Anisotropy in the Cosmic Microwave Background at Degree Angular Scales: Python V Results
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...
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ftdatacite:10.48550/arxiv.astro-ph/9902195 2023-05-15T13:24:26+02:00 Anisotropy in the Cosmic Microwave Background at Degree Angular Scales: Python V Results 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 https://dx.doi.org/10.48550/arxiv.astro-ph/9902195 https://arxiv.org/abs/astro-ph/9902195 unknown arXiv https://dx.doi.org/10.1086/312093 Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ Astrophysics astro-ph FOS Physical sciences article-journal Article ScholarlyArticle Text 1999 ftdatacite https://doi.org/10.48550/arxiv.astro-ph/9902195 https://doi.org/10.1086/312093 2022-04-01T17:19:08Z 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 37-45 GHz in two frequency bands. With a 0.91 deg x 1.02 deg beam the instrument fully sampled 598 deg^2 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. : 5 pages Text Amundsen-Scott Antarc* Antarctica South pole South pole DataCite Metadata Store (German National Library of Science and Technology) South Pole Amundsen-Scott ENVELOPE(0.000,0.000,-90.000,-90.000) Amundsen Scott South Pole Station ENVELOPE(0.000,0.000,-90.000,-90.000) Amundsen-Scott South Pole Station ENVELOPE(139.273,139.273,-89.998,-89.998) |
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Open Polar |
collection |
DataCite Metadata Store (German National Library of Science and Technology) |
op_collection_id |
ftdatacite |
language |
unknown |
topic |
Astrophysics astro-ph FOS Physical sciences |
spellingShingle |
Astrophysics astro-ph FOS Physical sciences 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. Anisotropy in the Cosmic Microwave Background at Degree Angular Scales: Python V Results |
topic_facet |
Astrophysics astro-ph FOS Physical sciences |
description |
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 37-45 GHz in two frequency bands. With a 0.91 deg x 1.02 deg beam the instrument fully sampled 598 deg^2 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. : 5 pages |
format |
Text |
author |
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. |
author_facet |
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. |
author_sort |
Coble, K. |
title |
Anisotropy in the Cosmic Microwave Background at Degree Angular Scales: Python V Results |
title_short |
Anisotropy in the Cosmic Microwave Background at Degree Angular Scales: Python V Results |
title_full |
Anisotropy in the Cosmic Microwave Background at Degree Angular Scales: Python V Results |
title_fullStr |
Anisotropy in the Cosmic Microwave Background at Degree Angular Scales: Python V Results |
title_full_unstemmed |
Anisotropy in the Cosmic Microwave Background at Degree Angular Scales: Python V Results |
title_sort |
anisotropy in the cosmic microwave background at degree angular scales: python v results |
publisher |
arXiv |
publishDate |
1999 |
url |
https://dx.doi.org/10.48550/arxiv.astro-ph/9902195 https://arxiv.org/abs/astro-ph/9902195 |
long_lat |
ENVELOPE(0.000,0.000,-90.000,-90.000) ENVELOPE(0.000,0.000,-90.000,-90.000) ENVELOPE(139.273,139.273,-89.998,-89.998) |
geographic |
South Pole Amundsen-Scott Amundsen Scott South Pole Station Amundsen-Scott South Pole Station |
geographic_facet |
South Pole Amundsen-Scott Amundsen Scott South Pole Station Amundsen-Scott South Pole Station |
genre |
Amundsen-Scott Antarc* Antarctica South pole South pole |
genre_facet |
Amundsen-Scott Antarc* Antarctica South pole South pole |
op_relation |
https://dx.doi.org/10.1086/312093 |
op_rights |
Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ |
op_doi |
https://doi.org/10.48550/arxiv.astro-ph/9902195 https://doi.org/10.1086/312093 |
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1766379679381454848 |