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107 results for “Juno”
MHD Model of Ganymede's Magnetosphere: Predicted OCFB and magnetic footprint surface locations for Juno's flyby
<p>This dataset contains model results from a magnetohydrodynamic (MHD) model of Ganymede's magnetosphere adapted to Juno's PJ34 flyby in 2021. Here we publish coordinates for the predicted location of the open-closed-field line-boundary (OCFB) on Ganymede's surface. Additionally we provide coordinates of Juno's magnetic footprint, namely the surface locations that connect to Juno's trajectory through magnetic field lines.</p> <p>For the surface locations we use a western longitude planetographic coordinate system where 0° longitude is in direction of the y-axis and 90° in direction of the x-axis of the cartesian GPhiO system. The GPhiO system is defined by the primary direction<br> z parallel to Jupiter’s rotation axis, the secondary direction y is pointing towards Jupiter barycenter<br> and x completes the right-handed system approximately in direction of plasma flow.</p> <p><strong>Duling2022_JunoGanymede_modeled_surface_OCFB.txt</strong></p> <p>Columns:</p> <p>Longitude [°]<br> Northern OCFB latitude [°]<br> Southern OCFB latitude [°]</p> <p><strong>Duling2022_JunoGanymede_modeled_magnetic_footprint.txt</strong></p> <p>Columns:</p> <p>Spacecraft time [UTC]<br> Magnetic footprint longitude [°]<br> Magnetic footprint latitude [°]<br> Length of field line between Juno and surface [radii]<br> Length of field line between Juno and surface [km]<br> r coordinate of Juno [radii]<br> Latitude of Juno [°]<br> Longitude of Juno [°]<br> x of Juno in GPhiO [km]<br> y of Juno in GPhiO [km]<br> z of Juno in GPhiO [km]</p> <p><strong>Duling2022_JunoGanymede_surface_map.png</strong></p> <p>A plot that visualizes the data of this repository.</p>
MHD Model of Ganymede's Magnetosphere: Predicted magnetic field on Juno's trajectory
<p>This dataset contains model results from a magnetohydrodynamic (MHD) model of Ganymede's magnetosphere adapted to Juno's PJ34 flyby in 2021. Here we publish predicted magnetic field components on Juno's trajectory that can be compared to MAG measurements and are displayed in Figure 3 of Duling et al. (2022).</p> <p>Each file contains data from one model. The dataset includes all models with parameter variations from Duling et al. (2022). These are summarized in Table 1 of Duling et al. (2022) and displayed in Figure 3 with the gray lines.</p> <p>If not varied, all models are run with the following parameters:</p> <p>Upstream Jovian background magnetic field B<sub>0 </sub>= (−15,24,−75) nT<br> Upstream plasma velocity v<sub>0</sub> = 140 km/s<br> Upstream plasma mass density <span class="math-tex">\(\rho\)</span><sub>0</sub> = 100 amu/cm<sup>3</sup><br> Upstream plasma thermal pressure p<sub>0</sub> = 2.8 nPa<br> Ionization frequency <span class="math-tex">\(\nu_{ion}\)</span> = 2.2e-8/s<br> Atmospheric surface mass density <span class="math-tex">\(n_{n,0}\)</span> = 8e6/cm<sup>3</sup><br> Dipole Gauss coefficient <span class="math-tex">\(g_1^0\)</span> = −716.8 nT</p> <p> </p> <p>The published data files correspond to the following models with each one parameter variation:</p> <table> <thead> <tr> <th scope="col">Parameter</th> <th scope="col">Value</th> <th scope="col">Filename Suffix</th> </tr> </thead> <tbody> <tr> <td>default model</td> <td> - </td> <td>default</td> </tr> <tr> <td>Upstream Jovian background magnetic field (measured before flyby)</td> <td>B<sub>0 </sub>= (−16,3,−70) nT</td> <td>B0before</td> </tr> <tr> <td>Upstream Jovian background magnetic field (measured after flyby)</td> <td>B<sub>0 </sub>= (−14,43,−80) nT</td> <td>B0after</td> </tr> <tr> <td>Upstream plasma velocity (min)</td> <td>v<sub>0</sub> = 120 km/s</td> <td>v-</td> </tr> <tr> <td>Upstream plasma velocity (max)</td> <td>v<sub>0</sub> = 160 km/s</td> <td>v+</td> </tr> <tr> <td>Upstream plasma mass density (min)</td> <td><span class="math-tex">\(\rho\)</span><sub>0</sub> = 10 amu/cm<sup>3</sup></td> <td>rho-</td> </tr> <tr> <td>Upstream plasma mass density (max)</td> <td><span class="math-tex">\(\rho\)</span><sub>0</sub> = 160 amu/cm<sup>3</sup></td> <td>rho+</td> </tr> <tr> <td>Upstream plasma thermal pressure (min)</td> <td>p<sub>0</sub> = 1.0 nPa</td> <td>p-</td> </tr> <tr> <td>Upstream plasma thermal pressure (max)</td> <td>p<sub>0</sub> = 5.0 nPa</td> <td>p+</td> </tr> <tr> <td>Ionization frequency (min)</td> <td> <span class="math-tex">\(\nu_{ion}\)</span> = 0.5e-8/s</td> <td>prod-</td> </tr> <tr> <td>Ionization frequency (max)</td> <td> <span class="math-tex">\(\nu_{ion}\)</span> = 10.0e-8/s</td> <td>prod+</td> </tr> <tr> <td>Atmospheric surface mass density (min)</td> <td> <span class="math-tex">\(n_{n,0}\)</span> = 1.6e6/cm<sup>3</sup></td> <td>nn-</td> </tr> <tr> <td>Atmospheric surface mass density (max)</td> <td> <span class="math-tex">\(n_{n,0}\)</span> = 40e6/cm<sup>3</sup></td> <td>nn+</td> </tr> <tr> <td>Dipole Gauss coefficient (min)</td> <td> <span class="math-tex">\(g_1^0\)</span> = −702.5 nT</td> <td>dipole-</td> </tr> <tr> <td>Dipole Gauss coefficient (max)</td> <td> <span class="math-tex">\(g_1^0\)</span> = −731.1 nT</td> <td>dipole+</td> </tr> </tbody> </table> <p>Magnetic Field components and Juno's position are in GPhiO system. GPhiO is defined by the primary direction z parallel to Jupiter’s rotation axis, the secondary direction y is pointing from Ganymede's towards Jupiter's barycenter and x completes the right-handed system approximately in direction of plasma flow.</p> <p>Columns:</p> <p>Spacecraft time [UTC]<br> Bx modeled magnetic field in GPhiO [nT]<br> By modeled magnetic field in GPhiO [nT]<br> Bz modeled magnetic field in GPhiO [nT]<br> B modeled magnetic field magnitude [nT]<br> x of Juno in GPhiO [km]<br> y of Juno in GPhiO [km]<br> z of Juno in GPhiO [km]</p>
List of HOM/DAM Radio Sources crossings during Juno's 45 first perijoves
<p>This data is associated with Collet 2024 (JGR) A new type of "Jovian hectometric radiation powered by monoenergetic electron beams" in review.</p> <p>This document shows a dataset of HOM/DAM sources detected during the 45 first Juno perijoves. These sources are identified from Juno/Waves measurements with the criterion fce<f<fce+1% from Louis (2019).</p>
Corresponding Dataset for "Ganymede's Ionosphere observed by a Dual-Frequency Radio Occultation with Juno"
<p> Corresponding Dataset for "Ganymede’s Ionosphere observed <br> by a Dual-Frequency Radio Occultation with Juno"<br> README FILE<br> VERSION 2<br> Dustin Buccino<br> April 22, 2024<br> Jet Propulsion Laboratory<br> California Institute of Technology</p> <p>=============================================================================<br>VERSION 2 INFORMATION<br>=============================================================================</p> <p> Version 2 of this dataset separates the Electron Density profile from the<br>main data files and makes a correction to the egress profile that was<br>discovered. Differences in egress profile are very small and within<br>the uncertainties. Furthermore egress is statistically a non-detection<br>(zero densities), but for sake of accuracy they are reposted to be<br>consistent with the publication.</p> <p>=============================================================================<br>INTRODUCTION<br>=============================================================================</p> <p> This dataset contains processed radio science data and results of the<br>Juno Ganymede radio occultation. This dataset is provided in order to <br>supplement the submitted article to the "Geophysical Research Letters"<br>journal:</p> <p> Buccino, D.R., et al (2022), Ganymede’s Ionosphere observed by a <br> Dual-Frequency Radio Occultation with Juno, Geophysical Research <br> Letters, submitted February 2022.</p> <p><br> Please note the raw data used in this analysis are not provided in this<br>supplementary dataset. The raw Juno Gravity Science Data may be found at <br>the Planetary Data System:</p> <p> Buccino, D. R. (2016). Juno jupiter gravity science raw data set <br> V1.0, JUNO-J-RSS-1 JUGR-V1.0, NASA planetary data system (PDS). <br> Retrieved from https://atmos.nmsu.edu/PDS/data/jnogrv_1001/<br> </p> <p>=============================================================================<br>ARCHIVE INFORMATION<br>=============================================================================</p> <p> This archive contains two files within the root directory.<br> <br> ROOT<br> `- JunoG34OccData_Egress_v2.csv</p> <p> This data file contains the EGRESS data relevant to the radio<br> occultation. The data is a timeseries of impact parameter, sky<br> sky frequency at X-band and Ka-band, the dual-frequency <br> combination, the calibrated dual-frequency, Total Electron <br> Content.