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1,211 results for “instrument”
Polar Plasma Wave Instrument (PWI), Low Frequency Waveform Receiver, ~0.01 sec resolution fields
The Low-Frequency Waveform Receiver (LFWR) is designed to provide an extension of the High Frequency Waveform Receiver into the frequency range below 25 Hz. The LFWR consists of six parallel low-pass filters connected to the three orthogonal electric field sensors and to the triaxial search coils. The input signals are band limited to a frequency range from 0.1 to 25 Hz and are sam- pled by a 12-bit analog-to-digital converter. The six LFWR channels are sampled simultaneously at a rate of 100 samples s-1. The dynamic range of the LFWRis approximately 72 dB with fixed gain. An FFT on 256 or 464 values, depending on the snapshot size, was used in calibrating the data; i.e., perform FFT, calibrate andin frequency domain, perform inverse FFT to get calibrated time series. Coordinate System Used: local magnetic field-aligned, a spacecraft centered coordinate system where Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a right-handed system and points eastward. The X- and Z-axes are contained in the north-south plane. The three orthogonal magnetic field components are given in units of nT/Sec rather than nT because the response of the searchcoils across the passband is not flat. In order to obtain units of nT, the data would need to be digitally filtered to the frequency of interest and then integrated over time. Integrating over the entire passband could possibly destroy the resolution of the higher frequency components since the low frequency noise, if present, will dominate. Data are bandpass filtered. The valid range of data in the frequency domain is from 0.5 to 22.5 Hz. Reference:..Gurnett, D.A. et al, The Polar plasma wave instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995.
THEMIS-A: Probe Electric Field Instrument and Search Coil Magnetometer Instrument, Digital Fields Board - digitally computed Filter Bank spectra and E12 peak and average in HF band (FBK).
The Filter Bank is part of the Digital fields board and provides band-pass filtering for EFI and SCM spectra as well as E12HF peak and average value calculations. The Filter Bank provides band-pass filtering for less computationally and power intensive spectra than the FFT would provide. The process is as follows: Signals are fed to the Filter Bank via a low-pass FIR filter with a cut-off frequency half that of the original signal maximum. The output is passed to the band-pass filters, is differenced from the original signal, then absolute value of the data is taken and averaged. The output from the low-pass filter is also sent to a second FIR filter with 2:1 decimation. This output is then fed back through the system. The process runs through 12 cascades for input at 8,192 samples/s and 13 for input at 16,384 samples/sec (EAC input only), reducing the signal and computing power by a factor 2 at each cascade. At each cascade a set of data is produced at a sampling frequency of 2^n from 2 Hz to the initial sampling frequency (frequency characteristics for each step are shown below in Table 1). The average from the Filter Bank is compressed to 8 bits with a pseudo-logarithmic encoder. The data is stored in sets of six frequency bins at 2.689 kHz, 572 Hz, 144.2 Hz, 36.2 Hz, 9.05 Hz, and 2.26 Hz. The average of the coupled E12HF signal and it's peak value are recorded over 62.5 ms windows (i.e. a 16 Hz sampling rate). Accumulation of values from signal 31.25 ms windows is performed externally. The analog signals fed into the FBK are E12DC and SCM1. Sensor and electronics design provided by UCB (J. W. Bonnell, F. S. Mozer), Digital Fields Board provided by LASP (R. Ergun), Search coil data provided by CETP (A. Roux). Table 1: Frequency Properties. Cascade Frequency content of Input Signal Low-pass Filter Cutoff Frequency Freuency Content of Low-pass Output Signal Filter Bank Frequency Band 0* 0 - 8 kHz 4 kHz 0 - 4 kHz 4 - 8 kHz 1 0 - 4 kHz 2 kHz 0 - 2 kHz 2 - 4 kHz 2 0 - 2 kHz 1 kHz 0 - 1 kHz 1 - 2 kHz 3 0 - 1 kHz 512 Hz 0 - 512 Hz 512 Hz - 1 kHz 4 0 - 512 Hz 256 Hz 0 - 256 Hz 256 - 512 Hz 5 0 - 256 Hz 128 Hz 0 - 128 Hz 128 - 256 Hz 6 0 - 128 Hz 64 Hz 0 - 64 Hz 64 - 128 Hz 7 0 - 64 Hz 32 Hz 0 - 32 Hz 32 - 64 Hz 8 0 - 32 Hz 16 Hz 0 - 16 Hz 16 - 32 Hz 9 0 - 16 Hz 8 Hz 0 - 8 Hz 8 - 16 Hz 10 0 - 8 Hz 4 Hz 0 - 4 Hz 4 - 8 Hz 11 0 - 4 Hz 2 Hz 0 - 2 Hz 2 - 4 Hz 12 0 - 2 Hz 1 Hz 0 - 1 Hz 1 - 2 Hz *Only available for 16,384 Hz sampling.
