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Dark Energy Task Force (DETF) Membership List Dr. Rocky Kolb (Chair) Dr. John Huth Particle Astrophysics Center MS209 Department of Physics Fermi National Accelerator Laboratory Harvard University P.O. Box 500 17 Oxford Street Batavia, Illinois 60510-0500 Cambridge, MA 02138 Phone: (630) 840-4695 Phone: (617) 495-8144 Email: [email protected] Email: [email protected] Dr. Andreas Albrecht Dr. Marc Kamionkowski Department of Physics Mail Code 130-33 University of California California Institute of Technology One Shields Ave Pasadena, CA 91125 Davis, CA 95616 Phone: (626) 395-2563 Phone: (530) 754-9269 Email: [email protected] Email: [email protected] Dr. Lloyd Knox Dr. Gary Bernstein Physics Department University of Pennsylvania University of California, Davis 4N1 David Rittenhouse Lab One Shields Avenue 209 S 33rd St Davis, CA 95616 Philadelphia, PA 19104 Phone: (530) 754-7352 Phone: (215) 573-6252 Email: [email protected] Email: [email protected] Dr. John Mather Dr. Bob Cahn NASA-GSFC 5101 Building 50A Code 685 Lawrence Berkeley National Laboratory Greenbelt, MD 20771 1 Cyclotron Road Phone: (301) 286-8720 Berkeley, CA 94720 Email: [email protected] Phone: (510) 486-4481 Email: [email protected] Dr. Suzanne Staggs Department of Physics Dr. Wendy Freedman Jadwin Hall, P.O. Box 708 Carnegie Observatories Princeton University 813 Santa Barbara Street Princeton, NJ 08544-0708 Pasadena, California 91101 Phone: (609) 258-5930 Phone: (626) 304-0204 Email: [email protected] Email: [email protected] Dr. Nicholas Suntzeff Dr. Jacqueline Hewitt Cerro Tololo Inter-American Observatory Department of Physics, Room 37-607 Casilla 603 Massachusetts Institute of Technology La Serena, Chile Cambridge, MA 02139 Phone: 011-56-51-205200 Phone: (617) 253-3071 Email: [email protected] Email: [email protected] Dr. Wayne Hu Department of Astronomy and Astrophysics University of Chicago Chicago, IL 60637 Phone: (773) 702-0160 Email: [email protected] .

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Arxiv:1803.02804V1 [Hep-Ph] 7 Mar 2018 It Must Have Some Rather Speciﬁc Characteristics
FERMILAB-PUB-18-066-A Severely Constraining Dark Matter Interpretations of the 21-cm Anomaly Asher Berlina,∗ Dan Hooperb;c;d,y Gordan Krnjaicb,z and Samuel D. McDermottbx aSLAC National Accelerator Laboratory, Menlo Park CA, 94025, USA bFermi National Accelerator Laboratory, Theoretical Astrophysics Group, Batavia, IL, USA cUniversity of Chicago, Kavli Institute for Cosmological Physics, Chicago IL, USA and dUniversity of Chicago, Department of Astronomy and Astrophysics, Chicago IL, USA (Dated: March 8, 2018) The EDGES Collaboration has recently reported the detection of a stronger-than-expected ab- sorption feature in the global 21-cm spectrum, centered at a frequency corresponding to a redshift of z ∼ 17. This observation has been interpreted as evidence that the gas was cooled during this era as a result of scattering with dark matter. In this study, we explore this possibility, applying constraints from the cosmic microwave background, light element abundances, Supernova 1987A, and a variety of laboratory experiments. After taking these constraints into account, we ﬁnd that the vast majority of the parameter space capable of generating the observed 21-cm signal is ruled out. The only range of models that remains viable is that in which a small fraction, ∼ 0:3 − 2%, of the dark matter consists of particles with a mass of ∼ 10 − 80 MeV and which couple to the photon through a small electric charge, ∼ 10−6 −10−4. Furthermore, in order to avoid being overproduced in the early universe, such models must be supplemented with an additional depletion mechanism, such as annihilations through a Lµ − Lτ gauge boson or annihilations to a pair of rapidly decaying hidden sector scalars.
