2018 Lightning Round – Physics Subfields

Total Page:16

File Type:pdf, Size:1020Kb

2018 Lightning Round – Physics Subfields 2018 Lightning Round – Physics Subfields Experimental Condensed Matter Physics – Lucas Peeters More is Different isn’t just the title of Phil Anderson’s classic essay on the limitations of reductionism in science - if condensed matter physics was ever in need of an official tagline, it would also be a prime candidate. Indeed, why do we even need a field dedicated to the behavior of the trillions of electrons in materials all around us? Haven’t particle physicists figured out all the fundamental properties of those particles a while ago? But more is indeed different. The zoo of emergent phenomena arising when we put myriads of such particles together - magnetism, superconductivity and multiferroicity, to name a few - requires its own language, its own concepts and its own tools. Our understanding of and control over such effects are not only a rewarding scientific enterprise in their own right, but have also spurred a host of technological breakthroughs which continue to transform our everyday lives. For example, having been at the root of our current, silicon-based computing architecture, condensed matter physics is now also one of the main contenders to deliver the first industrially useful quantum computing devices. Experimental condensed matter physicists have several approaches at their disposal to advance our understanding. Materials growth is one of these. This field, with its often-exceptional sensitivity to a slew of control parameters can appear like a dark art to many outsiders. Those who master it, though, can discover materials which combine effects in ways never seen before in nature, and their controlled realization of such systems can provide invaluable insight. Not all effects are visible at all length scales though, so others specialize in the fabrication of micro- or even nanoscale devices, combining different materials and techniques to create minute devices which bridge the gap between the single-atom scale and macroscopic scales. Another line of research focuses on the development of new measurement techniques; the boundary of spatial and temporal resolution is always being pushed, and increased access to the charge and spin properties of electrons can shed new light on long-standing questions. Since its debut about a century ago, condensed matter physics has dramatically advanced our understanding of electronic behavior in a wide range of contexts. If the past is any guide, the future will give us even more, and it’ll be even more different. Computational Condensed Matter Physics – Yanbing Zhu (some sections from Harrison Ruiz) What is it? Theoretical/computational condensed matter physics involves studying condensed phases of matter. This usually refers to solid states of matter (anything you can touch) plus liquids. A big goal is characterizing certain materials and their resulting phenomena - i.e. finding materials with certain properties, designing a new material from scratch, understanding a (quantum) phase transition, or studying how a material behaves under external influences. Examples of properties are studied are stability, conductivity, specific heat, and magnetic susceptibility. Often these properties studied are in exotic phases of matter such as superconductors, topological insulators, and spin liquids, where some unusual and often purely quantum mechanical phenomena are observed in solids. These phases can be studied both in out of equilibrium. There’s a big interplay between physics, materials science, chemistry, and of course, computational tools. The labels in research between the different subfields becomes blurred - i.e. statistical mechanics, scattering behavior, analytical models, and theories of strongly correlated phenomena are used from physics, physical considerations like the behavior of a material under strain or stress, dislocations, and grain boundaries are used from materials science, and elemental properties, reaction properties, and bonding rules are used from chemistry. Why do we do it? Research is driven by both understanding fundamental science problems and also more practical purposes. Oftentimes both goals can be part of the same project. For instance, topological materials are interesting its exotic behavior was only fairly recently understood, but they are also of interest for quantum computing purposes since there is no decoherence. Batteries and solar materials like new lithium based electrolytes or hybrid inorganic- perovskites are studied for their practical purposes (computational/theory work is often used to guide experiments or explain behavior seen in the lab). The work also enables us to better understand topics like conductivity or to figure out which models and approximations work in certain limits. What does a typical research do? The daily work consists of making calculations using various models and possibly collaborating with experimentalists working on the same problem. The way the calculations are done can vary depending on the type of research. On one end, you have computational condensed matter physicists who focus on numerical calculations. This can involve using methods such as density functional theory, quantum Monte Carlo simulations, molecular dynamics, or exact diagonalization. Running these types of calculations can either involve using libraries designed for ab initio simulations, such as density functional theory (DFT), or writing code for them from scratch. Common programming languages used for this are C++ and Python. In many cases parallel computing techniques are used as the problem is computationally intensive and even some of the simplest models can only be solved