Large Scale Structure: Basic Observations, Redshift Surveys, Biasing Structure Formation and Evolution from This (Δρ/Ρ ~ 10 -6) to This (Δρ/Ρ ~ 10 +2)
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Probing the Dark Flow Signal in WMAP 9Yr and PLANCK CMB Maps
Probing the Dark Flow signal in WMAP 9yr and PLANCK CMB Maps. Fernando Atrio-Barandela. Departamento de F´ısica Fundamental. Universidad de Salamanca. eml: [email protected] In collaboration with: H. Ebeling, D. Fixsen, A. Kashlinsky, D. Kocevski. Ibericos 2015 Aranjuez, March 30th - April 1st, 2015. 1 Summary. Introduction: The CMB dipole. Measuring Peculiar Velocities. Results with WMAP. Results with PLANCK (Planck Collaboration). Results with PLANCK (Our Analysis). Cosmological Implications and Conclusions. Ibericos 2015 Aranjuez, March 30th - April 1st, 2015. 2 Introduction: The CMB dipole. Ibericos 2015 Aranjuez, March 30th - April 1st, 2015. 3 The Cosmic Microwave Background. Monopole T=2.73K Dipole T=3mK Octupole O=33 K Planck Nominal Map at 353GHz Ibericos 2015 Aranjuez, March 30th - April 1st, 2015. 4 The CMB dipole. If density perturbations are adiabatic, generated during inflation, then the low order • multipoles verify: ℓ(ℓ + 1)C = const 2C = 12C = 12 1000(µK)2 D 70µ 1mK ℓ ⇒ 1 3 ∗ ⇒ ∼ ≪ Then, the dipole CAN NOT BE PRIMORDIAL. It is a Doppler effect due to the local motion of the Local Group with velocity 600km/s in the direction of l = 2700, b = 300. ∼ Ibericos 2015 Aranjuez, March 30th - April 1st, 2015. 5 The convergence of the CMB dipole. COMA VIRGO CENTAURUS HYDRA PERSEUS (Left) CMB dipole measured by COBE. (Right) Large Scale Structure and gas distribution in the Local Universe. What are the scales that contribute to the 600km/s peculiar velocity of the LG? ∼ Ibericos 2015 Aranjuez, March 30th - April 1st, 2015. 6 Bulk Flows. The zero order moment of the velocity field is the mean peculiar velocity of a sphere of radius R or bulk flow 1 V 2(R) = P (k)W 2(kR)dk P (k) = δ(k) 2. -
Fine-Tuning, Complexity, and Life in the Multiverse*
Fine-Tuning, Complexity, and Life in the Multiverse* Mario Livio Dept. of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA E-mail: [email protected] and Martin J. Rees Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UK E-mail: [email protected] Abstract The physical processes that determine the properties of our everyday world, and of the wider cosmos, are determined by some key numbers: the ‘constants’ of micro-physics and the parameters that describe the expanding universe in which we have emerged. We identify various steps in the emergence of stars, planets and life that are dependent on these fundamental numbers, and explore how these steps might have been changed — or completely prevented — if the numbers were different. We then outline some cosmological models where physical reality is vastly more extensive than the ‘universe’ that astronomers observe (perhaps even involving many ‘big bangs’) — which could perhaps encompass domains governed by different physics. Although the concept of a multiverse is still speculative, we argue that attempts to determine whether it exists constitute a genuinely scientific endeavor. If we indeed inhabit a multiverse, then we may have to accept that there can be no explanation other than anthropic reasoning for some features our world. _______________________ *Chapter for the book Consolidation of Fine Tuning 1 Introduction At their fundamental level, phenomena in our universe can be described by certain laws—the so-called “laws of nature” — and by the values of some three dozen parameters (e.g., [1]). Those parameters specify such physical quantities as the coupling constants of the weak and strong interactions in the Standard Model of particle physics, and the dark energy density, the baryon mass per photon, and the spatial curvature in cosmology. -
Cosmology Slides