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Report from the Dark Energy Task Force (DETF)
Fermi National Accelerator Laboratory Fermilab Particle Astrophysics Center P.O.Box 500 - MS209 Batavia, Il l i noi s • 60510 June 6, 2006 Dr. Garth Illingworth Chair, Astronomy and Astrophysics Advisory Committee Dr. Mel Shochet Chair, High Energy Physics Advisory Panel Dear Garth, Dear Mel, I am pleased to transmit to you the report of the Dark Energy Task Force. The report is a comprehensive study of the dark energy issue, perhaps the most compelling of all outstanding problems in physical science. In the Report, we outline the crucial need for a vigorous program to explore dark energy as fully as possible since it challenges our understanding of fundamental physical laws and the nature of the cosmos. We recommend that program elements include 1. Prompt critical evaluation of the benefits, costs, and risks of proposed long-term projects. 2. Commitment to a program combining observational techniques from one or more of these projects that will lead to a dramatic improvement in our understanding of dark energy. (A quantitative measure for that improvement is presented in the report.) 3. Immediately expanded support for long-term projects judged to be the most promising components of the long-term program. 4. Expanded support for ancillary measurements required for the long-term program and for projects that will improve our understanding and reduction of the dominant systematic measurement errors. 5. An immediate start for nearer term projects designed to advance our knowledge of dark energy and to develop the observational and analytical techniques that will be needed for the long-term program. Sincerely yours, on behalf of the Dark Energy Task Force, Edward Kolb Director, Particle Astrophysics Center Fermi National Accelerator Laboratory Professor of Astronomy and Astrophysics The University of Chicago REPORT OF THE DARK ENERGY TASK FORCE Dark energy appears to be the dominant component of the physical Universe, yet there is no persuasive theoretical explanation for its existence or magnitude.
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Kinetic Decoupling of Neutralino Dark Matter
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FARSIDE Probe Study Final Report
Study Participants List, Disclaimers, and Acknowledgements Study Participants List Principal Authors Jack O. Burns, University of Colorado Boulder Gregg Hallinan, California Institute of Technology Co-Authors Jim Lux, NASA Jet Propulsion Laboratory, California Institute of Andres Romero-Wolf, NASA Jet Propulsion Laboratory, California Technology Institute of Technology Lawrence Teitelbaum, NASA Jet Propulsion Laboratory, California Tzu-Ching Chang, NASA Jet Propulsion Laboratory, California Institute of Technology Institute of Technology Jonathon Kocz, California Institute of Technology Judd Bowman, Arizona State University Robert MacDowall, NASA Goddard Space Flight Center Justin Kasper, University of Michigan Richard Bradley, National Radio Astronomy Observatory Marin Anderson, California Institute of Technology David Rapetti, University of Colorado Boulder Zhongwen Zhen, California Institute of Technology Wenbo Wu, California Institute of Technology Jonathan Pober, Brown University Steven Furlanetto, UCLA Jordan Mirocha, McGill University Alex Austin, NASA Jet Propulsion Laboratory, California Institute of Technology Disclaimers/Acknowledgements Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The cost information contained in this document is of a budgetary and planning nature and is intended for informational purposes only. It does not constitute a commitment on the part of JPL and/or Caltech © 2019.
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Table of Contents (Print)
PHYSICAL REVIEW D PERIODICALS For editorial and subscription correspondence, Postmaster send address changes to: please see inside front cover (ISSN: 1550-7998) APS Subscription Services P.O. Box 41 Annapolis Junction, MD 20701 THIRD SERIES, VOLUME 97, NUMBER 12 CONTENTS D15 JUNE 2018 The Table of Contents is a total listing of Parts A and B. Part A consists of articles 121301–124019, and Part B articles 124020–129903(E) PART A RAPID COMMUNICATIONS Emergent dark energy from dark matter (6 pages) ................................................................................... 121301(R) Takeshi Kobayashi and Pedro G. Ferreira ARTICLES Search for gamma-ray emission from the nearby dwarf spheroidal galaxies with 9 years of Fermi-LAT data (7 pages) 122001 Shang Li, Kai-Kai Duan, Yun-Feng Liang, Zi-Qing Xia, Zhao-Qiang Shen, Xiang Li, Neng-Hui Liao, Lei Feng, Qiang Yuan, Yi-Zhong Fan, and Jin Chang Calibrating the system dynamics of LISA Pathfinder (14 pages) .................................................................. 122002 M. Armano et al. Particle swarm optimization of the sensitivity of a cryogenic gravitational wave detector (12 pages) ...................... 122003 Yuta Michimura, Kentaro Komori, Atsushi Nishizawa, Hiroki Takeda, Koji Nagano, Yutaro Enomoto, Kazuhiro Hayama, Kentaro Somiya, and Masaki Ando Reconstruction of cosmic ray air showers with Tunka-Rex data using template fitting of radio pulses (10 pages) ....... 122004 P. A. Bezyazeekov, N. M. Budnev, D. Chernykh, O. Fedorov, O. A. Gress, A. Haungs, R. Hiller, T. Huege, Y. Kazarina, M. Kleifges, D. Kostunin, E. E. Korosteleva, L. A. Kuzmichev, V. Lenok, N. Lubsandorzhiev, T. Marshalkina, R. R. Mirgazov, R. Monkhoev, E. Osipova, A. Pakhorukov, L. Pankov, V. V. Prosin, F.
