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3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites

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3D shape of asteroid (6) Hebe from VLT/SPHERE imaging : Implications for the origin of ordinary H chondrites. / Marsset, M.; Carry, B.; Dumas, C.; Hanuš, J.; Viikinkoski, M.; Vernazza, P.; Müller, T. G.; Delbo, M.; Jehin, E.; Gillon, M.; Grice, J.; Yang, B.; Fusco, T.; Berthier, J.; Sonnett, S.; Kugel, F.; Caron, J.; Behrend, R.

julkaisussa: Astronomy and Astrophysics, Vuosikerta 604, A64, 01.08.2017.

Tutkimustuotosvertaisarvioitu

Harvard

Marsset, M, Carry, B, Dumas, C, Hanuš, J, Viikinkoski, M, Vernazza, P, Müller, TG, Delbo, M, Jehin, E, Gillon, M, Grice, J, Yang, B, Fusco, T, Berthier, J, Sonnett, S, Kugel, F, Caron, J & Behrend, R 2017, '3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites', Astronomy and Astrophysics, Vuosikerta. 604, A64. https://doi.org/10.1051/0004-6361/201731021

APA

Marsset, M., Carry, B., Dumas, C., Hanuš, J., Viikinkoski, M., Vernazza, P., ... Behrend, R. (2017). 3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites. Astronomy and Astrophysics, 604, [A64]. https://doi.org/10.1051/0004-6361/201731021

Vancouver

Author

Marsset, M. ; Carry, B. ; Dumas, C. ; Hanuš, J. ; Viikinkoski, M. ; Vernazza, P. ; Müller, T. G. ; Delbo, M. ; Jehin, E. ; Gillon, M. ; Grice, J. ; Yang, B. ; Fusco, T. ; Berthier, J. ; Sonnett, S. ; Kugel, F. ; Caron, J. ; Behrend, R. / 3D shape of asteroid (6) Hebe from VLT/SPHERE imaging : Implications for the origin of ordinary H chondrites. Julkaisussa: Astronomy and Astrophysics. 2017 ; Vuosikerta 604.

Bibtex - Lataa

@article{f0ecde3b2ce84b6bb21a804811ba3b26,
title = "3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites",
abstract = "Context. The high-angular-resolution capability of the new-generation ground-based adaptive-optics camera SPHERE at ESO VLT allows us to assess, for the very first time, the cratering record of medium-sized (D ∼ 100-200 km) asteroids from the ground, opening the prospect of a new era of investigation of the asteroid belt's collisional history. Aims. We investigate here the collisional history of asteroid (6) Hebe and challenge the idea that Hebe may be the parent body of ordinary H chondrites, the most common type of meteorites found on Earth (∼34{\%} of the falls). Methods. We observed Hebe with SPHERE as part of the science verification of the instrument. Combined with earlier adaptive-optics images and optical light curves, we model the spin and three-dimensional (3D) shape of Hebe and check the consistency of the derived model against available stellar occultations and thermal measurements. Results. Our 3D shape model fits the images with sub-pixel residuals and the light curves to 0.02 mag. The rotation period (7.274 47 h), spin (ECJ2000 λ, β of 343°, +47°), and volume-equivalent diameter (193 ± 6 km) are consistent with previous determinations and thermophysical modeling. Hebe's inferred density is 3.48 ± 0.64 g cm-3, in agreement with an intact interior based on its H-chondrite composition. Using the 3D shape model to derive the volume of the largest depression (likely impact crater), it appears that the latter is significantly smaller than the total volume of close-by S-type H-chondrite-like asteroid families. Conclusions. Our results imply that (6) Hebe is not the most likely source of H chondrites. Over the coming years, our team will collect similar high-precision shape measurements with VLT/SPHERE for ∼40 asteroids covering the main compositional classes, thus providing an unprecedented dataset to investigate the origin and collisional evolution of the asteroid belt.",
keywords = "asteroids: individual: (6) Hebe, Meteorites, meteoroids, meteors, Minor planets, Techniques: high angular resolution",
author = "M. Marsset and B. Carry and C. Dumas and J. Hanuš and M. Viikinkoski and P. Vernazza and M{\"u}ller, {T. G.} and M. Delbo and E. Jehin and M. Gillon and J. Grice and B. Yang and T. Fusco and J. Berthier and S. Sonnett and F. Kugel and J. Caron and R. Behrend",
year = "2017",
month = "8",
day = "1",
doi = "10.1051/0004-6361/201731021",
language = "English",
volume = "604",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",

}

RIS (suitable for import to EndNote) - Lataa

TY - JOUR

T1 - 3D shape of asteroid (6) Hebe from VLT/SPHERE imaging

T2 - Implications for the origin of ordinary H chondrites

AU - Marsset, M.