Inhomogeneous cosmologies George Ellis, University of Cape Town 27th Texas Symposium on Relativistic Astrophyiscs Dallas, Texas Thursday 12th December 9h00-9h45 • The universe is inhomogeneous on all scales except the largest • This conclusion has often been resisted by theorists who have said it could not be so (e.g. walls and large scale motions) • Most of the universe is almost empty space, punctuated by very small very high density objects (e.g. solar system) • Very non-linear: / = 1030 in this room. Models in cosmology • Static: Einstein (1917), de Sitter (1917) • Spatially homogeneous and isotropic, evolving: - Friedmann (1922), Lemaitre (1927), Robertson-Walker, Tolman, Guth • Spatially homogeneous anisotropic (Bianchi/ Kantowski-Sachs) models: - Gödel, Schücking, Thorne, Misner, Collins and Hawking,Wainwright, … • Perturbed FLRW: Lifschitz, Hawking, Sachs and Wolfe, Peebles, Bardeen, Ellis and Bruni: structure formation (linear), CMB anisotropies, lensing Spherically symmetric inhomogeneous: • LTB: Lemaître, Tolman, Bondi, Silk, Krasinski, Celerier , Bolejko,…, • Szekeres (no symmetries): Sussman, Hellaby, Ishak, … • Swiss cheese: Einstein and Strauss, Schücking, Kantowski, Dyer,… • Lindquist and Wheeler: Perreira, Clifton, … • Black holes: Schwarzschild, Kerr The key observational point is that we can only observe on the past light cone (Hoyle, Schücking, Sachs) See the diagrams of our past light cone by Mark Whittle (Virginia) 5 Expand the spatial distances to see the causal structure: light cones at ±45o. Observable Geo Data Start of universe Particle Horizon (Rindler) Spacelike singularity (Penrose). 6 The cosmological principle The CP is the foundational assumption that the Universe obeys a cosmological law: It is necessarily spatially homogeneous and isotropic (Milne 1935, Bondi 1960) Thus a priori: geometry is Robertson-Walker Weaker form: the Copernican Principle: We do not live in a special place (Weinberg 1973). -
The Triple-Quasar Is an Optical Image of Milkyway, Andromeda and Triangulum Galaxies – Implies Expansion in the Direction of Dark Flow
The Triple-quasar is an optical image of Milkyway, Andromeda and Triangulum galaxies – implies expansion in the direction of Dark Flow Jose P Koshy [email protected] Abstract: Based on the concept that light follows a circular path of radius 2.5 billion light-years, here I show that the triple-quasar LBQS 1429-008 is the 10.5 billion years old image of 'Milkyway, Andromeda and Triangulum' galaxies. From this, the position of our galaxy at two different times can be ascertained, and the direction of expansion of the universe can be estimated. The 'surprise finding' is that the direction thus obtained is in agreement with the direction of so- called 'Dark flow', implying the possibility that the expansion is due to actual motion of bodies, and hence LCDM model is wrong. 1. Introduction: The standard cosmological model (LCDM) visualizes metric expansion of the universe. In such a model, the motion of galaxy clusters with respect to the cosmic microwave background should be randomly distributed in all directions. However, using WMAP data, Alexander Kashlinsky1 et al have found evidence for a possible non-random component in the motion of galaxy clusters; this is referred to as 'dark flow'. This implies the possibility that expansion is due to actual 'physical motion' of bodies. An alternate model, explained in my previous papers, visualizes expansion as a consequence of 'actual motion' of galaxy-clusters. Also, the model visualizes that light follows a 'circular path', and so the returning rays can create past images of bodies that have moved out. So, based on that model, it becomes possible to ascertain 'the direction' in which the universe in our region expands. -
Arxiv:1707.01004V1 [Astro-Ph.CO] 4 Jul 2017
July 5, 2017 0:15 WSPC/INSTRUCTION FILE coc2ijmpe International Journal of Modern Physics E c World Scientific Publishing Company Primordial Nucleosynthesis Alain Coc Centre de Sciences Nucl´eaires et de Sciences de la Mati`ere (CSNSM), CNRS/IN2P3, Univ. Paris-Sud, Universit´eParis–Saclay, Bˆatiment 104, F–91405 Orsay Campus, France [email protected] Elisabeth Vangioni Institut d’Astrophysique de Paris, UMR-7095 du CNRS, Universit´ePierre et Marie Curie, 98 bis bd Arago, 75014 Paris (France), Sorbonne Universit´es, Institut Lagrange de Paris, 98 bis bd Arago, 75014 Paris (France) [email protected] Received July 5, 2017 Revised Day Month Year Primordial nucleosynthesis, or big bang nucleosynthesis (BBN), is one of the three evi- dences for the big bang model, together with the expansion of the universe and the Cos- mic Microwave Background. There is a good global agreement over a range of nine orders of magnitude between abundances of 4He, D, 3He and 7Li deduced from observations, and calculated in primordial nucleosynthesis. However, there remains a yet–unexplained discrepancy of a factor ≈3, between the calculated and observed lithium primordial abundances, that has not been reduced, neither by recent nuclear physics experiments, nor by new observations. The precision in deuterium observations in cosmological clouds has recently improved dramatically, so that nuclear cross sections involved in deuterium BBN need to be known with similar precision. We will shortly discuss nuclear aspects re- lated to BBN of Li and D, BBN with non-standard neutron sources, and finally, improved sensitivity studies using Monte Carlo that can be used in other sites of nucleosynthesis. -
Astrophysics Notre Dame’S Partnership in the Large Binocular Telescope
NOTRE DAME ASTROPHYSICS NOTRE DAME’S PARTNERSHIP IN THE LARGE BINOCULAR TELESCOPE The Large Binocular Telescope (LBT) stands on carbon and oxygen are created, and the LBT will Mt. Graham in Arizona, at 10,700 feet above sea support our quest for understanding. level, and next to the 1.8-m Vatican Advanced Technology Telescope. The unique facility is Telescopes not only look at distant objects, actually two 8.4-m telescopes that act in tandem but also act as time machines. Because light to produce images unlike any seen before. The may travel for billions of years before being LBT has the equivalent collecting power of a captured by the LBT’s mirrors, the images 12-m and the resolution of a 22-m telescope, far reveal the Universe as it was long ago. One of better than any other telescope today. It is the the big mysteries uncovered by the Hubble forerunner of the next generation of ultra-large Space Telescope program is the existence of telescopes. fully formed galaxies in the early universe, much earlier than physicists predicted. Their formation The LBT has extraordinary capabilities. will be a key research program for the LBT and Its design allows it to directly observe distant Origins Institute faculty Dinshaw Balsara and stars systems and to actually see planets in the Christopher Howk, who aim to understand the systems. Its ability to measure very precise atomic dynamics that govern the formation of galaxies spectra even enables researchers to determine the and with them the beginnings of life. chemical makeup of the planets’ atmospheres. -
Cosmography of the Local Universe SDSS-III Map of the Universe
Cosmography of the Local Universe SDSS-III map of the universe Color = density (red=high) Tools of the Future: roBotic/piezo fiBer positioners AstroBot FiBer Positioners Collision-avoidance testing Echidna (for SuBaru FMOS) Las Campanas Redshift Survey The first survey to reach the quasi-homogeneous regime Large-scale structure within z<0.05, sliced in Galactic plane declination “Zone of Avoidance” 6dF Galaxy Survey, Jones et al. 2009 Large-scale structure within z<0.1, sliced in Galactic plane declination “Zone of Avoidance” 6dF Galaxy Survey, Jones et al. 2009 Southern Hemisphere, colored By redshift 6dF Galaxy Survey, Jones et al. 2009 SDSS-BOSS map of the universe Image credit: Jeremy Tinker and the SDSS-III collaBoration SDSS-III map of the universe Color = density (red=high) Millenium Simulation (2005) vs Galaxy Redshift Surveys Image Credit: Nina McCurdy and Joel Primack/University of California, Santa Cruz; Ralf Kaehler and Risa Wechsler/Stanford University; Klypin et al. 2011 Sloan Digital Sky Survey; Michael Busha/University of Zurich Trujillo-Gomez et al. 2011 Redshift-space distortion in the 2D correlation function of 6dFGS along line of sight on the sky Beutler et al. 2012 Matter power spectrum oBserved by SDSS (Tegmark et al. 2006) k-3 Solid red lines: linear theory (WMAP) Dashed red lines: nonlinear corrections Note we can push linear approx to a Bit further than k~0.02 h/Mpc Baryon acoustic peaks (analogous to CMB acoustic peaks; standard rulers) keq SDSS-BOSS map of the universe Color = distance (purple=far) Image credit: -