</p> <p> `- JunoG34_GRL_Egress_Profile_v2.csv</p> <p> This data file contains the EGRESS Electron density, and <br> 1-sigma electron density uncertainty.</p> <p> `- JunoG34OccData_Ingress_v2.csv</p> <p> This data file contains the INGRESS data relevant to the radio<br> occultation. The data is a timeseries of impact parameter, sky<br> sky frequency at X-band and Ka-band, the dual-frequency <br> combination, the calibrated dual-frequency, Total Electron <br> Content.</p> <p> `- JunoG34_GRL_Ingress_Profile_v2.csv</p> <p> This data file contains the INGRESS Electron density, and <br> 1-sigma electron density uncertainty.</p> <p>=============================================================================<br>FILE FORMAT<br>=============================================================================</p> <p> This dataset contains only a comma-separated text files which are<br>given with the "*.csv" extension.</p> <p><br> CSV FILES<br> -------------------------------------------------------------------------</p> <p> The Comma-Separated Value (CSV) files are plain-text files. Values in<br> each data file are separated using a comma ",". Each column is defined <br> by a header row which provides a description of each column.<br> </p> <p>=============================================================================<br>ACKNOWLEDGMENTS<br>=============================================================================</p> <p>This work was carried out at the Jet Propulsion Laboratory, <br>California Institute of Technology, under contract with the National <br>Aeronautics and Space Administration. Government sponsorship acknowledged.</p> <p>EG, LGC, PT, MZ and AC are grateful to the Italian Space Agency (ASI) for <br>financial support through Agreement No. 2018-25-HH.0 in the context of ESA's <br>JUICE mission, and Agreement No. 2017-40-H.1-2020, and its extension <br>2017-40-H.02020-13-HH.0, for ESA’s BepiColombo and NASAs Juno radio science <br>experiments. EG is grateful to "Fondazione Cassa dei Risparmi di Forlì" for <br>financial support of his PhD fellowship.</p> <p>PS and AH were supported by NASA Contract NNM06AA75C from the Marshall <br>Space Flight Center under subcontract 699054X from Southwest Research <br>Institute.</p> <p><br>=============================================================================<br>PRIMARY POINT OF CONTACT<br>=============================================================================</p> <p>Dustin Buccino<br>Jet Propulsion Laboratory<br>Planetary Radar and Radio Sciences<br>(818) 393 - 1072<br>Dustin.R.Buccino@jpl.nasa.gov</p> <p>=============================================================================<br>ACRONYMS AND ABBREVIATIONS<br>=============================================================================</p> <p> ASCII American Standard Code for Information Interchange<br> DOY Day of year<br> DSN Deep Space Network<br> JPL Jet Propulsion Laboratory<br> NAIF Navigation Ancillary Information Facility<br> NASA National Aeronautics and Space Administration<br> PDS Planetary Data System<br> RS Radio Science<br> RSS Radio Science Subsystem<br> SIS Software Interface Specification<br> TXT Text file<br> UTC Universal Time, Coordinated</p>
Distribution of interplanetary dust detected by the Juno spacecraft and its contribution to the Zodiacal Light
<p>The Zodiacal light is sunlight reflected by dust in the inner solar system. Variations in the Zodiacal light with ecliptic latitude reveal discrete bands of dust orbiting near the ecliptic plane. The Juno spacecraft, in transit from earth to Jupiter, recorded a sufficient number of impacts with this dust to characterize their distribution in space for the first time. </p> <p>This dataset (filename IDP_List.txt) contains a time-ordered list of all IDP impact detections along with supplementary engineering and ephemeris information. The file is an ASCII text file and the file format is described in the word document (IDP_List_Format.docx).</p>
Juno Plasma Wave Observations at Europa
