Determining Properties of LEGA-C Galaxies Through Spectral Star-Formation History Reconstruction
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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. -
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. -
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. -
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. -
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). -
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. -
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. -
A Derivation of Modified Newtonian Dynamics
Journal of The Korean Astronomical Society http://dx.doi.org/10.5303/JKAS.2013.46.2.93 46: 93 ∼ 96, 2013 April ISSN:1225-4614 c 2013 The Korean Astronomical Society. All Rights Reserved. http://jkas.kas.org A DERIVATION OF MODIFIED NEWTONIAN DYNAMICS Sascha Trippe Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea E-mail : [email protected] (Received February 14, 2013; Revised March 20, 2013; Accepted March 29, 2013) ABSTRACT Modified Newtonian Dynamics (MOND) is a possible solution for the missing mass problem in galac- tic dynamics; its predictions are in good agreement with observations in the limit of weak accelerations. However, MOND does not derive from a physical mechanism and does not make predictions on the transitional regime from Newtonian to modified dynamics; rather, empirical transition functions have to be constructed from the boundary conditions and comparisons with observations. I compare the formalism of classical MOND to the scaling law derived from a toy model of gravity based on virtual massive gravitons (the “graviton picture”) which I proposed recently. I conclude that MOND naturally derives from the “graviton picture” at least for the case of non-relativistic, highly symmetric dynamical systems. This suggests that – to first order – the “graviton picture” indeed provides a valid candidate for the physical mechanism behind MOND and gravity on galactic scales in general. Key words : Gravitation — Galaxies: kinematics and dynamics −10 −2 1. INTRODUCTION where x = ac/am, am ≈ 10 ms is Milgrom’s con- stant, and µ(x)isa transition function with the asymp- “ It is worth remembering that all of the discus- totic behavior µ(x) → 1 for x ≫ 1 and µ(x) → x for sion [on dark matter] so far has been based on x ≪ 1. -
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. -
The Contents of the Universe
Ay 127! The Contents of the Universe 0.5 % Stars and other visible stuff Supernovae alone ⇒ Accelerating expansion ⇒ Λ > 0 CMB alone ⇒ Flat universe ⇒ Λ > 0 Any two of SN, CMB, LSS ⇒ Dark energy ~70% Also in agreement with the age estimates (globular clusters, nucleocosmochronology, white dwarfs) Today’s Best Guess Universe Age: Best fit CMB model - consistent with ages of oldest stars t0 =13.82 ± 0.05 Gyr Hubble constant: CMB + HST Key Project to -1 -1 measure Cepheid distances H0 = 69 km s Mpc € Density of ordinary matter: CMB + comparison of nucleosynthesis with Lyman-a Ωbaryon = 0.04 € forest deuterium measurement Density of all forms of matter: Cluster dark matter estimate CMB power spectrum 0.31 € Ωmatter = Cosmological constant: Supernova data, CMB evidence Ω = 0.69 for a flat universe plus a low € Λ matter density € The Component Densities at z ~ 0, in critical density units, assuming h ≈ 0.7 Total matter/energy density: Ω0,tot ≈ 1.00 From CMB, and consistent with SNe, LSS From local dynamics and LSS, and Matter density: Ω0,m ≈ 0.31 consistent with SNe, CMB From cosmic nucleosynthesis, Baryon density: Ω0,b ≈ 0.045 and independently from CMB Luminous baryon density: Ω0,lum ≈ 0.005 From the census of luminous matter (stars, gas) Since: Ω0,tot > Ω0,m > Ω0,b > Ω0,lum There is baryonic dark matter There is non-baryonic dark matter There is dark energy The Luminosity Density Integrate galaxy luminosity function (obtained from large redshift surveys) to obtain the mean luminosity density at z ~ 0 8 3 SDSS, r band: ρL = (1.8 ± 0.2) 10 h70 L/Mpc 8 3 2dFGRS, b band: ρL = (1.4 ± 0.2) 10 h70 L/Mpc Luminosity To Mass Typical (M/L) ratios in the B band along the Hubble sequence, within the luminous portions of galaxies, are ~ 4 - 5 M/L This includes some dark matter - for pure stellar populations, (M/L) ratios should be slightly lower. -
Modified Newtonian Dynamics, an Introductory Review
Modified Newtonian Dynamics, an Introductory Review Riccardo Scarpa European Southern Observatory, Chile E-mail [email protected] Abstract. By the time, in 1937, the Swiss astronomer Zwicky measured the velocity dispersion of the Coma cluster of galaxies, astronomers somehow got acquainted with the idea that the universe is filled by some kind of dark matter. After almost a century of investigations, we have learned two things about dark matter, (i) it has to be non-baryonic -- that is, made of something new that interact with normal matter only by gravitation-- and, (ii) that its effects are observed in -8 -2 stellar systems when and only when their internal acceleration of gravity falls below a fix value a0=1.2×10 cm s . Being completely decoupled dark and normal matter can mix in any ratio to form the objects we see in the universe, and indeed observations show the relative content of dark matter to vary dramatically from object to object. This is in open contrast with point (ii). In fact, there is no reason why normal and dark matter should conspire to mix in just the right way for the mass discrepancy to appear always below a fixed acceleration. This systematic, more than anything else, tells us we might be facing a failure of the law of gravity in the weak field limit rather then the effects of dark matter. Thus, in an attempt to avoid the need for dark matter many modifications of the law of gravity have been proposed in the past decades. The most successful – and the only one that survived observational tests -- is the Modified Newtonian Dynamics. -
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.