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

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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 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

Keywords

Cosmic microwave background
Cosmology: observations

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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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

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

In: Astrophysical Journal, Vol. 469, No. 2 PART II, 01.10.1996, p. L69-L72.

Research output: Contribution to journal › Article

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

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. / The second measurement of anisotropy in the cosmic microwave background radiation at 0.°5 scales near the star μ Pegasi. In: Astrophysical Journal. 1996 ; Vol. 469, No. 2 PART II. pp. L69-L72.

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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 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.",

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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.}",

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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.

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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.

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