DOCSLIB.ORG

Katherine Freese Michigan Center for Theoretical Physics University of Michigan WIMP Searches EXCITING TIMES

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Katherine Freese Michigan Center for Theoretical Physics University of Michigan WIMP Searches EXCITING TIMES Katherine Freese Michigan Center for Theoretical Physics University of Michigan WIMP searches EXCITING TIMES • We made WIMP proposals twenty years ago: • It is coming to fruition! • My personal prediction: one of the anomalous results is right and we will know very soon. LHC-Making DM Coming Soon (We hope) Supersymmetric Particles in LHC • Signature: missing energy when SUSY particle is created and some energy leaves the detector • Problem with identification: degeneracy of interpretation • SUSY can be found, but, you still don’t know how long the particle lives: fractions of a second to leave detector or the age of the universe if it is dark matter • Proof that the dark matter has been found requires astrophysical particles to be found Direct Detection of WIMP dark matter A WIMP in the Galaxy travels through our detectors. It hits a nucleus, and deposits a tiny amount of energy. The nucleus recoils, and we detect this energy deposit. Expected Rate: less than one count/kg/day! Event rate (number of events)/(kg of detector)/(keV of recoil energy) dR N dσ = ∫ T × × nv f (v,t)d 3v dE MT dE ρσ F 2 (q) f (v,t) = 0 d 3v 2mµ2 ∫v> ME / 2µ 2 v € A2µ2 Spin-independent σ 0 = 2 σ p € µp 4µ2 2 Spin-dependent σ = S G + S G 0 π p p n n € € From DM Tools Website Many claims/hints of WIMP dark matter detection: how can we be sure? • 1) The DAMA annual modulation • 2) The HEAT, PAMELA, and ATIC positron excess • 3) Gamma-rays from Galactic Center • 4) WMAP Haze HAS DARK MATTER BEEN DISCOVERED? The DAMA Annual Modulation DAMA annual modulation Drukier, Freese, and Spergel (PRD 1986); Freese, Frieman, and Gould (PRD 1988) Bernabei et al 2003 Data do show a 8σ modulation WIMP interpretation??? DAMA/LIBRA (April 17, 2008) 8 sigma Can the positive signal in DAMA be compatible with null results from other experiments? Savage, Gelmini, Gondolo, and Freese, arxiv:0808:3607 (see also papers by Hooper and Zurek; Fairbairn and Schwetz; Chang, Pierce and Weiner 2008) DAMA: spin independent? DAMA CDMS XENON Small remaining region at 10 GeV WIMP mass DAMA and CDMS DAMA Spin- XENON dependent cross sections SUPER-K Hooper and Zurek extended Super-K bounds Remaining window around 10 GeV. Removing SuperK: WIMP mass up to 20 GeV allowed Savage, Gelmini, Gondolo, Freese 0808:3607 New measurements of Sun’s velocity relative to Halo: 250 km/sec (not 220 km/sec) CRESST • All curves move the left: • Remaining window moves to 7-8 GeV at 3 sigma (5-15 for SD) Savage, Freese, Gondolo, Spolyar 2009 To reconcile DAMA with null results from other experiements: • Popular theory: Direct Detection • In past two years, two orders of magnitude increase in sensitivity (the following results not included in our compatibility study): (i) CDMS (ii) XENON-10 (iii) ZEPLIN III New technology: liquid noble gases XENON, LUX, XMASS WARP (argon) DEAPCLEAN (argon and neon) New signals in direction detection 2010 • CDMS: Germanium (Berkeley, Stanford, Case Western, many others): two events • COGENT: low threshold germanium (Fermilab): one event at low WIMP mass, would be consistent with DAMA • Caveat: all statistically insignificant Electron recoils Nuclear Recoils n.b. if include 2008 data, this significance drops CDMS bounds Inelastic Dark Matter COGENT low threshold germanium (Fermilab) Direct Detection • In past two years, two orders of magnitude increase in sensitivity: (i) CDMS (ii) XENON-10 (iii) ZEPLIN II and III New technology: liquid noble gases XENON, LUX, XMASS WARP (argon) DEAPCLEAN (argon and neon) DEAP/ Miniclean Eureka MAX, GeoDM Slide from Pearl Sandick RED OVALS: THOSE EXPTS THAT ARE CURRENTLY UNDERGROUND Ultimate Searches? XENON,LZ,MAX,GEODM EUREKA,DARWIN The HEAT and PAMELA Positron Excess The Indirect Detection of Dark Matter 1. WIMP Annihilation χ Typical final states include heavyχ fermions, gauge or Higgs bosons 