This data set contains all of the Voyager images from Uranus in cleaned, calibrated and geometrically corrected forms. It is derived from data set VG2-U-ISS-2-EDR-V1.0.

This data set contains all of the Voyager images from Uranus in cleaned, calibrated and geometrically corrected forms. It is derived from data set VG2-N-ISS-2-EDR-V1.0.

This Voyager 2 Neptune data set is available on CD-ROM and magnetic tape.

The data set contains measurements from both the infrared interferometer spectrometer and the broadband reflected solar radiometer and ancillary data. The data set is ordered by time as measured by the Flight Data System Count (FDSC). This represents the data frame number, modulo 60. Also included is pointing and other information on the geometry associated with a given data record.

Published colors of Trans-Neptunian objects through December 2001.

This data set consists of 4-second edited, wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Uranian magnetosphere. For each 4-second interval, a field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kiloHertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of intensities (16 channels) is the time of the beginning of the scan. During data gaps where complete 4-second spectra are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. When one or more channels are missing within a scan, the missing measurements are zero-filled. Data are edited but not calibrated. The data numbers in this data set can be plotted in raw form for event searches and simple trend analysis since they are roughly proportional to the log of the electric field strength. Calibration procedures and tables are provided for use with this data set described below.

We processed 41 Voyager 2 images of Neptune’s moon Triton with pixel scales < 2 km/pixel form their raw, compressed, archived state to more usable cloud-optimized geotiffs, which can easily be used within spatial analysis software such as GIS. Processing was done using the USGS’ ISIS software and included geometric and radiometric calibration, and the removal of image reseaux and corner markers (originally used for geometric calibration). The images were also photogrammetrically controlled relative to one another to improve their locations on the surface, which were initially inaccurate by up to 200 km. After performing a least squares bundle adjustment, the root mean square (RMS) uncertainty in image locations was 0.50, 0.52, and 0.51 pixels in latitude, longitude, and radius, respectively, with minimum and maximum residuals of -4.21 and +3.197 pixels, respectively. Each individual image was warped to an orthographic projection centered at 15o W and 18o N at the native image resolution. Because reseaux removal introduces interpolated data, two versions of each image are provided: a fully processed version with reseaux removed, and a partially processed version that retains the reseaux (i.e., no interpolation). We also generated a mosaic of Triton images that is spatially consistent with the entire dataset and provides context for the individual images (not every image is included in the mosaic). The mosaic uses the same orthographic projection as the individual images, but a consistent scale of 600 m/pixel. Three versions of the mosaic are included: a fully processed version (reseaux removed, some interpolated pixel values), a partially processed version (reseaux retained, no interpolation), and a fully processed but sharpened (high pass filter with 100% albedo add-back) to enhance surface features. This data release improves the usability and accessibility of this singular dataset and enables new scientific investigations of Triton.

This dataset consists of edited browse data derived from an original dataset obtained from the Voyager 2 Planetary Radio Astronomy (PRA) instrument in the vicinity of Uranus. Data are provided for 70 instrument channels covering the range from 1.2 kHz to 1326 kHz in uniform 19.2 kHz steps, each 1 kHz wide. Data are included for the period 1986:019:00:00 through 1986:031:23:59. In order to produce this dataset from the original raw PRA data, several steps have been taken:

The data set contains measurements from both the infrared interferometer spectrometer and the broadband reflected solar radiometer and ancillary data. The data set is ordered by time as measured by the Flight Data System Count (FDSC). This represents the data frame number, modulo 60. Also included is pointing and other information on the geometry associated with a given data record.