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GO A PWS REFORMATTED IDA SPECTRUM ANALYZER FULL V1.0

This data set includes full resolution electric and magnetic wave spectra obtained during a ~ 15-minute period of contiguous observations near the closest approach to Ida and a number of non-contiguous spectra taken prior to closest approach. In addition waveform survey data (uncalibrated) and all instrument housekeeping data are included. The parameters provided for both the electric and magnetic field spectral data are uncalibrated data numbers. Software and calibration tables provided as part of this data set allow for fully calibrated data for the electric field measurements in raw data numbers, voltage at the antenna inputs (V), electric field (V/m), electric field spectral density (V**2/m**2/Hz), or power flux (W/m**2/Hz). The magnetic field measurements can be provided in units of magnetic field spectral density (nT**2/Hz). The sources of these data are the High Frequency Receiver, Sweep Frequency Receiver, and Spectrum Analyzer which make up the Low Rate Science portion of the PWS. During the included time interval, the instrument cycled between the electric and magnetic antennas for the Sweep Frequency Receiver and the Spectrum Analyzer. The High Frequency Receiver is always connected to the electric antenna. Hence, for the Sweep Frequency Receiver and the Spectrum Analyzer, the temporal resolution for electric measurements is basically one spectrum per 37.33 seconds. For the High Frequency Receiver, the time between spectra is 18.67 seconds. Note that the lowest 14 High Frequency Receiver channels are sampled twice per 18.67 seconds while the remaining channels are sampled only once. The four Spectrum Analyzer channels are each sampled 7 times in an 18.67 sec interval.

VG2 JUP PWS EDITED SPECTRUM ANALYZER 4.0SEC V1.0

This data set consists of 4-second edited, wave electric field intensities from the Voyager 2 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Jovian magnetosphere. For each 4-second interval, a field strength is determined for each of the 16 spectrum analyzer channels whose center frequencies range from 10 Hertz to 56.2 kiloHertz and which are logarithmically spaced in frequency, four channels per decade. The time associated with each set of intensities (16 channels) is the time of the beginning of the scan. During data gaps where complete 4-second spectra are missing, no entries exist in the file, that is, the gaps are not zero-filled or tagged in any other way. When one or more channels are missing within a scan, the missing measurements are zero-filled. Data are edited but not calibrated. The data numbers in this data set can be plotted in raw form for event searches and simple trend analysis since they are roughly proportional to the log of the electric field strength.

Predicting Engine Parameters using the Optical Spectrum

The Optical Plume Anomaly Detection (OPAD) system is under development to predict engine anomalies and engine parameters of the Space Shuttle's Main Engine (SSME). The anomaly detection is based on abnormal metal concentrations in the optical spectrum of the rocket plume. Such abnormalities could be indicative of engine corrosion or other malfunctions. Here, we focus on the second task of the OPAD system, namely the prediction of engine parameters such as rated power level (RPL) and mixture ratio (MR). Because of the high dimensionality of the spectrum, we developed a linear algorithm to resolve the optical spectrum of the exhaust plume into a number of separate components, each with a different physical interpretation. These components are used to predict the metal concentrations and engine parameters for online support of ground-level testing of the SSME. Currently, these predictions are labor intensive and cannot be done online. We predict RPL using neural networks and give preliminary results.