Structure Formation in a CDM Universe
Structure formation in a CDM Universe Thomas Quinn, University of Washington Greg Stinson, Charlotte Christensen, Alyson Brooks Ferah Munshi Fabio Governato, Andrew Pontzen, Chris Brook, James Wadsley Microwave Background Fluctuations Image courtesy NASA/WMAP Large Scale Clustering A well constrained cosmology ` Contents of the Universe Can it make one of these? Structure formation issues ● The substructure problem ● The angular momentum problem ● The cusp problem Light vs CDM structure Stars Gas Dark Matter The CDM Substructure Problem Moore et al 1998 Substructure down to 100 pc Stadel et al, 2009 Consequences for direct detection Afshordi etal 2010 Warm Dark Matter cold warm hot Constant Core Mass Strigari et al 2008 Light vs Mass Number density log(halo or galaxy mass) Simulations of Galaxy formation Guo e tal, 2010 Origin of Galaxy Spins ● Torques on the collapsing galaxy (Peebles, 1969; Ryden, 1988) λ ≡ L E1/2/GM5/2 ≈ 0.09 for galaxies Distribution of Halo Spins f(λ) Λ = LE1/2/GM5/2 Gardner, 2001 Angular momentum Problem Too few low-J baryons Van den Bosch 01 Bullock 01 Core/Cusps in Dwarfs Moore 1994 Warm DM doesn't help Moore et al 1999 Dwarf simulated to z=0 Stellar mass = 5e8 M sun` M = -16.8 i g - r = 0.53 V = 55 km/s rot R = 1 kpc d M /M = 2.5 HI * f = .3 f cosmic b b i band image Dwarf Light Profile Rotation Curve Resolution effects Low resolution: bad Low resolution star formation: worse Inner Profile Slopes vs Mass Governato, Zolotov etal 2012 Constant Core Masses Angular Momentum Outflows preferential remove low J baryons Simulation Results: Resolution and H2 Munshi, in prep. -
New Upper Limit on the Total Neutrino Mass from the 2 Degree Field Galaxy Redshift Survey
Swinburne Research Bank http://researchbank.swinburne.edu.au Elgary, O., et al. (2002). New upper limit on the total neutrino mass from the 2 Degree Field Galaxy Redshift Survey. Originally published in Physical Review Letters, 89(6). Available from: http://dx.doi.org/10.1103/PhysRevLett.89.061301 Copyright © 2002 The American Physical Society. This is the author’s version of the work, posted here with the permission of the publisher for your personal use. No further distribution is permitted. You may also be able to access the published version from your library. The definitive version is available at http://publish.aps.org/. Swinburne University of Technology | CRICOS Provider 00111D | swinburne.edu.au A new upper limit on the total neutrino mass from the 2dF Galaxy Redshift Survey Ø. Elgarøy1, O. Lahav1, W. J. Percival2, J. A. Peacock2, D. S. Madgwick1, S. L. Bridle1, C. M. Baugh3, I. K. Baldry4, J. Bland-Hawthorn5, T. Bridges5, R. Cannon5, S. Cole3, M. Colless6, C. Collins7, W. Couch8, G. Dalton9, R. De Propris8, S. P. Driver10, G. P. Efstathiou1, R. S. Ellis11, C. S. Frenk3, K. Glazebrook5, C. Jackson6, I. Lewis9, S. Lumsden12, S. Maddox13, P. Norberg3, B. A. Peterson6, W. Sutherland2, K. Taylor11 1 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 2 Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edingburgh EH9 3HJ, UK 3 Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK 4 Department of Physics & Astronomy, John Hopkins University, Baltimore, MD 21218-2686, USA 5 Anglo-Australian Observatory, P. -
The High Redshift Universe: Galaxies and the Intergalactic Medium
The High Redshift Universe: Galaxies and the Intergalactic Medium Koki Kakiichi M¨unchen2016 The High Redshift Universe: Galaxies and the Intergalactic Medium Koki Kakiichi Dissertation an der Fakult¨atf¨urPhysik der Ludwig{Maximilians{Universit¨at M¨unchen vorgelegt von Koki Kakiichi aus Komono, Mie, Japan M¨unchen, den 15 Juni 2016 Erstgutachter: Prof. Dr. Simon White Zweitgutachter: Prof. Dr. Jochen Weller Tag der m¨undlichen Pr¨ufung:Juli 2016 Contents Summary xiii 1 Extragalactic Astrophysics and Cosmology 1 1.1 Prologue . 1 1.2 Briefly Story about Reionization . 3 1.3 Foundation of Observational Cosmology . 3 1.4 Hierarchical Structure Formation . 5 1.5 Cosmological probes . 8 1.5.1 H0 measurement and the extragalactic distance scale . 8 1.5.2 Cosmic Microwave Background (CMB) . 