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

doi:10.1086/310276

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

Physics and Astronomy (Twin Cities)

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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 I_v ∝ v^βB_v(T_dust), where β = 1.3 and T_dust = 19 K and B_v 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 = 〈C_ll(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 language	English (US)
Pages (from-to)	L69-L72
Journal	Astrophysical Journal
Volume	469
Issue number	2 PART II
DOIs	https://doi.org/10.1086/310276
State	Published - Oct 1 1996

Bibliographical note

Funding 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.

Keywords

Cosmic microwave background
Cosmology: observations

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10.1086/310276

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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

Lim, MA, Clapp, AC, Devlin, MJ, Figueiredo, N, Gundersen, JO, Hanany, S, Hristov, VV, Lange, AE, Lubin, PM, Meinhold, PR, Richards, PL, Staren, JW, Smoot, GF & Tanaka, ST 1996, 'The second measurement of anisotropy in the cosmic microwave background radiation at 0.°5 scales near the star μ Pegasi', Astrophysical Journal, vol. 469, no. 2 PART II, pp. L69-L72. https://doi.org/10.1086/310276

@article{13f7e107f49e4adea08705a9401303ed,

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

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.",

keywords = "Cosmic microwave background, Cosmology: observations",

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

note = "Funding 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 Cient{\'i}fico e Tec-nol{\'o}gico, Brazil.",

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doi = "10.1086/310276",

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T1 - The second measurement of anisotropy in the cosmic microwave background radiation at 0.°5 scales near the star μ Pegasi

AU - Lim, M. A.

AU - Clapp, A. C.

AU - Devlin, M. J.

AU - Figueiredo, N.

AU - Gundersen, J. O.

AU - Hanany, S.

AU - Hristov, V. V.

AU - Lange, A. E.

AU - Lubin, P. M.

AU - Meinhold, P. R.

AU - Richards, P. L.

AU - Staren, J. W.

AU - Smoot, G. F.

AU - Tanaka, S. T.

N1 - Funding 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.

PY - 1996/10/1

Y1 - 1996/10/1

N2 - 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.

AB - 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.

KW - Cosmic microwave background

KW - Cosmology: observations

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SP - L69-L72

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 PART II

ER -

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

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