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics.</p><p><strong>Abstract</strong><br>Juno passed by Europa at an altitude of 355 km on 29 September, day 272, 2022. As one of Juno's in situ science instruments, the Waves instrument obtained observations of plasma waves that are essential contributors to Europa's interaction with its environment. Juno observed chorus, a band at the upper hybrid frequency providing the local plasma density, and electrostatic solitary structures in the wake. In addition, impulses due to micron-sized dust impacts on Juno were recorded with a local maximum very close to Europa. The peak electron density near Europa was ∼ 330 cm−3 while the surrounding magnetospheric density was in the range of 50 to 150 cm−3. There was a significant separation between the Europa flyby and Juno's crossing of Jupiter's magnetic equator, enabling a unique identification of effects associated with the moon as opposed to magnetospheric phenomena normally occurring at the magnetic equator near 10 Jovian radii.</p>
Corresponding Dataset for Gravity Field of Ganymede after the Juno Extended Mission
<p>Corresponding Dataset for Gravity Field of Ganymede after the Juno Extended Mission</p> <p> Luis Gomez Casajus August 2, 2022</p> <p>=============================================================================<br> Introduction<br> =============================================================================</p> <p> This dataset contains the estimated gravity field and its corresponding<br> full covariance matrix. This dataset is provided in order to <br> supplement the submitted article to the "Geophysical Research Letters"<br> journal:</p> <p> Gravity Field of Ganymede after the Juno Extended Mission.<br> L. Gomez Casajus (*), A. I. Ermakov, M. Zannoni, J. T. Keane, <br> D. Stevenson, D. R.Buccino, D. Durante, M. Parisi, R. S. Park, <br> P. Tortora and S. J. Bolton<br> <br> - (*) luis.gomezcasajus@unibo.it</p> <p>=============================================================================<br> File description<br> =============================================================================</p> <p> This archive contains two files within the root directory.<br> <br> ROOT<br> -SOI_gravity_field.txt</p> <p> This file contains the estimated normalized spherical harmonics <br> coefficients of the Ganymede gravity field.<br> The file contains a header row which provides a description of <br> the file.</p> <p> -SOI_cov_matrix.txt</p> <p> This file contains the estimated full covariance matrix (32x32) <br> of the normalized spherical harmonics coefficients of the <br> Ganymede gravity field. The file contains a header row which <br> provides a description of the file. The matrix is represented as<br> a 2 dimensional array whose coefficients follow the following <br> order scheme: C20 C21 S21 C22 S22 C30 C31 ...</p> <p>=============================================================================<br> ACKNOWLEDGMENTS<br> =============================================================================</p> <p> The authors are grateful to William Folkner, to the entire Solar System <br> Dynamics Group and to Robert Haw, former Galileo navigator, for the useful <br> discussions and suggestions regarding the procedures for Galileo data <br> analysis. L.G.C., M.Z., and P.T. are grateful to the Italian Space Agency <br> (ASI) for financial support through Agreement No. 2017-40-H.1-2020, and its <br> extension2017-40-H.02020-13-HH.0, for ESA’s BepiColombo and NASA’s Juno radio<br> science experiments. L.G.C., M.Z., and P.T. acknowledge Caltech and the Jet <br> Propulsion Laboratory for granting the University of Bologna a license to an <br> executable version of MONTE Project Edition S/W. JTK and AIE acknowledge <br> support from the Juno participating scientist program. The work of RP, DB, <br> JTK, and MP was carried out at the Jet Propulsion Lab, California Institute<br> of Technology, under a contract with the National Aeronautics and Space <br> Administration (80NM0018D0004). Government sponsorship acknowledged. </p>
MHD model output for Ganymede's magnetosphere during Juno's flyby
