PDF-4 Probes of Dark Energy:

Cerro Tololo InterAmerican Observatory Blanco 4meter telescopeFirst light Sept 12 2012Survey 20132018 525 nightsDECam 570 Mpix 3 deg2 FOV griZY. Josh Frieman. Fermilab. and the University of . Chicago. Astronomy 41100. Lecture 2, Oct. 15, 2010. DES Collaboration Meeting. 2. Go to:. http://astro.fnal.gov/desfall2010/Home.html. Science Working group meetings on Tuesday.. This . powerpoint. will show you the basics of dark matter and dark energy . Their place in the universe . By Jordan . Ilori. . DARK MATTER. Dark matter is a type of matter hypothesized in astronomy and cosmology to account for a large part of the mass that appears to be missing from the universe. Dark matter cannot be seen directly with telescopes; evidently it neither emits nor absorbs light or other electromagnetic radiation at any significant level. Instead, the existence and properties of dark matter are inferred from its gravitational effects on visible matter, radiation, and the large-scale structure of the universe. According to the Planck mission team, and based on the standard model of cosmology, the total mass–energy of the known universe contains 4.9% ordinary matter, 26.8% dark matter and 68.3% dark energy. Thus, dark matter is estimated to constitute 84.5% of the total matter in the universe and 26.8% of the total content of the universe.. :. Dark Matter & Dark Energy. WWK: Students will understand the theories of Dark Matter & Dark Energy and how they’re thought to affect the Universe. .. Dark Matter. Dark Matter . - . matter that influences the evolution of the universe . Jon Coleman, Royal Society Research Fellow . To detect and measure effects of Dark Energy density or any dark contents of the vacuum (DCV) . 2. Many thanks to the support of the:. Liverpool Particle Physics Group. Martin Kunz. University of . Geneva & AIMS South Africa. outline. what is the problem?. . dark energy theory. action based models. phenomenological approach. observations. simple principles. current constraints from Planck+. Observations. Josh . Frieman. DES Project Director. Fermilab. and the University of Chicago. Science with a Wide-. Field Infrared Telescope in Space. Pasadena, February. 2012. 2. 2011 Nobel Prize in Physics. Thomas Krühler (DARK). Thanks to J. . Fynbo. , D. . Malesani. , J. . Hjorth. ,. J. Greiner, D. A. . Kann. , D. . Perley. , N. . Tanvir. , . S. . Klose. and many others. Very High Energy Phenomena in the . direct dark matter detection. S. Moriyama . Institute for Cosmic Ray Research, University of Tokyo. Oct. 8. th. , 2011 @ FPUA2011, Okayama, Japan. Principle of direct detection in Lab.. Dark Energy and Dark Matter. Prof. Lawrence Wiencke. Department of Physics Engineering. Colorado School of Mines. Nov 9 2011. The Dark . Side. 95% of the. Universe Is Dark!. Energy budget of Universe. Josh Frieman. Fermilab. and the University of . Chicago. Astronomy 41100. Lecture 2, Oct. 15, 2010. DES Collaboration Meeting. 2. Go to:. http://astro.fnal.gov/desfall2010/Home.html. Science Working group meetings on Tuesday.. Expansion of the Universe. Early 1990’s – Universal expansion expected to slow. . - Universe is full of matter, and gravity pulls matter together. 1998 – Hubble Space Telescope observations show otherwise. VBC-321. Animal Biotechnology. A . probe. is a nucleic acid which has been . labeled. i.e., chemically modified in some way which allows it and hence anything it hybridizes to, to be detected.. There are three major types of probe: . Two types of non-radioactive labeling are performed- direct or indirect. Direct: Probes that are directly conjugated to a dye or an enzyme, which . generates the detection signal. Often such system involve incorporation of modified nucleotide containing a chemical group which can fluoresce when exposed to light of a certain wavelength. . Dynamics. of. FRWL Universes. . Dynamics. FRW Universe. Friedmann-Robertson-Walker-Lemaitre Universe. . Cosmic Constituents:. Evolving Energy Density . . FRW Energy Equation. To infer the evolving energy density .