Thermal Dark Matter Below an MeV
|
|
- Bryan Townsend
- 5 years ago
- Views:
Transcription
1 Thermal Dark Matter Below an MeV ASHER BERLIN TeVPA, Ohio State University August 9, 2017 Collaboration with Nikita Blinov, arxiv:
2 Dark Matter Mass dwarf galaxies MACHO GeV GeV
3 Dark Matter Mass dwarf galaxies QCD axion WIMP MACHO GeV 100 GeV GeV
4 Dark Matter Mass dwarf galaxies QCD axion WIMP MACHO GeV 100 GeV GeV
5 Dark Matter Mass dwarf galaxies QCD axion? WIMP MACHO GeV 100 GeV GeV
6 Dark Matter Mass dwarf galaxies QCD axion WIMP MACHO GeV 100 GeV GeV Thermal Contact
7 Dark Matter Mass dwarf galaxies QCD axion WIMP MACHO GeV 100 GeV GeV Thermal Contact BBN Light DM WIMPs Ω > GeV 10 GeV 10 5 GeV
8 Dark Matter Mass dwarf galaxies QCD axion WIMP MACHO GeV 100 GeV GeV Thermal Contact BBN Light DM WIMPs Ω > GeV 10 GeV 10 5 GeV
9 thermal dark matter noun Definition of THERMAL DARK MATTER : dark matter that acquired its cosmological abundance through thermal contact with the Standard Model bath at large temperatures. First Known Use: 1970s
10 Neff
11 Neff (standard assumption) DM-SM Equilibration > MeV Neutrino-Photon Decoupling ~ MeV T ~ mχ
12 Neff (standard assumption) DM-SM Equilibration > MeV Neutrino-Photon Decoupling ~ MeV T ~ mχ DM-Neutrino Equilibration N e ' /3 21 g & 3.78 &.
13 Sub-MeV: BBN + CMB
14 Sub-MeV: BBN + CMB. N e (BBN) ' 2.85 ± 0.28 ' ± K. Nollett, G. Steigman, arxiv:
15 inos at T & 2 MeV and T. 2 MeV N e ' (7) /41/3 21 g & 3.18 N e ' / 41/3 21 g & 3.18 (8) L ' L ' Sub-MeV: BBN + CMB (9) m. m m. m N e (BBN) (10) ' 2.85 ± 0.28 N e (BBN) ' 2.85 ± 0.28 N e (CMB) (11) ' 3.15 ± 0.23 N e (CMB) ' 3.15 ± 0.23 N e (CMB-S4) (12) ' ±0.027 N e (CMB-S4) ' ±0.027 (13) K. Nollett, G. Steigman, arxiv: Z. Hou, et al., arxiv:
16 inos at T & 2 MeV and T. 2 MeV N e ' (7) /41/3 21 g & 3.18 N e ' / 41/3 21 g & 3.18 (8) L ' L ' Sub-MeV: BBN + CMB (9) m. m m. m N e (BBN) (10) ' 2.85 ± 0.28 N e (BBN) ' 2.85 ± 0.28 N e (CMB) (11) ' 3.15 ± 0.23 N e (CMB) ' 3.15 ± 0.23 N e (CMB-S4) (12) ' ±0.027 N e (CMB-S4) ' ±0.027 (13) Thermal DM should be heavier than an MeV K. Nollett, G. Steigman, arxiv: Z. Hou, et al., arxiv:
17 How ubiquitous is DM-SM Equilibration Before Neutrino-Photon Decoupling?
18 How ubiquitous is DM-SM Equilibration Before Neutrino-Photon Decoupling? DM-Neutrino Equilibration N e ' /3 21 g & 3.78 &.
