PPT-Size and Scale of the Universe

SIZE and Scale Of The Universe What is your Cosmic Address Size and Scale of the Universe Street City State Country Continent Hemisphere Planet Orbit Star . Getting a big picture of the universe as a whole is a difficult challenge for professional astronomers as well as for students but its a challenge that has occupied humanity for ages To understand the vast ranges of scale of cosmic systems the stu 574175745957376574415744257455574615746057376573935739757392573765745157449574525745557453574455746057445574585745957376573845745557458573765740157395573765745357449574525745257449574555745457376574535744957452574455745957385 57424574415745857460574 ©2013 Michael J. Rosenfeld. Draft date: 1/14/2013. The sample frame, or sample universe, is the data that our sample is drawn from. In the case of the March, 2000 CPS, the sample universe includes all people residing in the US in March, 2000, who were not living in institutional settings. This sample frame has N members.. Lecture . 10; . May . 14 2013. Previously… on astro-2. If the universe is homogenous and isotropic and correctly described by General Relativity:. At any given time the universe is a 3D space. It could be open/close/flat. 26: . Sex, Religion, and Politics. University of Virginia . cs1120 Fall 2009. David Evans. Science’s . Endless Golden Age. . “If you’re going to use your computer to simulate some phenomenon in the universe, then it only becomes interesting if you change the scale of that phenomenon by at least a factor of 10. … For a 3D simulation, an increase by a factor of 10 in each of the three dimensions increases your volume by a factor of 1000.”. . Anthony Lasenby. Astrophysics Group. Cavendish Laboratory. Cambridge, UK. a.n.lasenby@mrao.cam.ac.uk. www.mrao.cam.ac.uk/~clifford. Overview. Want to share two recent exciting developments. Recent progress in cosmology. ur U. niverse and the . Effects of. . I. nhomogeneities. Akihiro. 　. Ishibashi. 　. RESCEU Symposium . . Nov. 14. th. 2008. Cosmophysics. IPNS KEK. 　. Introduction. Distant . SNe-Ia. & Large scale structure. Tarun Souradeep. I.U.C.A.A. .. Cosmology . IUCAA . VSP program. (. May 18-22, . 2012). Lec. . . 4:. Current frontiers. Mildly Perturbed universe at z=1100. Present universe at z=0. Taking a close look at the . Statue of Liberty. Statue of Liberty . She is big!. She weighs 450,000 pounds. Gift from France in late 1800’s. 154 steps from pedestal to head of statue. It was apparently much flatter in the past:. Inflation!. For definiteness, pick . g. eff. =200 and . k. B. T. = 3. . 10. 15. . GeV. You should memorize this value to about 54 digits or so. How did it happen to be so close to 1?. the Universe. The Uniform Temperature of the Early Universe. The brighter and darker spots in the microwave background correspond to hotter and cooler areas in the universe (at an age of 400,000 years). However, the hotter spots are only a tiny bit hotter than the cooler spots. So all . Wenting . Wang. Le Xu. Indranil Gupta. Department of Computer Science, University of Illinois, Urbana Champaign . 1. Scale up VS. Scale out. A dilemma for cloud application users: scale up or scale out? . Lecture 2; . April 9 2013. Previously.. On Astro-2. The goal of cosmology is to understand how the universe formed and evolved.. How can we build a theory of the universe valid at all times in every place? . Chapter 21. How does distance affect an image?. Telescope- device that makes an object in the sky appear closer.. Revolutionized astronomy (study of space)- allowed them to see objects in space for first time..