Study of systematics effects on the cross power spectrum of 21 cm line and cosmic microwave background using Murchison Widefield Array data
Observation of the 21 cm line signal from neutral hydrogen during the epoch of reionization is challenging due to extremely bright Galactic and extragalactic foregrounds and complicated instrumental calibration. A reasonable approach for mitigating these problems is the crosscorrelation with other o...
| Main Authors: | , , , , , |
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| Format: | Journal Article |
| Language: | English |
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OXFORD UNIV PRESS
2019
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| Online Access: | http://purl.org/au-research/grants/arc/CE170100013 http://hdl.handle.net/20.500.11937/91565 |
| _version_ | 1848765549239074816 |
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| author | Yoshiura, S. Ichiki, K. Pindor, B. Takahashi, K. Tashiro, H. Trott, Cathryn |
| author_facet | Yoshiura, S. Ichiki, K. Pindor, B. Takahashi, K. Tashiro, H. Trott, Cathryn |
| author_sort | Yoshiura, S. |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | Observation of the 21 cm line signal from neutral hydrogen during the epoch of reionization is challenging due to extremely bright Galactic and extragalactic foregrounds and complicated instrumental calibration. A reasonable approach for mitigating these problems is the crosscorrelation with other observables. In this work, we present the first results of the cross power spectrum (CPS) between radio images observed by the Murchison Widefield Array and the cosmic microwave background (CMB), measured by the Planck experiment. We study the systematics due to the ionospheric activity, the dependence of CPS on group of pointings, and frequency. The resulting CPS is consistent with zero because the error is dominated by the foregrounds in the 21 cm observation. Additionally, the variance of the signal indicates the presence of unexpected systematics error at small scales. Furthermore, we reduce the error by one order of magnitude with application of a foreground removal using a polynomial fitting method. Based on the results, we find that the detection of the 21 cm-CMB CPS with theMWA Phase I requires more than 99.95 per cent of the foreground signal removed, 2000 h of deep observation and 50 per cent of the sky fraction coverage. |
| first_indexed | 2025-11-14T11:37:01Z |
| format | Journal Article |
| id | curtin-20.500.11937-91565 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| language | English |
| last_indexed | 2025-11-14T11:37:01Z |
| publishDate | 2019 |
| publisher | OXFORD UNIV PRESS |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-915652023-05-11T02:45:03Z Study of systematics effects on the cross power spectrum of 21 cm line and cosmic microwave background using Murchison Widefield Array data Yoshiura, S. Ichiki, K. Pindor, B. Takahashi, K. Tashiro, H. Trott, Cathryn Science & Technology Physical Sciences Astronomy & Astrophysics dark ages, reionization first stars cosmic background radiation REIONIZATION HISTORY EPOCH Observation of the 21 cm line signal from neutral hydrogen during the epoch of reionization is challenging due to extremely bright Galactic and extragalactic foregrounds and complicated instrumental calibration. A reasonable approach for mitigating these problems is the crosscorrelation with other observables. In this work, we present the first results of the cross power spectrum (CPS) between radio images observed by the Murchison Widefield Array and the cosmic microwave background (CMB), measured by the Planck experiment. We study the systematics due to the ionospheric activity, the dependence of CPS on group of pointings, and frequency. The resulting CPS is consistent with zero because the error is dominated by the foregrounds in the 21 cm observation. Additionally, the variance of the signal indicates the presence of unexpected systematics error at small scales. Furthermore, we reduce the error by one order of magnitude with application of a foreground removal using a polynomial fitting method. Based on the results, we find that the detection of the 21 cm-CMB CPS with theMWA Phase I requires more than 99.95 per cent of the foreground signal removed, 2000 h of deep observation and 50 per cent of the sky fraction coverage. 2019 Journal Article http://hdl.handle.net/20.500.11937/91565 10.1093/mnras/sty3248 English http://purl.org/au-research/grants/arc/CE170100013 http://purl.org/au-research/grants/arc/DE140100316 http://purl.org/au-research/grants/arc/CE110001020 OXFORD UNIV PRESS fulltext |
| spellingShingle | Science & Technology Physical Sciences Astronomy & Astrophysics dark ages, reionization first stars cosmic background radiation REIONIZATION HISTORY EPOCH Yoshiura, S. Ichiki, K. Pindor, B. Takahashi, K. Tashiro, H. Trott, Cathryn Study of systematics effects on the cross power spectrum of 21 cm line and cosmic microwave background using Murchison Widefield Array data |
| title | Study of systematics effects on the cross power spectrum of 21 cm line and cosmic microwave background using Murchison Widefield Array data |
| title_full | Study of systematics effects on the cross power spectrum of 21 cm line and cosmic microwave background using Murchison Widefield Array data |
| title_fullStr | Study of systematics effects on the cross power spectrum of 21 cm line and cosmic microwave background using Murchison Widefield Array data |
| title_full_unstemmed | Study of systematics effects on the cross power spectrum of 21 cm line and cosmic microwave background using Murchison Widefield Array data |
| title_short | Study of systematics effects on the cross power spectrum of 21 cm line and cosmic microwave background using Murchison Widefield Array data |
| title_sort | study of systematics effects on the cross power spectrum of 21 cm line and cosmic microwave background using murchison widefield array data |
| topic | Science & Technology Physical Sciences Astronomy & Astrophysics dark ages, reionization first stars cosmic background radiation REIONIZATION HISTORY EPOCH |
| url | http://purl.org/au-research/grants/arc/CE170100013 http://purl.org/au-research/grants/arc/CE170100013 http://purl.org/au-research/grants/arc/CE170100013 http://hdl.handle.net/20.500.11937/91565 |