Introduction to Dark Matter
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Wimps and Machos ENCYCLOPEDIA of ASTRONOMY and ASTROPHYSICS
WIMPs and MACHOs ENCYCLOPEDIA OF ASTRONOMY AND ASTROPHYSICS WIMPs and MACHOs objects that could be the dark matter and still escape detection. For example, if the Galactic halo were filled –3 . WIMP is an acronym for weakly interacting massive par- with Jupiter mass objects (10 Mo) they would not have ticle and MACHO is an acronym for massive (astrophys- been detected by emission or absorption of light. Brown . ical) compact halo object. WIMPs and MACHOs are two dwarf stars with masses below 0.08Mo or the black hole of the most popular DARK MATTER candidates. They repre- remnants of an early generation of stars would be simi- sent two very different but reasonable possibilities of larly invisible. Thus these objects are examples of what the dominant component of the universe may be. MACHOs. Other examples of this class of dark matter It is well established that somewhere between 90% candidates include primordial black holes created during and 99% of the material in the universe is in some as yet the big bang, neutron stars, white dwarf stars and vari- undiscovered form. This material is the gravitational ous exotic stable configurations of quantum fields, such glue that holds together galaxies and clusters of galaxies as non-topological solitons. and plays an important role in the history and fate of the An important difference between WIMPs and universe. Yet this material has not been directly detected. MACHOs is that WIMPs are non-baryonic and Since extensive searches have been done, this means that MACHOS are typically (but not always) formed from this mysterious material must not emit or absorb appre- baryonic material. -
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. -
Adrien Christian René THOB
THE RELATIONSHIP BETWEEN THE MORPHOLOGY AND KINEMATICS OF GALAXIES AND ITS DEPENDENCE ON DARK MATTER HALO STRUCTURE IN SIMULATED GALAXIES Adrien Christian René THOB A thesis submitted in partial fulfilment of the requirements of Liverpool John Moores University for the degree of Doctor of Philosophy. 26 April 2019 To my grand-parents, René Roumeaux, Christian Thob, Yvette Roumeaux (née Bajaud) and Anne-Marie Thob (née Léglise). ii Abstract Galaxies are among nature’s most majestic and diverse structures. They can play host to as few as several thousands of stars, or as many as hundreds of billions. They exhibit a broad range of shapes, sizes, colours, and they can inhabit vastly differing cosmic environments. The physics of galaxy formation is highly non-linear and in- volves a variety of physical mechanisms, precluding the development of entirely an- alytic descriptions, thus requiring that theoretical ideas concerning the origin of this diversity are tested via the confrontation of numerical models (or “simulations”) with observational measurements. The EAGLE project (which stands for Evolution and Assembly of GaLaxies and their Environments) is a state-of-the-art suite of such cos- mological hydrodynamical simulations of the Universe. EAGLE is unique in that the ill-understood efficiencies of feedback mechanisms implemented in the model were calibrated to ensure that the observed stellar masses and sizes of present-day galaxies were reproduced. We investigate the connection between the morphology and internal 9:5 kinematics of the stellar component of central galaxies with mass M? > 10 M in the EAGLE simulations. We compare several kinematic diagnostics commonly used to describe simulated galaxies, and find good consistency between them. -
Current Perspectives on Dark Matter
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 problem of the Standard Model (SM). In Mirror Twin Higgs models, the SM is extended to include a complete mirror (“twin”) copy of the SM, with its own particle content and gauge groups. The SM and its twin counterpart are related by a discrete Z2 “twin” symmetry. Z2 SMA SMB The mirror particles are completely neutral under the SM strong, weak and electromagnetic forces. Only feel gravity. In Mirror Twin Higgs models, the one loop quadratic divergences that contribute to the Higgs mass are cancelled by twin sector states that carry no charge under the SM gauge groups. Discovery of these states at LHC is therefore difficult. May explain null results. The SM and twin SM primarily interact through the Higgs portal. This interaction is needed for cancellation of quadratic divergences. After electroweak symmetry breaking, SM Higgs and twin Higgs mix. • Higgs couplings to SM states are suppressed by the mixing. • Higgs now has (mixing suppressed) couplings to twin states. A soft breaking of the Z2 symmetry ensures that 퐯B, the VEV of the twin Higgs, is greater than 퐯A, the VEV of the SM Higgs. The mixing angle ~ 퐯A/퐯B. Higgs measurements constrain 퐯A/퐯B ≤ ퟏ/ퟑ. Twin fermions are heavier than SM fermions by a factor of 퐯B/퐯A . Naturalness requires 퐯A/퐯B ≥ ퟏ/ퟓ. (Twin top should not be too heavy.) The Higgs portal interaction has implications for cosmology. -
