Vesta Dawn FC HAMO Global DTM 93m

Primary Authors

NASA/JPL-Caltech/UCLA/MPS/DLR/IDA

Originators

Dawn Team

Publisher

USGS Astrogeology Science Center

Publication Date

2013-12-12

Abstract

Product Information: DAWN orbited Vesta during HAMO in 21 cycles between December 2011 and end of April 2012. Dawn orbited Vesta during HAMO in 6 cycles between end of September end early November 2011. The framing camera took about 2,500 clear filter images with a resolution of about 70 meters per pixel (m) during these cycles (Roatsch et al., 2012). This digital terrain model (DTM) was created from 5439 HAMO stereo FC clear filter images at ~92 m (48 pixels per degree). The value are in radii given in meters with an +-8 meter mean intersection error. Note: This preliminary file has been shifted 150 degrees eastward (such that Claudia crater is located at 146E) to match the IAU-approved Claudia Double Prime system (from the Dawn-Claudia system as released by DLR dated 2013-11-22). This should not be used for processing with in the ISIS3 software since the required SPICE is not available for this system. Mission and Instrument Information: The Dawn spacecraft launched on September 25, 2007 onboard a Delta II-Heavy Rocket. The instrument payload consisted of two identical framing cameras (FC1 & FC2), a visible and infrared mapping spectrometer (VIR, and a gamma ray and neutron detector (GRaND). DAWN is a National Aeronautics and Space Administration (NASA) Discovery Program mission managed by the Jet Propulsion Laboratory (JPL) with the principal investigator and science operations center located at the University of California, Los Angeles. The framing cameras were built by the Max Planck Institute for Solar System Research with significant contributions by the German Aerospace Center, Institute of Planetary Research (DLR) and in coordination with the Institute of Computer and Communication Network Engineering (Polansky et al., 2016). Dawn spacecraft orbited Vesta in a series of science orbits designed to gradually increase the resolution and quality of science measurements as the mission at each target (Vesta & Ceres) progressed. The four science orbits are: rotation characterizations (RC1 and RC2) at 14,000 km, survey at 4,900 km (RC3), high altitude mapping orbit (HAMO) 1,950 km, and low altitude mapping orbit (LAMO) 850 km. HAMO provided the opportunity to collect data for the global topography model by collecting six complete clear-image maps: two at nadir and four at off-nadir attitudes (Polansky et al., 2016). References: Polanskey, C., Joy, S., & Raymond, C. (2016). Dawn Ceres Mission: Science Operations Performance. Paper presented at the SpaceOps Conference, Daejeon, Korea. https://arc.aiaa.org/doi/abs/10.2514/6.2016-2442 Preusker, F., Scholten, F., Matz, K.-D., Roatsch, T., Jaumann, R., Raymond, C. A., & Russell, C. T. (2014). Global Shape of Vesta from Dawn FC stereo images. Paper presented at the 45th Lunar Planetary Science Conference, Lunar and Planetary Institute, Houston, TX. http://www.hou.usra.edu/meetings/vesta2014/pdf/2027.pdf Roatsch, T., Kersten, E., Matz, K.-D., Preusker, F., Scholten, F., Jaumann, R., Raymond, C. A., & Russell, C. T. (2012). High resolution Vesta High Altitude Mapping Orbit (HAMO) Atlas derived from Dawn framing camera images. Planetary and Space Science, 73(1), 283-286. https://doi.org/10.1016/j.pss.2012.08.021 Russell, C. T., & Raymond, C. A. (2011). The Dawn Mission to Vesta and Ceres. Space Science Reviews, 163(1-4), 3-23. https://doi.org/10.1007/s11214-011-9836-2

Purpose

One of the prime science goals was the determination of the global shape of Vesta represented by a digital terrain model (DTM). The DTM is particularly important, because it is essential for derivation of physical properties of Vesta as well as for precise ortho-image registration, mosaicking, and map generation of monochrome/color framing camera images. In addition a DTM is needed for quantitative geomorphologic analysis and precise photometric analysis from detailed local surface incli-nation. For this purpose the entire illuminated surface was imaged stereoscopically using the Dawn Framing Camera (Dawn FC).

