Letter of Interest the GAPS Experiment: Cosmic Antinuclei As
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Arxiv:1908.09037V3 [Astro-Ph.HE] 8 May 2020
NuSTAR tests of sterile-neutrino dark matter: New Galactic bulge observations and combined impact Brandon M. Roach,1, ∗ Kenny C. Y. Ng,2, y Kerstin Perez,1, z John F. Beacom,3, 4, 5, x Shunsaku Horiuchi,6, { Roman Krivonos,7, ∗∗ and Daniel R. Wik8, yy 1Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 2Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel 3Center for Cosmology and AstroParticle Physics (CCAPP), Ohio State University, Columbus, OH 43210, USA 4Department of Physics, Ohio State University, Columbus, OH 43210, USA 5Department of Astronomy, Ohio State University, Columbus, OH 43210, USA 6Center for Neutrino Physics, Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA 7Space Research Institute of the Russian Academy of Sciences (IKI), Moscow 117997, Russia 8Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA (Dated: Received 4 October 2019; accepted 2 April 2020; published 8 May 2020) We analyze two dedicated NuSTAR observations with exposure ∼190 ks located ∼10◦ from the Galactic plane, one above and the other below, to search for x-ray lines from the radiative decay of sterile-neutrino dark matter. These fields were chosen to minimize astrophysical x-ray backgrounds while remaining near the densest region of the dark matter halo. We find no evidence of anomalous x-ray lines in the energy range 5{20 keV, corresponding to sterile neutrino masses 10{40 keV. Interpreted in the context of sterile neutrinos produced via neutrino mixing, these observations provide the leading constraints in the mass range 10{12 keV, improving upon previous constraints in this range by a factor ∼2. -
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 . -
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. -
Kerstin M. Perez
Kerstin M. Perez Address Massachusetts Institute of Technology Laboratory of Nuclear Science 77 Massachusetts Ave, 26-541 Cambridge, MA 02139 Email [email protected] Phone (617) 324-1522 APPOINTMENTS Assistant Professor of Physics 2016 { present MIT, Cambridge, MA Assistant Professor of Physics 2015 { 2016 Haverford College, Haverford, PA NSF Astronomy & Astrophysics Postdoctoral Fellow 2012 { 2014 Postdoctoral Research Scientist 2011 { 2012 Columbia University, New York, NY EDUCATION California Institute of Technology, Pasadena, CA Ph.D., Physics 2011 Thesis: Inclusive Jet Cross Sections in Proton-Proton Collisions at 7.0 TeV Center-of-Mass Energy with the ATLAS Detector at the Large Hadron Collider Columbia University, New York, NY B.A. in Physics, Minor in Mathematics 2005 AWARDS AND HONORS Cottrell Scholar Award 2019 { 2022 Sloan Research Fellowship 2017 { 2019 MIT School of Science Teaching Prize for Undergraduate Education 2018 MIT Buechner Special Teaching Award 2018 NSF Astronomy and Astrophysics Postdoctoral Fellowship 2012 { 2014 NSF US LHC Graduate Student Support Award 2010 - 2011 Robert A. Millikan Graduate Fellowship 2006 { 2007 GRANTS RCSA Cottrell Scholar Award (PI) 2019 - 2022 Closing in on Sterile Neutrino Dark Matter, ID 25928. Cottrell Scholar Collaborative (Co-I) 2019 - 2021 Establishing a Network for Effective Interventions in STEM Classrooms Heising-Simons Foundation, Fundamental Physics Grant (PI) 2019 - 2020 Fabricating the Si(Li) Tracker Array for the GAPS Experiment, ID 2019-1357. NASA NuSTAR Guest Observer Cycle-5 (PI) 2019 - 2020 A Novel Probe of Low-Mass Axion Dark Matter Using Betelgeuse, Prop. 5057. Heising-Simons Foundation, Fundamental Physics Grant (PI) 2018 - 2021 Construction, flight, and first dark matter results of the GAPS Si system, ID 2018-0766. -
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. -
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 . -
1 KERSTIN MARIE PEREZ Curriculum Vitae MIT Physics Department Phone
