PDS_VERSION_ID = PDS3 RECORD_TYPE = "STREAM" LABEL_REVISION_NOTE = " 2016-08-22: Auto-generated by OLAF;" OBJECT = DATA_SET DATA_SET_ID = "EAR-A-I0046-3-REDDYMBSPEC-V1.0" OBJECT = DATA_SET_INFORMATION DATA_SET_NAME = "REDDY MAIN BELT ASTEROID SPECTRA V1.0" DATA_SET_COLLECTION_MEMBER_FLG = "N" DATA_OBJECT_TYPE = "TABLE" START_TIME = 2001-03-11 STOP_TIME = 2012-06-24T06:15:11 DATA_SET_RELEASE_DATE = 2016-06-02 /*Review Date*/ PRODUCER_FULL_NAME = "JUAN SANCHEZ" DETAILED_CATALOG_FLAG = "N" DATA_SET_TERSE_DESC = "This data set contains low-resolution near-infrared (0.7-2.5 microns) spectra of 90 main belt asteroids observed with the SpeX instrument on the NASA Infrared Telescope Facility." CITATION_DESC = "Reddy, V. and Sanchez, J.A., Reddy Main Belt Asteroid Spectra V1.0. EAR-A-I0046-3-REDDYMBSPEC-V1.0. NASA Planetary Data System, 2016." ABSTRACT_DESC = "This data set contains low-resolution (R~150) near-infrared (0.7-2.5 microns) spectra of 90 main belt asteroids observed with the SpeX instrument on the NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawai'i. This data set archives reduced, calibrated spectra of targets of opportunity observed from 2001 to 2012." DATA_SET_DESC = " Data Set Overview ================= All spectral observations were obtained using the SpeX instrument on the NASA IRTF in low-resolution prism mode. Observations were made remotely and in classical mode on site. SpeX in low resolution mode has resolving powers of R~100 across the wavelength region from ~0.7 to 2.5 microns. An infrared guider is available to guide on calibration stars (sidereal rates) and asteroids (non-sidereal rates). The main spectrograph uses a 1024x1024 Aladdin 3 InSb array and the guider uses a 512x512 Aladdin 2 InSb array [RAYNERETAL2004]. Low-resolution spectrographs like SpeX are ideal for resolving broad absorption features produced by abundant mafic minerals like olivine and pyroxene that make up many asteroid surface assemblages. The low resolution prism mode also helps in obtaining spectra with higher signal-to-noise-ratios (SNR) and asteroids as faint as Vmag~17.5 are routinely observed. Spectral observations for this data set were made by taking nodded spectral image pairs of the asteroid, local standard star (for telluric correction), solar-analog stars, and calibration flat-field and argon arc-lamp images. The placement of these stellar observations, temporally and spatially on the sky, in relation to the asteroid is important for producing good quality spectra. If the atmosphere over Mauna Kea is stable throughout the observing run (photometric), then the log of the flux (apparent magnitude) of the object will decrease linearly with increasing airmass. Hence, all objects are typically observed at airmasses less than 1.5, which corresponds to a zenith angle of less than 50 degrees. However, if the atmosphere is unstable over Mauna Kea, whether due to an orographic cap cloud or rapid variability of water vapor content, it often produces a non-linear magnitude- airmass relationship. Local (or extinction) standard stars close to the asteroid are observed to correct for the terrestrial atmospheric water vapor features. Generally, the greater the distance between the local standard star and the asteroid, the poorer the monitoring of the sky conditions for the asteroid. During a typical observing run, a local standard star with spectral properties similar to our Sun (i.e., G-type, main sequence stars) is paired with an asteroid and is observed over a wide airmass range that bracket the airmass range of the asteroid observations. Solar analog stars are observed to remove the solar continuum from the asteroid spectrum. At least two solar analog stars should be observed each night to eliminate the possibility of systematic errors that may be present in a single solar analog star spectrum. SpeX prism data was reduced using the IDL-based Spextool provided by the NASA IRTF [CUSHINGETAL2004]. The steps followed in the reduction process include: (1) sky background removal by subtracting the image pairs, (2) flat-fielding, (3) cosmic ray and spurious hit removals, (4) wavelength calibration, (5) division of asteroid spectra by the spectrum of the solar analog star, and (6) co-adding of individual spectra. NOTE: Definitions for keywords which may appear in the labels: IMAGE_COUNT is the number of individual observations which have been combined to produce the final spectrum. APPARENT_MAGNITUDE is the apparent V magnitude of the target. FILTER_NAME (always V) is the filter of the APPARENT_MAGNITUDE. STAR_NAME is the name of the solar analog star used to reduce the observation. PHASE_ANGLE, SOLAR_DISTANCE, and AIRMASS all refer to the target. Plots with all the NIR spectra are provided in a pdf file located in the document directory. Numbers in the plots refer to the asteroid number. Error bars are not included in the plots." CONFIDENCE_LEVEL_NOTE = " Confidence Level Overview ========================= Uncertainties in spectral parameters for near-IR data are crucial for detecting and quantifying surface composition. The average wavelength resolution of the Spextool data is ~ 0.0035 microns. This is just due to spectral resolution based on the wavelength calibration. When spectra were combined the statistic used was the robust weighted mean. For this, Spextool makes use of a sigma clipping algorithm to identify outliers. The value at each pixel is then the weighted average of the good pixels and the uncertainty is given by the propagated variance. Uncertainties in the data arise primarily due to low SNR of the final average spectrum, incomplete correction of telluric absorption features, and variable sky/weather conditions. Data corresponding to asteroids (45) Eugenia, (213) Lilaea, (256) Walpurga, (308) Polyxo, (389) Industria, (442) Eichsfeldia, (1145) Robelmonte, (1284) Latvia, (1329) Eliane have error values much larger than might be expected given the scatter in the spectrum data points. The cause for these large uncertainties was not identified, but could be related to the small number of individual spectra that were combined to obtain the final spectrum. For these spectra the point-to-point scatter of the data provides a better estimate of the uncertainty associated with these measurements." 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