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SOHO LASCO C2 Polarized Brightness FITS Data

The Polarized Brightness data from the LASCO C2 coronagraph.LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).

SOHO LASCO C3 Polarized Brightness FITS Data

The Polarized Brightness data from the LASCO C3 coronagraph.LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).

VOYAGER 1 SATURN PLASMA DERIVED ION FITS BROWSE 96 SEC

THIS DATA SET CONTAINS THE ION DENSITIES, TEMPERATURES, AND VELOCITIES OBTAINED FROM VOYAGER 1 PLS DATA (VOLTAGE RANGE 10-5950 EV/Q) AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS. IT IS A SUBSET OF THE DATA SET VG1-S-PLS-5-ION-FIT-96.0SEC WHICH SHOULD BE OBTAINED BEFORE THIS DATA IS USED. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE OXYGEN. OUTSIDE L=10-12 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. A COMPLETE DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: FIRST 5 COLUMNS ARE TIME TAG (YEAR, DAY, HOUR, MIN SEC.MSEC), FOLLOWED BY PROTON DENSITY (CM-3), PROTON TEMPERATURE (EV), HEAVY ION DENSITY (CM-3), HEAVY ION TEMPERATURE (EV), AND THREE VELOCITY COMPONENTS, (RHO, PHI,Z) IN KM/S. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. EACH ROW HAS THE FORMAT (2I4,2I3,F7.3,7E11.3). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

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).

VOYAGER 1 SATURN PLASMA DERIVED ION FITS 96 SEC

THIS DATA SET CONTAINS THE ION PARAMETERS IN THE PLS VOLTAGE RANGE (10-5950 EV/Q) WITH FORMAL 1 SIGMA ERRORS OBTAINED FROM VOYAGER 1 DATA AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS TO OBTAIN PLASMA DENSITIES, TEMPERATURES, AND VELOCITY. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE OXYGEN. OUTSIDE L~10 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. THE VALUES FOR POSITION AND MAGNETIC FIELD GIVEN IN THE DATA SET ARE ONLY APPROXIMATE AND SHOULD NOT BE USED FOR PUBLICATION. PARAMETERS WHICH ARE IDENTICALLY 0 AND HAVE UNCERTAINTIES OF 0 WERE NOT FIT DUE TO INSUFFICIENT DATA DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: EACH DATA RECORD CONSISTS OF 5+2N LINES, WHERE N IS THE NUMBER OF IONS FIT. LINE 1: S (A1, INDICATES THE START OF A NEW FIT) HRMIN(I5),SEC.MSEC(F7.3) RADIUS(F7.3),RHO(F7.3) MODE OF FITTER(I4) THIS DATA SET, INDICATING PROGRAMS INCORPORATING THE FULL RESPONSE FUNCTION OF THE INSTRUMENT FOR L MODES DATA): CHI-SQUARE FROM FIT (E7.3) TELL WHICH CHANNELS WERE FIT: CUP IDENTIFIER (A,B,C,D) (A1) NUMBER OF SETS OF CHANNELS FIT (I3) CHANNEL OF EACH SET (2-20I3): LINE 6 F (LINE IDENTIFIER) (A1) MASS, CHARGE (I3,I2) WHERE THE X* VARIABLES ARE FORMAL 1 SIGMA UNCERTAINTIES: LINE 7 NUMBER (A1, I1) 6 AND 7 REPEAT ONCE FOR EACH ION SPECIES. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. V'S ARE VELOCITIES IN KM/S, W'S THERMAL SPEEDS IN KM/S, AND DENSITIES IN CM-3. VALUES OF B AND POSITION INFORMATION MAY BE UNRELIABLE AND SHOULD BE VERIFIED BEFORE USE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