19 Dark Matter Mass Lee-Weinberg MeV GeV TeV χ SM Z m & m 2 Z GeV (T eq m pl ) 1/2 χ SM Sub-GeV thermal DM requires light mediators: m ' m B. Lee and S. Weinberg, Phys.Rev.Lett. 39 (1977)
20 Equilibration Light Mediator T,m 2 '/T Expansion H T 2 Heavy Mediator T ~ m j Heavy Mediator ' T 3 / 2 G H Light Mediator G = H ~ 1 ê T Æ
21 Equilibration Light Mediator T,m 2 '/T Expansion H T 2 Heavy Mediator T ~ m j Heavy Mediator ' T 3 / 2 G H Light Mediator G = H ~ 1 ê T Æ Light thermal DM naturally enters equilibrium (for high enough TRH)
22 Neff Neutrino-Photon Decoupling ~ MeV DM-SM Equilibration < MeV T ~ mχ DM-Neutrino & Equilibration. N e ' / 41/3 21 g & 3.18 L
23 Neff Neutrino-Photon Decoupling ~ MeV DM-SM Equilibration < MeV T ~ mχ DM-Neutrino & Equilibration. N e ' / 41/3 21 g & 3.18 L ' ± g. few
24 Neff i = Ti/T equil./e ± SM freeze-out T [MeV] ' decay
25 Thermal History Y DM WIMP ~ 1 ê T
26 Thermal History Light ''WIMP'' Y DM WIMP ~ 1 ê T
27 Thermal History Light ''WIMP'' Y DM Freeze-In WIMP ~ 1 ê T
28 A Toy Model ' L ' m. m χ ϕ ν ϕ ν χ ϕ (Freeze-Out) (Equilibration and Decay)
29 A Toy Model ' L ' Thermal Dark Matter Clusters l n = 10-8 mc ê m j 10 1 Ly-a l n = 10-9 Neff l n = m
30 Summary Sub-MeV DM that freezes-out thermally with the SM is possible. Equilibration predicts a limited range for DM-SM coupling. CMB-S4 and 21 cm observations will be sensitive to the entire parameter space.
31 Back Up Slides
32 Neff DM-SM Equilibration? Neutrino-Photon Decoupling ~ MeV End of BBN ~ 100 kev T Recombination ~ ev
33 Neff DM-SM Equilibration? Neutrino-Photon Decoupling ~ MeV End of BBN ~ 100 kev T Recombination ~ ev
34 Neff γ ν γ γ ν DM ν DM ν DM DM N e ' /3 21 g & 3.78 &.
35 Neff γ ν γ γ DM ν ν DM ν DM DM &. N e ' / 41/3 21 g L & 3.18
36 Neff γ ν γ γ DM ν ν DM ν DM DM &. N e ' / 41/3 21 g L & 3.18 (~ cyclic, but ds > 0)
37 Neff 5.5 Ne T eq >T dec 3.5 b 3.0 T eq <T dec a T [MeV]
Cosmological Production of Dark Matter
Dark Matter & Neutrino School ICTP-SAIFR July 23-27, 2018 Cosmological Production of Dark Matter Farinaldo Queiroz International Institute of Physics & ICTP-SAIFR Outline 1. Introduction Cold and hot thermal
More informationScalar field dark matter and the Higgs field
Scalar field dark matter and the Higgs field Catarina M. Cosme in collaboration with João Rosa and Orfeu Bertolami Phys. Lett., B759:1-8, 2016 COSMO-17, Paris Diderot University, 29 August 2017 Outline
More informationMaking Dark Matter. Manuel Drees. Bonn University & Bethe Center for Theoretical Physics. Making Dark Matter p. 1/35
Making Dark Matter Manuel Drees Bonn University & Bethe Center for Theoretical Physics Making Dark Matter p. 1/35 Contents 1 Introduction: The need for DM Making Dark Matter p. 2/35 Contents 1 Introduction:
More informationDark Matter in Particle Physics
High Energy Theory Group, Northwestern University July, 2006 Outline Framework - General Relativity and Particle Physics Observed Universe and Inference Dark Energy, (DM) DM DM Direct Detection DM at Colliders
More informationDark Matter from Non-Standard Cosmology
Dark Matter from Non-Standard Cosmology Bhaskar Dutta Texas A&M University Miami 2016 December 16, 2016 1 Some Outstanding Issues Questions 1. Dark Matter content ( is 27%) 2. Electroweak Scale 3. Baryon
More informationParticle Cosmology. V.A. Rubakov. Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Moscow State University
Particle Cosmology V.A. Rubakov Institute for Nuclear Research of the Russian Academy of Sciences, Moscow and Moscow State University Topics Basics of Hot Big Bang cosmology Dark matter: WIMPs Axions Warm
More informationParticles in the Early Universe
Particles in the Early Universe David Morrissey Saturday Morning Physics, October 16, 2010 Using Little Stuff to Explain Big Stuff David Morrissey Saturday Morning Physics, October 16, 2010 Can we explain
More informationsub-gev Dark Matter Theory Tien-Tien Yu (University of Oregon)
sub-gev Dark Matter Theory Tien-Tien Yu (University o Oregon) The Magniicent CEvNS University o Chicago Nov 2, 2018 WIMP miracle thermal equilibrium WIMP miracle reeze-out Ωh 2 10 37 cm 2 σ ann v 0.1 P.
