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MMS 1 Fast Plasma Investigation, Dual Ion Spectrometer (FPI, DIS) Partial Distribution Moments, Level 2 (L2), Burst Mode, 0.15 s Data

FPI usually operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution in this Mode. Data are also made available at Survey (4.5 s, etc.) Resolution. Per Mission Design, not all Burst Resolution Data are downlinked, but all Survey Data are downlinked. Planning around Calibration Activities, avoidance of Earth Radiation Belts, etc., when possible, FPI usually operates in Slow Survey (SS) Mode (60 s Resolution) outside of ROI, and then only the 60 s Resolution Survey Data are available. This Product contains Partial Moments that come from performing the Standard Moment Integrals over a limited Portion of Velocity Space. The resulting Quantities are named similarly to their corresponding Standard Moments, but are decorated with 'part' to differentiate. For example, density_part is the Density Moment integrated from a particular Energy Step to Infinity. These Partial Moments are formed from the indicated Data Type (DES/DIS Burst, FS or SS). For convenience, some additional Parameters are included to augment those most commonly found in a Moments Product of this sort, plus Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.

MMS 2 Flux Gate Magnetometer (FGM) DC Magnetic Field, Level 2 (L2), Burst Mode, 128 Sample/s, v4/5 Data

The Fluxgate Magnetometers (FGM) on Magnetospheric Multiscale consist of a traditional Analog Fluxgate Magnetometer (AFG) and a Digital Fluxgate magnetometer (DFG). The dual magnetometers are operated as a single instrument providing a single intercalibrated data product. Range changes occur at different times on the two instruments so the gains checked each periapsis can be carried out unambiguously to apoapsis. Cross correlation of calibration parameters can separate causes of the any apparent calibration changes. Use of Electron Drift Instrument (EDI) to determine the field along the rotation axis allows accurate monitoring of the zero levels along the rotation axis. Prior to launch the magnetometers were calibrated at the Technical University, Braunschweig, except for the AFG magnetometers on MMS3 and MMS4, which were calibrated at UCLA. Both sets of sensors are operated for the entire MMS orbit, with slow survey (8 samples per second) outside of the Region of Interest (ROI), and fast survey (16 samples per second) inside the ROI. Within the ROI, burst mode data (128 samples per second) are also acquired. A detailed description of the MMS fluxgate magnetometers, including science objectives, instrument description, calibration, magnetic cleanliness program, and data flow can be found at http://link.springer.com/article/10.1007%2Fs11214-014-0057-3 (DOI 10.1007/s11214-014-0057-3). Additional information can also be found at http://www-spc.igpp.ucla.edu/ssc/mms (UCLA), and http://www.iwf.oeaw.ac.at/de/forschung/erdnaher-weltraum/mms/dfg (IWF, Graz). For the purpose of creating a unified FGM Level 2 data product, burst mode data is taken from DFG and survey mode data is taken from AFG. Because AFG and DFG are cross-calibrated on an orbit-averaged basis, small differences in offset may be observed between Level 2 burst and survey mode data. Consequently, any differences are within the error of the measurement. Based on preliminary analysis of the data, the absolute error within the Region of Interest (ROI) is estimated to be no more than 0.1 nT in the spin-plane, 0.15 nT along the spin-axis and 0.2 nT in total magnitude.