AU - Carry, B.

AU - Dumas, C.

AU - Hanuš, J.

AU - Viikinkoski, M.

AU - Vernazza, P.

AU - Müller, T. G.

AU - Delbo, M.

AU - Jehin, E.

AU - Gillon, M.

AU - Grice, J.

AU - Yang, B.

AU - Fusco, T.

AU - Berthier, J.

AU - Sonnett, S.

AU - Kugel, F.

AU - Caron, J.

AU - Behrend, R.

PY - 2017/8/1

Y1 - 2017/8/1

N2 - Context. The high-angular-resolution capability of the new-generation ground-based adaptive-optics camera SPHERE at ESO VLT allows us to assess, for the very first time, the cratering record of medium-sized (D ∼ 100-200 km) asteroids from the ground, opening the prospect of a new era of investigation of the asteroid belt's collisional history. Aims. We investigate here the collisional history of asteroid (6) Hebe and challenge the idea that Hebe may be the parent body of ordinary H chondrites, the most common type of meteorites found on Earth (∼34% of the falls). Methods. We observed Hebe with SPHERE as part of the science verification of the instrument. Combined with earlier adaptive-optics images and optical light curves, we model the spin and three-dimensional (3D) shape of Hebe and check the consistency of the derived model against available stellar occultations and thermal measurements. Results. Our 3D shape model fits the images with sub-pixel residuals and the light curves to 0.02 mag. The rotation period (7.274 47 h), spin (ECJ2000 λ, β of 343°, +47°), and volume-equivalent diameter (193 ± 6 km) are consistent with previous determinations and thermophysical modeling. Hebe's inferred density is 3.48 ± 0.64 g cm-3, in agreement with an intact interior based on its H-chondrite composition. Using the 3D shape model to derive the volume of the largest depression (likely impact crater), it appears that the latter is significantly smaller than the total volume of close-by S-type H-chondrite-like asteroid families. Conclusions. Our results imply that (6) Hebe is not the most likely source of H chondrites. Over the coming years, our team will collect similar high-precision shape measurements with VLT/SPHERE for ∼40 asteroids covering the main compositional classes, thus providing an unprecedented dataset to investigate the origin and collisional evolution of the asteroid belt.

AB - Context. The high-angular-resolution capability of the new-generation ground-based adaptive-optics camera SPHERE at ESO VLT allows us to assess, for the very first time, the cratering record of medium-sized (D ∼ 100-200 km) asteroids from the ground, opening the prospect of a new era of investigation of the asteroid belt's collisional history. Aims. We investigate here the collisional history of asteroid (6) Hebe and challenge the idea that Hebe may be the parent body of ordinary H chondrites, the most common type of meteorites found on Earth (∼34% of the falls). Methods. We observed Hebe with SPHERE as part of the science verification of the instrument. Combined with earlier adaptive-optics images and optical light curves, we model the spin and three-dimensional (3D) shape of Hebe and check the consistency of the derived model against available stellar occultations and thermal measurements. Results. Our 3D shape model fits the images with sub-pixel residuals and the light curves to 0.02 mag. The rotation period (7.274 47 h), spin (ECJ2000 λ, β of 343°, +47°), and volume-equivalent diameter (193 ± 6 km) are consistent with previous determinations and thermophysical modeling. Hebe's inferred density is 3.48 ± 0.64 g cm-3, in agreement with an intact interior based on its H-chondrite composition. Using the 3D shape model to derive the volume of the largest depression (likely impact crater), it appears that the latter is significantly smaller than the total volume of close-by S-type H-chondrite-like asteroid families. Conclusions. Our results imply that (6) Hebe is not the most likely source of H chondrites. Over the coming years, our team will collect similar high-precision shape measurements with VLT/SPHERE for ∼40 asteroids covering the main compositional classes, thus providing an unprecedented dataset to investigate the origin and collisional evolution of the asteroid belt.

KW - asteroids: individual: (6) Hebe

KW - Meteorites

KW - meteoroids

KW - meteors

KW - Minor planets

KW - Techniques: high angular resolution

U2 - 10.1051/0004-6361/201731021

DO - 10.1051/0004-6361/201731021

M3 - Article

VL - 604

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A64

ER -