2. Fragmentation/Decay W- Annihilation products decay and/or q fragment into combinations of W+ electrons, protons, deuterium, neutrinos and gamma-rays q e+ ν 3. Synchrotron and Inverse Compton π0 Relativistic electrons up-scatter starlight/ CMB to MeV-GeV energies, and emit p synchrotron photons via interactions with γ γ magnetic fields γ e+ Annihilation Products • 1/3 electron/positrons • 1/3 gamma rays • 1/3 neutrinos • Typical particles have energies roughly 1/10 of the initial WIMP mass • All of these are detectable! Indirect Detection History • Indirect Detection (Neutrinos) • Sun (Silk,Olive,Srednicki ‘85) • Earth (Freese ‘86; Krauss, Srednicki, Wilczek ‘86) • Indirect Detection (Gamma Rays, positrons) • Milky Way Halo (Ellis, KF et al ‘87) • Galactic Center (Gondolo and Silk 2000) • Anomalous signals seen in HEAT (e+), HESS, CANGAROO, WMAP, EGRET, PAMELA. New Indirect Detection Results! (When it rains it pours) Pamela IceCube FERMI Dan Hooper - Direct and Indirect Searches For Particle Dark Matter Positron excess • HEAT balloon found anomaly in cosmic ray positron flux • Explanation 1: dark matter annihilation • Explanation 2: we do not understand cosmic ray propagation Baltz, Edsjo, Freese, Gondolo 2001 How to understand positron excess? • 0) Pulsars: the best bet? • 1) Astrophysics. Propagation of charged particles in the galaxy poorly understood. See Delahaye and Salati 08. • 2) proton background (misidentified as positrons), is known to rise with energy. PAMELA doesn’t identify each event (HEAT did) • 3) We happen to live in a hot spot of high dark matter density (boosted by at least factor 10) • 4) nonstandard WIMPs: e.g., nonthermal WIMPs; Kaluza Klein particles. MUST HAVE BOOSTED ANNIHILATION CROSS SECTION AND LEPTOPHILIC PRODUCTS • WHO KNOWS? ICECUBE/DEEPCORE will see neutrinos in five years if PAMELA anomaly is from DM Spolyar, Buckley, Freese, Hooper, Murayama 2009 String of phototubes in ice at South Pole DEEPCORE: Swedish contribution Per-Olaf Hulth Gamma-rays from the Galactic Center HESS Gamma-ray Data Aharonian et al 2004 FERMI satellite • NASA/DOE gamma-ray telescope • Launched June 2008 Where To Look For Dark Matter With FERMI? The Galactic Halo The Galactic Center -High statistics -Brightest spot in the sky -Requires detailed model -Considerable astrophysical of galactic backgrounds backgrounds Extragalactic Background -High statistics Individual Subhalos -potentially difficult to identify -Low backgrounds Diemand, Kuhlen, Madau, APJ, astro-ph/0611370 Latest bounds from FERMI diffuse gamma-rays (from talk of Elliott Bloom in UCLA) Latest bounds from FERMI diffuse flux for two muon final state Dobler, Finkbeiner,Cholis, Slatyer, Weiner 2009 I. FERMI HAZE: controversial (gamma rays from Galactic Center) II. See also model of Dan Hooper for yet another interpretation due to DM annihilation in FERMI Hooper/Goodenough model to explain FERMI data to GC Abazajian, Agrawal, Chacko claim to rule out PAMELA WMAP microwave emission interpreted as dark matter annihilation in inner galaxy? WMAP HAZE Consistent with 100 GeV WIMPs. Finkbeiner 2005; Hooper, Dobler 2007 Possible evidence for WIMP detection already now: • The DAMA annual modulation • The HEAT/PAMELA positron excess • Gamma-rays from Galactic Center • WMAP haze • Theorists are looking for models in which these results are consistent with one another (given an interpretation in terms of WIMPs) Upcoming Data: will the Dark Matter be found in 2010? • LHC (find SUSY) • Indirect Detection due to annihilation: • FERMI (gamma rays) • PAMELA (positrons) • ICECUBE (neutrinos) • GAPS (antideuterons) • Direct Detection: many experiments • Directional Detection: see talk of D. Snowden-Ifft What will it take for us to believe DM has been found? • I. Direct detection: compatible signals in a variety of experiments made of different detector materials, and all the parties agree • 2. Indirect detection: annihilation signals in a variety of channels (neutrinos, gamma-rays, etc) all coming from the same source Sagittarius stream Freese, Gondolo, Newberg 2003 Directional detection with DRIFT-II THE END .
