Anisotropy in the cosmic microwave background at degree angular scales: Python V results

K. Coble; M. Dragovan; J. Kovac; N. W. Halverson; W. L. Holzapfel; L. Knox; S. Dodelson; K. Ganga; D. Alvarez; J. B. Peterson; G. Griffin; M. Newcomb; K. Miller; S. R. Platt; G. Novak

doi:10.1086/312093

Anisotropy in the cosmic microwave background at degree angular scales: Python V results

K. Coble^*, M. Dragovan, J. Kovac, N. W. Halverson, W. L. Holzapfel, L. Knox, S. Dodelson, K. Ganga, D. Alvarez, J. B. Peterson, G. Griffin, M. Newcomb, K. Miller, S. R. Platt, G. Novak

^*Corresponding author for this work

Physics and Astronomy

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

43 Scopus citations

Abstract

Observations of the microwave sky using the Python telescope in its fifth season of operation at the Amundsen-Scott South Pole Station in Antarctica are presented. The system consists of a 0.75 m off-axis telescope instrumented with a HEMT amplifier-based radiometer having continuum sensitivity from 37 to 45 GHz in two frequency bands. With a 0°.91 × 1°.02 beam, the instrument fully sampled 598 deg² of sky, including fields measured during the previous four seasons of Python observations. Interpreting the observed fluctuations as anisotropy in the cosmic microwave background, we place constraints on the angular power spectrum of fluctuations in eight multipole bands up to l ∼ 260. The observed spectrum is consistent with both the COBE experiment and previous Python results. There is no significant contamination from known foregrounds. The results show a discernible rise in the angular power spectrum from large (l ∼ 40) to small (l ∼ 200) angular scales. The shape of the observed power spectrum is not a simple linear rise, but has a sharply increasing slope starting at l ∼ 150.

Original language	English (US)
Pages (from-to)	L5-L8
Journal	Astrophysical Journal
Volume	519
Issue number	1 PART 2
DOIs	https://doi.org/10.1086/312093
State	Published - Jul 1 1999

Funding

We would like to thank Bharat Ratra for helpful conversations and for aiding us in checking our window functions. This work was supported by the James S. McDonnell Foundation, PYI grant NSF AST 90-57089, and the NSF under a cooperative agreement with the Center for Astrophysical Research in Antarctica (CARA), grant NSF OPP 89-20223. CARA is an NSF Science and Technology Center. The work of S. D. was supported by NASA grant NAG5-7092 (in addition to the Department of Energy). K. G. acknowledges support from NASA ADP grant NASA-1260. K. C. is supported by NASA NGT 5-19.

Keywords

Cosmic microwave background
Cosmology: observations

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1086/312093

Cite this

Coble, K., Dragovan, M., Kovac, J., Halverson, N. W., Holzapfel, W. L., Knox, L., Dodelson, S., Ganga, K., Alvarez, D., Peterson, J. B., Griffin, G., Newcomb, M., Miller, K., Platt, S. R., & Novak, G. (1999). Anisotropy in the cosmic microwave background at degree angular scales: Python V results. Astrophysical Journal, 519(1 PART 2), L5-L8. https://doi.org/10.1086/312093

@article{384a4dfcc5f14ebf8ec1b776aac44249,

title = "Anisotropy in the cosmic microwave background at degree angular scales: Python V results",

abstract = "Observations of the microwave sky using the Python telescope in its fifth season of operation at the Amundsen-Scott South Pole Station in Antarctica are presented. The system consists of a 0.75 m off-axis telescope instrumented with a HEMT amplifier-based radiometer having continuum sensitivity from 37 to 45 GHz in two frequency bands. With a 0°.91 × 1°.02 beam, the instrument fully sampled 598 deg2 of sky, including fields measured during the previous four seasons of Python observations. Interpreting the observed fluctuations as anisotropy in the cosmic microwave background, we place constraints on the angular power spectrum of fluctuations in eight multipole bands up to l ∼ 260. The observed spectrum is consistent with both the COBE experiment and previous Python results. There is no significant contamination from known foregrounds. The results show a discernible rise in the angular power spectrum from large (l ∼ 40) to small (l ∼ 200) angular scales. The shape of the observed power spectrum is not a simple linear rise, but has a sharply increasing slope starting at l ∼ 150.",