Letter of Interest Cosmic Probes of Ultra-Light Axion Dark Matter
Snowmass2021 - Letter of Interest Cosmic probes of ultra-light axion dark matter Thematic Areas: (check all that apply /) (CF1) Dark Matter: Particle Like (CF2) Dark Matter: Wavelike (CF3) Dark Matter: Cosmic Probes (CF4) Dark Energy and Cosmic Acceleration: The Modern Universe (CF5) Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before (CF6) Dark Energy and Cosmic Acceleration: Complementarity of Probes and New Facilities (CF7) Cosmic Probes of Fundamental Physics (TF09) Astro-particle physics and cosmology Contact Information: Name (Institution) [email]: Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Institute, University of Toronto) [ [email protected]] Authors: Simeon Bird (UC Riverside), Simon Birrer (Stanford University), Djuna Croon (TRIUMF), Alex Drlica-Wagner (Fermilab, University of Chicago), Jeff A. Dror (UC Berkeley, Lawrence Berkeley National Laboratory), Daniel Grin (Haverford College), David J. E. Marsh (Georg-August University Goettingen), Philip Mocz (Princeton), Ethan Nadler (Stanford), Chanda Prescod-Weinstein (University of New Hamp- shire), Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Insti- tute, University of Toronto), Katelin Schutz (MIT), Neelima Sehgal (Stony Brook University), Yu-Dai Tsai (Fermilab), Tien-Tien Yu (University of Oregon), Yimin Zhong (University of Chicago). Abstract: Ultra-light axions are a compelling dark matter candidate, motivated by the string axiverse, the strong CP problem in QCD, and possible tensions in the CDM model. They are hard to probe experimentally, and so cosmological/astrophysical observations are very sensitive to the distinctive gravitational phenomena of ULA dark matter. There is the prospect of probing fifteen orders of magnitude in mass, often down to sub-percent contributions to the DM in the next ten to twenty years. -
Particle Dark Matter an Introduction Into Evidence, Models, and Direct Searches
Particle Dark Matter An Introduction into Evidence, Models, and Direct Searches Lecture for ESIPAP 2016 European School of Instrumentation in Particle & Astroparticle Physics Archamps Technopole XENON1T January 25th, 2016 Uwe Oberlack Institute of Physics & PRISMA Cluster of Excellence Johannes Gutenberg University Mainz http://xenon.physik.uni-mainz.de Outline ● Evidence for Dark Matter: ▸ The Problem of Missing Mass ▸ In galaxies ▸ In galaxy clusters ▸ In the universe as a whole ● DM Candidates: ▸ The DM particle zoo ▸ WIMPs ● DM Direct Searches: ▸ Detection principle, physics inputs ▸ Example experiments & results ▸ Outlook Uwe Oberlack ESIPAP 2016 2 Types of Evidences for Dark Matter ● Kinematic studies use luminous astrophysical objects to probe the gravitational potential of a massive environment, e.g.: ▸ Stars or gas clouds probing the gravitational potential of galaxies ▸ Galaxies or intergalactic gas probing the gravitational potential of galaxy clusters ● Gravitational lensing is an independent way to measure the total mass (profle) of a foreground object using the light of background sources (galaxies, active galactic nuclei). ● Comparison of mass profles with observed luminosity profles lead to a problem of missing mass, usually interpreted as evidence for Dark Matter. ● Measuring the geometry (curvature) of the universe, indicates a ”fat” universe with close to critical density. Comparison with luminous mass: → a major accounting problem! Including observations of the expansion history lead to the Standard Model of Cosmology: accounting defcit solved by ~68% Dark Energy, ~27% Dark Matter and <5% “regular” (baryonic) matter. ● Other lines of evidence probe properties of matter under the infuence of gravity: ▸ the equation of state of oscillating matter as observed through fuctuations of the Cosmic Microwave Background (acoustic peaks). -
Mixed Axion/Neutralino Cold Dark Matter in Supersymmetric Models