Load more

Recommended publications
  • Parallel Sessions
    Identification of Dark Matter July 23-27, 2012 9th International Conference Chicago, IL http://kicp-workshops.uchicago.edu/IDM2012/ PARALLEL SESSIONS http://kicp.uchicago.edu/ http://www.nsf.gov/ http://www.uchicago.edu/ http://www.fnal.gov/ International Advisory Committee Daniel Akerib Elena Aprile Rita Bernabei Case Western Reserve University, Columbia University, USA Universita degli Studi di Roma, Italy Cleveland, USA Gianfranco Bertone Joakim Edsjo Katherine Freese University of Amsterdam Oskar Klein Centre / Stockholm University of Michigan, USA University Richard Gaitskell Gilles Gerbier Anne Green Brown University, USA IRFU/ CEA Saclay, France University of Nottingham, UK Karsten Jedamzik Xiangdong Ji Lawrence Krauss Universite de Montpellier, France University of Maryland, USA Arizona State University, USA Vitaly Kudryavtsev Reina Maruyama Leszek Roszkowski University of Sheffield University of Wisconsin-Madison University of Sheffield, UK Bernard Sadoulet Pierre Salati Daniel Santos University of California, Berkeley, USA University of California, Berkeley, USA LPSC/UJF/CNRS Pierre Sikivie Daniel Snowden-Ifft Neil Spooner University of Florida, USA Occidental College University of Sheffield, UK Max Tegmark Karl van Bibber Kavli Institute for Astrophysics & Space Naval Postgraduate School Monterey, Research at MIT, USA USA Local Organizing Committee Daniel Bauer Matthew Buckley Juan Collar Fermi National Accelerator Laboratory Fermi National Accelerator Laboratory Kavli Institute for Cosmological Physics Scott Dodelson Aimee
    [Show full text]
  • THE COSMIC COCKTAIL Three Parts Dark Matter
    release For immediate release Contact: Andrew DeSio Publication Date: June 11, 2014 (609) 258-5165 [email protected] Weaving a tale of scientific discovery, adventures in cosmology, and the hunt for dark matter, Dr. Katherine Freese explores just what exactly the universe is made out of in THE COSMIC COCKTAIL Three Parts Dark Matter “Freese tells her trailblazing and very personal story of how the worlds of particle physics and astronomy have come together to unveil the mysterious ingredients of the cosmic cocktail that we call our universe.” Brian Schmidt, 2011 Nobel Laureate in Physics, Australian National University What is dark matter? Where is it? Where did it come from? How do scientists study the stuff when they can’t see it? According to current research, our universe consists of only 5% ordinary matter (planets, comets, galaxies) while the rest is made of dark matter (26%) and dark energy (69%). Scientists and researchers are hard at work trying to detect these mysterious phenomena. And there are none further ahead in the pursuit than Dr. Katherine Freese, one of today’s foremost pioneers in the study of dark matter. In her splendidly written new book THE COSMIC COCKTAIL: Three Parts Dark Matter (Publication Date: June 11, 2014; $29.95), Dr. Freese tells the inside story of the epic quest to solve one of the most compelling enigmas of modern science—what is the universe made of? Blending cutting-edge science with her own behind-the-scenes insights as a leading researcher in the field, acclaimed theoretical physicist Katherine Freese recounts the hunt for dark matter, from the predictions and discoveries of visionary scientists like Fritz Zwicky— the Swiss astronomer who coined the term "dark matter" in 1933—to the deluge of data today from underground laboratories, satellites in space, and the Large Hadron Collider.