exactly for around 20 particles. Recently, machine learning tools also become more popular. Other theorists may use analytical techniques to work on these problems. Some of the approaches they may use are mean-field theory, renormalization group, and quantum field theory. There is not always a clear division between the computational physicist and the traditional theorist so a combination of numerical and analytical methods. Some experimentalists also often use computational tools to compare with their experimental findings. Experimental Particle Physics - Kelly Stifter Particle physics is the study of the smallest pieces of matter and their interactions. The biggest success of the field is the Standard Model, which describes all known particles and the interactions between them (except gravity). Despite the success of the Standard Model, there are still many mysteries to be solved that are considered “beyond” the Standard Model, as well as some open questions within the Standard Model itself. On the experimental side, scientists build detectors in order to learn about these particles. When conducting these experiments, we often try to do one of two things. First, we search for new physics that is not included in the Standard Model. Second, we precisely measure, or look for deviations from, “known” physics. We can break it down even further and specify three main ways that we conduct these searches or measurements. They are often referred to as “frontiers”, since in each category, we push the limits of our current technology and understanding. First is the energy frontier, which uses the world’s largest particle accelerator, the LHC, to recreate the universe as it was a billionth of a second after the big bang and make huge discoveries about the smallest pieces of the universe. The two main experiments on the LHC are CMS and ATLAS. Together, these two detectors discovered the Higgs Boson in 2012. Now, in addition to precisely measuring the masses and couplings of all Standard Model particles, they are looking for dark matter and more exotic new physics such as supersymmetry and extra dimensions. Next is the intensity frontier, which investigates some of the rarest processes in nature, including unusual interactions of fundamental particles and subtle effects that require large data sets to observe and measure. Of particular note is the effort to measure neutrino properties, including their mass and parameters associated with their oscillations. Others open questions include matter-antimatter asymmetry, proton decay, the anomalous magnetic dipole moment of the muon, and many more. Last but not least is the cosmic frontier, which strives to understand the structure, evolution, and contents of the universe. It turns out that only 5% of the energy in the universe is regular matter, and then rest is dark matter and dark energy. There are many experiments trying to understand the physical nature of dark matter either by directly detecting dark matter particles that pass through a detector, or by indirectly detecting specific signatures in cosmic rays coming from the universe. Cosmic rays can also be used to look for other new particles beyond the Standard Model. The very beginning of the universe was marked by a period of intense inflation, and there are experiments that study the cosmic microwave background radiation in order to understand this phenomenon. A similar expansion is happening today and is driven by dark energy, which is being studied by large ground-based telescopes. Everything I have mentioned so far is considered “high energy” particle physics, since it deals with particles and interactions up at the scale of millions of electron volts (eV). Scientists also work on medium and low energy particle physics, which are concerned with structure and stability of hadrons and atomic nuclei. The interactions in these subfields have relatively lower energy - only
Recommended publications
  • Galaxy Formation Simulations: "Sub-Grid" Vs. Physics
    GalaxyGalaxy formationformation simulations:simulations: "sub-grid""sub-grid" vs.vs. physicsphysics DeboraDebora SijackiSijacki IoAIoA && KICCKICC CambridgeCambridge Cosmic Mergers Workshop Birmingham Sept 22th 2017 Cosmological simulations of galaxy and structure formation 2 Provide ab initio physical understanding on all scales Standard (and less standard) ingredients: ► “simple” ΛCDM assumption (WDM, SIDM,…, evolving w,…, coupled DM+DE models,…) ► Newtonian gravity (dark matter and baryons) (relativistic corrections, modified gravity models,...) ► Ideal gas hydrodynamics + collisionless dynamics of stars (conduction, viscosity, MHD,…, stellar collisions, stellar hydro) ► Gas radiative cooling/heating, star & BH formation and feedback (non equlibrium low T cooling, dust, turbulence, GMCs,…) ► Reionization in form of an uniform UV background (simple accounting for the local sources,…, full RT on the fly) Pure dark matter simulations in ΛCDM cosmology 3 Millennium XXL 40 yrs! See also: Horizon Run 3 (Kim 2011) MultiDark (Prada 2012) DEUS (Alimi et al. 2012) Watson et al. 2013 The importance of baryons 4 Baryons are directly observable and they affect the underlying dark matter distribution (contraction/expansion/shape/bias, WL,...) => profound implications for cosmology SDSS, BOSS, eBOSS Hubble UDF composite DES WL The importance of baryons 5 Vast range of spatial scales involved and very complex, non-linear physics → SUB-GRID models (“free parameters” constrained by obs) Cosmic web Galaxies 109 pc 103 pc GMCs 10-100 pc Massive stars SNae SMBHs -8 -6 0.1 pc 10 - 10 pc < 10-6 pc Current state-of-the-art in cosmological hydro simulations 6 The Eagle Project (Schaye et al. 2015) The Horizon AGN project (Dubois et al. 14) Magneticum (Dolag et al.