More informationThe Four Basic Ways of Creating Dark Matter Through a Portal
The Four Basic Ways of Creating Dark Matter Through a Portal DISCRETE 2012: Third Symposium on Prospects in the Physics of Discrete Symmetries December 4th 2012, Lisboa Based on arxiv:1112.0493, with Thomas
More informationDark Radiation from Particle Decay
Dark Radiation from Particle Decay Jörn Kersten University of Hamburg Based on Jasper Hasenkamp, JK, JCAP 08 (2013), 024 [arxiv:1212.4160] Jörn Kersten (Uni Hamburg) Dark Radiation from Particle Decay
More informationDark Matter and Dark Energy components chapter 7
Dark Matter and Dark Energy components chapter 7 Lecture 3 See also Dark Matter awareness week December 2010 http://www.sissa.it/ap/dmg/index.html The early universe chapters 5 to 8 Particle Astrophysics,
More informationThe Linear Collider and the Preposterous Universe
The Linear Collider and the Preposterous Universe Sean Carroll, University of Chicago 5% Ordinary Matter 25% Dark Matter 70% Dark Energy Why do these components dominate our universe? Would an Apollonian
More informationCalculation of Momentum Distribution Function of a Non-Thermal Fermionic Dark Matter
Calculation of Momentum Distribution Function of a Non-Thermal Fermionic Dark Matter, March 8, 2017. arxiv:1612.02793, with Anirban Biswas. Aritra Gupta Why Non-Thermal? 1 / 31 The most widely studied
More informationCosmology. Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation
Cosmology Thermal history of the universe Primordial nucleosynthesis WIMPs as dark matter Recombination Horizon problem Flatness problem Inflation Energy density versus scale factor z=1/a-1 Early times,
More informationkev sterile Neutrino Dark Matter in Extensions of the Standard Model
kev sterile Neutrino Dark Matter in Extensions of the Standard Model Manfred Lindner Max-Planck-Institut für Kernphysik, Heidelberg F. Bezrukov, H. Hettmannsperger, ML, arxiv:0912.4415, PRD81,085032 The
More informationDARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1
DARK MATTER Martti Raidal NICPB & University of Helsinki 28.05.2010 Tvärminne summer school 1 Energy budget of the Universe 73,4% - Dark Energy WMAP fits to the ΛCDM model Distant supernova 23% - Dark
More informationLecture 19 Nuclear Astrophysics. Baryons, Dark Matter, Dark Energy. Experimental Nuclear Physics PHYS 741
Lecture 19 Nuclear Astrophysics Baryons, Dark Matter, Dark Energy Experimental Nuclear Physics PHYS 741 heeger@wisc.edu References and Figures from: - Haxton, Nuclear Astrophysics - Basdevant, Fundamentals
More informationSuperheavy Thermal Dark Matter
Superheavy Thermal Dark Matter 13th April 2018 University of Illinois at Chicago Work /w Joe Bramante [1701.05859] & Saleh Hamdan [1710.03758] 1/18 Introduction Xenon1T Unitarity 2/18 Superheavy Dark Matter
More informationBeyond the WIMP Alternative dark matter candidates. Riccardo Catena. Chalmers University
Beyond the WIMP Alternative dark matter candidates Riccardo Catena Chalmers University April 3, 2017 Outline WIMPs and the thermal production mechanism Generalized WIMPs Other candidates / production mechanisms
More information7 Relic particles from the early universe
7 Relic particles from the early universe 7.1 Neutrino density today (14 December 2009) We have now collected the ingredients required to calculate the density of relic particles surviving from the early
More informationPossible sources of very energetic neutrinos. Active Galactic Nuclei
Possible sources of very energetic neutrinos Active Galactic Nuclei 1 What might we learn from astrophysical neutrinos? Neutrinos not attenuated/absorbed Information about central engines of astrophysical
More informationA Minimal Supersymmetric Cosmological Model
A Minimal Supersymmetric Cosmological Model Ewan Stewart KAIST COSMO/CosPA 2010 University of Tokyo 29 September 2010 EDS, M Kawasaki, T Yanagida D Jeong, K Kadota, W-I Park, EDS G N Felder, H Kim, W-I
