The second measurement of anisotropy in the cosmic microwave background radiation at 0.°5 scales near the star μ Pegasi

M. A. Lim, A. C. Clapp, M. J. Devlin, N. Figueiredo, J. O. Gundersen, S. Hanany, V. V. Hristov, A. E. Lange, P. M. Lubin, P. R. Meinhold, P. L. Richards, J. W. Staren, G. F. Smoot, S. T. Tanaka

Research output: Contribution to journalArticle

35 Scopus citations

Abstract

During the fifth flight of the Microwave Anisotropy Experiment (MAX5), we revisited a region with significant dust emission near the star μ Pegasi. A 3.5 cm-1 low-frequency channel has been added since the previous measurement (Meinhold et al. 1993a). The data in each channel clearly show structure correlated with IRAS 100 μm dust emission. The spectrum of the structure in the 6, 9, and 14 cm-1 channels is described by Iv ∝ vβBv(Tdust), where β = 1.3 and Tdust = 19 K and Bv is the Planck function. However, this model predicts a smaller amplitude in the 3.5 cm-1 band than is observed. Considering only linear combinations of the data independent of the best-fit foreground spectrum for the three lower channels, we find an upper limit to CMBR fluctuations of ΔT/T = 〈Cll(l + 1)/2π〉1/2 ≤ 1.3 × 10-5 at the 95% confidence level. The result is for a flat-band power spectrum and does not include a 10% uncertainty in calibration. It is consistent with our previous observation in the region.

Original languageEnglish (US)
Pages (from-to)L69-L72
JournalAstrophysical Journal
Volume469
Issue number2 PART II
DOIs
StatePublished - Oct 1 1996

Keywords

  • Cosmic microwave background
  • Cosmology: observations

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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    Lim, M. A., Clapp, A. C., Devlin, M. J., Figueiredo, N., Gundersen, J. O., Hanany, S., Hristov, V. V., Lange, A. E., Lubin, P. M., Meinhold, P. R., Richards, P. L., Staren, J. W., Smoot, G. F., & Tanaka, S. T. (1996). The second measurement of anisotropy in the cosmic microwave background radiation at 0.°5 scales near the star μ Pegasi. Astrophysical Journal, 469(2 PART II), L69-L72. https://doi.org/10.1086/310276