1 KERSTIN MARIE PEREZ Curriculum Vitae MIT Physics Department Phone: (617) 324-1522 77 Massachusetts Ave., 26-506 Email: [email protected] Cambridge MA 02139 Degrees: PhD in Physics, California Institute of Technology, 2011. Dissertation advisor: Emlyn Hughes. M.S. in Physics, California Institute of Technology, 2008. B.A. in Physics, Columbia University, 2005. Employment: Postdoctoral researcher, Columbia University, 2011-2012. Supervisor: Charles Hailey. NSF Astronomy & Astrophysics Postdoctoral Fellow, Columbia University, 2012-2014. Assistant Professor of Physics, Haverford College, 2015-2016. Assistant Professor of Physics, Massachusetts Institute of Technology, 2016-Current. Honors: Cottrell Scholar Award, Research Corporation for Science Advancement, 2019. Class of 1948 Career Development Professorship, MIT, 2019. School of Science Teaching Prize for Undergraduate Education, MIT, 2018. Buechner Faculty Teaching Prize, MIT Physics Department, 2018. Sloan Research Fellowship, Sloan Foundation, 2017. NASA Group Achievement Award for NuSTAR Galactic Plane Survey Team, NASA, 2016. Cottrell College Science Award, Research Corporation for Science Advancement, 2015. NASA Group Achievement Award for NuSTAR Science Team, NASA, 2015. Astronomy & Astrophysics Postdoctoral Fellowship, National Science Foundation, 2012. US Large Hadron Collider Graduate Student Support Award, National Science Foundation, 2010. Robert A. Millikan Graduate Fellowship, California Institute of Technology, 2006. Undergraduate Students Supervised: Wang, Cindy ('23): Summer 2020. Protyasha, Nishat (`22): Summer 2019, Fall 2019, Spring 2020. Seyler, Devin (`22): Fall 2019, Spring 2020, Summer 2020. Bouche, Ian ('21): Summer 2020. 2 Faustina, Aidan ('21): Summer 2020. Hernandez, Analyce ('21): Spring 2020, Summer 2020. Taylor, Afura (`21): Summer 2018, Fall 2018, Spring 2019. Brown, Jonathon (`20): Fall 2016, Spring 2017, Fall 2018, Spring 2018. Li, Ivy (`20): Summer 2017, Fall 2017, Spring 2018, Fall 2018, Spring 2019, Fall 2019; Currently: Fulbright Scholar and Rice University Ph.D. -
BESS-Polar Experiment
PSB1-0046-02 1 BESS-Polar experiment T. Yoshida1, A. Yamamoto1, J. Mitchell2, K. Abe3, H. Fuke1,3, S. Haino1,3, T. Hams2, N. Ikeda4, A. Itazaki4, K. Izumi1,3, M. H. Lee5, T. Maeno4, Y. Makida1, S. Matsuda3, H. Matsumoto3, A. Moiseev2, J. Nishimura3, M. Nozaki4, H. Omiya1, J. F. Ormes2, M. Sasaki2, E. S. Seo5, Y. Shikaze4, A. Stephens2, R. Streitmatter2, J. Suzuki1, Y. Takasugi4, K. Tanaka1, K. Tanizaki4, T. Yamagami6, Y. Yamamoto3, K. Yamato4, and K. Yoshimura1 1 High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan 2 Goddard Space Flight Center / NASA, Greenbelt, MD 20771, USA 3 The University of Tokyo, Bunkyo, Tokyo 113-0033, Japan 4 Kobe University, Kobe, Hyogo 657-8501, Japan 5 University of Maryland, College Park, MD 20742, USA 6 Institute of Space and Astronautical Science (ISAS), Sagamihara, Kanagawa 229-8510, Japan ABSTRACT For investigating elementary particle phenomena in the early Universe, the BESS-Polar experiment was proposed for highly sensitive studies of the low-energy antiprotons and extensive searches for antinuclei in the cosmic radiations. A new superconducting spectrometer is being developed for long-duration balloon flights. In order to extend detectable energy range of the antiprotons down to 100 MeV, materials along the trajectory of the incident particle is minimized. The spectrometer will be completed in 2003, and the first long-duration flight is planned in 2004. INTRODUCTION Observations of anomalous excess of antiproton ) flux (Bogolomov et al. 1979, Golden et al. 1979, 1 - -1 Buffington et al. 1981), compared to the predictions by V 10 e G the secondary production models, had suggested 1 - c existence of novel processes of the antiproton e s 1 production. -
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. -
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. -
The General Antiparticle Spectrometer (GAPS) - Dark Matter Search Using Cosmic-Ray Antideuterons
