|
Data Set Information |
||
| DATA_SET_NAME |
CASSINI SATURN UVIS SOLAR STELLAR BRIGHTNESS TIME SERIES 1.2 |
|
| DATA_SET_ID |
CO-S-UVIS-2-SSB-V1.2 |
|
| DATA_SET_TERSE_DESCRIPTION |
A series of multi-banded images. A set of time series of photometer data. A set of spectra. |
|
| DATASET_DESCRIPTION |
A set of spectra. |
|
| DATA_SET_RELEASE_DATE |
null |
|
| RESOURCE_LINK |
atmos.nmsu.edu:8443/pds/Browse |
|
| DATA_OBJECT_TYPE |
TIME SERIES |
|
| START_TIME |
1999-007T00:00:00 |
|
| STOP_TIME |
null |
|
| MISSION_NAME |
CASSINI-HUYGENS |
|
| MISSION_START_DATE |
1997-10-15 |
|
| MISSION_STOP_DATE |
null |
|
| TARGET_NAME |
S RINGS ATLAS CALYPSO DIONE ENCELADUS EPIMETHEUS HELENE HYPERION IAPETUS JANUS MIMAS PAN PANDORA PHOEBE PROMETHEUS RHEA TELESTO TETHYS DARK SKY STAR ALBIORIX TARVOS IJIRAQ SIARNAQ SKOLL PAALIAQ TITAN SATURN YMIR BESTIA SUTTUNGR S12_2004 |
|
| INSTRUMENT_NAME |
ULTRAVIOLET IMAGING SPECTROGRAPH |
|
| INSTRUMENT_ID |
UVIS |
|
| INSTRUMENT_TYPE |
SPECTROGRAPH |
|
| INSTRUMENT_HOST_ID |
CO |
|
| NODE_NAME | ||
| ARCHIVE_STATUS |
ACCUMULATING |
|
| CONFIDENCE_LEVEL_NOTE |
CONFIDENCE_LEVEL_NOTE = " Confidence Level Overview ========================= The UVIS data objects are organized into separate observations. Each observation contains data taken from one configuration of the instrument. There may be more than one observation generated from one instrument configuration. This may occur because science data generated by the UVIS instrument is dropped when corrupted data is detected or transmission failures occur. The UVIS ground system detects this and divides the data into two observations, one terminated prior to the data drop the next beginning immediately afterword. The start time and duration of an observation correspond to the end times of the first and last records in the observation. Incomplete observations are filled with zeroes. Over 95% of data taken by the instrument is contained in the UVIS archive. Only one hardware feature affects UVIS data. A light leak in the instrument casing causes an increase in the background counts in the lower half of the EUV channel wavelength range. This effect is detectable by visual inspection of a graph of the data. No tools for detection or correction of these background counts exists. One anomaly in the flight software caused data errors to appear when multiple windows which do not cover the entire EUV or FUV detector are defined. In an observation, the data errors appear as randomly located spikes in detector count values, and one completely incorrect spatial line located at a random spatial index. These errors are detectable by visual inspection of a plot of the data. The anomaly was fixed by a revison to the software and effects data between launch and 2001-071 09:00:00 UTC Review ====== This volume has completed a peer review by the PDS. The peer review panel consisted of Lyle Huber, Mitch Gordon, Steven Adams, Ron Joyner and Mark Vincent representing PDS, David Judd and Wayne Pryor from the, UVIS team Diane Connor from the Cassini Project and Kurt Retherford and John Clarke as outside users." |
|
| CITATION_DESC | " | |
| ABSTRACT_TEXT | ||
| RESOURCES | ||