VOYAGER 2 SATURN PLASMA DERIVED ION FITS BROWSE 96 SEC

THIS DATA SET CONTAINS THE ION DENSITIES, TEMPERATURES, AND VELOCITIES OBTAINED FROM VOYAGER 2 PLS DATA (VOLTAGE RANGE 10-5950 EV/Q) AT SATURN BY FITTING THE MEASURED SPECTRA WITH ISOTROPIC MAXWELLIAN DISTRIBUTIONS. IT IS A SUBSET OF THE DATA SET VG2-S-PLS-5-ION-FIT-96.0SEC WHICH SHOULD BE OBTAINED BEFORE THIS DATA IS USED. ONLY SPECTRA WHICH HAD DISTINCT CURRENT PEAKS WERE FIT. SPECTRA WERE FIT USING ONE OR TWO ION SPECIES, PROTONS AND/OR A HEAVY ION WHICH WAS TAKEN TO BE OXYGEN. OUTSIDE L=10-12 ION SPECTRA CHANGE RAPIDLY, SO THE VALUES IN THIS DATA SET DO NOT REPRESENT AVERAGE PLASMA CONDITIONS IN THE OUTER MAGNETOSPHERE. A COMPLETE DESCRIPTION OF THIS DATA SET IS GIVEN IN RICHARDSON (1986). DATA FORMAT: FIRST 5 COLUMNS ARE TIME TAG (YEAR, DAY, HOUR, MIN SEC.MSEC), FOLLOWED BY PROTON DENSITY (CM-3), PROTON TEMPERATURE (EV), HEAVY ION DENSITY (CM-3), HEAVY ION TEMPERATURE (EV), AND THREE VELOCITY COMPONENTS, (RHO, PHI,Z) IN KM/S. A CYLINDRICAL COORDINATE SYSTEM CENTERED ON THE PLANET IS USED, WITH RHO OUTWARDS FROM THE SPIN AXIS, PHI IN THE DIRECTION OF ROTATION, AND Z THE DISTANCE ABOVE THE EQUATOR. EACH ROW HAS THE FORMAT (2I4,2I3, F7.3,7E11.3). VALUES OF 1.E32 INDICATE THAT THE PARAMETER COULD NOT BE OBTAINED FROM THE DATA USING THE STANDARD ANALYSIS TECHNIQUE. ADDITIONAL INFORMATION ABOUT THIS DATASET AND THE INSTRUMENT WHICH PRODUCED IT CAN BE FOUND ELSEWHERE IN THIS CATALOG. AN OVERVIEW OF THE DATA IN THIS DATA SET CAN BE FOUND IN RICHARDSON (1986) AND A COMPLETE INSTRUMENT DESCRIPTION CAN BE FOUND IN BRIDGE (1977).

SOHO LASCO C3 Level 0.5 FITS Data

The LASCO C3 Raw FITS Data. LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).

SDO/AIA Synoptic FITS Data

The SDO/AIA Level 1.5 Synoptic FITS Data. The AIA Synoptic FITS data are reduced to 1024x1024 2.4 arc-sec pixels by summing with pixel value in DN per original 0.6 arc-sec pixel. The data cadence is 2 minutes. These images are produced approximately 7 days after T_OBS since they are derived from definitive level 1 data.

Cassini CAPS Fitted Parameters Bundle

This data set consists of all of the fits (both good and bad) that were found by Dr. Robert J. Wilson during the NASA Cassini Data Analysis Program grant (NNX12AG90G). The Cassini CAPS plasma data used in the forward model plasma parameter calculations given here came from volume CO-E/J/S/SW-CAPS-2-UNCALIBRATED-V1.0 in the Planetary Data System (PDS).

VOYAGER 2 SATURN PLASMA DERIVED ION FITS 96 SEC

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VOYAGER 1 SATURN PLASMA DERIVED ION FITS 96 SEC

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Voyager 1 Plasma Spectrometer (PLS) VIPER-Fit Plasma Ion Composition near Jupiter, 96 s Data

