Context. We present the results of the in-flight radiometric calibration performed for the ultraviolet (UV) H I Ly-α channel of the Metis coronagraph on board Solar Orbiter. Aims. The radiometric calibration is a fundamental procedure required to produce data in physical units. The quantity that allows us to pass from raw data into calibrated data is the radiometric calibration factor, ϵUV. Methods. To obtain the ϵUV results, we used observations of stellar targets transiting the Metis field of view. We derived ϵUV by determining the signal of each calibration star by means of the aperture photometry and evaluating its expected flux in the Metis narrow bandpass (121.6 ± 10 nm). The analyzed data cover a time range from the beginning of the Cruise Phase in June 2020, up until August 2021. Results. We find that the UV channel requires a significant additional correction of the response across the field of view, compared to that provided by the vignetting function measured on the ground and refined in flight, specifically tailored to the UV channel. This correction is provided by the ratio of images of the back-illumination of the closed door. Here, we use the stellar measurements to refine and improve such a correction map. After correcting for the spatial disuniformity, a radiometric calibration factor ϵUV = 0.20 ± 0.03 DN/photon was found. No significant changes in the UV channel throughput were observed during the period from June 2020 to August 2021. In addition, the analysis of a smaller number of stars observed in 2022 and 2023 enabled us to extend the validity of the radiometric calibration to that period, after considering a suitable scaling factor due to the change of operating voltages occurred in April 2022. From this second analysis, the value of the radiometric calibration factor is ϵUV = 0.11 ± 0.03 DN/photon. In order to support the radiometric calibration results, we performed a comparison between average radial profiles of the H I Ly-α intensity obtained from Metis UV images acquired in 2020-2021 and those measured with the UltraViolet Coronagraph Spectrometer (UVCS) on board the Solar and Heliospheric Observatory (SOHO) during the period of the activity minimum of solar cycle 22 in 1996. We found that intensity profiles of these instruments are consistent with each other.
In-flight radiometric calibration of the Metis UV H I Ly-αα channel and comparison with UVCS data / De Leo Y.; Burtovoi A.; Teriaca L.; Romoli M.; Andretta V.; Uslenghi M.; Giordano S.; Chioetto P.; Susino R.; Landini F.; Pancrazzi M.; Frassati F.; Russano G.; Spadaro D.; Abbo L.; Bemporad A.; Capobianco G.; Capuano G.; Casini C.; Casti M.; Corso A.J.; Da Deppo V.; Fabi M.; Fineschi S.; Frassetto F.; Giarrusso M.; Grimani C.; Guglielmino S.L.; Heinzel P.; Jerse G.; Liberatore A.; Magli E.; Massone G.; Messerotti M.; Moses J.D.; Naletto G.; Nicolini G.; Pelizzo M.G.; Romano P.; Sasso C.; Schuhle U.; Straus T.; Slemer A.; Stangalini M.; Telloni D.; Volpicelli C.A.; Zangrilli L.; Zuppella P.. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 1432-0746. - ELETTRONICO. - 697:(2025), pp. A73.0-A73.0. [10.1051/0004-6361/202450759]
In-flight radiometric calibration of the Metis UV H I Ly-αα channel and comparison with UVCS data
Burtovoi A.;Romoli M.;
2025
Abstract
Context. We present the results of the in-flight radiometric calibration performed for the ultraviolet (UV) H I Ly-α channel of the Metis coronagraph on board Solar Orbiter. Aims. The radiometric calibration is a fundamental procedure required to produce data in physical units. The quantity that allows us to pass from raw data into calibrated data is the radiometric calibration factor, ϵUV. Methods. To obtain the ϵUV results, we used observations of stellar targets transiting the Metis field of view. We derived ϵUV by determining the signal of each calibration star by means of the aperture photometry and evaluating its expected flux in the Metis narrow bandpass (121.6 ± 10 nm). The analyzed data cover a time range from the beginning of the Cruise Phase in June 2020, up until August 2021. Results. We find that the UV channel requires a significant additional correction of the response across the field of view, compared to that provided by the vignetting function measured on the ground and refined in flight, specifically tailored to the UV channel. This correction is provided by the ratio of images of the back-illumination of the closed door. Here, we use the stellar measurements to refine and improve such a correction map. After correcting for the spatial disuniformity, a radiometric calibration factor ϵUV = 0.20 ± 0.03 DN/photon was found. No significant changes in the UV channel throughput were observed during the period from June 2020 to August 2021. In addition, the analysis of a smaller number of stars observed in 2022 and 2023 enabled us to extend the validity of the radiometric calibration to that period, after considering a suitable scaling factor due to the change of operating voltages occurred in April 2022. From this second analysis, the value of the radiometric calibration factor is ϵUV = 0.11 ± 0.03 DN/photon. In order to support the radiometric calibration results, we performed a comparison between average radial profiles of the H I Ly-α intensity obtained from Metis UV images acquired in 2020-2021 and those measured with the UltraViolet Coronagraph Spectrometer (UVCS) on board the Solar and Heliospheric Observatory (SOHO) during the period of the activity minimum of solar cycle 22 in 1996. We found that intensity profiles of these instruments are consistent with each other.
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