Search arXiv⌕ Search

arXiv · 2602.12554

Bundle adjustment of Hayabusa2's ONC images and controlled color mosaic map of Ryugu

Abstract

JAXA's Hayabusa2 mission successfully returned samples from the asteroid Ryugu in December 2020. It executed two touchdowns to collect the surface and subsurface materials, one close to the crater created by an artificial impactor. The onboard camera system, Optical Navigation Camera (ONC), with two wide-angle cameras and one narrow-angle camera with seven color filters, was crucial for mapping geomorphology and composition such as hydrated minerals during navigation and scientific observation. More than 8,300 images revealed Ryugu's spinning-top shape and boulder-covered surface. However, most high-resolution images captured during descent/touchdown operations lacked precise location data and camera position/orientation information. Image geometry was refined using photogrammetric bundle adjustment. This method enabled the refinement of all high-resolution images captured during descent/touchdown operations. Furthermore, map-projected GeoTIFF images in GIS format containing geographic metadata were created for all ONC images, and these were integrated to construct global and regional mosaic maps. To facilitate scientific research on Ryugu, these refined image geometry information, maps, and mosaics are publicly available via https://doi.org/10.7910/DVN/WW3IH0

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Naoyuki Hirata, Eri Tatsumi, Mayumi Ichikawa, Kazuhiro Honda, Sayuri Tanaka. 2026-02-13. Bundle adjustment of Hayabusa2's ONC images and controlled color mosaic map of Ryugu. https://doi.org/10.7910/dvn%2Fww3ih0

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

Pulsed Accretion onto Eccentric Binaries in Highly Misaligned Circumbinary Disks

We present three-dimensional smoothed particle hydrodynamics simulations of highly misaligned circumbinary disks (CBDs) around moderately eccentric equal-mass binaries ($e_\mathrm{b}=0.5$). We show that the binary accretion is modulated on the binary orbital period and exhibits two pulses near periastron. The dominant pulse peaks before periastron for an initial binary-disk misalignment of $60^\circ$, shifts to after periastron at $90^\circ$, and occurs at an even later post-periastron phase at $120^\circ$. We further show that the two pulses are accompanied by a time-dependent response of the circumstellar disks (CSDs) and by different distributions of accreting material within the cavity and around the CSDs. The qualitative pre- versus post-periastron distinction is also present in individual binary orbits despite variations in pulse amplitude. Our results motivate future tests of whether pulse timing is related to binary-disk orientation.

astro-ph.EP↗

On the Compositions of Interstellar Objects

As physical samples of distant planetary systems, the compositions of interstellar objects (ISOs) should correlate with the properties of their diverse parent stars. We combine a chemical partition model with a sample of stellar elemental abundances from APOGEE DR17 to predict the abundances of commonly-observed cometary volatiles in ISOs. We find that the compositions of ISOs vary significantly between different stars. In particular, we predict a strong correlation between an ISO's ammonia abundance and its parent star's metallicity: high-metallicity stars will create ISOs rich in ammonia. This suggests the production rates of NH$_3$'s photolytic daughter products are an ideal observational tracer for the origins of ISOs. We infer that 2I/Borisov formed around a star of near-solar metallicity ($-0.4\lesssim[\mathrm{Fe}/\mathrm{H}]\lesssim0.3$), and corroborate the velocity- and isotope-based inferences that 3I/ATLAS formed around a lower-metallicity star ($-0.8\lesssim[\mathrm{Fe}/\mathrm{H}]\lesssim0.0$). The production rates of 2I and 3I imply both only contain hypervolatiles such as CO and N$_2$ that are trapped in other less-volatile ices, similar to typical Solar System comets. Despite this, we argue that true hypervolatile-ice-rich ISOs may exist; they would exhibit high CO and N$_2$ production rate ratios, possibly similar to those of C/2016 R2 (PanSTARRS). Our predictions provide context for future ISO discoveries, opening a path to link the properties of their origin systems to observable production rates.

astro-ph.EP↗

TS23/McDonald and FIES/NOT strike again. Two new warm Jupiter systems and outer companions in a third

Warm Jupiters (gas giant planets with orbital periods of P$\sim$8-200 d) are thought to be largely unaffected by the tidal interactions that can erase information about the dynamical histories of hot Jupiters. Their orbital eccentricities ($e$) and stellar obliquities are therefore expected to be preserved, making them valuable probes of giant-planet formation and migration. Our aim is to identify and characterise transiting warm Jupiters in order to expand the sample of well-characterised systems and enable further studies of giant-planet formation and migration. We analyse TESS transit photometry together with ground-based radial velocity measurements and perform a joint fit of the photometric and spectroscopic data from the TS23 and FIES spectrographs to determine the planetary and orbital parameters. We report on the discovery and characterisation of two new, transiting warm Jupiters; TOI-5120 b ($M_p = 1.23\pm0.05$ M$_{\rm Jup}$, $R_p = 0.969\pm0.017$ R$_{\rm Jup}$, $P = 24.91645\pm0.00002$ d, $e = 0.10\pm0.02$) and TOI-5699 b ($M_p = 0.25\pm0.03$ M$_{\rm Jup}$, $R_p = 0.996\pm0.015$ R$_{\rm Jup}$, $P = 22.01850\pm0.00004$ d, $e = 0.30^{+0.09}_{-0.08}$). We also refine the parameters of the known warm Jupiter TOI-2158 b ($M_p = 0.87\pm0.04$ M$_{\rm Jup}$, $R_p = 0.899\pm0.015$ R$_{\rm Jup}$, $P = 8.60079^{+0.00002}_{-0.00001}$ d, $e = 0.028^{+0.013}_{-0.014}$). In addition, we detect an outer planetary companion, TOI-2158 c ($M_p \sin i = 1.62\pm0.13$ M$_{\rm Jup}$, $P = 414.5^{+1.5}_{-1.6}$ d, $e = 0.54\pm0.04$), and identify a long-term radial velocity trend that may indicate another planetary companion on a wide orbit. The diverse architectures of these systems, in particular the presence and absence of outer companions, highlight the range of dynamical pathways leading to warm Jupiters.

astro-ph.EP↗