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Title:
The Anisotropy of the Microwave Background to l = 3500: Deep Field Observations with the Cosmic Background Imager
Authors:
Mason, B. S.; Pearson, T. J.; Readhead, A. C. S.; Shepherd, M. C.; Sievers, J.; Udomprasert, P. S.; Cartwright, J. K.; Farmer, A. J.; Padin, S.; Myers, S. T.; Bond, J. R.; Contaldi, C. R.; Pen, U.; Prunet, S.; Pogosyan, D.; Carlstrom, J. E.; Kovac, J.; Leitch, E. M.; Pryke, C.; Halverson, N. W.; Holzapfel, W. L.; Altamirano, P.; Bronfman, L.; Casassus, S.; May, J.; Joy, M.
Affiliation:
AA(Current address: National Radio Astronomy Observatory, P.O. Box 2, Green Bank, WV 24944.), AB(), AC(), AD(), AE(), AF(Owens Valley Radio Observatory, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125), AG(Owens Valley Radio Observatory, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125), AH(Owens Valley Radio Observatory, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125), AI(Owens Valley Radio Observatory, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125), AJ(National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801), AK(Canadian Institute for Theoretical Astrophysics, 60 St. George Street, Toronto, ON M5S 3H8, Canada), AL(Canadian Institute for Theoretical Astrophysics, 60 St. George Street, Toronto, ON M5S 3H8, Canada), AM(Canadian Institute for Theoretical Astrophysics, 60 St. George Street, Toronto, ON M5S 3H8, Canada), AN(Canadian Institute for Theoretical Astrophysics, 60 St. George Street, Toronto, ON M5S 3H8, Canada), AO(Avadh Bhatia Physics Laboratory, University of Alberta, Edmonton, AB T6G 2J1, Canada), AP(Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637), AQ(Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637), AR(Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637), AS(Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637), AT(Department of Physics, University of California, Berkeley, 366 Le Conte Hall, Berkeley, CA 94720-7300), AU(Department of Physics, University of California, Berkeley, 366 Le Conte Hall, Berkeley, CA 94720-7300), AV(Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile), AW(Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile), AX(Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile), AY(Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile), AZ(Department of Space Science, SD50, NASA Marshall Space Flight Center, Huntsville, AL 35812)
Publication:
The Astrophysical Journal, Volume 591, Issue 2, pp. 540-555. (ApJ Homepage)
Publication Date:
07/2003
Origin:
UCP
ApJ Keywords:
Cosmology: Cosmic Microwave Background, Cosmology: Observations
DOI:
10.1086/375507
Bibliographic Code:
2003ApJ...591..540M

Abstract

We report measurements of anisotropy in the cosmic microwave background radiation over the multipole range l~200-3500 with the Cosmic Background Imager based on deep observations of three fields. These results confirm the drop in power with increasing l first reported in earlier measurements with this instrument and extend the observations of this decline in power out to l~2000. The decline in power is consistent with the predicted damping of primary anisotropies. At larger multipoles, l=2000-3500, the power is 3.1 σ greater than standard models for intrinsic microwave background anisotropy in this multipole range and 3.5 σ greater than zero. This excess power is not consistent with expected levels of residual radio source contamination but, for σ8>~1, is consistent with predicted levels of a secondary Sunyaev-Zeldovich anisotropy. Further observations are necessary to confirm the level of this excess and, if confirmed, determine its origin.
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