The amplitude and spectral index of the large angular scale anisotropy in the cosmic microwave background radiation

Ken Ganga; Lyman Page; Edward Cheng; Stephan Meyer

doi:10.1086/187500

The amplitude and spectral index of the large angular scale anisotropy in the cosmic microwave background radiation

Ken Ganga, Lyman Page, Edward Cheng, Stephan Meyer

Research output: Contribution to journal › Article › peer-review

41 Scopus citations

Abstract

In many cosmological models, the large angular scale anisotropy in the cosmic microwave background is parameterized by a spectral index, n, and a quadrupolar amplitude, Q. For a Harrison-Peebles-Zel'dovich spectrum, n = 1. Using data from the Far Infrared Survey (FIRS) and a new statistical measure, a contour plot of the likelihood for cosmological models for which -1 < n < 3 and 0 ≤ Q ≤ 50 μK is obtained. Depending upon the details of the analysis, the maximum likelihood occurs at n between 0.8 and 1.4 and Q between 18 and 21 μK. Regardless of Q, the likelihood is always less than half its maximum for n < -0.4 and for n > 2.2, as it is for Q < 8 μK and Q > 44 μK.

Original language	English (US)
Pages (from-to)	L15-L18
Journal	Astrophysical Journal
Volume	432
Issue number	1 PART 2
DOIs	https://doi.org/10.1086/187500
State	Published - Sep 1 1994

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Cosmic microwave background

Access to Document

10.1086/187500

Fingerprint Dive into the research topics of 'The amplitude and spectral index of the large angular scale anisotropy in the cosmic microwave background radiation'. Together they form a unique fingerprint.

Cite this

@article{9efb2d430e174c96b6fb5ee03cb362c6,

title = "The amplitude and spectral index of the large angular scale anisotropy in the cosmic microwave background radiation",

abstract = "In many cosmological models, the large angular scale anisotropy in the cosmic microwave background is parameterized by a spectral index, n, and a quadrupolar amplitude, Q. For a Harrison-Peebles-Zel'dovich spectrum, n = 1. Using data from the Far Infrared Survey (FIRS) and a new statistical measure, a contour plot of the likelihood for cosmological models for which -1 < n < 3 and 0 ≤ Q ≤ 50 μK is obtained. Depending upon the details of the analysis, the maximum likelihood occurs at n between 0.8 and 1.4 and Q between 18 and 21 μK. Regardless of Q, the likelihood is always less than half its maximum for n < -0.4 and for n > 2.2, as it is for Q < 8 μK and Q > 44 μK.",

keywords = "Cosmic microwave background",

author = "Ken Ganga and Lyman Page and Edward Cheng and Stephan Meyer",

year = "1994",

month = sep,

day = "1",

doi = "10.1086/187500",

language = "English (US)",

volume = "432",

pages = "L15--L18",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "1 PART 2",

}

TY - JOUR

T1 - The amplitude and spectral index of the large angular scale anisotropy in the cosmic microwave background radiation

AU - Ganga, Ken

AU - Page, Lyman

AU - Cheng, Edward

AU - Meyer, Stephan

PY - 1994/9/1

Y1 - 1994/9/1

N2 - In many cosmological models, the large angular scale anisotropy in the cosmic microwave background is parameterized by a spectral index, n, and a quadrupolar amplitude, Q. For a Harrison-Peebles-Zel'dovich spectrum, n = 1. Using data from the Far Infrared Survey (FIRS) and a new statistical measure, a contour plot of the likelihood for cosmological models for which -1 < n < 3 and 0 ≤ Q ≤ 50 μK is obtained. Depending upon the details of the analysis, the maximum likelihood occurs at n between 0.8 and 1.4 and Q between 18 and 21 μK. Regardless of Q, the likelihood is always less than half its maximum for n < -0.4 and for n > 2.2, as it is for Q < 8 μK and Q > 44 μK.

AB - In many cosmological models, the large angular scale anisotropy in the cosmic microwave background is parameterized by a spectral index, n, and a quadrupolar amplitude, Q. For a Harrison-Peebles-Zel'dovich spectrum, n = 1. Using data from the Far Infrared Survey (FIRS) and a new statistical measure, a contour plot of the likelihood for cosmological models for which -1 < n < 3 and 0 ≤ Q ≤ 50 μK is obtained. Depending upon the details of the analysis, the maximum likelihood occurs at n between 0.8 and 1.4 and Q between 18 and 21 μK. Regardless of Q, the likelihood is always less than half its maximum for n < -0.4 and for n > 2.2, as it is for Q < 8 μK and Q > 44 μK.

KW - Cosmic microwave background

UR - http://www.scopus.com/inward/record.url?scp=12044255305&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=12044255305&partnerID=8YFLogxK

U2 - 10.1086/187500

DO - 10.1086/187500

M3 - Article

AN - SCOPUS:12044255305

VL - 432

SP - L15-L18

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1 PART 2

ER -