WISP Dark Matter Theory
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CERN Courier–Digital Edition
CERNMarch/April 2021 cerncourier.com COURIERReporting on international high-energy physics WELCOME CERN Courier – digital edition Welcome to the digital edition of the March/April 2021 issue of CERN Courier. Hadron colliders have contributed to a golden era of discovery in high-energy physics, hosting experiments that have enabled physicists to unearth the cornerstones of the Standard Model. This success story began 50 years ago with CERN’s Intersecting Storage Rings (featured on the cover of this issue) and culminated in the Large Hadron Collider (p38) – which has spawned thousands of papers in its first 10 years of operations alone (p47). It also bodes well for a potential future circular collider at CERN operating at a centre-of-mass energy of at least 100 TeV, a feasibility study for which is now in full swing. Even hadron colliders have their limits, however. To explore possible new physics at the highest energy scales, physicists are mounting a series of experiments to search for very weakly interacting “slim” particles that arise from extensions in the Standard Model (p25). Also celebrating a golden anniversary this year is the Institute for Nuclear Research in Moscow (p33), while, elsewhere in this issue: quantum sensors HADRON COLLIDERS target gravitational waves (p10); X-rays go behind the scenes of supernova 50 years of discovery 1987A (p12); a high-performance computing collaboration forms to handle the big-physics data onslaught (p22); Steven Weinberg talks about his latest work (p51); and much more. To sign up to the new-issue alert, please visit: http://comms.iop.org/k/iop/cerncourier To subscribe to the magazine, please visit: https://cerncourier.com/p/about-cern-courier EDITOR: MATTHEW CHALMERS, CERN DIGITAL EDITION CREATED BY IOP PUBLISHING ATLAS spots rare Higgs decay Weinberg on effective field theory Hunting for WISPs CCMarApr21_Cover_v1.indd 1 12/02/2021 09:24 CERNCOURIER www. -
Axions and Other Similar Particles
1 91. Axions and Other Similar Particles 91. Axions and Other Similar Particles Revised October 2019 by A. Ringwald (DESY, Hamburg), L.J. Rosenberg (U. Washington) and G. Rybka (U. Washington). 91.1 Introduction In this section, we list coupling-strength and mass limits for light neutral scalar or pseudoscalar bosons that couple weakly to normal matter and radiation. Such bosons may arise from the spon- taneous breaking of a global U(1) symmetry, resulting in a massless Nambu-Goldstone (NG) boson. If there is a small explicit symmetry breaking, either already in the Lagrangian or due to quantum effects such as anomalies, the boson acquires a mass and is called a pseudo-NG boson. Typical examples are axions (A0)[1–4] and majorons [5], associated, respectively, with a spontaneously broken Peccei-Quinn and lepton-number symmetry. A common feature of these light bosons φ is that their coupling to Standard-Model particles is suppressed by the energy scale that characterizes the symmetry breaking, i.e., the decay constant f. The interaction Lagrangian is −1 µ L = f J ∂µ φ , (91.1) where J µ is the Noether current of the spontaneously broken global symmetry. If f is very large, these new particles interact very weakly. Detecting them would provide a window to physics far beyond what can be probed at accelerators. Axions are of particular interest because the Peccei-Quinn (PQ) mechanism remains perhaps the most credible scheme to preserve CP-symmetry in QCD. Moreover, the cold dark matter (CDM) of the universe may well consist of axions and they are searched for in dedicated experiments with a realistic chance of discovery. -
Axions –Theory SLAC Summer Institute 2007
