PDS: The Planetary Atmospheres Node
The Corona Bundle
Software Interface Specification (SIS) - Description of the instrument and data structures
The data are in FITS format (Need to acquire a FITS reader?).
Raw Data - Raw Data - Maven/IUVS raw FITS files will contain both images and tables. Many fields are direct unconverted copies of telemetry produced by the instrument. The units for such fields, data numbers (DN), may represent ADC counts, encoder steps, discrete time intervals, and so on. See the SIS section 6.1.1.Table 18: Raw data file structure.
Calibrated Data
- Calibrated Data - Calibrated FITS are similar in structure to the raw products but the data are calibrated spectral radiance in units of kilorayleighs/nm, along with estimates of uncertainty and engineering telemetry has been translated from DN to physical units. See the SIS section 6.1.2 Table 19: Calibrated data file structure.
An Instrument Log (csv), containing URN, start and stop time, orbit, wavelength interval, geometry at the midpoint of the observation, Mars year, Ls and file size, can be used to select specific files.
Processed data
Processed data are stored as FITS files with detached XML labels and are calibrated data that have been reduced by isolating emission features and implementing spacial binning to facilitate processing. See the SIS section 6.1.3 Table 21: Corona processed data file structure.
A Instrument Log (csv), containing URN, start and stop time, orbit, wavelength interval, geometry at the midpoint of the observation, Mars year, Ls and file size, can be used to select specific files.
Derived data
IUVS derived data files vary among observation modes. They are stored as FITS files with detached XML labels and contain derived densities and column abundances at the native geometry of the observation and/or on a regular grid in altitude or latitude and longitude, as appropriate. See the SIS section 6.1.4 Table 28: Corona derived data file structure.
A Instrument Log (csv), containing URN, start and stop time, orbit, wavelength interval, geometry at the midpoint of the observation, Mars year, Ls and file size, can be used to select specific files.
In addition to the above files the Mission Time Line (csv) can be used to select time intervals of interest. This file contains geometry parameters that are associated with the periapse of each orbit and supporting notes that will be updated and enhanced over time.
Retrieving specific files -- Coming soon!!
An Instrument Log (csv), containing URN, start and stop time, orbit, wavelength interval, geometry at the midpoint of the observation, Mars year, Ls and file size, can be used to select specific files.
Processed data
Processed data are stored as FITS files with detached XML labels and are calibrated data that have been reduced by isolating emission features and implementing spacial binning to facilitate processing. See the SIS section 6.1.3 Table 21: Corona processed data file structure.
A Instrument Log (csv), containing URN, start and stop time, orbit, wavelength interval, geometry at the midpoint of the observation, Mars year, Ls and file size, can be used to select specific files.
Derived data
IUVS derived data files vary among observation modes. They are stored as FITS files with detached XML labels and contain derived densities and column abundances at the native geometry of the observation and/or on a regular grid in altitude or latitude and longitude, as appropriate. See the SIS section 6.1.4 Table 28: Corona derived data file structure.
A Instrument Log (csv), containing URN, start and stop time, orbit, wavelength interval, geometry at the midpoint of the observation, Mars year, Ls and file size, can be used to select specific files.
In addition to the above files the Mission Time Line (csv) can be used to select time intervals of interest. This file contains geometry parameters that are associated with the periapse of each orbit and supporting notes that will be updated and enhanced over time.
Retrieving specific files -- Coming soon!!
