Vesta Dawn FC HAMO Global Mosaic 60m

Primary Authors

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

Originators

Dawn Team

Publisher

USGS Astrogeology Science Center

Publication Date

2013-12-10

Abstract

Product Information: DAWN orbited Vesta during HAMO in 21 cycles between December 2011 and end of April 2012 and in 6 cycles between end of September end early November 2011. The FC took about 2,500 clear filter images with a resolution of about 60 meters per pixel (m) during these cycles. The images were taken with different viewing angles and different illumination conditions. Pixel resolution is 60 meters per pixel (m). We selected images from one cycle (cycle 3) for the mosaicking process to have similar viewing and illumination conditions. Cycle 3 with 518 images was selected since it was the first cycle with almost complete global coverage. Very minor gaps in the coverage were filled with a few images from cycle 2 (Roatsch et al., 2012). 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 in November 2013). 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

The NASA Dawn spacecraft entered orbit of the inner main belt asteroid 4 Vesta on July 16, 2011, and spent about one year in orbit to characterize the geology, elemental and mineralogical composition, topography, shape, and internal structure of Vesta. One of the major goals of the mission was a global mapping of Vesta. The DAWN mission was mapping Vesta from three different orbit heights during Survey orbit (3100 km altitude), HAMO (High Altitude Mapping Orbit, 700 km altitude), and LAMO (Low Altitude Mapping Orbit, 210 km altitude).

Contact and Distribution

Format

Global Mosaic, Raster Data, Remote-sensing Data

Access Constraints

None

Access Scope

PDS

Use Constraints

Please cite authors

Edition

20131210

Supplemental Information

http://www.sciencedirect.com/science/article/pii/S0032063312002589, http://dawndata.igpp.ucla.edu/tw.jsp?section=data/FC/Maps/HAMO_mosaic_DLR, 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, Image Processing, Remote Sensing

Mission Names

Dawn

Online Package Link

https://astrogeology.usgs.gov/search/map/vesta_dawn_fc_hamo_global_mosaic_60m

External File Size

341 MB

Online File Link

https://planetarymaps.usgs.gov/mosaic/Vesta_Dawn_FC_HAMO_Mosaic_Global_74ppd.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.

Completeness Report

The framing camera took about 2, 500 clear filter images with a resolution of about 70 meter per pixel during the various cycles.

Process Description

The first step of the processing chain is to ortho rectify the images to the proper scale and map projection type. This process requires detailed high-resolution information of the local topography of Vesta. The global topgraphy was calculated during the stereo processing of the HAMO images and was used here. The shape model was used for the calculation of the ray intersection points while the map projection itself was done onto a sphere with a mean radius of 255 km. The next step was the mosaicing of all images to one global mosaic of Vesta, the so called basemap. 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 in November 2013). At the original edge when wrapped a nodata line was pushed into the mosaic. This was covered using a couple neighboring pixels for artistic purposes only.

Source Title

Dawn FC HAMO Global Mosaic

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

Unknown

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)

13352

Raster Column Count (samples)

26704

Bit Type (8, 16, 32)

8

Quad Name

Radius A

255000

Radius C

255000

Bands

1

Pixel Resolution (meters/pixel)

59.99896095

Scale (pixels/degree)

74.1778

Map Projection Name

Simple Cylindrical

Latitude Type

Planetocentric

Longitude Direction

Positive East

Longitude Domain

-180 to 180