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 | |
| State | Published - Sep 1 1994 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Keywords
- Cosmic microwave background
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Ganga, K., Page, L., Cheng, E., & Meyer, S. (1994). The amplitude and spectral index of the large angular scale anisotropy in the cosmic microwave background radiation. Astrophysical Journal, 432(1 PART 2), L15-L18. https://doi.org/10.1086/187500