Contact and Distribution

Format

Digital Elevation Model, Global Mosaic, Raster Data

Access Constraints

None

Access Scope

PDS

Use Constraints

Please cite authors

Edition

20131210

Supplemental Information

http://www.hou.usra.edu/meetings/vesta2014/pdf/2027.pdf, http://dawndata.igpp.ucla.edu/download.jsp?file=documents/VESTA_COORDINATES/VESTA_COORDINATES_121214.PDF, http://dawndata.igpp.ucla.edu/

Native Data Set Environment

ISIS v3

Astrogeology Theme

Asteroids, Cartography, Image Processing, Topography

Mission Names

Dawn

Instrument Names

FC

Online Package Link

https://astrogeology.usgs.gov/search/map/vesta_dawn_fc_hamo_global_dtm_93m

External File Size

570 MB

Online File Link

https://planetarymaps.usgs.gov/mosaic/Vesta_Dawn_HAMO_DTM_DLR_Global_48ppd.tif

Contact Address

2255 N. Gemini Drive

Contact City

Flagstaff

Contact State

AZ

Contact Postal Code

86001

Contact Email

astroweb@usgs.gov

Data Status and Quality

Time Period of Content (start)

2011-12-01

Time Period of Content (stop)

2012-04-30

Currentness Reference

Ground condition

Progress

In Work

Update Frequency

As needed

Logical Consistency

The Framing Camera is a multispectral imager that also serves as an optical navigation camera. The detector is a 1024x1024 pixel Atmel/Thomson TH7888A CCD with 14 micron pixels. It has eight filters numbered F1 through F8, including a broadband (clear) filter and narrow band filters ranging from 438 nm to 965 nm. The Framing camera instrument includes two redundant cameras of identical design, referred to as FC1 and FC2. For full information about the FC instrument, see Schroeder and Gutierrez-Marques (2011). Reference: Schroeder, S.E., and P. Gutierrez-Marques, Calibration Pipeline, MPS Report DA-FC-MPAE-RP-272, Issue 2, Rev. a, 20 July 2011. The team constrained all HAMO clear filter images within their stereo requirements and achieved at least triple stereo image coverage for the entire illuminated surface. In total, about 35, 000 inde-pendent multi-stereo image combinations were used to determine selected image tie points by multi-image matching for the set-up of a 3D control network of about 83, 000 surface points.

Completeness Report

This DTM was created from 5439 HAMO stereo FC clear filter images at ~92 meters per pixel. The DTM covers approximately 95 percent of the surface for Vesta

Process Description

The stereo-photogrammetric processing for (4) Vesta is based on a software suite that has been developed within the last decade. It has been applied successfully to several planetary image data sets and covers the entire workflow from photogrammetric block adjustment to DTM and map generation. References: Gwinner K. et al., (2010), Earth Planet. Science Letters, 294, Issues 3-4, pp. 506-519.; Preusker F. et al., (2011), Planetary Space Science, 59, pp. 1910-1917. [5] Scholten F. et al., (2012), JGR, 117.; Jaumann R. et al., (2012), Science, 336, pp. 687-690.

Source Title

DLR_HAMO_DTM

Source Online Linkage

{https://sbn.psi.edu/pds/resource/dawn/dwnvfcmosaics.html,https://sbn.psi.edu/pds/archive/maps.html}

PDS Status

PDS 3 Archived

Attribute Accuracy Report

Best Effort

Horizontal Positional Accuracy Report

Unknown

Vertical Positional Accuracy Report

Accurate to Control Net

Geospatial Information

Target

Vesta

System

Small Bodies

Minimum Latitude

-90

Maximum Latitude

90

Minimum Longitude

-180

Maximum Longitude

180

Direct Spatial Reference Method

Raster

Object Type

Grid Cell

Raster Row Count (lines)

8640

Raster Column Count (samples)

17280

Bit Type (8, 16, 32)

32

Quad Name

Radius A

255000

Radius C

255000

Bands

1

Pixel Resolution (meters/pixel)

92.72061651

Scale (pixels/degree)

48

Vertical Coordinate System Units

Meters

Map Projection Name

Simple Cylindrical

Latitude Type

Planetocentric

Longitude Direction

Positive East

Longitude Domain

-180 to 180