Axions –Theory SLAC Summer Institute 2007 Helen Quinn Stanford Linear Accelerator Center Axions –Theory – p. 1/?? Lectures from an Axion Workshop Strong CP Problem and Axions Roberto Peccei hep-ph/0607268 Astrophysical Axion Bounds Georg Raffelt hep-ph/0611350 Axion Cosmology Pierre Sikivie astro-ph/0610440 Axions –Theory – p. 2/?? Symmetries Symmetry ⇔ Invariance of Lagrangian Familiar cases: Lorentz symmetries ⇔ Invariance under changes of coordinates Other symmetries: Invariances under field redefinitions e.g (local) gauge invariance in electromagnetism: Aµ(x) → Aµ(x)+ δµΩ(x) Fµν = δµAν − δνAµ → Fµν Axions –Theory – p. 3/?? How to build an (effective) Lagrangian Choose symmetries to impose on L: gauge, global and discrete. Choose representation content of matter fields Write down every (renormalizable) term allowed by the symmetries with arbitrary couplings (d ≤ 4) Add Hermitian conjugate (unitarity) - Fix renormalized coupling constants from match to data (subtractions, usually defined perturbatively) "Naturalness" - an artificial criterion to avoid arbitrarily "fine tuned" couplings Axions –Theory – p. 4/?? Symmetries of Standard Model Gauge Symmetries Strong interactions: SU(3)color unbroken but confined; quarks in triplets Electroweak SU(2)weak X U(1)Y more later:representations, "spontaneous breaking" Discrete Symmetries CPT –any field theory (local, Hermitian L); C and P but not CP broken by weak couplings CP (and thus T) breaking - to be explored below - arises from quark-Higgs couplings Global symmetries U(1)B−L accidental; more? Axions –Theory – p. 5/?? Chiral symmetry Massless four component Dirac fermion is two independent chiral fermions (1+γ5) (1−γ5) ψ = 2 ψ + 2 ψ = ψR + ψL γ5 ≡ γ0γ1γ2γ3 γ5γµ = −γµγ5 Chiral Rotations: rotate L and R independently ψ → ei(α+βγ5)ψ i(α+β) i(α−β) ψR → e ψR; ψL → e ψL Kinetic and gauge coupling terms in L are chirally invariant † ψγ¯ µψ = ψ¯RγµψR + ψ¯LγµψL since ψ¯ = ψ γ0 Axions –Theory – p. -
The WISP Paradigm
The WISP Paradigm Javier Redondo Max Planck Institut (Werner Heisenberg Institut) Munich MPI 14/12/2009 Hidden Sectors in PBSM Extensions of SM often include Hidden Sectors Fields coupled to SM only through gravity or high energy “messenger” fields... This is the case in string theory (compactifications produce many particles, new gauge symmetries, and KKs) Desirable for SUSY Also in GUT theories... Massive Messengers Standard Model Hidden Sector e−, ν, q, γ, W ±, Z, g...H a, γ, ψMCP... Hidden Sectors can be quite complicated we certainly don’t know! Hidden Sector BIG guys Light guys (live in the mountains) (mass is protected by a symmetry) Goldstone Chiral Bosons fermions Gauge and more... Bosons hard to detect; not only as hidden they have suppressed interactions but as hidden, also heavy! light they have no thresholds and they can have maybe at LHC or ILC... coherent forces Let symmetry be our guide ! Hidden Sectors can be quite complicated we certainly don’t know! Hidden Sector BIG guys Light guys (live in the mountains) (mass is protected by a symmetry) Goldstone Chiral Bosons WISPsfermions (very) weakly interacting sub-eV Particles Gauge and more... Bosons hard to detect; not only as hidden they have suppressed interactions but as hidden, also heavy! light they have no thresholds and they can have maybe at LHC or ILC... coherent forces Let symmetry be our guide ! Axion-like-Particles and Axions 1 µν Axions are GB of a color anomalous U(1) Tr Gµν G a 4fa { } The color anomalous term creates a potential with CP conserving minimum Solution to Strong CP which gives the axion a mass m f 10 10GeV 1 m π π 0.6 meV − − . -
Cosmology Falling in Love with Sterile Neutrinos
Cosmology Falling in Love with Sterile Neutrinos Jörn Kersten Based on Torsten Bringmann, Jasper Hasenkamp, JK, JCAP 07 (2014) [arXiv:1312.4947] Outline 1 Introduction 2 Self-Interacting Dark Matter 3 Dark Matter Interacting with Neutrinos 3 / 23 1 Introduction 2 Self-Interacting Dark Matter 3 Dark Matter Interacting with Neutrinos 4 / 23 Or does it? Tensions in ΛCDM cosmology The Universe after Planck Flat ΛCDM cosmology fits data perfectly Planck, arXiv:1303.5062 5 / 23 The Universe after Planck Flat ΛCDM cosmology fits data perfectly Planck, arXiv:1303.5062 Or does it? Tensions in ΛCDM cosmology 5 / 23 Measurements of Cosmic Microwave Background (CMB): ∆Neff = 1:51 ± 0:75 at 68% CL ACT, ApJ 739 (2011) ∆Neff = 0:81 ± 0:42 at 68% CL SPT, ApJ 743 (2011) +0:68 ∆Neff = 0:31−0:64 at 95% CL Planck, arXiv:1303.5076 Hints for Dark Radiation Dark radiation: relativistic particles 6= γ; νSM Parameterized via radiation energy density " # 7 T 4 ρ ≡ 1 + N ν ρ rad eff 8 T γ T ≡ Tγ Neff: effective number of neutrino species Standard Model: Neff = 3:046 Existence of dark radiation , ∆Neff ≡ Neff − 3:046 > 0 6 / 23 Hints for Dark Radiation Dark radiation: relativistic particles 6= γ; νSM Parameterized via radiation energy density " # 7 T 4 ρ ≡ 1 + N ν ρ rad eff 8 T γ T ≡ Tγ Neff: effective number of neutrino species Standard Model: Neff = 3:046 Existence of dark radiation , ∆Neff ≡ Neff − 3:046 > 0 Measurements of Cosmic Microwave Background (CMB): ∆Neff = 1:51 ± 0:75 at 68% CL ACT, ApJ 739 (2011) ∆Neff = 0:81 ± 0:42 at 68% CL SPT, ApJ 743 (2011) +0:68 -