Preprint typeset in JHEP style - HYPER VERSION Mixed axion/neutralino cold dark matter in supersymmetric models Howard Baera, Andre Lessaa, Shibi Rajagopalana,b and Warintorn Sreethawonga aDept. of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USA bLaboratoire de Physique Subatomique et de Cosmologie, UJF Grenoble 1, CNRS/IN2P3, INPG, 53 Avenue des Martyrs, F-38026 Grenoble, France E-mail: [email protected], [email protected], [email protected],[email protected] Abstract: We consider supersymmetric (SUSY) models wherein the strong CP problem is solved by the Peccei-Quinn (PQ) mechanism with a concommitant axion/axino supermul- tiplet. We examine R-parity conserving models where the neutralino is the lightest SUSY particle, so that a mixture of neutralinos and axions serve as cold dark matter (aZ1 CDM). The mixed aZ1 CDM scenario can match the measured dark matter abundance for SUSY models which typically give too low a value of the usual thermal neutralino abundance,e such as modelse with wino-like or higgsino-like dark matter. The usual thermal neutralino abundance can be greatly enhanced by the decay of thermally-produced axinos (˜a) to neu- tralinos, followed by neutralino re-annihilation at temperatures much lower than freeze-out. In this case, the relic density is usually neutralino dominated, and goes as (f /N)/m3/2. ∼ a a˜ If axino decay occurs before neutralino freeze-out, then instead the neutralino abundance can be augmented by relic axions to match the measured abundance. Entropy production from late-time axino decays can diminish the axion abundance, but ultimately not the arXiv:1103.5413v1 [hep-ph] 28 Mar 2011 neutralino abundance. -
Dark Energy and Dark Matter
Dark Energy and Dark Matter Jeevan Regmi Department of Physics, Prithvi Narayan Campus, Pokhara [email protected] Abstract: The new discoveries and evidences in the field of astrophysics have explored new area of discussion each day. It provides an inspiration for the search of new laws and symmetries in nature. One of the interesting issues of the decade is the accelerating universe. Though much is known about universe, still a lot of mysteries are present about it. The new concepts of dark energy and dark matter are being explained to answer the mysterious facts. However it unfolds the rays of hope for solving the various properties and dimensions of space. Keywords: dark energy, dark matter, accelerating universe, space-time curvature, cosmological constant, gravitational lensing. 1. INTRODUCTION observations. Precision measurements of the cosmic It was Albert Einstein first to realize that empty microwave background (CMB) have shown that the space is not 'nothing'. Space has amazing properties. total energy density of the universe is very near the Many of which are just beginning to be understood. critical density needed to make the universe flat The first property that Einstein discovered is that it is (i.e. the curvature of space-time, defined in General possible for more space to come into existence. And Relativity, goes to zero on large scales). Since energy his cosmological constant makes a prediction that is equivalent to mass (Special Relativity: E = mc2), empty space can possess its own energy. Theorists this is usually expressed in terms of a critical mass still don't have correct explanation for this but they density needed to make the universe flat. -
DARK MATTER and NEUTRINOS Arxiv:1711.10564V1 [Physics.Pop-Ph]
Physics Education 1 dateline DARK MATTER AND NEUTRINOS Gazal Sharma1, Anu2 and B. C. Chauhan3 Department of Physics & Astronomical Science School of Physical & Material Sciences Central University of Himachal Pradesh (CUHP) Dharamshala, Kangra (HP) INDIA-176215. [email protected] [email protected] [email protected] (Submitted 03-08-2015) Abstract The Keplerian distribution of velocities is not observed in the rotation of large scale structures, such as found in the rotation of spiral galaxies. The deviation from Keplerian distribution provides compelling evidence of the presence of non-luminous matter i.e. called dark matter. There are several astrophysical motivations for investigating the dark matter in and around the galaxy as halo. In this work we address various theoretical and experimental indications pointing towards the existence of this unknown form of matter. Amongst its constituents neutrino is one of the most prospective candidates. We know the neutrinos oscillate and have tiny masses, but there are also signatures for existence of heavy and light sterile neutrinos and possibility of their mixing. Altogether, the role of neutrinos is of great interests in cosmology and understanding dark matter. arXiv:1711.10564v1 [physics.pop-ph] 23 Nov 2017 1 Introduction revealed in 2013 that our Universe contains 68:3% of dark energy, 26:8% of dark matter, and only 4:9% of the Universe is known mat- As a human being the biggest surprise for us ter which includes all the stars, planetary sys- was, that the Universe in which we live in tems, galaxies, and interstellar gas etc.. This is mostly dark. -
Signs of Dark Matter May Point to Mirror Matter Candidate 27 April 2010, by Lisa Zyga