Low-Frequency Radio Catalog of Flat-Spectrum Sources

A well-known property of the gamma-ray sources detected by Cos-B in the 1970s, by the Compton Gamma-Ray Observatory in the 1990s, and recently by the Fermi Gamma-ray Observatory is the presence of radio counterparts, particularly for those associated with extragalactic objects. This observational evidence is the basis of the radio/gamma-ray connection established for the class of active galactic nuclei known as blazars. In particular, the main spectral property of the radio counterparts associated with gamma-ray blazars is that they show a flat spectrum in the GHz frequency range. The authors' recent analysis dedicated to search for blazar-like candidates as potential counterparts for the unidentified gamma-ray sources allowed them to extend the radio/gamma-ray connection in the MHz regime. They also showed that blazars below 1 GHz maintain flat radio spectra. Thus, on the basis of these new results, the authors have assembled a low-frequency radio catalog of flat-spectrum sources built by combining the radio observations of the Westerbork Northern Sky Survey (WENSS) and of the Westerbork in the southern hemisphere (WISH) catalogs with those of the NRAO Very Large Array Sky survey (NVSS). This catalog could be used in the future to search for new, unknown blazar-like counterparts of gamma-ray sources. First, the authors found NVSS counterparts of Westerbork Synthesis Radio Telescope (WSRT) radio sources, and then they selected flat-spectrum radio sources according to a new spectral criterion, specifically defined for radio observations performed below 1 GHz. In their paper, they also describe the main properties of the catalog listing 28,358 radio sources with spectral indices between 1400 and 325/352 MHz between -1.0 and +0.4, and their log N - log S distributions. Finally, a comparison with the Green Bank 6 cm radio source catalog was performed so as to investigate the spectral shape of the low-frequency flat-spectrum radio sources at higher frequencies. This table was created by the HEASARC in July 2014 based on a machine-readable version of Table 1 from the reference paper which was obtained from the ApJS web site. This is a service provided by NASA HEASARC .

GO E PWS RESAMP SUMMARY EARTH 2 SPECTRUM ANALYZER 60S V1.0

This data set includes 1-minute averages of the electric and magnetic wave spectra obtained during the period that the Galileo plasma wave receiver was operated during the second flyby of Earth. The parameter provided for the electric field spectrum is the electric field spectral density in units of V^2/m^2/Hz. The magnetic field spectrum is provided in units of magnetic field spectral density, nT^2/Hz.

GO V PWS RESAMP SUMMARY VENUS SPECTRUM ANALYZER 60S V1.0

This data set includes 1-minute averages of the electric and magnetic wave spectra obtained during the ~ 53-minute period that the Galileo plasma wave receiver was operated at Venus.

GO A PWS REFORMATTED GASPRA SPECTRUM ANALYZER FULL V1.0

This data set includes full resolution electric and magnetic wave spectra obtained during a ~ 2-hour period of contiguous observations near the closest approach to Gaspra and a number of non-contiguous spectra taken prior and subsequent to closest approach. In addition waveform survey data (uncalibrated) and all instrument housekeeping data are included.

Hawkeye Electric and Magnetic Field Radio Frequency Spectrum Analyzer High Time Resolution

The CDF file contains approximately 22 second time resolution Electric and Magnetic field data, average magnetic field magnitude, and orbital position data from Hawkeye 1. The VLF experiment measured electric and magnetic fields using a 42.45-m electric dipole (tip-to-tip) which extended perpendicular to the spin axis and a search coil antenna deployed 1.58 m from the spacecraft. The electric field spectrum measurements were made in 16 logarithmically spaced frequency channels extending from 1.78 Hz to 178 kHz, and dc electric fields were also measured. The bandwidth of these channels varied from 7.5% to 30% depending on center frequency. Channel sensitivity and dynamic range were 1E-6 V/m and 100 dB, respectively. A wideband receiver was also used, with two selectable bandwidth ranges: 0.15 to 10 kHz or 1 to 45 kHz. The magnetic field spectrum was measured in eight discrete, logarithmically spaced channels from 1.78 Hz to 5.62 kHz. The bandwidth of these channels varied from 7.5% to 30% depending on frequency. The dynamic range was 100 dB, and the sensitivity ranged from 0.1 nT at 1.78 Hz to 3.4E-4 nT at 5.62 kHz. The wideband receiver described above could be used with the magnetic antenna. Each discrete channel was sampled once every 11.52 s.

FIELD EXP EARTH PARABOLA CALIBRATED RDR SPECTRUM V1.0

PARABOLA data were obtained at three GRSFE modeling sites in the Lunar Crater Volcanic Field. The playa site, the cobble site, and the mantled flow site. Each site was imaged by PARABOLA at a variety of solar incidence angles to characterize the scattering properties of the surface completely. This information can be used as a reference to correct airborne data from ASAS and AVIRIS from any lighting and viewing geometry, or as a base data set to test radiative transfer models. Six sets of data from the playa site were gathered primarily on July 17, 1989 with solar incidence angles that varied from 28 to 71 degrees. Five sets of cobble site data were gathered during the morning of July 18, 1989 with incidence angles from 19 to 57 degrees. Data from the mantled flow site was obtained six times during the afternoon of July 18 with incidence angles from 21 to 73 degrees. In all, over 1000 data points exist for each site to characterize its scattering properties. Additionally, an equal number of points exist for the sky above the sites.

VG2 J/S/U/N/SS PWS RESAMP SPECTRUM ANALYZER HOUR AVG V1.0

This data set contains hourly RMS averages and peaks of calibrated electric field measurements taken by the spectrum analyzer component of the Plasma Wave System (PWS) onboard Voyager 2 for the entire mission. Most noise spikes were removed prior to processing in order to provide more reliable values. Each record contains the spacecraft event time at the beginning of the processed hour, 16 RMS electric field averages corresponding to the 16 frequency channels of the instrument ranging from50 Hz to 10 kHz, and 16 maximum values in the same units for the same frequencies.

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FIELD EXP EARTH PFES CALIBRATED RDR SPECTRUM V1.0

Portable Field Emission Spectrometer (PFES) data were acquired on July 15 and 17, 1989. A total of 31 measurements were collected for GRSFE. Of these measurements, 13 were calibrations and 18 were of representative surfaces. The data were collected primarily to support the calibration of the TIMS data and to assist in interpreting spectral mixing in the mid-infrared. Sites were selected for calibration that covered a range of emissivities. On July 15, PFES data were collected at Kelso Dunes and the Cima Volcanic Field as part of the Calibration Team effort. Daedalus and SIRIS data were collected over the same sites. For the PFES data, the Kelso Dunes Bright Target site represented the silica-rich endmember and the Cima basalt tephra Dark Target site represented the more silica-poor endmember. On July 17, PFES data were collected at two of the modelling sites at Lunar Lake (the playa and the cobble sites). Several spectra were also collected at the playa surface next to the Lunar Lake thermistor site.

VG1 JUP PWS EDITED SPECTRUM ANALYZER 4.0SEC V1.1

This data set consists of 4-second edited, wave electric field intensities from the Voyager 1 Plasma Wave Receiver spectrum analyzer obtained in the vicinity of the Jovian magnetosphere.

VG2 J/S/U/N/SS PWS EDITED SPECTRUM ANALYZER FULL RES V1.0

This data set includes nearly all measurements collected from the spectrum analyzer component of the Plasma Wave Spectrometer (PWS) onboard Voyager 2 for the entire mission. Some noise lines during the planetary encounters have been edited from the data set. Each sweep of the PWS spectrum analyzer records spectral densities in 16 frequency channels from 50 Hz to 10 kHz. The values in this data set are given as instrument data numbers. Instructions for producing calibrated values are provided. An example C-language program which reads this data set and produces calibrated values is also provided.

VG1 J/S/SS PWS RESAMP SPECTRUM ANALYZER HOUR AVG V1.0

This data set contains hourly RMS averages and peaks of calibrated electric field measurements taken by the spectrum analyzer component of the Plasma Wave System (PWS) onboard Voyager 1 for the entire mission. Most noise spikes were removed prior to processing in order to provide more reliable values. Each record contains the spacecraft event time at the beginning of the processed hour, 16 RMS electric field averages corresponding to the 16 frequency channels of the instrument ranging from 50 Hz to 10 kHz, and 16 maximum values in the same units for the same frequencies.

FIELD EXP E SIRIS RESAMP REDUCED DATA RECORD SPECTRUM V1.0

The SIRIS measurement objectives were: 1) to measure reflectance spectra of a bright and dark target at each GRSFE site for potential use in AVIRIS calibration characterize selected sites at the GRSFE modeling site (Lunar Lake, NV) using visible/infrared reflectance reflectance spectra for selected endmember materials at each of the GRSFE sites inter-instrument calibration.

GO JUP PWS REFORMATTED REALTIME SPECTRUM ANALYZER FULL V1.0

This data set includes full resolution electric and magnetic wave spectra obtained during the period for which real time science data was acquired from the Galileo plasma wave receiver during Jupiter orbital operations. The parameters provided for both the electric and magnetic field spectral data are uncalibrated data numbers. Software and calibration tables provided as part of this data set allow for fully calibrated data for the electric field measurements in raw data numbers, voltage at the antenna inputs (V), electric field (V/m), electric field spectral density (V**2/m**2/Hz), or power flux (W/m**2/Hz). The magnetic field measurements can be provided in units of magnetic field spectral density (nT**2/Hz). The sources of these data are the High Frequency Receiver, Sweep Frequency Receiver, and Spectrum Analyzer which make up the Low Rate Science portion of the PWS.

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VG1 J/S/SS PWS EDITED SPECTRUM ANALYZER FULL RES V1.0

This data set includes nearly all measurements collected from the spectrum analyzer component of the Plasma Wave Spectrometer (PWS) onboard Voyager 1 for the entire mission. Some noise lines during the planetary encounters have been edited from the data set. Each sweep of the PWS spectrum analyzer records spectral densities in 16 frequency channels from 50 Hz to 10 kHz. The values in this data set are given as instrument data numbers. Instructions for producing calibrated values are provided. An example C-language program which reads this data set and produces calibrated values is also provided.

CRATES Flat-Spectrum Radio Source Catalog

The authors have assembled an 8.4 GHz survey of bright, flat-spectrum (alpha > -0.5) radio sources with nearly uniform extragalactic (|b| > 10 degrees) coverage for sources brighter than a 4.8 GHz flux density S_4.8GHz = 65 mJy. The catalog is assembled from existing observations (especially the Cosmic Lens All-Sky Survey, CLASS, and the Wright et al. PMN-CA survey), augmented by reprocessing of archival VLA and ATCA data and by new observations to fill in coverage gaps. The authors refer to this program as CRATES, the Combined Radio All-Sky Targeted Eight-GHz Survey. The resulting catalog provides precise positions, subarcsecond structures, and spectral indices for some 11,000 sources. The authors describe the morphology and spectral index distribution of the sample and comment on the survey's power to select several classes of interesting sources, especially high-energy blazars. Comparison of CRATES with other high-frequency surveys also provides unique opportunities for identification of high-power radio sources. This table contains 14467 entries, where each entry corresponds to an 8.4-GHz counterpart source (or absence thereof) to one of 11,131 4.8-GHz sources. The number of entries exceeds the number of 4.8-GHz sources because there are many cases in which there are multiple (from 2 - 20) 8.4-GHz counterparts to a single 4.8-GHz source. There are also 762 entries in which no 8.4-GHz counterpart was detected (morph_type = 'N'). This table was created by the HEASARC in August 2007 based on the electronic version of Table 5 obtained from the electronic ApJ web site. This is a service provided by NASA HEASARC .

ROSAT Hard-Spectrum X-Ray Source Catalog

This table contains a catalog of 147 serendipitous X-ray sources selected to have hard spectra (spectral indices Alpha < 0.5) from a survey of 188 ROSAT fields. Such sources must be the dominant contributors to the X-ray background at faint fluxes. The authors have used Monte Carlo simulations to verify that their technique is very efficient at selecting hard sources: the survey has >= 10 times as much effective area for hard sources as it has for soft sources above a 0.5 - 2 keV flux level of 10-14 erg cm-2 s-1. The distribution of best-fitting spectral slopes of the hard sources suggests that a typical ROSAT hard source in this survey has a spectral slope Alpha ~ 0. The hard sources have a steep number-flux relation (dN/dS ~ _S-Gamma, with a best-fitting value of Gamma = 2.72 +/- 0.12), and make up about 15% of all 0.5 - 2 keV sources with S > 10-14 erg cm-2 s-1. If their N(S) continues to fainter fluxes, the hard sources will comprise ~ 40% of sources with 5 x 10-15 < S < 10-14 erg cm-2 s-1. The population of hard sources can therefore account for the harder average spectra of ROSAT sources with S < 10-14erg cm-2 s-1. They probably make a strong contribution to the X-ray background at faint fluxes and could be the solution to the X-ray background spectral paradox. This table was created by the HEASARC in March 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/318/1073">CDS Catalog J/MNRAS/318/1073</a> file table2.dat, the ROSAT hard X-ray source catalog. This is a service provided by NASA HEASARC .

SUISEI ENERGY SPECTRUM PARTICLE MEASUREMENTS V1.0

A floppy was received at IHW-Lead Center through Dr. Oyama. It contained the following description: ***SUISEI ESP / Solar Wind Parameters *** T. Mukai Institute of Space and Astronautical Science Sagamihara, Kanagawa 229 Japan