Axions & Wisps
FACULTY OF SCIENCE AXIONS & WISPS STEPHEN PARKER 2nd Joint CoEPP-CAASTRO Workshop September 28 – 30, 2014 Great Western, Victoria 2 Talk Outline • Frequency & Quantum Metrology Group at UWA • Basic background / theory for axions and hidden sector photons • Photon-based experimental searches + bounds • Focus on resonant cavity “Haloscope” experiments for CDM axions • Work at UWA: Past, Present, Future A Few Useful Review Articles: J.E. Kim & G. Carosi, Axions and the strong CP problem, Rev. Mod. Phys., 82(1), 557 – 601, 2010. M. Kuster et al. (Eds.), Axions: Theory, Cosmology, and Experimental Searches, Lect. Notes Phys. 741 (Springer), 2008. P. Arias et al., WISPy Cold Dark Matter, arXiv:1201.5902, 2012. [email protected] The University of Western Australia 3 Frequency & Quantum Metrology Research Group ~ 3 staff, 6 postdocs, 8 students Hosts node of ARC CoE EQuS Many areas of research from fundamental to applied: Cryogenic Sapphire Oscillator Tests of Lorentz Symmetry & fundamental constants Ytterbium Lattice Clock for ACES mission Material characterization Frequency sources, synthesis, measurement Low noise microwaves + millimetrewaves …and lab based searches for WISPs! Core WISP team: Stephen Parker, Ben McAllister, Eugene Ivanov, Mike Tobar [email protected] The University of Western Australia 4 Axions, ALPs and WISPs Weakly Interacting Slim Particles Axion Like Particles Slim = sub-eV Origins in particle physics (see: strong CP problem, extensions to Standard Model) but become pretty handy elsewhere WISPs Can be formulated as: Dark Matter (i.e. Axions, hidden photons) ALPs Dark Energy (i.e. Chameleons) Low energy scale dictates experimental approach Axions WISP searches are complementary to WIMP searches [email protected] The University of Western Australia 5 The Axion – Origins in Particle Physics CP violating term in QCD Lagrangian implies neutron electric dipole moment: But measurements place constraint: Why is the neutron electric dipole moment (and thus θ) so small? This is the Strong CP Problem. -
Cosmological Anomalies Shed Light on the Dark Sector
COSMOLOGICAL ANOMALIES SHED LIGHT ON THE DARK SECTOR by Tanvi Karwal A dissertation submitted to The Johns Hopkins University in conformity with the requirements for the degree of Doctor of Philosophy. Baltimore, Maryland June, 2019 c 2019 Tanvi Karwal ⃝ All rights reserved Abstract Little is known about dark energy and dark matter; but their simple descriptions in the ΛCDM model of cosmology fit numerous datasets well. Recently however, tensions have emerged between the results of different datasets, as have certain unex- pected results. These anomalies may indicate new physics beyond ΛCDM; a revision of how we describe the dark sector. My work uses cosmological anomalies to explore the dark sector. My research resolves perhaps the most exciting tension in cosmology, the Hubble tension, with early dark energy (EDE). I developed two physical models for EDE and find that these models not only solve the Hubble tension, but also fit mostcosmolog- ical datasets well. No other solution to the Hubble tension proposed thus far can do both - fully solve the tension while still fitting early and late-time measurements of the Universe. The model that succeeds ΛCDM should solve not only the Hubble tension but ii ABSTRACT also other cosmological tensions such as the S8 anomaly. My research investigates a decaying dark matter model to address both tensions simultaneously but finds the constraints from late-universe observations too stringent to permit a full resolution. I am also building a phenomenological tool to model the dark sector in a widely- used cosmological code. This tool, generalised dark matter, is a powerful formalism capable of emulating the effects of a wide variety of dark matter and dark energy models, simplifying placing constraints on different fundamentally-motivated models. -