More informationCosmological Signatures of a Mirror Twin Higgs
Cosmological Signatures of a Mirror Twin Higgs Zackaria Chacko University of Maryland, College Park Curtin, Geller & Tsai Introduction The Twin Higgs framework is a promising approach to the naturalness
More informationMaking Light from the Dark Universe
Oxford University Physics Society, 1st May 2014 Talk Structure 1. Prelude: What is Dark Radiation? 2. Experimental motivation for dark radiation: CMB and BBN 3. Theoretical motivation for dark radiation:
More informationIntroduction: Cosmic Neutrinos Dark Radiation and the QGP Era Darkness Production: Universe Laboratory
Outline of the talk 1. Introduction: CMB fluctuation analysis observes N ν, number of invisible Cosmic Neutrinos pushing the Universe apart Anything else out there adding to the pressure? 2. Impact of
More informationDark Matter II. Marco Cirelli. (CNRS IPhT Saclay) December th TRR Winter School - Passo del Tonale. Reviews on Dark Matter: NewDark
10-14 December 2012 6 th TRR Winter School - Passo del Tonale Dark Matter II Marco Cirelli (CNRS IPhT Saclay) in collaboration with: A.Strumia (Pisa) N.Fornengo (Torino) M.Tamburini (Pisa) R.Franceschini
More informationBrief Introduction to Cosmology
Brief Introduction to Cosmology Matias Zaldarriaga Harvard University August 2006 Basic Questions in Cosmology: How does the Universe evolve? What is the universe made off? How is matter distributed? How
More information4. Nucleosynthesis. I. Aretxaga
4. Nucleosynthesis I. Aretxaga 2017 Radiation era We have that ρ M R -3 ρ rad R -4 There must be a z at which ρ M = ρ rad Taking into account that nucleosynthesis predicts n ν =0.68 n γ, then Ω rad =4.2
More informationDark matter and entropy dilution
Dark matter and entropy dilution Miha Nemevšek Goran Senjanović, Yue Zhang 1205.0844 Dark workshop TÜM/IAS, December 2015 Dark Matter stability Discrete symmetries MSSM & R-parity extended Higgs Inert
More informationChern-Simons portal Dark Matter
Chern-Simons portal Dark Matter III Saha Theory Workshop: Aspects of Early Universe Cosmology Mathias Pierre Laboratoire de Physique Théorique d Orsay In collaboration with G. Arcadi, G.Bhattacharyya,
More informationASTROPHYSICAL PROPERTIES OF MIRROR DARK MATTER
16 December 2011 ASTROPHYSICAL PROPERTIES OF MIRROR DARK MATTER Paolo Ciarcelluti Motivation of this research We are now in the ERA OF PRECISION COSMOLOGY and... Motivation of this research We are now
More informationBig Bang Nucleosynthesis and Particle Physics
New Generation Quantum Theory -Particle Physics, Cosmology and Chemistry- Kyoto University Mar.7-9 2016 Big Bang Nucleosynthesis and Particle Physics Masahiro Kawasaki (ICRR & Kavli IPMU, University of
More informationNeutrino mass and neutrino dark matter. Do non-relativistic neutrinos constitute the dark matter? Europhysics Letters 86 (2009) 59001
Neutrino mass and neutrino dark matter Do non-relativistic neutrinos constitute the dark matter? Europhysics Letters 86 (2009) 59001 Dr. Theo M. Nieuwenhuizen Institute for Theoretical Physics University
More informationNon-detection of the 3.55 kev line from M31/ Galactic center/limiting Window with Chandra
Non-detection of the 3.55 kev line from M31/ Galactic center/limiting Window with Chandra Meng Su (MIT)! Pappalardo/Einstein fellow!! In Collaboration with Zhiyuan Li (NJU)!! 15 Years of Science with Chandra!
More informationDecaying Dark Matter, Bulk Viscosity, and Dark Energy
Decaying Dark Matter, Bulk Viscosity, and Dark Energy Dallas, SMU; April 5, 2010 Outline Outline Standard Views Dark Matter Standard Views of Dark Energy Alternative Views of Dark Energy/Dark Matter Dark
More informationCMB & Light Degrees of Freedom
CMB & Light Degrees of Freedom Joel Meyers Canadian Institute for Theoretical Astrophysics SLAC Summer Institute 2017 Cosmic Opportunities August 21, 2017 Image Credits: Planck, ANL Light Relics What and
More informationDown-to-earth searches for cosmological dark matter
