The Level 1C Dayside Disk Images are interrupted via stored instrument commands when
target stars suitable for occultation measurements approach either limb.
To perform the occultation measurement, the slit mechanism inserts the 1 degree wide occultation (OCC)
slit at the spectrometer focal plane, and the scan mirrors slew the Field of View to the star.
The mirror is centered at a 225 km tangent point altitude. Occultations require 6 minutes to
execute (30 seconds to configure the instrument, 30 seconds for uncertainty in timing and pointing,
4 minutes for the actual occultation, 30 seconds for uncertainty in timing and pointing, and 30
seconds to return to HR slit). Once the occultation is complete, the HR slit is inserted, the scan
mirror returns to its departure point in the original mapping observation, and Dayside Disk Image is
resumed. By choice GOLD is limited to performing ~10 occultations a day for most of the year,
reducing the dayside mapping duty cycle by ~5%.
Version:2.3.1
The Level 1C Dayside Disk Images are interrupted via stored instrument commands when
target stars suitable for occultation measurements approach either limb.
To perform the occultation measurement, the slit mechanism inserts the 1 degree wide occultation (OCC)
slit at the spectrometer focal plane, and the scan mirrors slew the Field of View to the star.
The mirror is centered at a 225 km tangent point altitude. Occultations require 6 minutes to
execute (30 seconds to configure the instrument, 30 seconds for uncertainty in timing and pointing,
4 minutes for the actual occultation, 30 seconds for uncertainty in timing and pointing, and 30
seconds to return to HR slit). Once the occultation is complete, the HR slit is inserted, the scan
mirror returns to its departure point in the original mapping observation, and Dayside Disk Image is
resumed. By choice GOLD is limited to performing ~10 occultations a day for most of the year,
reducing the dayside mapping duty cycle by ~5%.
| Role | Person | |
|---|---|---|
| 1. | PrincipalInvestigator | spase://SMWG/Person/Richard.Eastes |
| 2. | MetadataContact | spase://SMWG/Person/James.M.Weygand |
GOLD web page with news and other information.
Eastes, R.W., McClintock, W.E., Burns, A.G. et al. Space Sci. Rev. (2017) vol. 212, pp.383.
FTPS access to Gold Level 1C data
HTTPS access to Gold Level 1C data
TDB seconds from January 1, 2000, 11:58:55.816 UTC at start of L1B time bin.
UTC date/time string: "2017-06-21T23:46:38.015Z".
The number of L1B dwells in each L1C pixel.
The number of L1B pixels in each L1C pixel.
Per pixel quality flags.
The wavelengths at each row.
The co-added raw count data.
The random uncertainty of the raw counts.
The co-added corrected counts.
Systematic uncertainty of the corrected counts.
Random uncertainty of the corrected counts.
The spectral radiance at each grid position.
The spectral radiance systematic uncertainty.
The spectral radiance random uncertainty.
The background counts subtracted in the background correction.
Latitude of the reference point.
Longitude of the reference point.
The tangent height of the pixel center ray from the Earth's crust.
The planar angle between the pixel ray from center and the sun direction.
The planar angle between the pixel ray from center and the spacecraft nadir.
The planar angle between the pixel ray from center and the normal to the reference point.
The planar angle between the sun direction to the reference point and the normal to the reference point.
The tangent height of the reference star with respect to GOLD.
The planar angle between the sun direction to the star tangent point normal.
Tangent point Latitude relative to fixed Earth frame of line to star.
Tangent point Longitude relative to fixed Earth frame of line to star.