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

Research output: Contribution to journal › Article › peer-review

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
Externally published	Yes

Keywords

Cosmic microwave background
Cosmology: observations

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1086/310276

Fingerprint Dive into the research topics of 'The second measurement of anisotropy in the cosmic microwave background radiation at 0.°5 scales near the star μ Pegasi'. Together they form a unique fingerprint.

Cite this

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 › peer-review

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.

@article{3ddd52afd8c24f9ea3694c3fd438d2eb,

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.}",

year = "1996",

month = oct,

day = "1",

doi = "10.1086/310276",

language = "English (US)",

volume = "469",

pages = "L69--L72",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "2 PART II",

}

TY - JOUR

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.

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

UR - http://www.scopus.com/inward/record.url?scp=4244190018&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=4244190018&partnerID=8YFLogxK

U2 - 10.1086/310276

DO - 10.1086/310276

M3 - Article

AN - SCOPUS:4244190018

VL - 469

SP - L69-L72

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 PART II

ER -