    [Show full text]
  • A Statistical Framework for the Characterisation of WIMP Dark Matter with the LUX-ZEPLIN Experiment
    A statistical framework for the characterisation of WIMP dark matter with the LUX-ZEPLIN experiment Ibles Olcina Samblas Department of Physics A thesis submitted for the degree of Doctor of Philosophy November 2019 Abstract Several pieces of astrophysical evidence, from galactic to cosmological scales, indicate that most of the mass in the universe is composed of an invisible and essentially collisionless substance known as dark matter. A leading particle candidate that could provide the role of dark matter is the Weakly Interacting Massive Particle (WIMP), which can be searched for directly on Earth via its scattering off atomic nuclei. The LUX-ZEPLIN (LZ) experiment, currently under construction, employs a multi-tonne dual-phase xenon time projection chamber to search for WIMPs in the low background environment of the Davis Campus at the Sanford Underground Research Facility (South Dakota, USA). LZ will probe WIMP interactions with unprecedented sensitivity, starting to explore regions of the WIMP parameter space where new backgrounds are expected to arise from the elastic scattering of neutrinos off xenon nuclei. In this work the theoretical and computational framework underlying the calculation of the sensitivity of the LZ experiment to WIMP-nucleus scattering interactions is presented. After its planned 1000 live days of exposure, LZ will be able to achieve a 3σ discovery for spin independent cross sections above 3.0 10 48 cm2 at 40 GeV/c2 WIMP mass or exclude at × − 90% CL a cross section of 1.3 10 48 cm2 in the absence of signal. The sensitivity of LZ × − to spin-dependent WIMP-neutron and WIMP-proton interactions is also presented.
    [Show full text]
  • The Illustris Simulation: the Evolving Population of Black Holes Across Cosmic Time
    MNRAS 452, 575–596 (2015) doi:10.1093/mnras/stv1340 The Illustris simulation: the evolving population of black holes across cosmic time Debora Sijacki,1‹ Mark Vogelsberger,2 Shy Genel,3,4† Volker Springel,5,6 Paul Torrey,2,3,7 Gregory F. Snyder,8 Dylan Nelson3 and Lars Hernquist3 1Institute of Astronomy and Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 2Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 3Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 4Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA 5Heidelberg Institute for Theoretical Studies, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany 6Zentrum fur¨ Astronomie der Universitat¨ Heidelberg, ARI, Monchhofstr.¨ 12-14, D-69120 Heidelberg, Germany Downloaded from 7Caltech, TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA 8Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA Accepted 2015 June 12. Received 2015 June 12; in original form 2014 August 28 http://mnras.oxfordjournals.org/ ABSTRACT We study the properties of black holes and their host galaxies across cosmic time in the Illustris simulation. Illustris is a large-scale cosmological hydrodynamical simulation which resolves a (106.5 Mpc)3 volume with more than 12 billion resolution elements and includes state-of-the-art physical models relevant for galaxy formation. We find that the black hole mass density for redshifts z = 0–5 and the black hole mass function at z = 0 predicted by Illustris are in very good agreement with the most recent observational constraints.