Radio-Selected Gamma-Ray Burst Afterglow Catalog

This table contains a catalog of radio afterglow observations of gamma-ray bursts (GRBs) over a 14 year period from 1997 to 2011. This sample of 304 afterglows consists of 2,995 flux density measurements (including upper limits) at frequencies between 0.6 GHz and 660 GHz, with the majority of data taken in the 8.5-GHz frequency band (1,539 measurements). The authors use this dataset to carry out a statistical analysis of the radio-selected sample. The detection rate of radio afterglows stayed unchanged almost at 31% before and after the launch of the Swift satellite. The canonical long-duration GRB radio light curve at 8.5 GHz peaks at three to six days in the source rest frame, with a median peak luminosity of 1031 erg/s/Hz. The peak radio luminosities for short-hard bursts, X-ray flashes, and the supernova-GRB classes are an order of magnitude or more fainter than this value. There are clear relationships between the detectability of a radio afterglow and the fluence or energy of a GRB, and the X-ray or optical brightness of the afterglow. However, the authors find few significant correlations between these same GRB and afterglow properties and the peak radio flux density. In their paper, they also produce synthetic light curves at centimeter and millimeter bands using a range of blast wave and microphysics parameters derived from multi-wavelength afterglow modeling, and use them to compare with the radio sample. Finding agreement, the authors extrapolate this behavior to predict the centimeter and millimeter behavior of GRBs which will observed by the Expanded Very Large Array and the Atacama Large Millimeter Array. The compiled sample consists of 304 GRBs observed with radio telescopes between 1997 January and 2011 January, along with the 2011 April 28 Fermi burst, GRB 110428A. The sample consists of a total of 2,995 flux density measurements taken in the frequency range from 0.6 to 660 GHz and spanning a time range from 0.026 to 1,339 days. Most of the afterglows (270 in total) in this sample were observed as part of VLA radio afterglow programs, whereas 15 bursts were observed by the Expanded VLA (EVLA), and 19 southern bursts with the Australia Telescope Compact Array (ATCA). This catalog describes the radio, optical and X-ray afterglow detections (see Section 2.2 of the reference paper): out of the 304 bursts, 123 bursts were observed in the pre-Swift epoch from 1997 until 2004. The remaining 181 bursts were observed between 2005 and 2011 April (the post-Swift epoch). Out of the 95 radio-detected afterglows (see Section 2.2 of the reference paper), 63 had radio lightcurves (i.e., three or more detections in a single radio band), whereas 32 bursts had less than three detections. For the GRBs for which the light curves were available, the authors determined the peak flux density and the time of the peak in the VLA frequency bands (i.e., 1.4 GHz, 4.9 GHz, 8.5 GHz, 15 GHz, and 22.5 GHz bands) by fitting the data with forward shock formula of the form (Frail 2005, IAU Coll. 192, p. 451) given in equation (1) of the reference paper. This formula may not accurately represent the full complexity of the radio lightcurve evolution. However, it is good enough to determine the approximate values for the peak flux density Fm and the time of the peak tm. See the discussion in Section 3.5 of the reference paper for more details and some caveats. For the remaining bursts, the flux density values were taken directly from the data, and hence do not have the best-fit errors for the peak flux, peak time and rest-frame peak time parameters Fm, tm and tm/(1+z), respectively. This table was created by the HEASARC in November 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/746/156">CDS catalog J/ApJ/746/156</a> files table1.dat and table4.dat. This is a service provided by NASA HEASARC .

MMS 3 Hot Plasma Composition Analyzer (HPCA) Ions, Level 2 (L2), Burst Mode, 0.625 s Data

Hot Plasma Composition Analyzer (HPCA) Ions, Level 2, Burst Survey, 0.625 s Data. The MMS HPCA instruments measure the energy and composition of magnetospheric plasmas in the energy range from 1 eV to 40 keV. An electrostatic energy analyzer (ESA) that is optically coupled to a carbon-foil based Time-of-Flight (TOF) section comprises each HPCA. The basic HPCA data product is an array of counts for 5 ion species, at 63 energies, for each of 16 elevation anodes. Sixteen basic products, also called azimuths, are acquired every 0.625 s; half a spacecraft spin period nominally has 16 azimuths. The five ion species are protons (H+), alpha particles (He++), helium ions (He+), singly charged Oxygen (O+), and background counts.

STEREO-B In-Situ Measurements of Particles and CME Transients (IMPACT) Fluxgate Magnetometer (MAG) Burst Mode, Magnetic Field Vector, Radial-Tangential-Normal (RTN) Coordinates, Level 1 (L1), 31 ms Data

This data product contains Level 1 0.03125-s or 32 Hz burst-mode values of solar wind magnetic field data measured by the IMPACT Magnetometer on STEREO-B in Radial-Tangential-Normal, RTN, coordinates.