These Data are from a Re-Analysis of the Voyager Plasma Spectrometer, PLS, Data at Jupiter by the PLS Group at the Laboratory for Atmospheric and Space Physics, LASP, at the University of Colorado. Density, Temperature, and Flow Velocity Fits for total and individual Ions were done using the Voyager Ion PLS Experiment Response, VIPER, Code and Error Analysis as described at http://lasp.colorado.edu/home.mop/missions/voyager/viper/. Fits are determined from processing of the Ion Currents from the A, B, C, and D Cups of the Instrument. As per the Fit Case Variable, one of five different Constraints were used in the VIPER Fits for each 96 s Time Interval: (1) Free Variation of all Parameters (mainly for the cold Ion Torus), (2) Constraint of the Ion Abundances for the five major Species (O+, O++, S+, S++, S+++) to standard Composition as determined from Delamere et al., (2005), (3) fixed Ion Composition and Flow Speed, (4) Cold Blobs in the Plasmasheet where resolved Peaks can be Fit with allowance for some Variance in Composition, (5) Interpolation between Composition of Cold Torus and standard Abundances at 6 RJ from Delamere et al., (2005). Reference: Delamere, P.A., Bagenal, F., and Steffl, A. (2005), Radial Variations in the Io Plasma Torus During the Cassini Era, J. of Geophys. Res., Space Phys., 110(A12), A12223, doi:10.1029/2005JA011251.

VOYAGER 1 SATURN PLASMA DERIVED ION FITS BROWSE 96 SEC

THIS DATA SET CONTAINS ESTIMATES OF THE ION MOMENT DENSITY IN THE PLS VOLTAGE RANGE (10-5950 EV/Q) AT SATURN DURING THE VOYAGER 1 ENCOUNTER. RIGID COROTATION IS ASSUMED, WHICH LEADS TO AN UNDERESTIMATE OF THE DENSITY IN SOME REGIONS, AS DOES THE USE OF AN ACCEPTANCE AREA RELEVANT FOR A COLD BEAM FOR PLASMA WHICH IS TRANSONIC IN SOME REGIONS. DENSITIES MAY BE UNDERESTIMATED BY A FACTOR OF 2-3 IN THE INNER MAGNETOSPHERE, SO THIS DATA SET SHOULD BE USED PRIMARILY FOR STUDIES USING VARIATIONS IN PLASMA DENSITY. THE FIT DENSITIES GIVE A BETTER ESTIMATE OF THE ABSOLUTE DENSITY. THIS IS THE DATA SHOWN AND DESCRIBED IN DETAIL IN LAZARUS AND MCNUTT (1983).

SOHO LASCO C3 Level 1.0 FITS Data

The LASCO C3 Calibrated FITS Data. LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).

SOHO LASCO C2 Level 1.0 FITS Data

The LASCO C2 Calibrated FITS Data. LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).

PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPC Ion Number Density, Velocity, and Thermal Speed Momemts and Fits, Level 3 (L3), 0.2185 s Data

SPC Level 3 Ion Data--------------------File Naming Format: psp_swp_spc_l3i_YYYYMMDD_v01.cdfThis data product contains derived measurements of ion properties in the solar wind, including those for density, temperature, and velocity. These are determined both by a direct computation of the velocity moments of the reduced distribution function and by attempting to fit the primary peak in the ion I(V) curve with a Maxwellian model. These measurements correspond one to one with spectra in the psp_swp_spc_l2i file for the same date. It may be convenient for some applications to cross-reference the two. For example, the corresponding l3i file contains ephemeris and data quality flag information that may be useful for an investigator who is concerned only with l2i type measurements.Conditions that impact measurement quality are documented in the DQF variable, which contains a 32 element flag array for each measurement time. Each element of the array is reserved to signify a specific condition. These conditions are described in the DQF_FLAGNAMES variable. In this version, for example, DQF_FLAGNAMES.DAT[23] is set to "spacecraft maneuver". If measurement "i" was made during a spacecraft maneuver, it is thus flagged with DQF.DAT[23,i] = 1.In Version 01, measurements are not provided, i.e. variables are set to fill, during spacecraft maneuvers, under conditions of low signal-to-noise, and during certain observed transients. Such conditions are rare during encounters, but increasingly frequent in interplanetary cruise. These conditions are documented in the DQF variable. Remarks are also provided in the "SPC Reduced Data Quality Periods" table. In Version 01, the solar wind alpha particle component is not measured. Thus, variables are set equal to fill values.SPC Encounter 1 Remarks-----------------------Data quality is very good for the duration of the encounter. The solar wind flow was within the optimal field of view for the SPC instrument for nearly the entire encounter. See the data flags for specific exceptions. As with all encounters, signal-to-noise is higher during ingress than egress, which is reflected in the typically smaller uncertainties and less frequent "primary peak low signal" flag events.SPC Cruise Phase Remarks------------------------Measurements recorded during cruise phase are not all transmitted to Earth. The typical return is one spectrum out of every 32.SPC Encounter 2 Remarks-----------------------Due to an erroneous setting in the operating mode for this encounter, ion full scan spectra and certain spectra immediately following ion full scans are of reduced quality. In the affected full scan spectra, the energy steps over an initial portion of the measurement spectra have zero width, i.e. the Level 2 ion variables MV_LO.DAT = MV_HI.DAT, and the corresponding measurements are purely noise. In some cases, this results in a poor determination of the proton "primary peak" energy, which renders additional subsequent full scans that follow subject to the same incompleteness. In other cases, the energy range for the subsequent "ion peak tracking mode" scan is not ideal. The affected Level 3 ion measurements have been flagged with DQF.DAT[22]=1, which stands for "energy ranging/peak tracking error" and/or set to fill. The operating mode has been revised such that future encounters will not be so affected.Parker Solar Probe SWEAP Rules of the Road------------------------------------------As part of the development of collaboration with the broader Heliophysics community, the mission has drafted a "Rules of the Road" to govern how PSP instrument data are to be used.* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: "We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.".* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.