    [Show full text]
  • Formation of Structure in Dark Energy Cosmologies
    HELSINKI INSTITUTE OF PHYSICS INTERNAL REPORT SERIES HIP-2006-08 Formation of Structure in Dark Energy Cosmologies Tomi Sebastian Koivisto Helsinki Institute of Physics, and Division of Theoretical Physics, Department of Physical Sciences Faculty of Science University of Helsinki P.O. Box 64, FIN-00014 University of Helsinki Finland ACADEMIC DISSERTATION To be presented for public criticism, with the permission of the Faculty of Science of the University of Helsinki, in Auditorium CK112 at Exactum, Gustaf H¨allstr¨omin katu 2, on November 17, 2006, at 2 p.m.. Helsinki 2006 ISBN 952-10-2360-9 (printed version) ISSN 1455-0563 Helsinki 2006 Yliopistopaino ISBN 952-10-2961-7 (pdf version) http://ethesis.helsinki.fi Helsinki 2006 Helsingin yliopiston verkkojulkaisut Contents Abstract vii Acknowledgements viii List of publications ix 1 Introduction 1 1.1Darkenergy:observationsandtheories..................... 1 1.2Structureandcontentsofthethesis...................... 6 2Gravity 8 2.1Generalrelativisticdescriptionoftheuniverse................. 8 2.2Extensionsofgeneralrelativity......................... 10 2.2.1 Conformalframes............................ 13 2.3ThePalatinivariation.............................. 15 2.3.1 Noethervariationoftheaction..................... 17 2.3.2 Conformalandgeodesicstructure.................... 18 3 Cosmology 21 3.1Thecontentsoftheuniverse........................... 21 3.1.1 Darkmatter............................... 22 3.1.2 Thecosmologicalconstant........................ 23 3.2Alternativeexplanations............................
    [Show full text]
  • Conference Program
    Identification of Dark Matter July 23-27, 2012 9th International Conference Chicago, IL http://kicp-workshops.uchicago.edu/IDM2012/ CONFERENCE PROGRAM http://kicp.uchicago.edu/ http://www.nsf.gov/ http://www.uchicago.edu/ http://www.fnal.gov/ International Advisory Committee Daniel Akerib Elena Aprile Rita Bernabei Case Western Reserve University, Columbia University, USA Universita degli Studi di Roma, Italy Cleveland, USA Gianfranco Bertone Joakim Edsjo Katherine Freese University of Amsterdam Oskar Klein Centre / Stockholm University of Michigan, USA University Richard Gaitskell Gilles Gerbier Anne Green Brown University, USA IRFU/ CEA Saclay, France University of Nottingham, UK Karsten Jedamzik Xiangdong Ji Lawrence Krauss Universite de Montpellier, France University of Maryland, USA Arizona State University, USA Vitaly Kudryavtsev Reina Maruyama Leszek Roszkowski University of Sheffield University of Wisconsin-Madison University of Sheffield, UK Bernard Sadoulet Pierre Salati Daniel Santos University of California, Berkeley, USA University of California, Berkeley, USA LPSC/UJF/CNRS Pierre Sikivie Daniel Snowden-Ifft Neil Spooner University of Florida, USA Occidental College University of Sheffield, UK Max Tegmark Karl van Bibber Kavli Institute for Astrophysics & Space Naval Postgraduate School Monterey, Research at MIT, USA USA Local Organizing Committee Daniel Bauer Matthew Buckley Juan Collar Fermi National Accelerator Laboratory Fermi National Accelerator Laboratory Kavli Institute for Cosmological Physics Scott Dodelson Aimee
    [Show full text]
  • Matthew Robert Buckley
    Matthew Robert Buckley Rutgers, The State University of New Jersey Cell: 626 379 4337 Department of Physics & Astronomy E-mail: [email protected] 136 Frelinghuysen Rd, Piscataway, NJ 08854 [email protected] Citizenship United States of America Education • 2003-2008 University of California, Berkeley Ph.D. Theoretical Particle Physics (received May 2008) Advisor: Professor Hitoshi Murayama M.A. Physics (received May 2005) • 1999-2003 Kenyon College B.A. summa cum laude Mathematics and Physics (received May 2003) Work Experience • September 2013-Present Assistant Research Professor, Rutgers, The State University of New Jersey • August 2010-August 2013 David N. Schramm Fellow, Fermi National Accel- erator Laboratory • September 2008-August 2010 Du Bridge Postdoctoral Scholar, Prize Fellow, California Institute of Technology • January-May 2008 Foreign Researcher, Institute of Physics and Mathematics of the Universe, Tokyo University • 2006-2008 Graduate Student Researcher with Hitoshi Murayama, University of California, Berkeley • 2003-2006 Graduate Student Instructor, University of California, Berkeley 1 Fellowships and Awards • 2010 David N. Schramm Fellow, Fermi National Accelerator Laboratory • 2008 Prize Fellowship, California Institute of Technology • 2004 Outstanding Graduate Student Instructor Award, University of California, Berkeley • 2002 Phi Beta Kappa, Kenyon College • 2002 Franklin Miller Award for Undergraduate Research, Kenyon College • 2001 Goldwater Scholar in Mathematics, Science and Engineering (Barry