MMS 2 Energetic Particle Detector, Energetic Ion Spectrometer (EPD-EIS) Energy by Time of Flight, Level 2 (L2), Burst Mode, 0.605 s Data

Energetic Particle Detector (EPD), Energetic Ion Spectrometer (EIS) Energy by Time of Flight, Level 2, Burst Survey, 0.605 s Data. The EIS provides ion composition measurements (protons versus oxygen ions) and angular distributions over the energy range from approximately 45 to 500 keV.

MMS 3 Hot Plasma Composition Analyzer (HPCA) Moments, Level 2 (L2), Burst Mode, 10 s Data

Hot Plasma Composition Analyzer (HPCA) Moments, Level 2, Burst Survey, 10 s Data. The MMS HPCA instruments measure the energy and composition of magnetospheric plasmas in the energy range from 1 eV to 40 keV. An electrostatic energy analyzer (ESA) that is optically coupled to a carbon-foil based Time-of-Flight (TOF) section comprises each HPCA. The basic HPCA data product is an array of counts for 5 ion species, at 63 energies, for each of 16 elevation anodes. Sixteen basic products, also called azimuths, are acquired every 10 s; half a spacecraft spin period nominally has 16 azimuths. The five ion species are protons (H+), alpha particles (He++), helium ions (He+), singly charged Oxygen (O+), and background counts.

MMS 1 Magnetic Ephemeris and Coordinates (MEC) and Support (Tsyganenko 1989 model, Quiet conditions), Level 2 (L2), Burst Mode, 30 ms Data

Magnetospheric Multiscale 1 (MMS 1) spacecraft position, velocity, attitude, angular momentum vector, and magnetic ephemeris and coordinates (MEC), Level-2 science data at Burst (30 ms) time resolution. The Magnetic ephemeris data are calculated by using the Tsyganenko 1989 magnetic field model for quiet magnetospheric conditions. Many variables are included in this data product including the magnetic field measured at the spacecraft. If possible, the northern and southern hemisphere footpoints of the spacecraft are found by tracing along the magnetic field line threading through the spacecraft per the given Tsyganenko and internal magnetic field models. The northern and southern hemisphere loss cone angles are also given. The magnetic field strength at the footpoints and the minimum magnetic field strength along the field line are also calculated by using the field models. Other variables list the spacecraft L-shell, the magnetic local time, the magnetic latitude and longitude, and whether the threading field line is open, closed, etc. Rotational quaternions are provided to allow coordinate transformation from GEI into 11 other coordinate systems including BSC, GEO, GSE, GSE2000, GSE, and SM. The list of ancillary variables includes the dipole tilt angle, the Dst and Kp actvity indices, and separate flags that denote satellite eclipse by the Earth and Moon.

MMS 4 Fast Plasma Investigation, Dual Electron Spectrometer (FPI, DES) Instrument Distributions, Level 2 (L2), Burst Mode, 30 ms Data

The Fast Plasma Instrument (FPI) usually Operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution in this Mode. Data are also made available at Survey (4.5 s, etc.) Resolution. Per Mission Design, not all Burst Resolution Data are downlinked, but all Survey Data are downlinked. This Product contains Phase Space Distribution Maps of those Burst Resolution Data selected for downlink. In particular, the (highest possible Quality at the Time of Release) corrected/converted "Burst Sky Map" Distributions are reported with Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.

PSP FIELDS Digital Fields Board (DFB) Differential Voltage Burst Waveform, Level 2 (L2), 0.873813 s Data