    [Show full text]
  • Astrophysical Uncertainties of Direct Dark Matter Searches
    Technische Universit¨atM¨unchen Astrophysical uncertainties of direct dark matter searches Dissertation by Andreas G¨unter Rappelt Physik Department, T30d & Collaborative Research Center SFB 1258 “Neutrinos and Dark Matter in Astro- and Particlephysics” Technische Universit¨atM¨unchen Physik Department T30d Astrophysical uncertainties of direct dark matter searches Andreas G¨unter Rappelt Vollst¨andigerAbdruck der von der Fakult¨atf¨urPhysik der Technischen Universit¨at M¨unchen zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften genehmigten Dissertation. Vorsitzender: Prof. Dr. Lothar Oberauer Pr¨uferder Dissertation: 1. Prof. Dr. Alejandro Ibarra 2. Prof. Dr. Bj¨ornGarbrecht Die Dissertation wurde am 12.11.2019 bei der Technischen Universit¨at M¨unchen eingereicht und durch die Fakult¨atf¨urPhysik am 24.01.2020 angenommen. Abstract Although the first hints towards dark matter were discovered almost 100 years ago, little is known today about its properties. Also, dark matter has so far only been inferred through astronomical and cosmological observations. In this work, we therefore investi- gate the influence of astrophysical assumptions on the interpretation of direct searches for dark matter. For this, we assume that dark matter is a weakly interacting massive particle. First, we discuss the development of a new analysis method for direct dark matter searches. Starting from the decomposition of the dark matter velocity distribu- tion into streams, we present a method that is completely independent of astrophysical assumptions. We extend this by using an effective theory for the interaction of dark matter with nucleons. This allows to analyze experiments with minimal assumptions on the particle physics of dark matter. Finally, we improve our method so that arbitrarily strong deviations from a reference velocity distribution can be considered.
    [Show full text]
  • Jhep07(2020)081
    Published for SISSA by Springer Received: February 10, 2020 Revised: May 28, 2020 Accepted: June 9, 2020 Published: July 13, 2020 Impact of uncertainties in the halo velocity profile on JHEP07(2020)081 direct detection of sub-GeV dark matter Andrzej Hryczuk,a Ekaterina Karukes,b Leszek Roszkowskib;a and Matthew Taliab aNational Centre for Nuclear Research, Pasteura 7, Warsaw 02-093, Poland bAstroCeNT, Nicolaus Copernicus Astronomical Center Polish Academy of Sciences, ul. Rektorska 4, Warsaw 00-614, Poland E-mail: [email protected], [email protected], [email protected], [email protected] Abstract: We use the state-of-the-art high-resolution cosmological simulations by Illus- trisTNG to derive the velocity distribution and local density of dark matter in galaxies like our Milky Way and find a substantial spread in both quantities. Next we use our find- ings to examine the sensitivity to the dark matter velocity profile of underground searches using electron scattering in germanium and silicon targets. We find that sub-GeV dark matter search is strongly affected by these uncertainties, unlike nuclear recoil searches for heavier dark matter, especially in multiple electron-hole modes, for which the sensitivity to the scattering cross-section is also weaker. Therefore, by improving the sensitivity to lower ionization thresholds not only projected sensitivities will be boosted but also the dependence on the astrophysical uncertainties will become significantly reduced. Keywords: Cosmology of Theories beyond the SM, Beyond Standard Model ArXiv ePrint: 2001.09156 Open Access, c The Authors. https://doi.org/10.1007/JHEP07(2020)081 Article funded by SCOAP3.