    [Show full text]
  • Inelastic Dark Matter Scattering Off Thallium Cannot Save DAMA
    NORDITA-2020-123; UTTG-24-2020 Inelastic dark matter scattering off Thallium cannot save DAMA Sunniva Jacobsen,a Katherine Freese,a;b;c Chris Kelso,d Pearl Sandick,e Patrick Stengela;f;g;h aThe Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, 10691 Stockholm, Sweden bNordita, KTH Royal Institute of Technology and Stockholm University Roslagstullsbacken 23, 10691 Stockholm, Sweden cDepartment of Physics, University of Texas, Austin, TX 78722 dDepartment of Physics, University of North Florida, Jacksonville, FL 32224, USA eDepartment of Physics and Astronomy, University of Utah, Salt Lake City, UT 84102, USA f Scuola Internazionale Superiore di Studi Avanzati (SISSA), via Bonomea 265, 34136 Trieste, Italy gINFN, Sezione di Trieste, via Valerio 2, 34127 Trieste, Italy hInstitute for Fundamental Physics of the Universe (IFPU), via Beirut 2, 34151 Trieste, Italy Abstract. We study the compatibility of the observed DAMA modulation signal with in- elastic scattering of dark matter (DM) off of the 0:1% Thallium (Tl) dopant in DAMA. In this work we test whether there exist regions of parameter space where the Tl interpretation gives a good fit to the most recent data from DAMA, and whether these regions are compati- ble with the latest constraints from other direct detection experiments. Previously, Chang et al. in 2010 [1], had proposed the Tl interpretation of the DAMA data, and more recently (in arXiv:2102.08367v2 [hep-ph] 17 Mar 2021 2019) the DAMA/LIBRA collaboration [2] found regions in parameter space of Tl inelastic scattering that differ by more than 10σ from a no modulation hypothesis.
    [Show full text]
  • Arxiv:2010.00015V3 [Hep-Ph] 26 Apr 2021 Galactic Halo Can Scatter with Exoplanets, Lose Energy, and Gles Are the Same Set of Planets, Without DM Heating
    MIT-CTP/5230 SLAC-PUB-17556 Exoplanets as Sub-GeV Dark Matter Detectors Rebecca K. Leane1, 2, ∗ and Juri Smirnov3, 4, y 1Center for Theoretical Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 2SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94039, USA 3Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, Columbus, OH 43210, USA 4Department of Physics, The Ohio State University, Columbus, OH 43210, USA (Dated: April 27, 2021) We present exoplanets as new targets to discover Dark Matter (DM). Throughout the Milky Way, DM can scatter, become captured, deposit annihilation energy, and increase the heat flow within exoplanets. We estimate upcoming infrared telescope sensitivity to this scenario, finding actionable discovery or exclusion searches. We find that DM with masses above about an MeV can be probed with exoplanets, with DM-proton and DM-electron scattering cross sections down to about 10−37cm2, stronger than existing limits by up to six orders of magnitude. Supporting evidence of a DM origin can be identified through DM-induced exoplanet heating correlated with Galactic position, and hence DM density. This provides new motivation to measure the temperature of the billions of brown dwarfs, rogue planets, and gas giants peppered throughout our Galaxy. Introduction{Are we alone in the Universe? This ques- Exoplanet Temperatures tion has driven wide-reaching interest in discovering a 104 planet like our own. Regardless of whether or not we ever find alien life, the scientific advances from finding DM Heating and understanding other planets will be enormous. From a particle physics perspective, new celestial bodies pro- vide a vast playground to discover new physics.