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

author = "K. Coble and M. Dragovan and J. Kovac and Halverson, {N. W.} and Holzapfel, {W. L.} and L. Knox and S. Dodelson and K. Ganga and D. Alvarez and Peterson, {J. B.} and G. Griffin and M. Newcomb and K. Miller and Platt, {S. R.} and G. Novak",

note = "Funding Information: We would like to thank Bharat Ratra for helpful conversations and for aiding us in checking our window functions. This work was supported by the James S. McDonnell Foundation, PYI grant NSF AST 90-57089, and the NSF under a cooperative agreement with the Center for Astrophysical Research in Antarctica (CARA), grant NSF OPP 89-20223. CARA is an NSF Science and Technology Center. The work of S. D. was supported by NASA grant NAG5-7092 (in addition to the Department of Energy). K. G. acknowledges support from NASA ADP grant NASA-1260. K. C. is supported by NASA NGT 5-19.",

year = "1999",

month = jul,

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doi = "10.1086/312093",

language = "English (US)",

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T2 - Python V results

AU - Coble, K.

AU - Dragovan, M.

AU - Kovac, J.

AU - Halverson, N. W.

AU - Holzapfel, W. L.

AU - Knox, L.

AU - Dodelson, S.

AU - Ganga, K.

AU - Alvarez, D.

AU - Peterson, J. B.

AU - Griffin, G.

AU - Newcomb, M.

AU - Miller, K.

AU - Platt, S. R.

AU - Novak, G.

N1 - Funding Information: We would like to thank Bharat Ratra for helpful conversations and for aiding us in checking our window functions. This work was supported by the James S. McDonnell Foundation, PYI grant NSF AST 90-57089, and the NSF under a cooperative agreement with the Center for Astrophysical Research in Antarctica (CARA), grant NSF OPP 89-20223. CARA is an NSF Science and Technology Center. The work of S. D. was supported by NASA grant NAG5-7092 (in addition to the Department of Energy). K. G. acknowledges support from NASA ADP grant NASA-1260. K. C. is supported by NASA NGT 5-19.

PY - 1999/7/1

Y1 - 1999/7/1

N2 - Observations of the microwave sky using the Python telescope in its fifth season of operation at the Amundsen-Scott South Pole Station in Antarctica are presented. The system consists of a 0.75 m off-axis telescope instrumented with a HEMT amplifier-based radiometer having continuum sensitivity from 37 to 45 GHz in two frequency bands. With a 0°.91 × 1°.02 beam, the instrument fully sampled 598 deg2 of sky, including fields measured during the previous four seasons of Python observations. Interpreting the observed fluctuations as anisotropy in the cosmic microwave background, we place constraints on the angular power spectrum of fluctuations in eight multipole bands up to l ∼ 260. The observed spectrum is consistent with both the COBE experiment and previous Python results. There is no significant contamination from known foregrounds. The results show a discernible rise in the angular power spectrum from large (l ∼ 40) to small (l ∼ 200) angular scales. The shape of the observed power spectrum is not a simple linear rise, but has a sharply increasing slope starting at l ∼ 150.

AB - Observations of the microwave sky using the Python telescope in its fifth season of operation at the Amundsen-Scott South Pole Station in Antarctica are presented. The system consists of a 0.75 m off-axis telescope instrumented with a HEMT amplifier-based radiometer having continuum sensitivity from 37 to 45 GHz in two frequency bands. With a 0°.91 × 1°.02 beam, the instrument fully sampled 598 deg2 of sky, including fields measured during the previous four seasons of Python observations. Interpreting the observed fluctuations as anisotropy in the cosmic microwave background, we place constraints on the angular power spectrum of fluctuations in eight multipole bands up to l ∼ 260. The observed spectrum is consistent with both the COBE experiment and previous Python results. There is no significant contamination from known foregrounds. The results show a discernible rise in the angular power spectrum from large (l ∼ 40) to small (l ∼ 200) angular scales. The shape of the observed power spectrum is not a simple linear rise, but has a sharply increasing slope starting at l ∼ 150.

KW - Cosmic microwave background

KW - Cosmology: observations

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JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART 2

ER -

Anisotropy in the cosmic microwave background at degree angular scales: Python V results

Abstract

Funding

Keywords

ASJC Scopus subject areas

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