Mathilde

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Stooke shape model (left). Near Image (center). SPC shape model (Right).

Topography of the lunar poles, constructed using stereophotoclinometry (SPC) and Clementine images, is compared with results from LOLA and LRO wide-angle camera analyses.

Publications

Digital Terrain Models of Mathilde and the Moon

Reference Citation: Weirich, J.~R., Palmer, E.~E., Domingue, D.~L.\ 2019.\ Digital Terrain Models of Mathilde and the Moon.\ Lunar and Planetary Science Conference 2681.

Abstracts

https://ui.adsabs.harvard.edu/abs/2011LPI….42.2535G/abstract 50th Lunar and Planetary Science Conference, held 18-22 March, 2019 at The Woodlands, Texas. LPI Contribution No. 2132, id.2681

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Ryugu

Preview
An SPC model of Ryugus carbonaceous aster at a resolution of 3cm

This SPC model was generated during the JAXA Hayabusa 2 mission.

Data: https://www.darts.isas.jaxa.jp/pub/hayabusa2/paper/Watanabe_2019/README.html

Bennu

OSIRIS REx NASA Mission

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A SPC rendered shape model of Bennu

The accuracy of the global digital terrain model (GDTM) of Bennu obtained by the OSIRIS-REx mission to date has achieved global requirements earlier than anticipated. Additionally, a comparison between real images and synthetic images derived from the GDTM using normalized cross correlation show an exceptionally good match.

Data

101955 Bennu Shape Model PDS SBN OSIRIS-REx SPICE Data Archive

Publications:

Image Cross Correlation as a Measurement of Shape Model Quality

Reference Citation: Palmer, E.~E., Weirich, J.~R., Campbell, T., Barnouin, O.~S., Daly, M.~G., Lauretta, D.~S.\ 2018.\ Image Cross Correlation as a Measurement of Shape Model Quality.\ Lunar and Planetary Science Conference 1106.

Stereophotoclinometry Models in Support of the OSIRIS-REx Mission .

Reference Citation: Palmer, E.~E., and 11 colleagues 2019.\ Stereophotoclinometry Models in Support of the OSIRIS-REx Mission.\ Lunar and Planetary Science Conference 2588.

Evaluation of the Bennu Global Digital Terrain Model for OSIRIS-REx

Reference Citation: Palmer, E., and 7 colleagues 2019.\ Evaluation of the Bennu Global Digital Terrain Model for OSIRIS-REx.\ EPSC-DPS Joint Meeting 2019 2019, EPSC-DPS2019-387.

Abstracts:

Evaluation of the Bennu Global Digital Terrain Model for OSIRIS-REx EPSC AbstractsVol. 13, EPSC-DPS2019-387-1, 2019 EPSC-DPS Joint Meeting 2019

Stereophotoclinometry Models in Support of the OSIRIS-REx Mission 50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132)

Image Cross Correlation as a Measurement of Shape Model Quality 49th Lunar and Planetary Science Conference 19-23 March, 2018, held at The Woodlands, Texas LPI Contribution No. 2083, id.1106

Evaluation of Topographic Error and Quality with Stereophotoclinometry 49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083)

Error Analysis of Stereophotoclinometry in Support of the OSIRIS-REx Mission American Astronomical Society, DPS meeting #47, id.213.17

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A progression of the SPC process throughout the OSRIS-REx mission

2013 Nolan Model
The first shape model was done by Dr. Nolan and was based on radar imaging of Bennu (Nolan, 2013). This model was the basic reference for the mission planning of OSIRIS-REx. One can see that the basic shape of Bennu was well characterized. The comparison image was from early November 2018.
12 November Early Limb-based model
Altimetry Working Group used early Approach Phase rotation images, every 10°, to determine the limbs and construct a model with a 3m ground sample distance. It improved the accuracy of the shape model, and Navigation Team had exceptional success with its center-finding routines.
22 November Early SPC model
While SPC can be used earlier, we used the limb-based model until the imaging data was exceptional. This reduces artifacts and improves accuracy for following models. OSIRIS-REx approached the asteroid at a low phase, so there are limited shadows from the topography.
2nd December – End of approach
At the end of the Approach Phase, a 1.5m model was generated from the full suite of approach images. Limb, albedo and topography agreement was very good; however, the poles lacked imaging so there is only limb-based data there. Final imagery pixel size was 32cm near the equator.
End of PreSurvey Model
At the end of preliminary Survey, we generated a model with a 75cm ground sample distance. Both the topography and albedo representation were excellent and exceeded our expectations. Preliminary Survey data was 50-75 cm in pixel size.