Rare Event Physics WG1
Rare event physics WG1 Our ambitious mission : ● Show the state of the art of the physics of rare events ● Cover for both experimental and theoretical aspects ● Provide hints for the exploration of next generation experiments (link with WG5) ● Provide a guideline for experimental and technological efforts, like constraints for low cosmo- and radio-purity techniques(WG2), for detection methods (WG3) and analysis tools (WG4) ● Being inclusive to any other scientific field that would profit of deep underground sites Christine Marquet, CENBG Mariangela Settimo, Subatech May 31, 2021 - visioconference Luca Scotto Lavina, LPNHE Two major axes 1. Dark Matter WG1 We will keep a particular eye on direct search of dark matter : ● Scoping the whole zoology of models (WIMP, WISP, axions, …), nucleo- or lepto-philic ● Exploring a wide (and experimentally accessible) range of masses/energies ( >GeV, sub-GeV, down to μeV) ● Looking for any trace of daily and seasonal modulation ● Using a plethora of targets and combinations of energy losses ● Complementarity with colliders (new particles) and indirect evidences (annihilation) Christine Marquet, CENBG Mariangela Settimo, Subatech May 31, 2021 - visioconference Luca Scotto Lavina, LPNHE Two major axes 2. Neutrinoless double beta decay WG1 We will keep an eye on the search for the intimate nature of neutrinos : ● Nature of neutrino (Majorana/Dirac) ● Fixing the neutrino mass scale and possible mass scenarii ● Proof of a lepton number violation ● Neutrino hierarchy ● Impact on baryon asymmetry of the Universe -
Dark Radiation and Dark Matter from Primordial Black Holes
DARK RADIATION AND DARK MATTER FROM PRIMORDIAL BLACK HOLES Dan Hooper – Fermilab and the University of Chicago Next Frontiers in the Search for Dark Matter, GGI September 26, 2019 Dan Hooper – Dark Radiation & Dark Matter from PBHs This talk is based on Dark Radiation and Superheavy Dark Matter from Black Hole Domination With Gordan Krnjaic and Sam McDermott, JHEP 1908 (2019) 001, arXiv:1905.01301 For related work, see Morrison and Profumo, arXiv:1812.10606 and Lennon et al, arXiv:1712.07664 Dan Hooper – Dark Radiation & Dark Matter from PBHs Was the Early Universe Dominated by Black Holes? § Inhomogeneities in the early universe can led to the formation of primordial black holes § Very roughly, we expect the mass of these black holes to be similar to the energy enclosed within the horizon at or near the end of inflation: § In this mass range, black holes evaporate very rapidly, disappearing well before BBN § If even a small fraction of the energy density after inflation was in the form of black holes, this fraction would grow as the universe expands -3 (black holes evolve as matter, �BH � a , rather -4 than radiation, �rad � a ); § From this perspective, it is well-motivated to consider scenarios in which the early universe included an era in which the energy density was dominated by black holes Dan Hooper – Dark Radiation & Dark Matter from PBHs Was the Early Universe Dominated by Black Holes? § Quantitatively, the density of black holes will ultimately exceed the energy density in SM radiation (before the black holes evaporate) if the -
Dark Radiation from the Axino Solution of the Gravitino Problem
21st of July 2011 Dark radiation from the axino solution of the gravitino problem Jasper Hasenkamp II. Institute for Theoretical Physics, University of Hamburg, Hamburg, Germany [email protected] Abstract Current observations of the cosmic microwave background could confirm an in- crease in the radiation energy density after primordial nucleosynthesis but before photon decoupling. We show that, if the gravitino problem is solved by a light axino, dark (decoupled) radiation emerges naturally in this period leading to a new upper 11 bound on the reheating temperature TR . 