PSP FIELDS Digital Fields Board (DFB), Differential Voltage data:The DFB is the low frequency, less than 75 kHz, component of the FIELDS experiment on the Parker Solar Probe spacecraft, see reference [1] below. For a full description of the FIELDS experiment, see reference [2]. For a description of the DFB, see reference [3].DFB burst waveform data consist of short bursts of time-series data from various FIELDS sensors. These data have been filtered by both analog and digital filters [3]. These data are pre-sorted by onboard competitive selection algorithms described in [3] before storage by FIELDS. A subset of this stored burst data is telemetered to Earth for scientist-selected regions of interest.The Level 2 data products contained in this data file have been calibrated for:* 1) DFB in-band gain* 2) DFB analog filter gain/phase response* 3) DFB digital filter phase response* 4) The search coil preamplifier gain/phase response, when applicableCalibrations for the FIELDS voltage sensor preamplifiers have not been implemented as the preamplifier response is flat and equal to one through the DFB frequency range. Corrections for plasma sheath impedance gain and antenna effective length have not been applied to voltage sensor signals. These corrections will be applied in the Level 3 DFB data products. Therefore, all voltage sensor quantities when present in these Level 2 data products are expressed by using units of Volts. Likewise, all magnetic field quantities when present in these Level 2 data products are expressed by using units of nT.The Level 2 voltage data products when present in these data files are expressed in sensor coordinates: [dV12,dV34] for voltage measurements. Likewise, the Level 2 search coil magnetomete data products when present in these data files are expressed in sensor coordinates: [u,v,w] for magnetic field measurements.The time resolution of the DFB burst waveform data can vary by multiples of 2^N. During encounter when PSP is within 0.25 AU of the Sun, the DFB burst waveform data cadence is typically 150,000 samples/s. This rate is the sample rate of the analog to digital converters, ADC, and data taken at this rate do not pass through a digital filter.References:* 1) Fox, N.J., Velli, M.C., Bale, S.D. et al., Space Sci Rev (2016) 204:7. https://doi.org/10.1007/s1121401502116* 2) Bale, S.D., Goetz, K., Harvey, P.R. et al., Space Sci Rev (2016) 204:49. https://doi.org/10.1007/s1121401602445* 3) Malaspina, D.M., Ergun, R.E., Bolton, M. et al., JGR Space Phys. (2016), 121, 5088-5096. https://doi.org/10.1002/2016JA022344

MMS 1 Fast Plasma Investigation, Dual Ion Spectrometer (FPI, DIS) Distribution Moments, Level 2 (L2), Burst Mode, 0.15 s Data

The Fast Plasma Instrument (FPI) usually Operates in Fast Survey (FS) Mode in the MMS Region Of Interest (ROI) for the current Mission Phase. Data are taken at Burst (30/150 ms for DES/DIS) Resolution in this Mode. Data are also made available at Survey (4.5 s, etc.) Resolution. Per Mission Design, not all Burst Resolution Data are downlinked, but all Survey Data are downlinked. Planning around Calibration Activities, avoidance of Earth Radiation Belts, etc., when possible, FPI usually Operates in Slow Survey (SS) Mode outside of ROI, and then only the 60 s Resolution Survey Data are available. This Product contains Results from integrating the standard Moments of Phase Space Distributions formed from the indicated Data Type (DES/DIS Burst, FS or SS). For Convenience, some additional Parameters are included to augment those most commonly found in a Moments Product of this sort, plus Time Stamps and other Annotation characterizing the State of the Instrument System at the indicated Time.

MMS 2 Hot Plasma Composition Analyzer (HPCA) Ions, Level 2 (L2), Burst Mode, 0.625 s Data

MMS 3 Energetic Particle Detector, Energetic Ion Spectrometer (EPD-EIS) Energy by Time of Flight, Level 2 (L2), Burst Mode, 0.605 s Data