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New Views of Cosmology and the Microworld
XXX SLAC Summer Institute (SSI2002), Stanford, CA, 5-16 August, 2002 NEW VIEWS OF COSMOLOGY AND THE MICROWORLD Marc Kamionkowski∗ California Institute of Technology Mail Code 130-33 Pasadena, CA 91125 ABSTRACT The past few years have seen several breakthroughs in particle astrophysics and cosmology. In several cases, new observations can only be explained with the introduction of new fundamental physics. In this talk I summarize some of these recent advances and describe several areas where progress may well be made in the future. More specifically, I focus on supersymmet- ric and axion dark matter, self-interacting dark matter, cosmic-microwave- background and large-scale-structure tests of inflation, and the dark-energy problem. ∗Supported by NASA NAG5-9821 and DoE DE-FG03-92-ER40701. c 2002 by Marc Kamionkowski. TF04 713 XXX SLAC Summer Institute (SSI2002), Stanford, CA, 5-16 August, 2002 1 Introduction The aim of particle physics is to understand the fundamental laws of nature. The primary tools in this endeavor have been and continue to be accelerator experiments which provide controlled environments for precise experiments. However, this avenue may have limitations, especially considering that many of the most promising ideas for new physics beyond the standard model—e.g., grand unification and quantum gravity—can be tested only at energies many orders of magnitude greater than those accessible by current and planned accelerators. We have recently seen an increased effort to develop cosmological and astrophysical tools to search for and/or constrain new physics beyond the standard model. These efforts do have precedents: Newton’s law of universal gravitation was motivated by planetary orbits.
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Dark Matter Astrophysics 3 2.1 Galactic Rotation Curves
Dark Matter Astrophysics Guido D’Amico, Marc Kamionkowski and Kris Sigurdson Abstract These lectures are intended to provide a brief pedagogical review of dark matter for the newcomer to the subject. We begin with a discussion of the astro- physical evidence for dark matter. The standard weakly-interacting massive particle (WIMP) scenario—the motivation, particle models, and detection techniques—is then reviewed. We provide a brief sampling of some recent variations to the stan- dard WIMP scenario as well as some alternatives (axions and sterile neutrinos). Exercises are provided for the reader.1 1 Introduction Dark matter is an essential ingredient in a good fraction of the literature on extra- galactic astronomy and cosmology. Since dark matter cannot be made of any of the usual standard-model particles (as we will discuss below), dark matter is also a cen- tral focus of elementary-particle physics. The purpose of this review is to provide a pedagogical introduction to the principle astrophysical evidence for dark matter and to some of the particle candidates. Rather than present a comprehensive survey of the vast and increasingly precise measurements of the amount and distribution of dark matter, we will present very Guido D’Amico SISSA, via Beirut 2-4, 34014 Trieste, Italy; e-mail: [email protected] Marc Kamionkowski arXiv:0907.1912v1 [astro-ph.CO] 10 Jul 2009 California Institute of Technology, Mail Code 350-17, Pasadena, CA 91125, USA; e-mail: [email protected] Kris Sigurdson Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, Canada; e-mail: [email protected] 1 Based on lectures given by MK at the Villa Olmo School on “The Dark Side of the Universe,” 14–18 May 2007 and by KS at the XIX Heidelberg Physics Graduate Days, 8-12 October 2007.
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Patrick C. Breysse's CV
Patrick C. Breysse Postdoctoral Fellow, Canadian Institute for Theoretical Astrophysics 60 St. George Street, Rm 1302, Toronto, ON Canada M5S 3H8 [email protected] • +1 (647) 534-0268 PROFESSIONAL Canadian Institute for Theoretical Astrophysics, Toronto, ON, Canada HISTORY Postdoctoral Fellow Sep 2017- Present EDUCATION Johns Hopkins University, Baltimore, MD, USA Doctor of Philosophy (Ph.D.) in Physics and Astronomy Jun 2012 – May 2017 • Adviser: Professor Marc Kamionkowski • Research areas: Theoretical cosmology, large scale structure, intensity mapping • Thesis: High-Redshift Astrophysics and Cosmology with Intensity Mapping Master of Arts (M.A.) in Physics and Astronomy Jun 2012 – May 2015 The Pennsylvania State University, University Park, Pennsylvania, USA Bachelor of Science (B.S.) in Physics Bachelor of Science (B.S.) in Astronomy and Astrophysics Aug 2008 – May 2012 • Graduated with Distinction and with Honors in Physics. COLLABORATION Carbon Monoxide Mapping Array Pathfinder (COMAP) MEMBERSHIPS Lead, Science & Modeling Working Group 2018 – Present Cerro Chajnantor Atacama Telescope – PRIME (CCATp) Member, Science Working Group 2018 – Present EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) Member, Science Working Group 2019 – Present SELECTED Participant, 66th Lindau Nobel Laureate Meeting, Jun 2016 AWARDS Max Bodmer Graduate Research Fellowship, Sep 2012 Penn State Astronomy and Astrophysics Student Marshall, May 2012 Astronaut Scholarship, 2011 STUDENTS Anubhav Mathur MENTORED former Univ. of Toronto undergraduate (now grad student at JHU) Henry Liu UBC undergraduate TEACHING Summer Astro 101 Course Summer 2018, 2019 Lecturer CITA cosmology blackboard talks 2017–Present Speaker, 6× CITA pedagogical blackboard talks 2017–present Speaker, 4× General Physics I, JHU Spring 2014 Teaching Assistant Special Relativity and Waves, JHU Fall 2013 Teaching Assistant Page 1 of 4 PROFESSIONAL CITA Cosmology Discussion Group SERVICE Lead Organizer 2019–Present Univ.