Signs of dark matter may point to mirror matter candidate 27 April 2010, by Lisa Zyga (PhysOrg.com) -- Dark matter, which contains the At first, mirror matter may sound a bit like antimatter "missing mass" that's needed to explain why (which is ordinary matter with an opposite charge). galaxies stay together, could take any number of In both theories, the number of known particles forms. The main possible candidates include would double. However, while antimatter interacts MACHOS and WIMPS, but there is no shortage of very strongly with ordinary matter, annihilating itself proposals. Rather, the biggest challenge is finding into photons, mirror matter would interact very some evidence that would support one or more of weakly with ordinary matter. For this reason, some these candidates. Currently, more than 30 physicists have speculated that mirror particles experiments are underway trying to detect a sign of could be candidates for dark matter. Even though dark matter. So far, only two experiments claim to mirror matter would produce light, we would not see have found signals, with the most recent it, and it would be very difficult to detect. observations coming just a month ago. Now, physicist Robert Foot from the University of However, mirror matter would not be impossible to Melbourne has shown that the results of these two detect, and Foot thinks that the DAMA experiment experiments can be simultaneously explained by and the CoGeNT experiment may have detected an intriguing dark matter candidate called mirror mirror matter. In DAMA, scientists observed a piece matter. of sodium iodide, which should generate a photon when struck by a dark matter particle. -
Latest Results of the Direct Dark Matter Search with the EDELWEISS-II Experiment
Latest results of the direct dark matter search with the EDELWEISS-II experiment Gilles Gerbier1 for the EDELWEISS collaboration 1IRFU/SPP, CEA Saclay, , 91191 Gif s Yvette, France DOI: http://dx.doi.org/10.3204/DESY-PROC-2010-03/gerbier gilles The EDELWEISS-II experiment uses cryogenic heat-and-ionization Germanium detectors in order to detect the rare interactions from WIMP dark matter particles of local halo. New-generation detectors with an interleaved electrode geometry were developped and val- idated, enabling an outstanding gamma-ray and surface interaction rejection. We present here preliminary results of a one-year WIMP search carried out with 10 of such detectors in the Laboratoire Souterrain de Modane. A sensitivity to the spin-independent WIMP- 8 nucleon cross-section of 5 10− pb was achieved using a 322 kg.days effective exposure. × We also present the current status of the experiment and prospects to improve the present sensitivity by an order of magnitude in the near future. 1 The Edelweiss II set up and the detectors Weakly Interacting Massive Particles (WIMPs) are a class of particles now widely considered as one of the most likely explanation for the various observations of dark matter from the largest scales of the Universe to galactic scales. The collisions of WIMPs on ordinary matter are ex- pected to generate mostly elastic scatters off nuclei, characterised by low-energy deposits (<100 keV) with an exponential-like spectrum, and a very low interaction rate, currently constrained at the level of 1 event/kg/year. Detecting these events requires an ultralow radioactivity envi- ronment as well as detectors with a low energy threshold and an active rejection of the residual backgrounds [1]. -
Ultra-Weak Gravitational Field Theory Daniel Korenblum
Ultra-weak gravitational field theory Daniel Korenblum To cite this version: Daniel Korenblum. Ultra-weak gravitational field theory. 2018. hal-01888978 HAL Id: hal-01888978 https://hal.archives-ouvertes.fr/hal-01888978 Preprint submitted on 5 Oct 2018 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Ultra-weak gravitational field theory Daniel KORENBLUM [email protected] April 2018 Abstract The standard model of the Big Bang cosmology model ΛCDM 1 considers that more than 95 % of the matter of the Universe consists of particles and energy of unknown forms. It is likely that General Relativity (GR)2, which is not a quantum theory of gravitation, needs to be revised in order to free the cosmological model of dark matter and dark energy. The purpose of this document, whose approach is to hypothesize the existence of the graviton, is to enrich the GR to make it consistent with astronomical observations and the hypothesis of a fully baryonic Universe while maintaining the formalism at the origin of its success. The proposed new model is based on the quantum character of the gravitational field. This non-intrusive approach offers a privileged theoretical framework for probing the properties of the regime of ultra-weak gravitational fields in which the large structures of the Universe are im- mersed.