Down-to-earth searches for cosmological dark matter Carter Hall, University of Maryland October 19, 2016 Astrophysical evidence for dark matter Galaxy cluster collisions Rotation curves Ω 380,000 years
More informationDirect Detection of the Dark Mediated DM
Direct Detection of the Dark Mediated DM Yuhsin Tsai In collaboration with David Curtin, Ze ev Surujon, and Yue Zhao 1312.2618 and 1402.XXXX UC Davis Jan 16 2014 Main questions χ χ How does the direct
More informationSterile Neutrinos as Dark Matter. Manfred Lindner
Sterile Neutrinos as Dark Matter Manfred Lindner 13-20 December 2012 SM works perfectly & Higgs seems to be there - mass range was shrinking and is now rather precisely known - no signs for anything else
More informationAxion in Large Extra Dimensions
Axion in Large Extra Dimensions Talk at ASK2011 Sanghyeon Chang Konkuk Univ. April 11, 2011 Sanghyeon Chang (Konkuk Univ.) Axion in Large Extra Dimensions April 11, 2011 1 / 27 Table of Contents 1 Introduction
More informationGravitino LSP as Dark Matter in the Constrained MSSM
Gravitino LSP as Dark Matter in the Constrained MSSM Ki Young Choi The Dark Side of the Universe, Madrid, 20-24 June 2006 Astro-Particle Theory and Cosmology Group The University of Sheffield, UK In collaboration
More informationLearning from WIMPs. Manuel Drees. Bonn University. Learning from WIMPs p. 1/29
Learning from WIMPs Manuel Drees Bonn University Learning from WIMPs p. 1/29 Contents 1 Introduction Learning from WIMPs p. 2/29 Contents 1 Introduction 2 Learning about the early Universe Learning from
More informationThe Dark Matter Problem
The Dark Matter Problem matter : anything with equation of state w=0 more obvious contribution to matter: baryons (stars, planets, us!) and both Big Bang Nucleosynthesis and WMAP tell us that Ω baryons
More informationLATE DECAYING TWO-COMPONENT DARK MATTER (LD2DM) CAN EXPLAIN THE AMS-02 POSITRON EXCESS
LATE DECAYING TWO-COMPONENT DARK MATTER (LD2DM) CAN EXPLAIN THE AMS-02 POSITRON EXCESS (WITH A FEW BONUS FEATURES!) (BASED ON 1609.04821 W/ P. RALEGANKAR AND V. RENTALA) JATAN BUCH (BROWN U.) 1 THE DARK
More informationGauged U(1) clockwork
Gauged U(1) clockwork Hyun Min Lee Chung-Ang University, Korea Based on arxiv: 1708.03564 Workshop on the Standard Model and Beyond Corfu, Greece, Sept 2-10, 2017. Outline Introduction & motivation Gauged
More informationOn Symmetric/Asymmetric Light Dark Matter
On Symmetric/Asymmetric Light Dark Matter Hai-Bo Yu University of Michigan, Ann Arbor Exploring Low-Mass Dark Matter Candidates PITT PACC, 11/16/2011 Motivations Traditionally, we focus on O(100 GeV) dark
More informationDark matter: evidence and candidates
.... Dark matter: evidence and candidates Zhao-Huan Yu ( 余钊焕 ) Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, CAS March 14, 2014 Zhao-Huan Yu (IHEP) Dark matter: evidence and
More informationThe Story of Wino Dark matter
The Story of Wino Dark matter Varun Vaidya Dept. of Physics, CMU DIS 2015 Based on the work with M. Baumgart and I. Rothstein, 1409.4415 (PRL) & 1412.8698 (JHEP) Evidence for dark matter Rotation curves
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 12 Nov. 18, 2015 Today Big Bang Nucleosynthesis and Neutrinos Particle Physics & the Early Universe Standard Model of Particle
More informationMICROPHYSICS AND THE DARK UNIVERSE
MICROPHYSICS AND THE DARK UNIVERSE Jonathan Feng University of California, Irvine CAP Congress 20 June 2007 20 June 07 Feng 1 WHAT IS THE UNIVERSE MADE OF? Recently there have been remarkable advances
More informationPrimordial (Big Bang) Nucleosynthesis
Primordial (Big Bang) Nucleosynthesis H Li Be Which elements? He METALS - 1942: Gamow suggests a Big Bang origin of the elements. - 1948: Alpher, Bethe & Gamow: all elements are synthesized minutes after
More informationChiral Dark Sector. Keisuke Harigaya (UC Berkeley, LBNL) KH, Yasunori Nomura Raymond Co, KH, Yasunori Nomura 1610.