SOHO LASCO C3 Percent Polarized FITS Data

The Percent Polarized data from the LASCO C3 coronagraph.LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).

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Voyager 2 Plasma Spectrometer (PLS) VIPER-Fit Plasma Ion Composition near Jupiter, 96 s Data

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SOHO LASCO C1 Level 0.5 FITS Data

The LASCO C1 Raw FITS Data. LASCO (Large Angle Spectroscopic Coronagraph) is comprised of three nested coronagraphs (C1, C2, and C3) that image the solar corona from 1.1--30 solar radii (C1: 1.1--3; C2: 1.5--6; and C3: 3--30). The inner coronagraph (C1) is a newly developed mirror version of the classic Lyot coronagraph without an external occulter, while the middle coronagraph (C2) and the outer one (C3) are externally occulted. C1 is equipped with a Fabry-Perot interferometer that can take monochromatic images over the whole field of view with a spectral resolution of 0.07 nm. By stepping the bandpass across a spectral line, line profiles and Doppler shifts can be derived from all 1024 x 1024 pixels simultaneously. With an equivalent pixel size of 5.6 arcsec, the spatial resolution of C1 is ~11 arcsec. The resolution is ~23 arcsec for C2, and 112 arcsec for C3. The calculated expected precision of the emission line measurements, for example, of the 637.4 nm Fe X line is 0.05 Km/s at 1.1 solar radii, 1.0 km/s at 2 solar radii, and 8.0 km/s at 3 solar radii, all for a 60 s exposure. All three devices use a 1024 x 1024 pixel CCD. The CCDs are passively cooled to 193 K, but can be heated above ambient temperatures to drive off condensed material. The readout rate is ~21 s for a full image, but any line on the CCD can be accessed within about 60 ms, the unwanted lines being dumped. The electronics box provides overall control, including observation programs and scheduling. An observation program can be scheduled to be run at an absolute time or just next in sequence. It can run for a certain number of iterations, an interval of time, or stop at an absolute time. The observation program tasks included, e.g., taking single images from one of the telescopes, a series of images through the three linear polarizers, and a sequence of images at a series of Fabry-Perot wavelength steps. The image processing tasks are primarily image compression, with seven different techniques being available. On average, the readout time should be ~6 minutes or about 200 images/day. This information is from the paper ``The Large Angle Spectroscopic Coronagraph (LASCO): Visible Light Coronal Imaging and Spectroscopy,'' by G. E. Brueckner et al. (Proceedings of the First SOHO Workshop, ESA SP-348, pp. 27-34, November 1992).