Data Set Information
DATA_SET_NAME 52 COLOR ASTEROID SURVEY V1.0
DATA_SET_ID EAR-A-RDR-3-52COLOR-V1.0
NSSDC_DATA_SET_ID
DATA_SET_TERSE_DESCRIPTION
DATA_SET_DESCRIPTION Data Set Overview : The observations were made using a double CVF (circularly variable filter). The short wavelength portion of the CVF covered the octave from 0.8 to 1.6 microns with 3 percent resolution, while the long wavelength portion covered 1.5 to 2.6 microns with 5 percent resolution. There is some overlap in the spectral coverage between 1.5 and 1.6 microns, which is evident as a discontinuity in the wavelengths after the first 32 values, which were obtained with the short wavelength portion, while the remaining 20 values were obtained with the long wavelength portion. Errors were computed from the standard deviation of the multiple scans through the CVF. If only one scan was performed, the error is left blank. Note that due to the small number of scans, the errors are often both underestimated and overestimated. Some wavelength positions correspond to telluric features and were intentionally blanked. In other cases, especially near the ends of the CVF, the data were either not taken or were hopelessly noisy, so those entries were also blanked. The following code letters are used for the various solar analog stars: A : 18 Aquarii B : 16 Cygni B O : 13 Orionis V : 70 Virginis The observation date for 113 Amalthea is given as 054/05/85 in the original machine readable data file. The assumption has been made that the 4 is a typographical error, based on the fact that other observations were made on 05/05/85. Not all dates of observation are available. In particular, those asteroid observations contributed by R.H. Brown did not include observation dates in the original machine readable data file. One observation was taken from the literature, namely Cruikshank and Hartmann (1984) [CRUIKSHANK&HARTM1984]. Reference: Cruikshank, D.P., and W.K. Hartmann 1984. The meteorite- asteroid connection: Two olivine-rich asteroids. Science 223, 281-283. Parameters : The data tables have one entry for each observation, with fields for the following parameters. Asteroid catalog number, a code for the solar analog star used with that observation, the date of observation, and reflectances and error values for each of 52 bandpasses. Data : The reflectances in each of the 52 bands are given in the table '52color.tab'. The errors are given in the table '52error.tab'. The asteroid identification, solar analog code, and observation date are provided in each of these two files. Ancillary Data : The ancillary file '52waves.tab' presents the effective wavelengths of each of the 52 positions of the CVF which were used for the survey, arranged in a single record with a separate field for each wavelength. The file '52waves2.tab gives the same information arranged with one wavelength per record. Each record also contains the FWHM of the bandpass. Media/Format : This dataset is released in the form of ASCII files which may be stored on disk or other magnetic medium and which may be distributed by ftp, email, real-time access by remote login, or by whatever means is most convenient.
DATA_SET_RELEASE_DATE 1995-03-31T00:00:00.000Z
START_TIME 1983-01-01T12:00:00.000Z
STOP_TIME 1987-01-01T12:00:00.000Z
MISSION_NAME SUPPORT ARCHIVES
MISSION_START_DATE 2004-03-22T12:00:00.000Z
MISSION_STOP_DATE N/A (ongoing)
TARGET_NAME ASTEROID
TARGET_TYPE ASTEROID
INSTRUMENT_HOST_ID
INSTRUMENT_NAME
INSTRUMENT_ID
INSTRUMENT_TYPE
NODE_NAME Small Bodies
ARCHIVE_STATUS SUPERSEDED
CONFIDENCE_LEVEL_NOTE Review : This dataset was included in an external review on March 31, 1995.
CITATION_DESCRIPTION Citation TBD
ABSTRACT_TEXT The observations were made using a double CVF (circularly variable filter). The short wavelength portion of the CVF covered the octave from 0.8 to 1.6 microns with 3 percent resolution, while the long wavelength portion covered 1.5 to 2.6 microns with 5 percent resolution. There is some overlap in the spectral coverage between 1.5 and 1.6 microns, which is evident as a discontinuity in the wavelengths after the first 32 values, which were obtained with the short wavelength portion, while the remaining 20 values were obtained with the long wavelength portion.
PRODUCER_FULL_NAME JEFFREY F. BELL
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