04/21/2017 Lattice for BSM Chiral Dark Sector Keisuke Harigaya (UC Berkeley, LBNL) KH, Yasunori Nomura 1603.03430 Raymond Co, KH, Yasunori Nomura 1610.03848 Plan of Talk Introduction Set up of our model
More informationINTRODUCTION TO DARK MATTER
Universität Heidelberg Carl Zeiss Stiftung INTRODUCTION TO DARK MATTER Susanne Westhoff 2nd Colima Winter School on High Energy hysics! January 8-19, 2018 Colima, Mexico GALAXY VELOCITIES IN CLUSTERS Redshift
More informationInvisible Sterile Neutrinos
Invisible Sterile Neutrinos March 25, 2010 Outline Overview of Sterile Neutrino Dark Matter The Inert Doublet Model with 3 Singlet Fermions Non-thermal Dark Matter Conclusion Work done in collaboration
More informationWeek 3: Thermal History of the Universe
Week 3: Thermal History of the Universe Cosmology, Ay127, Spring 2008 April 21, 2008 1 Brief Overview Before moving on, let s review some of the high points in the history of the Universe: T 10 4 ev, t
More informationOverview of Dark Matter models. Kai Schmidt-Hoberg
Overview of Dark Matter models. Kai Schmidt-Hoberg Evidence for dark matter. Compelling evidence for dark matter on all astrophysical scales: Galactic scales: Rotation curves of Galaxies Kai Schmidt-Hoberg
More informationNeutrino bounds on dark matter. Alejandro Ibarra Technische Universität München
Neutrino bounds on dark matter Alejandro Ibarra Technische Universität München NOW 2012 10 September 2012 Introduction Many pieces of evidence for particle dark matter. However, very little is known about
More informationImplications of cosmological observables for particle physics: an overview
Implications of cosmological observables for particle physics: an overview Yvonne Y. Y. Wong The University of New South Wales Sydney, Australia TAUP 2015, Torino, September 7 11, 2015 The concordance
More informationProspects for the Direct Detection of the Cosmic Neutrino Background
Prospects for the Direct Detection of the Cosmic Neutrino Background Andreas Ringwald http://www.desy.de/ ringwald DESY PANIC 2008 November 9 14, 2008, Eilat, Israel Prospects for the Direct Detection
More informationWeek 3 - Part 2 Recombination and Dark Matter. Joel Primack
Astro/Phys 224 Spring 2012 Origin and Evolution of the Universe Week 3 - Part 2 Recombination and Dark Matter Joel Primack University of California, Santa Cruz http://pdg.lbl.gov/ In addition to the textbooks
More informationLecture 3: Big Bang Nucleosynthesis
Lecture 3: Big Bang Nucleosynthesis Last time: particle anti-particle soup --> quark soup --> neutron-proton soup. Today: Form 2 D and 4 He Form heavier nuclei? Discuss primordial abundances X p, Y p,
More information3.5 kev X-ray line and Supersymmetry
Miami-2014, Fort Lauderdale, Florida Bartol Research Institute Department Physics and Astronomy University of Delaware, USA in collaboration with Bhaskar Dutta, Rizwan Khalid and Qaisar Shafi, JHEP 1411,
More informationFeebly coupled hidden sectors. Kimmo Tuominen University of Helsinki
Feebly coupled hidden sectors Kimmo Tuominen University of Helsinki Outline Background Scalar portal models Outlook Collaborators: N. Bernal, K. Enqvist, M. Heikinheimo, K. Kainulainen, S. Nurmi, T. Tenkanen,
More informationThermalisation of Sterile Neutrinos. Thomas Tram LPPC/ITP EPFL
Thermalisation of Sterile Neutrinos Thomas Tram LPPC/ITP EPFL Outline Introduction to ev sterile neutrinos. Bounds from Cosmology. Standard sterile neutrino thermalisation. Thermalisation suppression by
More informationCMB constraints on dark matter annihilation
CMB constraints on dark matter annihilation Tracy Slatyer, Harvard University NEPPSR 12 August 2009 arxiv:0906.1197 with Nikhil Padmanabhan & Douglas Finkbeiner Dark matter!standard cosmological model:
More informationLecture 12. Dark Matter. Part II What it could be and what it could do
Dark Matter Part II What it could be and what it could do Theories of Dark Matter What makes a good dark matter candidate? Charge/color neutral (doesn't have to be though) Heavy We know KE ~ kev CDM ~
More informationThermalization of axion dark matter
Thermalization of axion dark matter Ken ichi Saikawa ICRR, The University of Tokyo Collaborate with M. Yamaguchi (Tokyo Institute of Technology) Reference: KS and M. Yamaguchi, arxiv:1210.7080 [hep-ph]
More informationNew experiment for axion dark matter
New experiment for axion dark matter J. Redondo and J. Jaeckel Feb 27th 2014 Outline - x-summary of Axion and ALP DM - Axion DM waves in Magnetic fields - Dish experiment - Understanding cavity experiments
More informationBaryogenesis in Higher Dimension Operators. Koji Ishiwata
Baryogenesis in Higher Dimension Operators Koji Ishiwata Caltech In collaboration with Clifford Cheung (Caltech) Based on arxiv:1304.0468 BLV2013 Heidelberg, April 9, 2013 1. Introduction The origin of
More informationThe Influence of DE on the Expansion Rate of the Universe and its Effects on DM Relic Abundance
The Influence of DE on the Expansion Rate of the Universe and its Effects on DM Relic Abundance Esteban Jimenez Texas A&M University XI International Conference on Interconnections Between Particle Physics