STARDUST C/E/L DUST FLUX MONITOR INSTRUMENT-2-EDR-V1.0
Data collected by the Dust Flux Monitor Instrument (DFMI) of the Stardust satellite, taken during the early cruise phase of the mission. These data were determined by peer review to be of no scientific use.
Polar Plasma Wave Instrument (PWI), Wideband Receiver (WBR) 4.016 microsecond resolution
PWI>Plasma Wave Instrument Reference: Gurnett, D.A. et al, The Polar Plasma Wave Instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. donald-gurnett@uiowa.edu An FFT on 1992 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. Coordinate system used: antenna coordinate system, where the u-axis is offset by -45 degrees from the spacecraft x-axis, the v-axis is offset by -45 degrees from the spacecraft y-axis, and the z-axis is identical to the spacecraft z-axis. The effective noise bandwidth is the data sampling frequency divided by the size of the FFT (number of input samples) multiplied by 1.5 to to correct for the effects of a Hanning window applied to the time- domain samples. Hence, the effective noise bandwidth is 1.5 * delta_f. These data come in snapshots of 1992 or 3984 points every 0.064 seconds. Duration of a snapshot is less when the instrument is in duty cycle modes. Since Epoch time is in milliseconds, the times for the data points will not be unique unless the fmsec (fraction of milliseconds) is appended to the Epoch0 time for that point. The frequency filters used for the wideband receiver have a range that limits the calibration. The following table specifies the range of frequencies for which the calibration is certified. Outside this range the amplitude values may be in error and should not be used. +------------------------------------------------+ Translation Filter Freq Range ------------------------------------------------ 0 kHz 90 kHz 7.5 kHz- 90.0 kHz 125 kHz 90 kHz 131.9 kHz-214.8 kHz 250 kHz 90 kHz 254.3 kHz-341.2 kHz 500 kHz 90 kHz 504.79 kHz-591.1 kHz 0 kHz 10 kHz 0.035 kHz- 11.64 kHz 0 kHz 22 kHz 0.065 kHz- 21.59 kHz 0 kHz 1-3 kHz 1.0 kHz- 3.0 kHz 0 kHz 3-6 kHz 3.0 kHz- 6.0 kHz +------------------------------------------------+ The cadence value given here is computed from the inverse of the sampling rate (249 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html
SAMPEX Polar-Cap-Averaged Fluxes, all instruments
This data set contains 17 differential fluxes of protons (mainly), helium ions, Z.GE.6 ions, and electrons, plus one integral flux of protons and electrons, as averaged over polar cap passes of the SAMPEX spacecraft. A polar cap pass covers the time poleward of geomagnetic latitude 70 deg. (Not all orbits have two polar cap passes.). For any given species, the fluxes typically come from more than one of the sensors (LICA, HILT, MAST, PET). Hence the inclusion of all instruments' data in each single record. Differential fluxes are those for (mainly) protons (Z.GE.1 channels at 5-12 and 19-27 MeV/n), helium ions (0.50-6.6, 4-9, 8-15, 9-38 MeV/n), Z.GE.6 ions (0.49-8.3, 8-42, 19.3-22.8, 22.8-31.0, 31.0-51.7, 41-220, 51.7-76.2, 76.2-113, 113-156 MeV/n), and electrons (1.5-6.0 MeV from PET only). One LICA channel measured integral fluxes of ions .GT. 0.8 MeV/n plus electrons .GT. 0.6 MeV). Data available for each polar cap pass are time tags of the begin and end points of the averaging interval, the fluxes, statistical uncertainties in the fluxes, instrument-specific flags, and a flag indicating a north or south polar cap pass. Data are organized in two different ways. Monthly ~500-KB ASCII files with records organized by instrument are available from the SAMPEX Data Center at Caltech and from nssdcftp at GSFC/SPDF, while monthly ~260 KB CDF-formatted files with records organized by species are available from the ftp area underlying CDAWeb. The parameter level information given below in this descriptor corresponds to the CDAWeb organization of data. Format information for the ASCII version is given in the Information URL of this descriptor.
