TY - JOUR
T1 - Shape and spin state model of contact binary (388188) 2006 DP14 using combined radar and optical observations
AU - Cannon, Richard E.
AU - Rożek, Agata
AU - Brozović, Marina
AU - Pravec, Petr
AU - Snodgrass, Colin
AU - Busch, Michael W.
AU - Robinson, James E.
AU - Donaldson, Abbie
AU - Holc, Tanja
AU - Benner, Lance A. M.
AU - Naidu, Shantanu
AU - Kušnirák, Peter
AU - Gardener, Daniel
AU - Kučáková, Hana
AU - Khalouei, Elahe
AU - Pollock, Joseph
AU - Bonavita, Mariangela
AU - Fatka, Petr
AU - Hornoch, Kamil
AU - Sajadian, Sedighe
AU - Alegre, Lara
AU - Amadio, Flavia
AU - Andersen, Michael I.
AU - Bozza, Valerio
AU - Burgdorf, Martin J.
AU - Columba, Gabriele
AU - Dominik, Martin
AU - Figuera Jaimes, R.
AU - Hinse, Tobias C.
AU - Hundertmark, Markus
AU - Jørgensen, Uffe G.
AU - Longa-Peña, Penelope
AU - Peixinho, Nuno
AU - Rabus, Markus
AU - Rahvar, Sohrab
AU - Rota, Paolo
AU - Skottfelt, Jesper
AU - Southworth, John
AU - Tregloan-Reed, Jeremy
N1 - Funding: This material is based in part upon work supported by NASA under the Science Mission Directorate Research and Analysis Programs. REC, AR, CS, and AD acknowledge the support from the UK Science and Technology Facilities Council. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (80NM0018D0004). The work at Ondřejov was supported by Praemium Academiae award to PP by the Academy of Sciences of the Czech Republic. TH acknowledges funding from the Public Scholarship, Development, Disability and Maintenance Fund of the Republic of Slovenia. UGJ acknowledges funding from the Novo Nordisk Foundation Interdisciplinary Synergy Programme grant no. NNF19OC0057374. EK was supported by the National Research Foundation of Korea (2021M3F7A1082056). PL-P was partly funded by the FONDECYT Initiation Project No. 11241572. RFJ acknowledges support for this project provided by ANID’s Millennium Science Initiative through grant ICN12_009, awarded to the Millennium Institute of Astrophysics (MAS), and by ANID’s Basal project FB210003.
PY - 2025/4/1
Y1 - 2025/4/1
N2 - Contact binaries are found throughout the Solar System. The recent discovery of Selam, the satellite of main-belt asteroid (152830) Dinkinesh, by the NASA Lucy mission has made it clear that the term ‘contact binary’ covers a variety of different types of bimodal mass distributions and formation mechanisms. Only by modelling more contact binaries can this population be properly understood. We determined a spin state and shape model for the Apollo group contact binary asteroid (388188) 2006 DP14 using ground-based optical and radar observations collected between 2014 and 2023. Radar delay-Doppler images and continuous-wave spectra were collected over 2 d in February 2014, while 16 light curves in the Cousins R and SDSS-r filters were collected in 2014, 2022, and 2023. We modelled the spin state using convex inversion before using the SHAPE modelling software to include the radar observations in modelling concavities and the distinctive neck structure connecting the two lobes. We find a spin state with a period of (5.7860 ± 0.0001) h and pole solution of λ = (180 ± 121)◦ and β = (−80 ± 7)◦ with morphology indicating a 520 m long bilobed shape. The model’s asymmetrical bimodal mass distribution resembles other small near-Earth asteroid contact binaries such as (85990) 1999 JV6 or (8567) 1996 HW1, which also feature a smaller ‘head’ attached to a larger ‘body’. The final model features a crater on the larger lobe, similar to several other modelled contact binaries. The model’s resolution is 25 m, comparable to that of the radar images used.
AB - Contact binaries are found throughout the Solar System. The recent discovery of Selam, the satellite of main-belt asteroid (152830) Dinkinesh, by the NASA Lucy mission has made it clear that the term ‘contact binary’ covers a variety of different types of bimodal mass distributions and formation mechanisms. Only by modelling more contact binaries can this population be properly understood. We determined a spin state and shape model for the Apollo group contact binary asteroid (388188) 2006 DP14 using ground-based optical and radar observations collected between 2014 and 2023. Radar delay-Doppler images and continuous-wave spectra were collected over 2 d in February 2014, while 16 light curves in the Cousins R and SDSS-r filters were collected in 2014, 2022, and 2023. We modelled the spin state using convex inversion before using the SHAPE modelling software to include the radar observations in modelling concavities and the distinctive neck structure connecting the two lobes. We find a spin state with a period of (5.7860 ± 0.0001) h and pole solution of λ = (180 ± 121)◦ and β = (−80 ± 7)◦ with morphology indicating a 520 m long bilobed shape. The model’s asymmetrical bimodal mass distribution resembles other small near-Earth asteroid contact binaries such as (85990) 1999 JV6 or (8567) 1996 HW1, which also feature a smaller ‘head’ attached to a larger ‘body’. The final model features a crater on the larger lobe, similar to several other modelled contact binaries. The model’s resolution is 25 m, comparable to that of the radar images used.
KW - Methods: observational
KW - Techniques: photometric
KW - Techniques: radar astronomy
KW - Minor planets, asteroids: individual: (388188) 2006 DP14
U2 - 10.1093/mnras/staf371
DO - 10.1093/mnras/staf371
M3 - Article
SN - 0035-8711
VL - 538
SP - 2311
EP - 2329
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -