperature for superfluidity— as much (of a modification of) spacetime as anything could possibly be. A sequel paper examines possible interpretations of SFDM in light of this result, as well as the consequences for our understanding of (the importance of) the modified gravity/ dark matter distinction and the broader spacetime–matter arXiv:2009.03890v1 [physics.hist-ph] 8 Sep 2020 distinction.
    [Show full text]