    [Show full text]
  • David Norman Schramm October 25, 1945–December 19, 1997
    NATIONAL ACADEMY OF SCIENCES D AVID NORMAN SCHRAMM 1 9 4 5 — 1 9 9 7 A Biographical Memoir by M I C H A E L S . T URNER Any opinions expressed in this memoir are those of the author and do not necessarily reflect the views of the National Academy of Sciences. Biographical Memoir COPYRIGHT 2009 NATIONAL ACADEMY OF SCIENCES WASHINGTON, D.C. DAVID NORMAN SCHRAMM October 25, 1945–December 19, 1997 B Y MICHAEL S . TURNER “ E LIVED LARGE IN ALL DIMENSIONS.” That is how Leon HLederman began his eulogy of David N. Schramm at a memorial service held in Aspen, Colorado, in December 1997. His large presence in space went beyond his 6-foot, 4-inch, 240-pound frame and bright red hair. In spite of his tragic death in a plane crash at age 52, Schramm lived large in the time dimension, too. At 18, he was married, a father, and a freshman physics major at MIT. After receiving his Ph.D. in physics from Caltech at 25, Schramm joined the faculty at the University of Texas at Austin. He left for Chicago two years later, and became the chair of the Astronomy and Astrophysics Department at the University of Chicago at age 2. He was elected to the National Academy of Sciences in 1986 at 40, became chair of the National Research Council’s Board on Physics and Astronomy at 47, and two years later became vice president for research at Chicago. He also had time for mountain climbing, summiting the highest peaks in five of the seven continents (missing Asia and Antarctica), driving a red Porsche with license plates that read “Big Bang,” and flying—owning four airplanes over his 12-year flying career and logging hundreds of hours annually.
    [Show full text]
  • Department of Physics and Astronomy
    DEPARTMENT OF PHYSICS AND ASTRONOMY PHY326 Dark Matter and the Universe (please note was PHY323 for 13/14) PHY426 Autumn 10 Credits Staff contact Prof Neil Spooner - [email protected] - 0114 222 4422 Outline Description The topic of Dark Matter in the Universe is arguably the most exciting and important area in physics and cosmology at the current time. It concerns one of the biggest mysteries in science, that the vast majority of the Universe is not normal baryonic matter but is something much stranger, something non- luminous and as yet of unknown form. The journey that scientists are undertaking now to understand this problem is already leading to new fundamental physics and is revolutionizing our understanding of the Universe. This course will explore the topic in detail. It will explain the overwhelming observational evidence for the existence of the so-called Dark Matter and Dark energy, explore what scientists believe it is most likely to be and study what is happening in the world-wide race to confirm the most likely explanation, that it is new fundamental particles from the Big Bang. Dark Matter determines our very existence, it holds galaxies together, makes life possible and is crucial to the eventual fate of our Universe. No topic in physics covers such a range of scale, from the smallest particle to the structure of the whole Universe, or holds such importance to our understanding of nature. To do this justice the course has a highly multidisciplinary flavour, combining work in astronomy, particle physics, solid state physics, detector technology and philosophy, encouraging development of skills in all these.