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Here is a regional model at the end of Preliminary Survey, with 50 to 75 cm resolution. This is of DL15 aka Nightingale aka the Primary TAG site. Images below are the progression as we processed more images.
14 cm model resolution of the Primary TAG site.
5 to 6 cm resolution of the Primary TAG site.
State of the model after Natural Feature Tracking (NFT) landmarks have been generated. Some regions have high resolution (up to 1.7 cm) while others are the same as in the above image.
Animate GIF showing the comparison between spacecraft image and model for Primary TAG site. 6 second loop.

Ceres

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Ceres Shape model

Data

Ceres Shape model SBN PDS 2018

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Vesta

An SPC rendering of Cornelia Crater on the asteroid Vesta

The DAWN spacecraft has now left Vesta, leaving a legacy of more than 16000 clear filter images of the asteroid. During the last month of Dawn’s stay at Vesta, the sun slowly crept northward, enabling the spacecraft to view topography closer to the north pole. We have used these images with our stereophotoclinometry (SPC) software to construct topography for most of Vesta’s surface to 50 meter resolution, and below about 60 degrees south to 20 meter resolution. We present this topography as a 1/64 degree gridded map (about 70 m resolution), as a stereographic projection of the south polar region at 25 m resolution and as a global shape model with 1.57 million vectors. In addition, we present solutions for the s/c position and camera pointing at all imaging times during DAWN’s entire stay at Vesta.

Publications

SPC Shape and Topography of Vesta from DAWN Imaging Data

Reference Citation: Gaskell, R.~W.\ 2012.\ SPC Shape and Topography of Vesta from DAWN Imaging Data.\ AAS/Division for Planetary Sciences Meeting Abstracts #44 209.03.Paragraph

Abstracts

SPC Shape and Topography of Vesta from DAWN Imaging Data American Astronomical Society, DPS meeting #44, id.209.03

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Eros

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Eros Shape Model
September 2008

The shape model of 433 Eros derived by Robert Gaskell from NEAR MSI images. The model is provided in the implicitly connected quadrilateral (ICQ) format in four levels of resolution. This version of the model was prepared on Feb. 23, 2008.

Data

Gaskell Eros Shape Model Gaskell PDS SBN data archive 2008

Publications

Gaskell Eros Shape Model V1.0

Reference Citation: Gaskell, R.~W.\ 2008.\ Gaskell Eros Shape Model V1.0.\ NASA Planetary Data System NEAR-A-MSI-5-EROSSHAPE-V1.0.

Abstracts

Eros shape model abstract NASA Planetary Data System, id. NEAR-A-MSI-5-EROSSHAPE-V1.0

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Itokawa

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Hayabusa AMICA mission – August 2007

The shape model of 25143 Itokawa derived by Robert Gaskell from Hayabusa AMICA images. The model is provided in the implicitly connected quadrilateral (ICQ) format in four levels of resolution. This version of the model was prepared on August 29, 2007.

Data

Itokawa shape model, Gaskell 2007, PDS SBN data archive

Publications

Gaskell Itokawa Shape Model V1.0

Reference Citation: Gaskell, R., and 8 colleagues 2008.\ Gaskell Itokawa Shape Model V1.0.\ NASA Planetary Data System HAY-A-AMICA-5-ITOKAWASHAPE-V1.0.

Abstracts

Gaskell Itokawa Shape Model V1.0 NASA Planetary Data System, id. HAY-A-AMICA-5-ITOKAWASHAPE-V1.0

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