More informationProbing the nature of Dark matter with radio astronomy. Céline Boehm
Probing the nature of Dark matter with radio astronomy Céline Boehm IPPP, Durham LAPTH, Annecy SKA, Flic en Flac, May 2017 The DM Physics scale strong or weak / stable or decaying strong and stable Electromagnetic
More informationTriple unification of inflation, dark matter and dark energy
Triple unification of inflation, dark matter and dark energy May 9, 2008 Leonard Susskind, The Anthropic Landscape of String Theory (2003) A. Liddle, A. Ureña-López, Inflation, dark matter and dark energy
More informationLecture 3: Big Bang Nucleosynthesis The First Three Minutes
Lecture 3: Big Bang Nucleosynthesis The First Three Minutes Last time: particle anti-particle soup --> quark soup --> neutron-proton soup p / n ratio at onset of 2 D formation Today: Form 2 D and 4 He
More informationTheory Group. Masahiro Kawasaki
Theory Group Masahiro Kawasaki Current members of theory group Staffs Masahiro Kawasaki (2004~) cosmology Masahiro Ibe (2011~) particle physics Postdoctoral Fellows Shuichiro Yokoyama Shohei Sugiyama Daisuke
More informationDark Matter Models. Stephen West. and. Fellow\Lecturer. RHUL and RAL
Dark Matter Models Stephen West and Fellow\Lecturer RHUL and RAL Introduction Research Interests Important Experiments Dark Matter - explaining PAMELA and ATIC Some models to explain data Freeze out Sommerfeld
More informationMarco Drewes, Université catholique de Louvain. The Other Neutrinos IAP Meeting. Université libre de Bruxelles
Marco Drewes, Université catholique de Louvain The Other Neutrinos 21.12.2017 IAP Meeting Université libre de Bruxelles The Standard Model of Particle 125 GeV The periodic table of elementary particles
More informationConcordance Cosmology and Particle Physics. Richard Easther (Yale University)
Concordance Cosmology and Particle Physics Richard Easther (Yale University) Concordance Cosmology The standard model for cosmology Simplest model that fits the data Smallest number of free parameters
More informationNuclear Astrophysics - I
Nuclear Astrophysics - I Carl Brune Ohio University, Athens Ohio Exotic Beam Summer School 2016 July 20, 2016 Astrophysics and Cosmology Observations Underlying Physics Electromagnetic Spectrum: radio,
More informationTHERMAL HISTORY OF THE UNIVERSE
M. Pettini: Introduction to Cosmology Lecture 7 THERMAL HISTORY OF THE UNIVERSE The Universe today is bathed in an all-pervasive radiation field, the Cosmic Microwave Background (CMB) which we introduced
More informationSaturday Morning Physics (2007) Prof. Bhaskar Dutta and Prof. Teruki Kamon. Department of Physics Texas A&M University. Question
Dark Puzzles of the Universe Saturday Morning Physics (2007) Prof. Bhaskar Dutta and Prof. Teruki Kamon Department of Physics Texas A&M University Question March 24, 2007 Dark Puzzles of the Universe 2
More informationDark Puzzles of the Universe
Dark Puzzles of the Universe Saturday Morning Physics (2007) Prof. Bhaskar Dutta and Prof. Teruki Kamon Department of Physics Texas A&M University Question March 24, 2007 Dark Puzzles of the Universe 2
More informationcomponents Particle Astrophysics, chapter 7
Dark matter and dark energy components Particle Astrophysics, chapter 7 Overview lecture 3 Observation of dark matter as gravitational ti effects Rotation curves galaxies, mass/light ratios in galaxies
More informationCosmology II: The thermal history of the Universe
.. Cosmology II: The thermal history of the Universe Ruth Durrer Département de Physique Théorique et CAP Université de Genève Suisse August 6, 2014 Ruth Durrer (Université de Genève) Cosmology II August
More informationDirect Search for Dark Matter
Direct Search for Dark Matter Herbstschule für Hochenergiephysik Maria Laach 2013, September 2013 Institut für Kernphysik, Westfälische Wilhelms-Universität Münster weinheimer@uni-muenster.de - Astrophysical
More informationNucleosíntesis primordial
Tema 5 Nucleosíntesis primordial Asignatura de Física Nuclear Curso académico 2009/2010 Universidad de Santiago de Compostela Big Bang cosmology 1.1 The Universe today The present state of the Universe
More informationLeptogenesis via the Relaxation of Higgs and other Scalar Fields
Leptogenesis via the Relaxation of Higgs and other Scalar Fields Louis Yang Department of Physics and Astronomy University of California, Los Angeles PACIFIC 2016 September 13th, 2016 Collaborators: Alex
More informationCosmological constraints on (elastic) Dark Matter self-interactions
Cosmological constraints on (elastic Dark Matter self-interactions Rainer Stiele Work done together with J. Schaffner-Bielich & T. Boeckel (University Heidelberg Institut für Theoretische Physik Goethe-Universität
More informationM. Lattanzi. 12 th Marcel Grossmann Meeting Paris, 17 July 2009
M. Lattanzi ICRA and Dip. di Fisica - Università di Roma La Sapienza In collaboration with L. Pieri (IAP, Paris) and J. Silk (Oxford) Based on ML, Silk, PRD 79, 083523 (2009) and Pieri, ML, Silk, MNRAS
More informationEntropy, Baryon Asymmetry and Dark Matter from Heavy Neutrino Decays.