SAMPEX Fluxes, all instruments
This set of 30-s averaged fluxes are derived from measurements made by all 4 instruments (HILT, LICA, MAST and PET) onboard the Solar Anomalous and Magnetospheric Particle Explorer (SAMPEX). Each file covers one full day of 30-s averaged fluxes of cosmic rays from selected channels from all experiments. There are 156 variables per record, and the file size is about 4 MB. After an extensive list of ancillary data, the particle fluxes follow. (1) LICA provides fluxes of electrons and protons in the energy range of about >0.7 Mev, of (mainly) helium in the range 0.49-8.3 MeV/nucleon. (2) HILT provides fluxes of helium from two channels, 4-9 and 9-38, of Z > 5 from two channels, 8.2-42 and 41-220 MeV/n. (3) MAST provides fluxes protons (mainly) in 5-12 MeV range, of helium in 8-15, and of Z > 5 in 19.3-22.8, 22.8-31.0, 31.0-51.7, 51.7-76.2, 76.2-113, 113-156 MeV/n. (4) PET provides fluxes of electrons in the ranges 1.5-6, and 2.5-14 MeV, and of (mainly) protons in 19-27 MeV/n. All flux values are accompanied by their standard deviations and quality flags. The fluxes available in this file are from a subset of (30-s resolution) rate channels. Energy spectra are assembled by pick-and-choose across instrument boundaries; an example is the eight-element array of Z>3 fluxes that have contributions from all four instruments
EPOXI HRII/HRIV/MRI INSTRUMENT TEMPERATURES V2.0
This dataset contains the raw and smoothed (averaged) instrument thermal telemetry for the entire EPOXI mission, from 04 October 2007 through 06 February 2011. Measurements were collected by 59 thermal sensors located in the HRII, HRIV, and MRI instruments, on the instrument platform, and on the solar wings of the Deep Impact flyby spacecraft.
Polar Plasma Wave Instrument, High Frequency Waveform Receiver, 2 kHz, Time Domain Fields
PWI>Plasma Wave Instrument Reference: Gurnett, D.A., et al., The Polar Plasma Wave Instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. donald-gurnett@uiowa.edu An FFT on 2048 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. The coordinate system used is local magnetic field-aligned, a spacecraft centered coordinate system where Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a right-handed system and points eastward. The X- and Z-axes are contained in the north-south plane. Effective Bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t. The unattenuated frequency range for this file type is 20Hz to 2000Hz. These data come in snapshots of 2048 samples per channel, every 128.8 seconds, with a cadence equal to the inverse of the sampling rate (4464 Hz), and individual time tags given in CDF TT2000 format. For a description of the PWI receivers and the different operational modes see https://space.physics.uiowa.edu/plasma-wave/polar/modes.html
STEREO-B In-Situ Measurements of Particles and CME Transients from the Magnetometer and the Plasma and Suprathermal Ion and Composition Instruments (IMPACT/MAG, PLASTIC) Solar Wind Plasma Data
STEREO-B In-situ Measurements of Particles and CME Transients, IMPACT, Magnetometer Instrument, MAG, Magnetic Field Vector and PLAsma and SupraThermal Ion Composition, PLASTIC, Solar Wind Parameter, Level 2, Data
Polar Plasma Wave Instrument (PWI), High Frequency Waveform Receiver, 25kHz bandwidth, 6-channel fields
PWI>Plasma Wave Instrument Reference: Gurnett, D.A. et al, The Polar Plasma Wave Instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. donald-gurnett@uiowa.edu An FFT on 1024 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. Coordinate system used: local magnetic field-aligned, a spacecraft centered coordinate system where Z is parallel to the local B-field determined from Polar MFE, X points outward and lies in the plane defined by the Z-axis and the radial vector from the earth to the spacecraft, and Y completes a right-handed system and points eastward. The X- and Z-axes are contained in the north-south plane. Effective bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t. These data come in snapshots of 31816 points per channel, every 9.2 seconds, where the duration of each snapshot is 0.045 seconds. The time for individual samples is the epoch time of the snapshot incremented by delta_t in milliseconds for each successive sample. That is: sample_time = epoch_time + sample_offset * delta_t The data in this file will be in sets of 31744 (31*1024) points per channel because the FFT size does not come out even within the number of points per snapshot. To obtain the time for each point in the snapshot, increment each Epoch time after the first with Delta_T (in ms). The unattenuated frequency range for this file type is 20Hz to 25000Hz. The cadence value given here is computed from the inverse of the sampling rate (71.43 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html