    [Show full text]
  • Dark Energy Survey Year 3 Results: Multi-Probe Modeling Strategy and Validation
    DES-2020-0554 FERMILAB-PUB-21-240-AE Dark Energy Survey Year 3 Results: Multi-Probe Modeling Strategy and Validation E. Krause,1, ∗ X. Fang,1 S. Pandey,2 L. F. Secco,2, 3 O. Alves,4, 5, 6 H. Huang,7 J. Blazek,8, 9 J. Prat,10, 3 J. Zuntz,11 T. F. Eifler,1 N. MacCrann,12 J. DeRose,13 M. Crocce,14, 15 A. Porredon,16, 17 B. Jain,2 M. A. Troxel,18 S. Dodelson,19, 20 D. Huterer,4 A. R. Liddle,11, 21, 22 C. D. Leonard,23 A. Amon,24 A. Chen,4 J. Elvin-Poole,16, 17 A. Fert´e,25 J. Muir,24 Y. Park,26 S. Samuroff,19 A. Brandao-Souza,27, 6 N. Weaverdyck,4 G. Zacharegkas,3 R. Rosenfeld,28, 6 A. Campos,19 P. Chintalapati,29 A. Choi,16 E. Di Valentino,30 C. Doux,2 K. Herner,29 P. Lemos,31, 32 J. Mena-Fern´andez,33 Y. Omori,10, 3, 24 M. Paterno,29 M. Rodriguez-Monroy,33 P. Rogozenski,7 R. P. Rollins,30 A. Troja,28, 6 I. Tutusaus,14, 15 R. H. Wechsler,34, 24, 35 T. M. C. Abbott,36 M. Aguena,6 S. Allam,29 F. Andrade-Oliveira,5, 6 J. Annis,29 D. Bacon,37 E. Baxter,38 K. Bechtol,39 G. M. Bernstein,2 D. Brooks,31 E. Buckley-Geer,10, 29 D. L. Burke,24, 35 A. Carnero Rosell,40, 6, 41 M. Carrasco Kind,42, 43 J. Carretero,44 F. J. Castander,14, 15 R.
    [Show full text]
  • TECHNICAL ASPECTS of ILLUSTRIS- a COSMOLOGICAL SIMULATION Dr Sheshappa SN1, Megha S Kencha Reddy2 , N Chandana3
    International Research Journal of Engineering and Technology (IRJET) e-ISSN: 2395-0056 Volume: 07 Issue: 05 | May 2020 www.irjet.net p-ISSN: 2395-0072 TECHNICAL ASPECTS OF ILLUSTRIS- A COSMOLOGICAL SIMULATION Dr Sheshappa SN1, Megha S Kencha Reddy2 , N Chandana3, Ranjitha N4, Sushma Fouzdar5 1Faculty, Dept. of ISE, Sir MVIT, Karnataka, India, [email protected], 2VIII semester, Dept. of ISE, Sir MVIT ---------------------------------------------------------------------------***--------------------------------------------------------------------------- Abstract - THE BIG QUESTION - Where did we come galaxy formation. Recent simulations follow the from and where are we going?Humans have been trying formation of individual galaxies and galaxy populations to figure out the origin of the known universe since the from well-defined initial conditions and yield realistic beginning of time and Since the early part of the 1900s, galaxy properties. At the core of these simulations are the Big Bang theory is the most accepted explanation and detailed galaxy formation models. Of the many aspects has dominated the discussion of the origin and fate of the these models are capable of, they describe the cooling of universe. And the future of the universe can only be gas, the formation of stars, and the energy and hypothesized based on our knowledge but the question momentum injection caused by supermassive black does not seem to get irrelevant anytime in the near holes and massive stars. Nowadays, simulations also future. With the advancement technology and the model the impact of radiation fields, relativistic particles available research, data and techniques like data mining and magnetic fields, leading to an increasingly complex and machine learning the problems can be visualised description of the galactic ecosystem and the detailed through accurate digital representations and simulations evolution of galaxies in the cosmological context.