Entropy, Baryon Asymmetry and Dark Matter from Heavy Neutrino Decays. Kai Schmitz Deutsches Elektronen-Synchrotron DESY, Hamburg, Germany Based on arxiv:1008.2355 [hep-ph] and arxiv:1104.2750 [hep-ph].
More informationDark Matter and Dark Energy components chapter 7
Dark Matter and Dark Energy components chapter 7 Lecture 4 See also Dark Matter awareness week December 2010 http://www.sissa.it/ap/dmg/index.html The early universe chapters 5 to 8 Particle Astrophysics,
More informationFeebly Interacting Massive Particles and their signatures
Feebly Interacting Massive Particles and their signatures Geneviève Bélanger LAPTH Annecy-le-Vieux See : GB, Boudjema, Goudelis, Pukhov, Zaldivar, 1801.03509 GB, Desai, Goudelis, Harz, Lessa, No, Pukhov,
More informationDark Sectors at the Fermilab SeaQuest Experiment
Dark Sectors at the Fermilab SeaQuest Experiment Stefania Gori University of Cincinnati New Probes for Physics Beyond the Standard Model KITP April 9, 2018 Dark sectors Dark matter (DM) exists! The stronger
More informationSignatures of clumpy dark matter in the global 21 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:
Signatures of clumpy dark matter in the global 2 cm background signal D.T. Cumberland, M. Lattanzi, and J.Silk arxiv:0808.088 Daniel Grin Ay. Journal Club /23/2009 /8 Signatures of clumpy dark matter in
More informationNovember 24, Scalar Dark Matter from Grand Unified Theories. T. Daniel Brennan. Standard Model. Dark Matter. GUTs. Babu- Mohapatra Model
Scalar from November 24, 2014 1 2 3 4 5 What is the? Gauge theory that explains strong weak, and electromagnetic forces SU(3) C SU(2) W U(1) Y Each generation (3) has 2 quark flavors (each comes in one
More informationAstroparticle Physics at Colliders
Astroparticle Physics at Colliders Manuel Drees Bonn University Astroparticle Physics p. 1/29 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/29 Contents 1) Introduction:
More informationCosmology Neutrinos Connect to QGP Dark Radiation and the QGP Era Darkness Production: Universe Laboratory
Cosmology Neutrinos Connect to QGP Dark Radiation and the QGP Era Darkness Production: Universe Laboratory What has CMB to do with QGP? Figure: Photons freeze-out around 0.25 ev and today they make up
More informationStandard Model Thermodynamics: Effect on Gravitational Wave and Dark Matter
Standard Model Thermodynamics: Effect on Gravitational Wave and Dark Matter Satoshi Shirai (Kavli IPMU) based on Ken'ichi Saikawa and SS, 1803.01038 Remnant of Early Universe The present Universe is made
More informationTowards micromegas 5: Freeze-in
Towards micromegas 5: Freeze-in Work in progress in collaboration with G. Bélanger, F. Boudjema, A. Pukhov, B. Zaldivar Coming up, soon! Andreas Goudelis LPTHE - Jussieu IRN - Terascale 2017, Montpellier
More informationTesting a DM explanation of the positron excess with the Inverse Compton scattering
Testing a DM explanation of the positron excess with the Inverse Compton scattering Gabrijela Zaharijaš Oskar Klein Center, Stockholm University Work with A. Sellerholm, L. Bergstrom, J. Edsjo on behalf
More informationDark Radiation and Inflationary Freedom
Dark Radiation and Inflationary Freedom Based on [SG et al., JCAP 1504 (2015) 023] [Di Valentino et al., PRD 91 (2015) 123505] Stefano Gariazzo University of Torino, INFN of Torino http://personalpages.to.infn.it/~gariazzo/
More information