10 1.5.3 Large-Scale Structure: galaxy surveys and Lyα forests . 11 1.6 Astrophysics of Galaxies and the IGM . 13 1.6.1 Physical processes in galaxies . 14 1.6.2 Physical processes in the IGM . 17 1.6.3 Radiation Hydrodynamics of Galaxies and the IGM . 20 1.7 Bridging theory and observations . 23 1.8 Observations of the High-Redshift Universe . 23 1.8.1 General demographics of galaxies . 23 1.8.2 Lyman-break galaxies, Lyα emitters, Lyα emitting galaxies . 26 1.8.3 Luminosity functions of LBGs and LAEs . 26 1.8.4 Lyα emission and absorption in LBGs: the physical state of high-z star forming galaxies . 27 1.8.5 Clustering properties of LBGs and LAEs: host dark matter haloes and galaxy environment . 30 1.8.6 Circum-/intergalactic gas environment of LBGs and LAEs . -
Week 5: More on Structure Formation
Week 5: More on Structure Formation Cosmology, Ay127, Spring 2008 April 23, 2008 1 Mass function (Press-Schechter theory) In CDM models, the power spectrum determines everything about structure in the Universe. In particular, it leads to what people refer to as “bottom-up” and/or “hierarchical clustering.” To begin, note that the power spectrum P (k), which decreases at large k (small wavelength) is psy- chologically inferior to the scaled power spectrum ∆2(k) = (1/2π2)k3P (k). This latter quantity is monotonically increasing with k, or with smaller wavelength, and thus represents what is going on physically a bit more intuitively. Equivalently, the variance σ2(M) of the mass distribution on scales of mean mass M is a monotonically decreasing function of M; the variance in the mass distribution is largest at the smallest scales and smallest at the largest scales. Either way, the density-perturbation amplitude is larger at smaller scales. It is therefore smaller structures that go nonlinear and undergo gravitational collapse earliest in the Universe. With time, larger and larger structures undergo gravitational collapse. Thus, the first objects to undergo gravitational collapse after recombination are probably globular-cluster–sized halos (although the halos won’t produce stars. As we will see in Week 8, the first dark-matter halos to undergo gravitational collapse and produce stars are probably 106 M halos at redshifts z 20. A typical L galaxy probably forms ∼ ⊙ ∼ ∗ at redshifts z 1, and at the current epoch, it is galaxy groups or poor clusters that are the largest ∼ mass scales currently undergoing gravitational collapse. -
Neutrino Cosmology
International Workshop on Astroparticle and High Energy Physics PROCEEDINGS Neutrino cosmology Julien Lesgourgues∗† LAPTH Annecy E-mail: [email protected] Abstract: I will briefly summarize the main effects of neutrinos in cosmology – in particular, on the Cosmic Microwave Background anisotropies and on the Large Scale Structure power spectrum. Then, I will present the constraints on neutrino parameters following from current experiments. 1. A powerful tool: cosmological perturbations The theory of cosmological perturbations has been developed mainly in the 70’s and 80’s, in order to explain the clustering of matter observed in the Large Scale Structure (LSS) of the Universe, and to predict the anisotropy distribution in the Cosmic Microwave Background (CMB). This theory has been confronted with observations with great success, and accounts perfectly for the most recent CMB data (the WMAP satellite, see Spergel et al. 2003 [1]) and LSS observations (the 2dF redshift survey, see Percival et al. 2003 [2]). LSS data gives a measurement of the two-point correlation function of matter pertur- bations in our Universe, which is related to the linear power spectrum predicted by the theory of cosmological perturbations on scales between 40 Mega-parsecs (smaller scales cor- respond to non-linear perturbations, because they were enhanced by gravitational collapse) and 600 Mega-parsecs (larger scales are difficult to observe because galaxies are too faint). On should keep in mind that the reconstruction of the power spectrum starting from a red- shift survey is complicated by many technical issues, like the correction of redshift–space distortions, and relies on strong assumptions concerning the light–to–mass biasing factor.