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.
Bibliographical noteFunding Information:
This work was supported by the National Science Foundation through the Center for Particle Astrophysics (cooperative agreement AST 91-20005), the National Aeronautics and Space Administration under grants NAGW-1062 and FD-NAGW-2121, the University of California, and previously the California Space Institute. We would like to thank O. Levy for his assistance with the flight preparation and the MSAM team for borrowed equipment during the flight campaign. The IRAS map used in the analysis was created by Skyview, maintained by Goddard Space Flight Center. N. F. was partially supported by Conselho Nacional de Desenvolvimento Científico e Tec-nológico, Brazil.
- Cosmic microwave background
- Cosmology: observations