講演情報
[PPS07-P03]Visible Wavelength Normal Albedo Map of Ryugu Derived by Hayabusa2 Optical Navigation Camera
*横田 康弘1,2、本田 理恵2、巽 瑛理3,4,5、Domingue Deborah6、Schröder Stefanus7、松岡 萌1、杉田 精司5、諸田 智克5,8、亀田 真吾9、神山 徹10、鈴木 秀彦11、山田 学12、坂谷 尚哉1、本田 親寿13、早川 雅彦1、吉岡 和夫5、長 勇一郎5、澤⽥ 弘崇1、小川 和律1,14 (1.宇宙航空研究開発機構 宇宙科学研究所、2.高知大学、3.Instituto de Astrofisica de Canarias, Spain、4.Univ. of La Laguna, Spain、5.東京大学、6.Planetary Science Institute, USA、7.DLR, Germany、8.名古屋大学、9.立教大学、10.産総研、11.明治大学、12.千葉工業大学、13.会津大学、14.神戸大学)
キーワード：
はやぶさ２、小惑星、リュウグウ、測光、アルベド
Asteroid explorer Hayabusa2 observed Cb-type asteroid 162173 Ryugu between June 2018 and November 2019 at a distance below 20km. The Telescopic Optical Navigation Camera (ONC-T) [1–4] onboard Hayabusa2 observed Ryugu with 7 broadband filters ranging in wavelength from 0.40–0.95 μm. On 8 January 2019, ONC-T observed the asteroid in the opposition geometry from ~20 km distance, through one rotation period (7.6 hr) in 7-band. The local solar phase angle of each pixel ranges from 0.0° to ~1.7°. This data set is well suited to derive the normal albedo, defined as the radiance factor (I/F) at phase angle 0° [5]. We present the normal albedo map from this observation.
The data number of the raw image pixels are converted [4] to I/F. The observation geometry of each pixel is calculated using the Ryugu shape model [6] produced by the Hayabusa2 shape model team. We fit a linear function to the phase function plot within the phase angle range 0.2–1.7°. Using this phase function, each pixel's I/F was extrapolated to normal albedo. Finally, we create a mosaic map of normal albedo for each band.
Since the observed brightness at the opposition condition is less affected by shadows or topographic undulation than other geometries, the derived map successfully shows the albedo distribution under minimal noise conditions. The color study [e.g. 1, 6, 7, 8] of Ryugu reported that the spectral slope from b-band (0.48 μm) to x-band (0.86 μm) exhibits the greatest regional variation on Ryugu. We found that the normal albedo is well correlated with the b-x spectral slope. Further study is necessary to interpret this relationship.
Acknowledgment: We thank the entire Hayabusa2 team to achieve the observation and analysis. This study was supported by Japan Society for the Promotion of Science (JSPS) Core-to-Core Program "International Network of Planetary Sciences”, NASA’s Hayabusa2 participating scientist program (grant number NNX16AL34G), and NASA’s Solar System Exploration Research Virtual Institute 2016 (SSERVI16) Cooperative Agreement (NNH16ZDA001N) for TREX (Toolbox for Research and Exploration).
References: [1] Sugita S. et al. (2019) Science 10.1126/science.aaw0422. [2] Kameda S. et al. (2017) SSR 208, 17–31. [3] Suzuki H. et al. (2018) Icarus 300, 341–359. [4] Tatsumi E. et al. (2019) Icarus 325, 153–195. [5] Li J.-Y., et al. (2015) Asteroids IV, University of Arizona Press, 129–150. [6] Watanabe S. et al. (2019) Science 364, 268-272. [7] Morota T. et al. (2020) (submitted). [8] Tatsumi E. et al. (2020) (in preparation).
The data number of the raw image pixels are converted [4] to I/F. The observation geometry of each pixel is calculated using the Ryugu shape model [6] produced by the Hayabusa2 shape model team. We fit a linear function to the phase function plot within the phase angle range 0.2–1.7°. Using this phase function, each pixel's I/F was extrapolated to normal albedo. Finally, we create a mosaic map of normal albedo for each band.
Since the observed brightness at the opposition condition is less affected by shadows or topographic undulation than other geometries, the derived map successfully shows the albedo distribution under minimal noise conditions. The color study [e.g. 1, 6, 7, 8] of Ryugu reported that the spectral slope from b-band (0.48 μm) to x-band (0.86 μm) exhibits the greatest regional variation on Ryugu. We found that the normal albedo is well correlated with the b-x spectral slope. Further study is necessary to interpret this relationship.
Acknowledgment: We thank the entire Hayabusa2 team to achieve the observation and analysis. This study was supported by Japan Society for the Promotion of Science (JSPS) Core-to-Core Program "International Network of Planetary Sciences”, NASA’s Hayabusa2 participating scientist program (grant number NNX16AL34G), and NASA’s Solar System Exploration Research Virtual Institute 2016 (SSERVI16) Cooperative Agreement (NNH16ZDA001N) for TREX (Toolbox for Research and Exploration).
References: [1] Sugita S. et al. (2019) Science 10.1126/science.aaw0422. [2] Kameda S. et al. (2017) SSR 208, 17–31. [3] Suzuki H. et al. (2018) Icarus 300, 341–359. [4] Tatsumi E. et al. (2019) Icarus 325, 153–195. [5] Li J.-Y., et al. (2015) Asteroids IV, University of Arizona Press, 129–150. [6] Watanabe S. et al. (2019) Science 364, 268-272. [7] Morota T. et al. (2020) (submitted). [8] Tatsumi E. et al. (2020) (in preparation).