Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:astro-ph/0402359)
· References in the article
· Citations to the Article (302) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· Also-Read Articles (Reads History)
· HEP/Spires Information
·
· Translate This Page
Title:
Extended Mosaic Observations with the Cosmic Background Imager
Authors:
Readhead, A. C. S.; Mason, B. S.; Contaldi, C. R.; Pearson, T. J.; Bond, J. R.; Myers, S. T.; Padin, S.; Sievers, J. L.; Cartwright, J. K.; Shepherd, M. C.; Pogosyan, D.; Prunet, S.; Altamirano, P.; Bustos, R.; Bronfman, L.; Casassus, S.; Holzapfel, W. L.; May, J.; Pen, U.-L.; Torres, S.; Udomprasert, P. S.
Affiliation:
AA(Owens Valley Radio Observatory, California Institute of Technology, Pasadena, CA 91125.), AB(National Radio Astronomy Observatory, Green Bank, WV 24944.), AC(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, Ontario, M5S 3H8, Canada.), AD(Owens Valley Radio Observatory, California Institute of Technology, Pasadena, CA 91125.), AE(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, Ontario, M5S 3H8, Canada.), AF(National Radio Astronomy Observatory, Socorro, NM 87801.), AG(Owens Valley Radio Observatory, California Institute of Technology, Pasadena, CA 91125; University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637.), AH(Owens Valley Radio Observatory, California Institute of Technology, Pasadena, CA 91125; Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, Ontario, M5S 3H8, Canada.), AI(Owens Valley Radio Observatory, California Institute of Technology, Pasadena, CA 91125; University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637.), AJ(Owens Valley Radio Observatory, California Institute of Technology, Pasadena, CA 91125.), AK(Department of Physics, University of Alberta, Edmonton, Alberta T6G 2J1, Canada; Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, Ontario, M5S 3H8, Canada.), AL(Institut d'astrophysique de Paris, 98bis, Boulevard Arago, 75014 Paris, France), AM(Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile.), AN(Departamento de Ingeniería Eléctrica, Universidad de Concepción, Casilla 160-C, Concepción, Chile.), AO(Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile.), AP(Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile.), AQ(University of California, 366 LeConte Hall, Berkeley, CA 94720-7300.), AR(Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile.), AS(Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, Ontario, M5S 3H8, Canada.), AT(Departamento de Ingeniería Eléctrica, Universidad de Concepción, Casilla 160-C, Concepción, Chile.), AU(Owens Valley Radio Observatory, California Institute of Technology, Pasadena, CA 91125.)
Publication:
The Astrophysical Journal, Volume 609, Issue 2, pp. 498-512. (ApJ Homepage)
Publication Date:
07/2004
Origin:
UCP
Astronomy Keywords:
Cosmology: Cosmic Microwave Background, Cosmology: Cosmological Parameters, Cosmology: Observations
DOI:
10.1086/421105
Bibliographic Code:
2004ApJ...609..498R

Abstract

Two years of microwave background observations with the Cosmic Background Imager (CBI) have been combined to give a sensitive, high-resolution angular power spectrum over the range 400<l<3500. This power spectrum has been referenced to a more accurate overall calibration derived from the Wilkinson Microwave Anisotropy Probe (WMAP). The data cover 90 deg 2, including three pointings targeted for deep observations. The uncertainty on the l>2000 power previously seen with the CBI is reduced. Under the assumption that any signal in excess of the primary anisotropy is due to a secondary Sunyaev-Zeldovich anisotropy in distant galaxy clusters, we use CBI, Arcminute Cosmology Bolometer Array Receiver, and Berkeley-Illinois-Maryland Association array data to place a constraint on the present-day rms mass fluctuation on 8 h-1 Mpc scales, σ8. We present the results of a cosmological parameter analysis on the l<2000 primary anisotropy data that show significant improvements in the parameters as compared to WMAP alone, and we explore the role of the small-scale cosmic microwave background data in breaking parameter degeneracies.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

   


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints