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107 results for “PLS”
Gene expression profile analysis of PLS-123 in xenograft model.
GEO Series GSE65817. Homo sapiens. 10 samples. Type: Expression profiling by array.
Gene expression profile analysis of PLS-123 in OCI-Ly7 cells
GEO Series GSE65816. Homo sapiens. 12 samples. Type: Expression profiling by array.
Language Error Type Evaluation in Developmental Delay Preschool Children by PLS-C
ClinicalTrials.gov study NCT02663011. IPD Sharing: Not stated. Countries: 0. Publications: 0.
A Post-Market Study of Transfacet Lumbar Spine Fixation and Fusion Utilizing the PERPOS™ PLS System
ClinicalTrials.gov study NCT00887835. IPD Sharing: Not stated. Countries: 0. Publications: 0.
VG2 JUP PLS DERIVED ION INBOUND SOLAR WIND 96SEC V1.0
This data set contains solar wind plasma data upstream of Jupiter before the Voyager 2 encounter. Fit and moment parameters are given; the fit parameters assume a convected isotropic proton Maxwellian distribution. Use of fit parameters is recommended as these are normally more accurate. Since only the first 72 or last 72 energy/charge channels are telemetered to Earth from each M-mode spectra, derived parameters change significantly only every other set of spectra so the effective time resolution is 196 s.
VG2 JUP PLS PLASMA DERIVED ION MOMENTS 96.0 SEC V1.0
This data set contains the best estimates of the total ion density from Voyager 2 at Jupiter in the PLS voltage range (10-5950 eV/Q). It is calculated using the method of which to first order consists of taking the total measured current and dividing by the collector area and plasma bulk velocity. This method is only accurate for high mach number flows directly into the detector, and may result in underestimates of the total density of a factor of 2 in the outer magnetosphere. Thus absolute densities should be treated with caution, but density variations in the data set can be trusted. The low resolution mode density is used at all times except day 190 2100-2200 when the larger of the high and low resolution mode densities in a 96 sec period is used. Corotation is assumed inside L=17.5, and a constant velocity component of 200 km/s into the D cup is used outside of this. Data format: column 1 is time (yyyy-mm-ddThh:mm:ss.sssZ), column 2 is the moment density in cm^-3. Each row has format (a24, 1x, 1pe9.2). Values of -9.99e+10 indicate that the parameter could not be obtained from the data using the standard analysis technique. Additional information about this data set and the instrument which produced it can be found elsewhere in this catalog.
VG2 NEP PLS DERIVED RDR 2 PROTON MAGSPHERE 48SEC V1.0
This data set gives the best available values for ion densities, temperatures, and velocities near Neptune derived from data obtained by the Voyager 2 plasma experiment. All parameters are obtained by fitting the observed spectra (current as a function of energy) with Maxwellian plasma distributions, using a non-linear least squares fitting routine to find the plasma parameters which, when coupled with the full instrument response, best simulate the data. The PLS instrument measures energy/charge, so composition is not uniquely determined but can be deduced in some cases by the separation of the observed current peaks in energy (assuming the plasma is co-moving).
VG2 URA PLS DERIVED SUMMARY ION FIT 48SEC V1.0
This data set contains the total ion density obtained from Voyager 2 PLS data (voltage range 10-5950 eV/Q) at Uranus by fitting the measured spectra with isotropic Maxwellian distributions.
VG2 NEP PLS DERIVED RDR ELECTRON MAGNETOSPHERE 96SEC V1.0
The electron spectra are fit using several isotropic Maxwellian distribution functions to find electron parameters. The spacecraft charge may seriously affect the density measurements. The temperature of each component is, however, independent of the spacecraft potential. To obtain the best estimate of the electron density, the encounter period is divided into four regions and four different analysis methods are used.
VG2 URA PLS DERIVED RDR ION FIT 48SEC V1.0
This data set contains the ion densities and temperatures along with formal 1 Sigma errors obtained from Voyager 2 PLS data (voltage range 10-5950 eV/Q) at Uranus by fitting the measured spectra with isotropic Maxwellian distributions. Up to three isotropic proton components (warm, hot and intermediate) were used to match the observations. The plasma was assumed to be rigidly corotating. Uncertainties in plasma parameters are a factor of 2 in the charging region from 19:39-21:58 on day 24, less than 20% elsewhere. A complete description of this data set is given in McNutt et al. (1987) and Selesnick and McNutt (1987).
GO ASTROID PLS SUMM IDA ET V1.0
This file is a listing of particle energy spectra from the Galileo Plasma Instrument (PLS) during the Ida Flyby. Detector reponses from ion detetors 2P, 4P, and 6P, and from electron detector 4E are available through the PDS as separate files. The energy resolution, angular fields of view, and nominal geometric factors for the detectors are specified in the Instrument Description file.
VG1 JUP PLS PLASMA DERIVED ION MOMENTS 96.0 SEC V1.1
This data set contains the best estimates of the total ion density at Jupiter during the Voyager 1 encounter in the PLS voltage range (10-5950 eV/Q).
VG2 URA PLS DERIVED SUMM ELECTRON BROWSE 48SEC V1.0
This data set contains the thermal electron density and temperature in the PLS energy range (10-5950 eV) from Voyager 2 at Uranus derived by fitting the low energy electron component with a Maxwellian distribution, and the moment density and temperature of the hot electrons calculated after the signal from the thermal component is subtracted from the electron spectra. The moment density and temperature obtained by integrating over the entire measured distribution function are also given.
GO ASTROID PLS SUMM GASPRA ET V1.0
This file is a listing of particle energy spectra from the Galileo Plasma Instrument (PLS) during the Gaspra Flyby. Detector reponses from ion detetors 2P, 4P, and 6P, and from electron detector 4E are available through the PDS as separate files. The energy resolution, angular fields of view, and nominal geometric factors for the detectors are specified in the Instrument Description file.
GO EARTH PLS SUMM EARTH2 ET V1.0
This file is a listing of particle energy spectra from the Galileo Plasma Instrument (PLS) during the second Earth Encounter. Detector reponses from ion detetors 2P, 4P, and 6P, and from electron detector 4E are available through the PDS as separate files.
VG1 SAT PLS DERIVED ION SOLAR WIND BROWSE 96SEC V1.0
This data set contains solar wind plasma browse data near the Voyager 1 Saturn encounter. Moment parameters are given. Since only the first 72 or last 72 energy/charge channels are telemetered to Earth from each M-mode spectra, derived parameters change significantly only every other set of spectra so the effective time resolution is 96 second.
VG2 URA PLS DERIVED RDR ELECTRON FIT 48SEC V1.0
This data set contains electron parameters in the PLS energy range (10-5950 eV) at Uranus during the Voyager 2 encounter. Parameters are calculated in several ways. Total moment density and temperature are given. Each electron spectrum is also fit with a thermal component and 1-3 hot components depending on how many Maxwellians are needed to fit the entire distribution. The moment density and temperature of the hot component is calculated after the thermal component is subtracted from the spectrum. The CHI-Square value for each fit is given. The spacecraft charge is not calculated consistently, and may result in factor of 2-3 errors in the thermal electron density. Data is unreliable inside 5 RU and in the occultation regions. At Uranus measurements were taken using both a long and a short integration time. Each 48 SEC measurement frame contained either an E1-Short and an E2-Long measurement or an E2-Short and an EI-Long. To reduce systematic errors, complete electron spectra were obtained only by combining two long or two short spectra. The instrument threshold is at a density of about 0.001 CM-3; thus fits which yield data close to this value should be treated with caution. Flags in the data indicate whether the full analysis could be performed and if the data was contaminated by LECP stepping. A complete description of this data set is in Sittler et al. (1987).
VG2 NEP PLS DERIVED RDR ION OUTBND MAGSHTH M-MODE 12MIN V1.0
This data set gives the best available values for ion densities, temperatures, and velocities near Neptune derived from data obtained by the Voyager 2 plasma experiment. All parameters are obtained by fitting the observed spectra (current as a function of energy) with Maxwellian plasma distributions, using a non-linear least squares fitting routine to find the plasma parameters which, when coupled with the full instrument response, best simulate the data.
VG2 SAT PLS DERIVED ION SOLAR WIND 96SEC V1.0
This Voyagers 2 data set contains two solar wind plasma data, one spanning from August 19 to September 4 , 1981, and near encounter specific data covering August 24-25. Moment parameters are given in the broader data while the near encounter data is more detailed. The fit parameters assume a convected isotropic proton Maxwellian distribution. Use of fit parameters is recommended as these are normally more accurate. Since only the first 72 or last 72 energy/charge channels are telemetered to Earth from each M-mode spectra, derived parameters change significantly only every other set of spectra so the effective time resolution is 96 second.
VG2 NEP PLS DERIVED RDR ION MAGNETOSPHERE 48SEC V1.0
This data set gives the best available values for ion densities, temperatures, and velocities near Neptune derived from data obtained by the Voyager 2 plasma experiment. All parameters are obtained by fitting the observed spectra (current as a function of energy) with Maxwellian plasma distributions, using a non-linear least squares fitting routine to find the plasma parameters which, when coupled with the full instrument response, best simulate the data. The PLS instrument measures energy/charge, so composition is not uniquely determined but can be deduced in some cases by the separation of the observed current peaks in energy (assuming the plasma is co-moving).
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