    [Show full text]
  • University of Zurich Preparations for Measurements of the Low Energy
    University of Zurich Physics institute Spring 2012 Master Thesis Preparations for measurements of the low energy response of liquid xenon Composer : Payam Pakarha Supervisors: Prof. L. Baudis & Prof. M. Ribordy Cosupervisor: Dr. A. Manalaysay 1 Acknowledgments During the period of my Master thesis, I have been communicating with many peo- ple who supported me kindly while, to only some of whom it is possible to give particular mention here. First, I would like to mention Hesam, Ehsan, Mehrdad and Iman whom I lived to- gether with among the first year of my studies as a master student in Lausanne. Specially, I'd like to thank Ehsan since he introduced me Latex and tried to recom- mend me using it. Hesam also for his powerful ability in computer handling who resolved any problem I had with computers. Thank to Prof. Riccardo Rattazzi and Dr. Simone Andrea who supervised me on my two semester projects (TP(I),(II)) at cole Polytechnique Fdrale de Lausanne. It was very helpful and enjoying working with your group on theoretical particle physics. To David Heymes, my best friend in first two semesters in Lausanne. I enjoyed studying together for the exams and still remember the last time we met before you leave to Germany. I hope to see you soon again. I particularly thank Carmelina Genovese first, as our secretary at physics depart- ment, university of Zurich since helping me for documentations and paperwork. Second, as a friend who helped me out of her duty to find a flat in Zurich. Giovanni Benato for hosting me and my wife while we had nowhere to stay in Zurich and helping us to move to our new flat and also it was very nice to have breaks with you while I was working on my project.
    [Show full text]
  • List of Participants
    COSMO 2014 August 25-29, 2014 International Conference on Particle Physics and Cosmology, 2014 Chicago, IL http://cosmo2014.uchicago.edu/ LIST OF PARTICIPANTS http://kicp.uchicago.edu/ http://www.nsf.gov/ http://www.kavlifoundation.org/ http://www.uchicago.edu/ The 18th annual International Conference on Particle Physics and Cosmology (COSMO 2014) will be held in Chicago on August 25 29, 2014. The meeting is being hosted by the Kavli Institute for Cosmological Physics (KICP) at the University of Chicago, and will be held at the University of Chicago's Gleacher Center in downtown Chicago. Plenary Speakers Nima Arkani-Hamed Laura Baudis Stefano Borgani Institute for Advanced Study University of Zurich Astronomical Observatory of Trieste Kiwoon Choi Ryan Foley Wendy Freedman Institute for Basic Science (IBS) University of Illinois, Urbana-Champaign Carnegie Observatories Daniel Green Catherine Heymans Justin Khoury CITA University of Edinburgh University of Pennsylvania Will Kinney Lloyd Knox John Kovac University at Buffalo, SUNY UC Davis Harvard University Andrei Linde Nikhil Padmanabhan Hiranya Peiris Stanford University Yale University University College London Sarah Shandera Eva Silverstein Tracy Slatyer Pennsylvania State University Stanford University Massachusetts Institute of Technology Mark Trodden Neal Weiner University of Pennsylvania New York University International Steering Committee Vernon Barger Daniel Baumann John Beacom University of Wisconsin-Madison Cambridge University Ohio State University David Caldwell Jonathan Ellis
    [Show full text]
  • Searching for Dark Matter with Paleo-Detectors
    NORDITA-2018-043 LCTP-18-15 Searching for Dark Matter with Paleo-Detectors Sebastian Baum,1, 2, 3, ∗ Andrzej K. Drukier,1, y Katherine Freese,1, 2, 4, 5, z Maciej G´orski,6, x and Patrick Stengel1, { 1The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, Alba Nova, 10691 Stockholm, Sweden 2Nordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, 10691 Stockholm, Sweden 3Stanford Institute for Theoretical Physics, Department of Physics, Stanford University, Stanford, CA 94305, USA 4Leinweber Center for Theoretical Physics, University of Michigan, Ann Arbor, MI 48109, USA 5Department of Physics, University of Texas, Austin, TX 78712, USA 6National Centre for Nuclear Research, 05-400 Otwock, Swierk,´ Poland A large experimental program is underway to extend the sensitivity of direct detection experi- ments, searching for interaction of Dark Matter with nuclei, down to the neutrino floor. However, such experiments are becoming increasingly difficult and costly due to the large target masses and exquisite background rejection needed for the necessary improvements in sensitivity. We investigate an alternative approach to the detection of Dark Matter{nucleon interactions: Searching for the persistent traces left by Dark Matter scattering in ancient minerals obtained from much deeper than current underground laboratories. We estimate the sensitivity of paleo-detectors, which ex- tends far beyond current upper limits for a wide range of Dark Matter masses. The sensitivity of our proposal also far exceeds the upper limits set by Snowden-Ifft et al. more than three decades ago using ancient Mica in an approach similar to paleo-detectors. I.
    [Show full text]