The General Antiparticle Spectrometer (GAPS) - Dark matter search using cosmic-ray antideuterons KAVLI, Stanford University October 2011 Philip von Doetinchem on behalf of the GAPS collaboration Space Sciences Laboratory, UC Berkeley [email protected] T. Aramaki1, N. Bando4, St. Boggs2, W. Craig3, B. Donakowski2, H. Fuke4, F. Gahbauer1,5 , Ch. Hailey1(PI), J. Hoberman2, P. Kaplan1, J. Koglin1, N. Madden1, St. McBride2, I. Mognet6, B. Mochizuki2, K. Mori1, R. Ong6, K. Perez1, D. Stefanik1, M. Lopez-Thibodeaux2, T. Yoshida4, R. Zambelli1, J. Zweerink6 1 Columbia University, 2 UC Berkeley, 3 Lawrence Livermore National Laboratory, 4 Japan Aerospace Exploration Agency 5 University of Latvia, 6 UC Los Angeles Outline Why are antideuterons interesting? How to measure them? cosmic rays antideuteron physics GAPS concept GAPS prototype instrument Ph. von Doetinchem The General Antiparticle Spectrometer (GAPS) Oct. 2011 – p. 2 Cosmic rays in the GeV to TeV range • in general good agreement of models and data • what we already learned: – particle physics – interstellar medium – astronomical objects – … • small fluxes with no primary astronomical source are especially sensitive to new effects Ph. von Doetinchem The General Antiparticle Spectrometer (GAPS) Oct. 2011 – p. 3 Positron fraction & electron flux E. Mocchiutti et al. arxiv:0905.2551 D. Grasso et al. arxiv:0905.0636 pulsar DM: KK SNR DM: SUSY nearby pulsars • unexplained features in positron and electron spectra • proposed theories: – γ-ray pulsars can produce electron and positrons via pair production in the magnetosphere – positrons and electrons can also be accelerated in PWN or SNR shocks – dark matter self-annihilation Ph. von Doetinchem The General Antiparticle Spectrometer (GAPS) Oct. -
Proceedings of the 3Rd Workshop on BALLOON-BORNE EXPERIMENTS with SUPERCONDUCTING MAGNET SPECTROMETERS" class="text-overflow-clamp2"> V^ " > Proceedings of the 3Rd Workshop on BALLOON-BORNE EXPERIMENTS with SUPERCONDUCTING MAGNET SPECTROMETERS
KEK-PR0C--92- JP9304099 ^ ,-*.«?* ?*! S-;V^ " > Proceedings of the 3rd Workshop on BALLOON-BORNE EXPERIMENTS WITH SUPERCONDUCTING MAGNET SPECTROMETERS held at National Laboratory for High Energy Physics (KEK) February 24-25, 1992 Edited by Akira Yamamoto [ r National Laboratory for High Energy Physics, 1992 KEK Reports are available from: Technical Information & Library National Laboratory for High Energy Physics 1-1 Oho, Tsukuba-shi Ibaraki-ken, 305 JAPAN Phone: 0298-64-1171 Telex: 3652-534 (Domestic) (0)3652-534 (International) Fax: 0298-64-4604 Cable: KEKOHO II '•J % Foreword The Third Work Shop on Balloon Borne Experiment with a Superconducting Magnet Spectrometer was held at National Laboratory for High Energy Physics (KEK), Tsukuba, Japan on February 24 - 25, 1992. The workshop was supported by a Grant for Joint Research under The Monbusho International Scientific Research Program (No. 02044151). Two invited review talks were presented on " Progress of Measurement of Cosmic Ray Antiprotons and Search for Primordial Antimatter" and on " High Rate Data Acquisition System in Balloon Borne Experiments." The main effort for this workshop was focused on the progress of the BESS (Balloon Borne Experiment with a Superconducting Spectrometer) experiment and on the scope for scientific investigation with the BESS detector. The progress was reviewed and further investigation was discussed for the BESS further scientific collaboration among Univ. of Tokyo, Kobe University, KEK, ISAS and NMSU. The 30 scientists and engineers participated to the workshop and there were extensive discussions to verify and to complete the BESS detector to be launched in Canada, this summer. New technologies for future balloon and space experiments were also discussed on triggering by using Neural Network and on Scientific investigation with Japanese Experimental Module (JEM) on the Space Station.