A measurement of the angular power spectrum of the microwave background made from the high Chilean Andes

E. Torbet; M. J. Devlin; W. B. Dorwart; T. Herbig; A. D. Miller; M. R. Nolta; L. Page; J. Puchalla; H. T. Tran

doi:10.1086/312197

A measurement of the angular power spectrum of the microwave background made from the high Chilean Andes

E. Torbet, M. J. Devlin, W. B. Dorwart, T. Herbig, A. D. Miller, M. R. Nolta, L. Page, J. Puchalla, H. T. Tran

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Abstract

We report on a measurement of the angular spectrum of the anisotropy of the microwave sky at 30 and 40 GHz between l = 50 and l = 200. The data, covering roughly 600 deg², support a rise in the angular spectrum to a maximum with δΤ₁ ≈ 85 μΚ at l = 200. We also give a 2 σ upper limit of δΤ₁ < 122 μΚ at l = 432 at 144 GHz. These results come from the first campaign of the Mobile Anisotropy Telescope on Cerro Toco, Chile. To assist in assessing the site, we present plots of the fluctuations in atmospheric emission at 30 and 144 GHz.

Original language	English (US)
Pages (from-to)	L79-L82
Journal	Astrophysical Journal
Volume	521
Issue number	2 PART 2
DOIs	https://doi.org/10.1086/312197
State	Published - Aug 20 1999

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Atmospheric effects
Cosmic microwave background
Cosmology: observations

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10.1086/312197

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title = "A measurement of the angular power spectrum of the microwave background made from the high Chilean Andes",

abstract = "We report on a measurement of the angular spectrum of the anisotropy of the microwave sky at 30 and 40 GHz between l = 50 and l = 200. The data, covering roughly 600 deg2, support a rise in the angular spectrum to a maximum with δΤ1 ≈ 85 μΚ at l = 200. We also give a 2 σ upper limit of δΤ1 < 122 μΚ at l = 432 at 144 GHz. These results come from the first campaign of the Mobile Anisotropy Telescope on Cerro Toco, Chile. To assist in assessing the site, we present plots of the fluctuations in atmospheric emission at 30 and 144 GHz.",

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

author = "E. Torbet and Devlin, {M. J.} and Dorwart, {W. B.} and T. Herbig and Miller, {A. D.} and Nolta, {M. R.} and L. Page and J. Puchalla and Tran, {H. T.}",

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doi = "10.1086/312197",

language = "English (US)",

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T1 - A measurement of the angular power spectrum of the microwave background made from the high Chilean Andes

AU - Torbet, E.

AU - Devlin, M. J.

AU - Dorwart, W. B.

AU - Herbig, T.

AU - Miller, A. D.

AU - Nolta, M. R.

AU - Page, L.

AU - Puchalla, J.

AU - Tran, H. T.

PY - 1999/8/20

Y1 - 1999/8/20

N2 - We report on a measurement of the angular spectrum of the anisotropy of the microwave sky at 30 and 40 GHz between l = 50 and l = 200. The data, covering roughly 600 deg2, support a rise in the angular spectrum to a maximum with δΤ1 ≈ 85 μΚ at l = 200. We also give a 2 σ upper limit of δΤ1 < 122 μΚ at l = 432 at 144 GHz. These results come from the first campaign of the Mobile Anisotropy Telescope on Cerro Toco, Chile. To assist in assessing the site, we present plots of the fluctuations in atmospheric emission at 30 and 144 GHz.

AB - We report on a measurement of the angular spectrum of the anisotropy of the microwave sky at 30 and 40 GHz between l = 50 and l = 200. The data, covering roughly 600 deg2, support a rise in the angular spectrum to a maximum with δΤ1 ≈ 85 μΚ at l = 200. We also give a 2 σ upper limit of δΤ1 < 122 μΚ at l = 432 at 144 GHz. These results come from the first campaign of the Mobile Anisotropy Telescope on Cerro Toco, Chile. To assist in assessing the site, we present plots of the fluctuations in atmospheric emission at 30 and 144 GHz.

KW - Atmospheric effects

KW - Cosmic microwave background

KW - Cosmology: observations

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JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 PART 2

ER -

A measurement of the angular power spectrum of the microwave background made from the high Chilean Andes

Abstract

All Science Journal Classification (ASJC) codes

Keywords

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