Polar Plasma Wave Instrument (PWI), High Frequency Waveform Receiver, 25kHz bandwidth interferometry fields
PWI>Plasma Wave Instrument Reference: Gurnett, D.A. et al, The Polar Plasma Wave Instrument, Space Science Reviews, Vol. 71, pp. 597-622, 1995. donald-gurnett@uiowa.edu An FFT on 1024 values was used in calibrating the data; i.e., perform FFT, calibrate in frequency domain, perform inverse FFT to get calibrated time series. Coordinate system used: antenna coordinate system, where the u-axis is offset by -45 degrees from the spacecraft x-axis, the v-axis is offset by -45 degrees from the spacecraft y-axis, and the z-axis is identical to the spacecraft z-axis. Effective bandwidth is 1.5*delta_f, where delta_f depends on the size of the FFT used to convert to the frequency domain, and delta_t. These data come in snapshots of 190902 points distributed among 2 to 6 channels every 9.2 seconds, where the duration of the snapshot is 0.045 seconds. Since Epoch time is in milliseconds, the times for the data points will not be unique unless the Delta_T in milliseconds is added to the Epoch time for the snapshot. The unattenuated frequency range for this file type is 20Hz to 25000Hz. The cadence value given here is computed from the inverse of the sampling rate (71.43 kHz). For a description of the PWI receivers and the different operational modes see: http://www-pw.physics.uiowa.edu/plasma-wave/istp/polar/modes.html
Measurement of NOx and NOy with a thermal dissociation cavity ring-down spectrometer (TD-CRDS): Instrument characterisation and first deployment
<p>NOx mixing ratios measured by TD-CRDS during the 2017 AQABA ship campaign. 1 minute averages and standard deviations.</p>
Data_Effects of Environmental Financial Support Instruments on Firm Productivity
<p>Recent research provides inconsistent evidence of the effectiveness of European Union (EU) renewable energy policies. Therefore, this paper aims at empirically verifying the effectiveness of three major EU renewable energy policies at the micro level. Using pooled OLS, fixed effects, random effects, and system generalized method-of-movements, it analyzes panel data for EU countries over a twenty-year period. The paper first examines in what extent the Emission Trading Scheme (EU ETS) in combination with other renewable support instruments, such as Feed-in Tariff (FIT) and Renewable Portfolio Standard (RPS), contribute to the reduction of emissions by regulated firms. Second, as regulated firms switch to new and more energy-efficient technologies in order to meet the regulation, this paper estimates the impact of the EU ETS, together with the FIT and RPS instruments, on firms’ productivity premia and productivity growth. The main results show that the EU ETS does not have a significant impact on firms’ productivity (except in periods around the implementation phase, i.e. in years <em>t<sub>0</sub></em> and <em>t<sub>1</sub></em>). Firms that are using the FIT support already had higher relative productivity before the EU ETS implementation and continue to maintain the productivity premia over non-EU ETS firms after the ETS implementation, while RPS is shown to boost firms’ productivity after implementation of the EU ETS. The interactions between EU ETS and FIT-RPS measures do not seem to have an additional systematic impact on the productivity of firms affected.</p> <p><strong>Keywords: </strong>renewable energy, FIT, RPS, EU ETS, technology diffusion, firm productivity</p> <p> </p>
CAWT Instrumental Song
<p>Rhythm.</p>
CAWT Instrumental
<p>Instrumental guitar.</p>
Otte Instrumental Song
<p>Instrumental guitar song (Name Otte).</p>
Machine_Learning_to_Hardware_for_Instrumentation
<p>Data used in "Exploring_Machine_Learning_to_Hardware_for_Instrumentation" paper, which is under review by IOP Machine learning: Science and technology journal</p>
MSL MARS CHEMISTRY & MINERALOGY X-RAY INSTRUMENT 2 EDR V1.0
Unprocessed experiment data from the CheMin instrument aboard the Mars Science Laboratory rover.
Instrumental Rock Guitar
<p>Music composing.</p>
Masi Instrumental
<p>Music</p>
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