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Julian B. Muñoz, Ph.D
Julian B. Muñoz, Ph.D. Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 (443) 683-4277; [email protected]; www.julianbmunoz.com RESEARCH INTERESTS I am a broadly trained theoretical astrophysicist with an emphasis in cosmology and particle physics. I am interested in using novel data-sets, like the 21-cm line of hydrogen or fast radio bursts, to learn about dark matter and dark energy in the cosmos. I am proud to have discovered a new velocity-based standard ruler to measure the expansion rate of the universe during cosmic dawn. My research also involves understanding outstanding astrophysical events, such as gravitational waves from black-hole mergers and the formation of the first galaxies during cosmic dawn and the epoch of reionization. RESEARCH EXPERIENCE 2020-25 Clay Fellow, Harvard-Smithsonian Center for Astrophysics, Cambridge, MA. 2017-20 Postdoctoral Fellow, Department of Physics, Harvard University, Cambridge, MA. Faculty Advisors: Cora Dvorkin and Abraham Loeb, Professors. 2013-17 Graduate Student, Physics & Astronomy Department, JHU, Baltimore, MD. Faculty Advisor: Marc Kamionkowski, Professor. 2013 Research Assistant, Complutense University of Madrid, Spain. Faculty Advisor: Gabriel Álvarez Galindo, Professor. 2012 Research Intern, Instituto Astrofísico de Canarias, Tenerife, Spain. Faculty Advisors: Carlos Allende and Andrés Asensio, Professors. EDUCATION 2017 Ph.D. in Physics, Johns Hopkins University. Thesis: “New Cosmological Probes for Old Fundamental Questions”. Ph.D. Advisor: Marc Kamionkowski, Professor. 2013 Graduado en Física (B.A. in Physics), Complutense University of Madrid. SELECTED INVITED TALKS “Searching for new physics with the 21-cm line”, Colloquium at ETH Zurich (2020), and seminar at Cornell, KIAS, CERN, YITP, PSU, Perimeter, Yale, ETH Zurich, NYU, IFT, Weizmann (2019-20).
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Table of Contents (Print)
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Weighing the Universe with the Cosmic Microwave Background
CU-TP-703 SU-4240-614 POP-629 CfA-4136 astro-ph/9507080 Weighing the Universe with the Cosmic Microwave Background Gerard Jungman∗ Department of Physics, Syracuse University, Syracuse, New York 13244 Marc Kamionkowski† Department of Physics, Columbia University, New York, New York 10027 Arthur Kosowsky‡ Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138 and Department of Physics, Lyman Laboratory, Harvard University, Cambridge, Massachusetts 02138 David N. Spergel§ Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544 (July, 1995) arXiv:astro-ph/9507080v1 21 Jul 1995 ∗[email protected] †[email protected] ‡[email protected] §[email protected] 1 Abstract Variations in Ω, the total density of the Universe, leave a clear and distinctive imprint on the power spectrum of temperature ﬂuctuations in the cosmic mi- crowave background (CMB). This signature is virtually independent of other cosmological parameters or details of particular cosmological models. We evaluate the precision with which Ω can be determined by a CMB map as a function of sky coverage, pixel noise, and beam size. For example, assuming only that the primordial density perturbations were adiabatic and with no prior information on the values of any other cosmological parameters, a full- sky CMB map at 0.5◦ angular resolution and a noise level of 15 µK per pixel can determine Ω with a variance of 5%. If all other cosmological parameters are ﬁxed, Ω can be measured to better than 1%. 98.70.V, 98.80.C Typeset using REVTEX 2 Determination of the geometry of the Universe remains perhaps the most compelling problem in cosmology.
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The Discovery Potential of Space-Based Gravitational Wave Astronomy
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