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Future radio observations of the high redshift universe

Future radio observations of the high redshift universe

Future radio observations of the high redshift universe. Open Questions in Cosmology Munich Aug 22-26 2005 Ron Ekers CSIRO. Overview of new facilities at radio wavelengths. Many other talks on mm and submm results so I will concentrate on cm and m wavelengths ie freq < 30GHz

By aimee
(148 views)

How can CMB help constraining dark energy?

How can CMB help constraining dark energy?

How can CMB help constraining dark energy?. Licia Verde ICREA & Institute of space Sciences (ICE CSIC-IEEC). The standard cosmological model.  CDM model. . Spatially flat Universe. Power-law, primordial power spectrum. Only 6 parameters: WMAP5yr analysis. recombination.

By vartouhi
(93 views)

Future radio observations of the high redshift universe

Future radio observations of the high redshift universe

Future radio observations of the high redshift universe. Open Questions in Cosmology Munich Aug 22-26 2005 Ron Ekers CSIRO. Overview of new facilities at radio wavelengths. Many other talks on mm and submm results so I will concentrate on cm and m wavelengths ie freq < 30GHz

By flann
(113 views)

Lensing of the CMB

Lensing of the CMB

Lensing of the CMB. Antony Lewis Institute of Astronomy, Cambridge http://cosmologist.info/. Review ref: Lewis, Challinor , Phys. Rep: astro-ph/0601594. Evolution of the universe. Opaque. Transparent. Hu & White, Sci. Am., 290 44 (2004).

By danelle
(91 views)

Measurements of Cosmological Parameters

Measurements of Cosmological Parameters

Measurements of Cosmological Parameters. Amedeo Balbi Dipartimento di Fisica & INFN Università di Roma “Tor Vergata”. Background Cosmology. Expanding universe, described by Friedmann equation:. Perturbations & Inflation.

By lise
(84 views)

Steven T. Myers

Steven T. Myers

Cosmology: The effect of cosmological parameters on the angular power spectrum of the Cosmic Microwave Background. Steven T. Myers. University of Bologna and the National Radio Astronomy Observatory – Socorro, NM. The Standard Model. THE PILLARS OF INFLATION

By aliya
(130 views)

Dark Energy and Cosmic Sound

Dark Energy and Cosmic Sound

Dark Energy and Cosmic Sound. Daniel Eisenstein (University of Arizona) Michael Blanton, David Hogg, Bob Nichol, Roman Scoccimarro, Ryan Scranton, Hee-Jong Seo , Max Tegmark, Martin White, Idit Zehavi, Zheng Zheng, and the SDSS. Outline. Baryon acoustic oscillations as a standard ruler.

By hiroko
(125 views)

CMB acoustic peaks

CMB acoustic peaks

CMB acoustic peaks. Potential fluctuations broken up by mode. hill. well. r, or time. Fluid oscillations in a potential well. Maximum fluid rarification. Maximum velocity – maximum contribution to the Doppler term. Maximum fluid compression. Graphic – Wayne Hu.

By burke
(91 views)

CMB acoustic peaks

CMB acoustic peaks

CMB acoustic peaks. 3 rd acoustic peak fluid compression in potential wells. Potential fluctuations broken up by mode. hill. well. time. 2 nd acoustic peak fluid compression in potential hills. 1 st acoustic peak fluid compression in potential wells.

By merrill-donaldson
(100 views)

Dark Energy and Cosmic Sound

Dark Energy and Cosmic Sound

Dark Energy and Cosmic Sound. Daniel Eisenstein (University of Arizona) Michael Blanton, David Hogg, Bob Nichol, Nikhil Padmanabhan, Will Percival, David Schlegel, Roman Scoccimarro, Ryan Scranton, Hee-Jong Seo, Ed Sirko, David Spergel, Max Tegmark, Martin White, Idit Zehavi, and the SDSS.

By pburleson
(1 views)


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