    [Show full text]
  • The Next Generation of Hydrodynamical Simulations of Galaxy Formation
    HLRS Golden Spike Award 2016 The Next Generation of Hydrodynamical Simulations of Galaxy Formation Scientific background galaxies in clusters and the characteristics of Galaxies are comprised of up to several hundred hydrogen on large scales, and at the same time billion stars and display a variety of shapes and matched the metal and hydrogen content of sizes. Their formation involves a complicated galaxies on small scales. Indeed, the virtual uni- blend of astrophysics, including gravitational, verse created by Illustris resembles the real one hydrodynamical and radiative processes, as well so closely that it can be adopted as a powerful as dynamics in the enigmatic „dark sector“ of laboratory to further explore and characterize the Universe, which is composed of dark mat- galaxy formation physics. This is underscored ter and dark energy. Dark matter is thought to by the nearly 100 publications that have been consist of a yet unidentified elementary parti- written using the simulation thus far. cle, making up about 85% of all matter, whereas dark energy opposes gravity and has induced However, the Illustris simulation also showed an accelerated expansion of the Universe in the some tensions between its predictions and recent past. Because the governing equations observations of the real Universe, calling for both, are too complicated to be solved analytically, improvements in the physical model as well as numerical simulations have become a primary in the numerical accuracy and size of the simu- tool in theoretical astrophysics to study cosmic lations used to represent the cosmos. For exam- structure formation. Such calculations connect ple, one important physical ingredient that was the comparatively simple initial state left behind missing are magnetic fields.
    [Show full text]
  • Determining Properties of LEGA-C Galaxies Through Spectral Star-Formation History Reconstruction
    Determining Properties of LEGA-C Galaxies through Spectral Star-formation History Reconstruction Priscilla Chauke Dissertation submitted to the Combined Faculties for the Natural Sciences and for Mathematics of the Ruperto-Carola University of Heidelberg, Germany for the degree of Doctor of Natural Sciences Put forward by Priscilla Chauke Born in Giyani, South Africa Oral Examination: 24 July 2019 Determining Properties of LEGA-C Galaxies through Spectral Star-formation History Reconstruction Referees: Prof. Dr. Arjen van der Wel Prof. Dr. Jochen Heidt Va ka hina “My work amounts to a drop in a limitless ocean. Yet what is any ocean, but a multitude of drops?” -Adapted from David Mitchell, Cloud Atlas Acknowledgements I thank Arjen van der Wel for giving me the opportunity to pursue a PhD at the Max Planck Institut für Astronomy and for being my advisor throughout the years. I thank IMPRS and the DAAD for supporting me financially for the last four years. Lastly, I thank my family and friends for their love, support and encouragement. Abstract Over the past decade, photometric and spectroscopic surveys have enabled us to obtain an integrated view of galaxy evolution. We have measured the cosmic star formation history, and we know that about half of the stars we observe formed before the Universe was half of its current age. However, crucial knowledge of individual galaxy evolution has been limited because the detailed stellar population proper- ties that we know about galaxies, such as ages, metallicities and kinematics, have mostly been obtained from nearby galaxies, which contain mostly old stellar popu- lations.
    [Show full text]
  • The Diversity and Variability of Star Formation Histories in Different Simulations
    Draft version September 14, 2018 Typeset using LATEX twocolumn style in AASTeX61 THE DIVERSITY AND VARIABILITY OF STAR FORMATION HISTORIES IN DIFFERENT SIMULATIONS Kartheik Iyer, Sandro Tacchella, Lars Hernquist, Shy Genel, Chris Hayward, Neven Caplar, Phil Hopkins, Rachel Somerville, Romeel Dave, Ena Choi, and Viraj Pandya ABSTRACT As observational constraints on the star formation histories of galaxies improve due to higher S/N data and sophis- ticated analysis techniques, we have a better understanding of how galaxy scaling relations, such as the stellar mass star-formation rate and mass metallicity relations, evolve over the last 10 billion years. Despite these constraints, we have still a poor understanding of how individual galaxies evolve in these parameter spaces and therefore the physical processes that govern these scaling relations. We compile SFHs from an extensive set of simulations at z = 0 and z = 1, ranging from cosmological hydrodynamical simulations (Illustris, IllustrisTNG, MUFASA, SIMBA), zoom-in simula- tions (FIRE-2, VELA, Choi+17), semi-analytic models (Santa-Cruz SAM) and empirical models (UniverseMachine) to investigate the timescales on which star formation rates vary in different models. We quantify the diversity in SFHs from different simulations using the Hurst index and use a random forest based analysis to quantify the factors that drive this diversity. We then use a power spectral density based analysis to quantify the SFH variability as a function of the different timescales on which different physical processes act. This allows us to assess the impact of different (stellar / black hole) feedback processes, which affect the star formation on short timescales, versus gas accretion physics, which affect the star formation on longer timescales.