CGRO/BATSE Gamma-Ray Burst Catalog

This database table comprises the gamma-ray bursts detected by the BATSE instrument on the Compton Gamma-Ray Observatory (CGRO). It includes the gamma-ray bursts from the BATSE 4B Catalog (triggers 105 through 5586, observed between April 19, 1991, and August 29, 1996) as well as a large number of triggered bursts since the publication of the BATSE 4B Catalog. All BATSE trigger data from the CGRO mission are available through this facility. As part of a final archiving effort, the BATSE instrument team is making minor refinements to certain data products. These revised products will be delivered to the HEASARC as soon as they are produced and tested. Certain burst catalog parameters, notably the position information, may be revised through improved analyses and instrumental calibration. The final catalog will be posted here as soon as it is completed. The data files used to construct this database table are obtained from the following pages on the BATSE GRB Team website: <pre> BATSE Current Gamma-Ray Burst Catalog: <a href="http://gammaray.msfc.nasa.gov/batse/grb/catalog/current/">http://gammaray.msfc.nasa.gov/batse/grb/catalog/current/</a> Some flux and fluence data and all the comments are from the BATSE 4B Catalog: <a href="http://gammaray.msfc.nasa.gov/batse/grb/catalog/4b/">http://gammaray.msfc.nasa.gov/batse/grb/catalog/4b/</a> </pre> This database table was first created at the HEASARC in June 2001. The HEASARC version is automatically updated within one week of whenever the data files located at <a href="http://gammaray.msfc.nasa.gov/batse/grb/catalog/current/">http://gammaray.msfc.nasa.gov/batse/grb/catalog/current/</a> are changed. This is a service provided by NASA HEASARC .

MMS 2 Search Coil Magnetometer (SCM) AC Magnetic Field Level 2 (L2), High Speed Burst Mode, 16384 Sample/s Data

Search Coil Magnetometer (SCM) AC Magnetic Field (16384 samples/s), Level 2, High Speed Burst Mode Data. The tri-axial Search-Coil Magnetometer with its associated preamplifier measures three-dimensional magnetic field fluctuations. The analog magnetic waveforms measured by the SCM are digitized and processed inside the Digital Signal Processor (DSP), collected and stored by the Central Instrument Data Processor (CIDP) via the Fields Central Electronics Box (CEB). Prior to launch, all SCM Flight models were calibrated by LPP team members at the National Magnetic Observatory, Chambon-la-Foret (Orleans). Once per orbit, each SCM transfer function is checked thanks to the onboard calibration signal provided by the DSP. The SCM is operated for the entire MMS orbit in survey mode. Within scientific Regions Of Interest (ROI), burst mode data are also acquired as well as high speed burst mode data. This SCM data set corresponds to the AC magnetic field waveforms in nanoTesla and in the GSE frame. The SCM instrument paper for SCM can be found at http://link.springer.com/article/10.1007/s11214-014-0096-9 and the SCM data product guide at https://lasp.colorado.edu/mms/sdc/public/datasets/fields/.

MMS 1 Energetic Particle Detector, Energetic Ion Spectrometer (EPD-EIS) Energy by Time of Flight, Level 2 (L2), Burst Mode, 0.605 s Data

MMS 4 Electric Particle Detector, Fly's Eye Energetic Particle Sensor (EPD, FEEPS) Electrons, Level 2 (L2), Burst Mode, 0.3025 s Data

Fly's Eye Electron Proton Spectrometer (FEEPS) Burst Data. The Energetic Particle Detector (EPD) investigation aboard the four MMS spacecraft consists of two instrument designs, the FEEPS and the EIS (Energetic Ion Spectrometer). A FEEPS consists of six Heads, each composed of two Eyes. Each eye is a particle telescope with a single silicon detector. There are nine electron eyes and three ion eyes per FEEPS. The energy coverage is from 25 keV to 650 keV for electrons and 45 keV to 650 keV for ions. Each eye has sixteen energy channels, the spacing of which can be modified by command. The fields of view and pointing of each eye are designed to provide a broad, instantaneous field of view for the twelve eyes per FEEPS.

MMS 2 Energetic Particle Detector, Energetic Ion Spectrometer (EPD-EIS) Pulse Height by Time of Flight, Level 2 (L2), Burst Mode, 0.605 s Data

Energetic Particle Detector (EPD), Energetic Ion Spectrometer (EIS) Pulse Height by Time of Flight, Level 2, Burst Survey, 0.605 s Data. The EIS provides ion composition measurements (protons versus oxygen ions) and angular distributions over the energy range from approximately 45 to 500 keV.

MMS 3 Flux Gate Magnetometer (FGM) DC Magnetic Field, Level 2 (L2), Burst Mode, 128 Sample/s, v4/5 Data