10 GeV. In turn, successful thermal leptogenesis might predict such an increase. The Large Hadron Collider could en- dorse this opportunity. At the same time, axion and axino can naturally form the observed dark matter. arXiv:1107.4319v2 [hep-ph] 13 Dec 2011 1 Introduction It is a new opportunity to determine the amount of radiation in the Universe from obser- vations of the cosmic microwave background (CMB) alone with precision comparable to that from big bang nucleosynthesis (BBN). Recent measurements by the Wilkinson Mi- crowave Anisotropy Probe (WMAP) [1], the Atacama Cosmology Telescope (ACT) [2] and the South Pole Telescope (SPT) [3] indicate|statistically not significant|the radi- ation energy density at the time of photon decoupling to be higher than inferred from primordial nucleosynthesis in standard cosmology making use of the Standard Model of particle physics, cf. [4,5]. This could be taken as another hint for physics beyond the two standard models. The Planck satellite, which is already taking data, could turn the hint into a discovery. We should search for explanations from particle physics for such an increase in ra- diation [6,7], especially, because other explanations are missing, if the current mean values are accurate. -
Evidence for a New 17 Mev Boson
PROTOPHOBIC 8Be TRANSITION EVIDENCE FOR A NEW 17 MEV BOSON Flip Tanedo arXiv:1604.07411 & work in progress SLAC Dark Sectors 2016 (28 — 30 April) with Jonathan Feng, Bart Fornal, Susan Gardner, Iftah Galon, Jordan Smolinsky, & Tim Tait BART SUSAN IFTAH 1 flip . tanedo @ uci . edu EVIDENCE FOR A 17 MEV NEW BOSON 14 week ending A 6.8σ nuclear transitionPRL 116, 042501 (2016) anomalyPHYSICAL REVIEW LETTERS 29 JANUARY 2016 shape of the resonance [40], but it is definitelyweek different ending pairs (rescaled for better separation) compared with the PRL 116, 042501 (2016) PHYSICAL REVIEW LETTERS 29 JANUARY 2016 from the shape of the forward or backward asymmetry [40]. simulations (full curve) including only M1 and E1 con- Therefore, the above experimental data make the interpre- tributions. The experimental data do not deviate from the Observation of Anomalous Internal Pairtation Creation of the in observed8Be: A Possible anomaly Indication less probable of a as Light, being the normal IPC. This fact supports also the assumption of the Neutralconsequence Boson of some kind of interference effects. boson decay. The deviation cannot be explained by any γ-ray related The χ2 analysis mentioned above to judge the signifi- A. J. Krasznahorkay,* M. Csatlós, L. Csige, Z. Gácsi,background J. Gulyás, M. either, Hunyadi, since I. Kuti, we B. cannot M. Nyakó, see any L. Stuhl, effect J. Timár, at off cance of the observed anomaly was extended to extract the T. G. Tornyi,resonance, and Zs. where Vajta the γ-ray background is almost the same. mass of the hypothetical boson. The simulated angular Institute for Nuclear Research, Hungarian Academy ofTo Sciences the best (MTA of Atomki), our knowledge, P.O. -
The Early Universe As a Laboratory for Particle Physics
The Early Universe as a Laboratory for Particle Physics Nikita Blinov April 6, 2021 York University Triumph of the Standard Model Standard Model describes properties and interactions of leptons, quarks and force carriers 100+ years of science !"#N $ift Shop 2 Triumph of the Standard Model Standard Model describes properties and interactions of leptons, quarks and force carriers 100+ years of science !"#N $ift Shop Enormous dynamic range when combined with gravity ,ar)e Hadron Collider probes ~10-20 m Cosmic Micro(ave Background: ~10+24 m 3 The Cosmological Fine Print 4n largest scales, the universe is (ell-described by a %andf l of para'eters Planck ‘18 Only 'eas red indirectly 2%y not 03 .nconsistent (it% q ant m estimates No candidate in Standard Model 4 The Expanding Universe 6ar-a(ay ob7ects (like )alaxies) are receding fro' s - bble (1929) "arlier estimates by Lemaitre (1927) and #obertson (1928) 5 The Expanding Universe 6ar-a(ay ob7ects (like )alaxies) are receding fro' s - bble (1929) 6 #iess et al 2019 Expansion in General Relativity $eneral #elativity relates expansion rate to t%e contents of the niverse Hotter and denser in the past! 7 Early Universe Primer =%e niverse e9panded from a %ot dense state "volution described by C>1 $yr 1 !o'pare (it%* Solar s rface* = ~ 0>? e@ #oo' te'p* = ~ 1AB0 e@ Galaxy formation, life etc 8 Early Universe Primer =%e niverse e9panded from a %ot dense state "volution described by C10 000 yr 1C>1 $yr !o'pare (it%* Solar s rface* = ~ 0>? e@ #oo' te'p* = ~ 1AB0 e@ -ydrogen recombination: Galaxy formation,