    [Show full text]
  • Ultra-Light Dark Matter
    Noname manuscript No. (will be inserted by the editor) Ultra-light dark matter Elisa G. M. Ferreira the date of receipt and acceptance should be inserted later Abstract Ultra-light dark matter is a class of dark matter models (DM) where DM is composed by bosons with masses ranging from 10−24 eV < m < eV. These models have been receiving a lot of attention in the past few years given their interesting property of forming a Bose{Einstein condensate (BEC) or a superfluid on galactic scales. BEC and superfluidity are some of the most striking quantum mechanical phenomena manifest on macroscopic scales, and upon condensation the particles behave as a single coherent state, described by the wavefunction of the condensate. The idea is that condensation takes place inside galaxies while outside, on large scales, it recovers the successes of ΛCDM. This wave nature of DM on galactic scales that arise upon condensation can address some of the curiosities of the behaviour of DM on small scales. There are many models in the literature that describe a DM component that condenses in galaxies. In this review, we are going to describe those models, and classify them into three classes, according to the different non-linear evolution and structures they form in galaxies: the fuzzy dark matter (FDM), the self-interacting fuzzy dark matter (SIFDM), and the DM superfluid. Each of these classes comprises many models, each presenting a similar phenomenology in galaxies. They also include some microscopic models like the axions and axion-like particles. To understand and describe this phenomenology in galaxies, we are going to review the phenomena of BEC and superfluidity that arise in condensed matter physics, and apply this knowledge to DM.
    [Show full text]
  • Impact of Uncertainties in the Halo Velocity Profile on Direct Detection Of
    Prepared for submission to JHEP Impact of uncertainties in the halo velocity profile on direct detection of sub-GeV dark matter Andrzej Hryczuk,a Ekaterina Karukes,b Leszek Roszkowski,b;a Matthew Taliab aNational Centre for Nuclear Research, Pasteura 7, 02-093 Warsaw, Poland bAstroCeNT, Nicolaus Copernicus Astronomical Center Polish Academy of Sciences, ul. Rektorska 4, 00-614 Warsaw, Poland E-mail: [email protected], [email protected], [email protected], [email protected] Abstract: We use the state-of-the-art high-resolution cosmological simulations by IllustrisTNG to derive the velocity distribution and local density of dark matter in galaxies like our Milky Way and find a substantial spread in both quantities. Next we use our findings to examine the sensitivity to the dark matter velocity profile of underground searches using electron scattering in germanium and silicon targets. We find that sub-GeV dark matter search is strongly affected by these uncertainties, unlike nuclear recoil searches for heavier dark matter, especially in multiple electron-hole modes, for which the sensitivity to the scattering cross-section is also weaker. Therefore, by improving the sensitivity to lower ionization thresholds not only projected sensitivities will be boosted but also the dependence on the astrophysical uncertainties will become significantly reduced. arXiv:2001.09156v1 [hep-ph] 24 Jan 2020 Contents 1 Introduction 1 2 Dark matter velocity distributions from IllustrisTNG simulation2 2.1 Selection of MW-like galaxies2 2.2 Dark matter velocity distributions3 3 Uncertainties in sub-GeV DM electron recoil5 4 Discussion and conclusions8 1 Introduction Our limited understanding of the dark matter (DM) halo structure, both local and Galactic, consti- tutes one of the largest sources of uncertainty in direct and indirect DM searches.
    [Show full text]