Optical properties of (162173) 1999 JU3: in preparation for the JAXA Hayabusa 2 sample return mission
- Department of Physics and Astronomy, Seoul National University, Gwanak, Seoul 151-742 (Korea, Republic of)
- Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Asakuchi, Okayama 719-0232 (Japan)
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 252-5210 (Japan)
- Department of Astronomy, Yonsei University, 50 Yonsei-ro, Seodaemun-gu, Seoul 120-749 (Korea, Republic of)
- Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 305-348 (Korea, Republic of)
- Lowell Observatory, 1400 W. Mars Hill Road, Flagstaff, AZ 86001 (United States)
- Department of Aerospace Engineering, Nihon University, 7-24-1 Narashinodai Funabashi, Chiba 274-8501 (Japan)
- Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli, Taoyuan 32001, Taiwan (China)
- Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, Sayo, Hyogo 679-5313 (Japan)
- Sayo Town Office, 2611-1 Sayo, Sayo-cho, Sayo, Hyogo 679-5380 (Japan)
- Academia Sinica Institute of Astronomy and Astrophysics, Roosevelt Road, Taipei 10617, Taiwan (China)
- The Observatories of the Carnegie Institute of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, La Serena (Chile)
- Bisei Spaceguard Center, Japan Spaceguard Association, 1716-3 Okura, Bisei-cho, Ibara, Okayama 714-1411 (Japan)
- Ishigakijima Astronomical Observatory, National Astronomical Observatory of Japan, 1024-1 Arakawa, Ishigaki, Okinawa 907-0024 (Japan)
- Department of Teacher Training, Hokkaido University of Education, 9 Hokumon, Asahikawa 070-8621 (Japan)
We investigated the magnitude-phase relation of (162173) 1999 JU3, a target asteroid for the JAXA Hayabusa 2 sample return mission. We initially employed the International Astronomical Union's H-G formalism but found that it fits less well using a single set of parameters. To improve the inadequate fit, we employed two photometric functions: the Shevchenko and Hapke functions. With the Shevchenko function, we found that the magnitude-phase relation exhibits linear behavior in a wide phase angle range (α = 5°-75°) and shows weak nonlinear opposition brightening at α < 5°, providing a more reliable absolute magnitude of H {sub V} = 19.25 ± 0.03. The phase slope (0.039 ± 0.001 mag deg{sup –1}) and opposition effect amplitude (parameterized by the ratio of intensity at α = 0.°3 to that at α = 5°, I(0.°3)/I(5°) = 1.31 ± 0.05) are consistent with those of typical C-type asteroids. We also attempted to determine the parameters for the Hapke model, which are applicable for constructing the surface reflectance map with the Hayabusa 2 onboard cameras. Although we could not constrain the full set of Hapke parameters, we obtained possible values, w = 0.041, g = –0.38, B {sub 0} = 1.43, and h = 0.050, assuming a surface roughness parameter θ-bar = 20°. By combining our photometric study with a thermal model of the asteroid, we obtained a geometric albedo of p {sub v} = 0.047 ± 0.003, phase integral q = 0.32 ± 0.03, and Bond albedo A {sub B} = 0.014 ± 0.002, which are commensurate with the values for common C-type asteroids.
- OSTI ID:
- 22365176
- Journal Information:
- Astrophysical Journal, Vol. 792, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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