The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source
Calibrating solar radio flux has always been a concern in the solar community. Previously, fluxes were calibrated by matching load or the new Moon for relative calibration, and at times with the assistance of other stations’ data. Moreover, the frequency coverage seldom exceeded 26 GHz. This paper r...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal Supplement Series |
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| Online Access: | https://doi.org/10.3847/1538-4365/acee00 |
| _version_ | 1797680485153898496 |
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| author | ZiQian Shang Zhao Wu Yan Liu Yu Bai Guang Lu YuanYuan Zhang Lei Zhang YanRui Su Yao Chen FaBao Yan |
| author_facet | ZiQian Shang Zhao Wu Yan Liu Yu Bai Guang Lu YuanYuan Zhang Lei Zhang YanRui Su Yao Chen FaBao Yan |
| author_sort | ZiQian Shang |
| collection | DOAJ |
| description | Calibrating solar radio flux has always been a concern in the solar community. Previously, fluxes were calibrated by matching load or the new Moon for relative calibration, and at times with the assistance of other stations’ data. Moreover, the frequency coverage seldom exceeded 26 GHz. This paper reports the upgraded and calibrated Chashan Broadband Solar millimeter spectrometer (CBS) working from 35 to 40 GHz at the Chashan Solar Observatory (CSO). Initially, the calibration of the solar radiation brightness temperature is accomplished using the new Moon as the definitive source. Subsequently, the 35–40 GHz standard flux is achieved by establishing the correlation between the solar radio flux, brightness temperature, and frequency. Finally, the calibration of the solar radio flux is implemented by utilizing a constant temperature-controlled noise source as a reference. The calibration in 2023 February and March reveals that the solar brightness temperature is 11,636 K at 37.25 GHz with a standard deviation (STD) of 652 K. The solar radio flux’s intensity is ∼3000–4000 solar flux units (SFU) in the range of 35–40 GHz with a consistency bias of ±5.3%. The system sensitivity is about ∼5–8 SFU by a rough evaluation, a noise factor of about 200 K, and the coefficient of variation of the system transmission slope of 6.5% @ 12 hr at 37.25 GHz. It is expected that the upgraded CBS will capture more activity during the upcoming solar cycle. |
| first_indexed | 2024-03-11T23:30:42Z |
| format | Article |
| id | doaj.art-4bccf72cc5bd4350bd9d7261dab64a40 |
| institution | Directory Open Access Journal |
| issn | 0067-0049 |
| language | English |
| last_indexed | 2024-03-11T23:30:42Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Supplement Series |
| spelling | doaj.art-4bccf72cc5bd4350bd9d7261dab64a402023-09-20T08:42:23ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492023-01-0126824510.3847/1538-4365/acee00The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise SourceZiQian Shang0Zhao Wu1Yan Liu2Yu Bai3Guang Lu4https://orcid.org/0000-0002-2154-263XYuanYuan Zhang5Lei Zhang6YanRui Su7Yao Chen8https://orcid.org/0000-0001-6449-8838FaBao Yan9https://orcid.org/0000-0002-4451-7293Laboratory for Electromagnetic Detection (LEAD), Institute of Space Sciences, Shandong University , Weihai 264209, People's Republic of China yanfabao2022@163.comLaboratory for Electromagnetic Detection (LEAD), Institute of Space Sciences, Shandong University , Weihai 264209, People's Republic of China yanfabao2022@163.comLaboratory for Electromagnetic Detection (LEAD), Institute of Space Sciences, Shandong University , Weihai 264209, People's Republic of China yanfabao2022@163.comLaboratory for Electromagnetic Detection (LEAD), Institute of Space Sciences, Shandong University , Weihai 264209, People's Republic of China yanfabao2022@163.comLaboratory for Electromagnetic Detection (LEAD), Institute of Space Sciences, Shandong University , Weihai 264209, People's Republic of China yanfabao2022@163.comLaboratory for Electromagnetic Detection (LEAD), Institute of Space Sciences, Shandong University , Weihai 264209, People's Republic of China yanfabao2022@163.comLaboratory for Electromagnetic Detection (LEAD), Institute of Space Sciences, Shandong University , Weihai 264209, People's Republic of China yanfabao2022@163.comSchool of Mechanical, Electrical & Information Engineering, Shandong University , Weihai 264209, People's Republic of ChinaLaboratory for Electromagnetic Detection (LEAD), Institute of Space Sciences, Shandong University , Weihai 264209, People's Republic of China yanfabao2022@163.comLaboratory for Electromagnetic Detection (LEAD), Institute of Space Sciences, Shandong University , Weihai 264209, People's Republic of China yanfabao2022@163.com; School of Mechanical, Electrical & Information Engineering, Shandong University , Weihai 264209, People's Republic of ChinaCalibrating solar radio flux has always been a concern in the solar community. Previously, fluxes were calibrated by matching load or the new Moon for relative calibration, and at times with the assistance of other stations’ data. Moreover, the frequency coverage seldom exceeded 26 GHz. This paper reports the upgraded and calibrated Chashan Broadband Solar millimeter spectrometer (CBS) working from 35 to 40 GHz at the Chashan Solar Observatory (CSO). Initially, the calibration of the solar radiation brightness temperature is accomplished using the new Moon as the definitive source. Subsequently, the 35–40 GHz standard flux is achieved by establishing the correlation between the solar radio flux, brightness temperature, and frequency. Finally, the calibration of the solar radio flux is implemented by utilizing a constant temperature-controlled noise source as a reference. The calibration in 2023 February and March reveals that the solar brightness temperature is 11,636 K at 37.25 GHz with a standard deviation (STD) of 652 K. The solar radio flux’s intensity is ∼3000–4000 solar flux units (SFU) in the range of 35–40 GHz with a consistency bias of ±5.3%. The system sensitivity is about ∼5–8 SFU by a rough evaluation, a noise factor of about 200 K, and the coefficient of variation of the system transmission slope of 6.5% @ 12 hr at 37.25 GHz. It is expected that the upgraded CBS will capture more activity during the upcoming solar cycle.https://doi.org/10.3847/1538-4365/acee00CalibrationAstronomical techniques |
| spellingShingle | ZiQian Shang Zhao Wu Yan Liu Yu Bai Guang Lu YuanYuan Zhang Lei Zhang YanRui Su Yao Chen FaBao Yan The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source The Astrophysical Journal Supplement Series Calibration Astronomical techniques |
| title | The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source |
| title_full | The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source |
| title_fullStr | The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source |
| title_full_unstemmed | The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source |
| title_short | The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source |
| title_sort | calibration of the 35 40 ghz solar radio spectrometer with the new moon and a noise source |
| topic | Calibration Astronomical techniques |
| url | https://doi.org/10.3847/1538-4365/acee00 |
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