<p>This dataset contains the complete simulation output from our MHD model of Ganymede's magnetosphere adapted to Juno's PJ34 flyby in 2021 (Duling et al. 2022).</p> <p>The data was obtained by our application of the PLUTO simulation code v4.4 (Mignone et al. 2007) (http://plutocode.ph.unito.it/) described in Duling et al. 2022.</p> <p>The dataset includes the simulation variables on the simulation grid for a single timestep after steady state was reached. The grid has spherical geometry (r, theta, phi) with phi=0° longitude pointing towards Jupiter (positive y axis of the GPhiO system), phi=90° longitude pointing in the upstream direction (negative x axis of GPhiO) and theta=0° latitude at Ganymede's north pole (positive z axis of GPhiO). The following model variables are included:</p> <p>rho: plasma mass density<br> prs: thermal plasma pressure<br> vx1: plasma velocity radial component<br> vx2: plasma velocity theta component<br> vx3: plasma velocity phi component<br> Bx1: magnetic field radial component<br> Bx2: magnetic field theta component<br> Bx3: magnetic field phi component</p> <p>Additionally the following derived variables are included:</p> <p>Jx1: electric current density radial component<br> Jx2: electric current density theta component<br> Jx3: electric current density phi component<br> Bpx1: plasma magnetic field radial component<br> Bpx2: plasma magnetic field theta component<br> Bpx3: plasma magnetic field phi component</p> <p>Plasma magnetic field means that part of the total magnetic field that results from the plasma interaction. It equals the total magnetic field subtracted by the homogeneous upstream field and Ganymede's intrinsic and induced field.</p> <p>All values are in normalized units with these normalization factors:</p> <p>NORMR = 2.631e8 cm<br> NORMV = 1.4e7 cm/s<br> NORMRHO = 1.661e-22 g/cm^3<br> NORMPRS = 3.255e-08 dyne/cm^2<br> NORMB = 6.395e-04 Gauss<br> NORMJ = 5.801e-03 statA/cm^2</p> <p>In Duling et al. 2022 we present results of a model sensitivity study. This dataset includes model output from our best guess setup (default setup) only.</p> <p>Since the data is in PLUTO's binary format "flt" we provide a Python code snippet that reads the data to data arrays.</p> <p><strong>grid.out</strong><br> This ASCII file contains the grid dimensions and coordinates of the cell boundaries.</p> <p><strong>data.0020.flt</strong><br> This binary file contains the simulation variables on the cell centers of the grid.</p> <p><strong>pluto.0.log</strong><br> This ASCII file contains the header of the PLUTO logfile.</p> <p><strong>read_data.py</strong><br> This Python code snippet helps with reading the data.</p>
Figure 1 in Brachymeria koehleri (Hymenoptera: Chalcididae): first record as hyperparasitoid in Dione juno juno (Lepidoptera: Nymphalidae) pupae
Figure 1. Primary parasitoid Chetogena aff. scutellaris (Diptera: Tachinidae) (A) size: 1.0 cm; Hyperparasitoid Brachymeria koehleri (Hymenoptera: Chalcididae) (B) size: 0.6 mm; and parasitized pupa of Dione juno juno (Lepidoptera: Nymphalidae) (C) size: 2.7 cm.
Linked collectors and determiners for: Juno in Central Asia.
Natural history specimen data linked to collectors and determiners held within, "Juno in Central Asia". Claims or attributions were made on Bionomia by volunteer Scribes, <a href="https://bionomia.net/dataset/506de6ea-1c7b-4149-b85f-e2a01e3c8d1a">https://bionomia.net/dataset/506de6ea-1c7b-4149-b85f-e2a01e3c8d1a</a> using specimen data from the dataset aggregated by the Global Biodiversity Information Facility, <a href="https://gbif.org/dataset/506de6ea-1c7b-4149-b85f-e2a01e3c8d1a">https://gbif.org/dataset/506de6ea-1c7b-4149-b85f-e2a01e3c8d1a</a>. Formatted as a Frictionless Data package.
Low-Latitude Whistler-Mode and Higher-Latitude Z-mode Emission at Jupiter Observed by Juno
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics, <a href="https://doi.org/10.1029/2020JA028742">10.1029/2020JA028742</a></p> <p><strong>Abstract</strong></p> <p>Whistler-mode chorus emission is important in the scattering and acceleration of electrons and filling of the radiation belts at Jupiter. In this work whistler mode magnetic intensity levels at Jupiter are comprehensively binned and parameterized. The frequency range of whistler mode under study extends from the proton cyclotron frequency, f<sub>cH</sub>, to f<sub>ceq</sub>/2, where f<sub>ceq</sub> is the cyclotron frequency mapped to the magnetic equator. Parametric dependence of magnetic plasma wave intensity is obtained versus frequency, latitude, and M-shell, as determined using a current magnetic field model based on Juno data. The results extend similar analyses of Jupiter whistler-mode emission obtained by the Galileo spacecraft, particularly on the nightside, and provide better coverage in latitude. Peaks in whistler-mode emission occur near M ~ 8-9, similar to previous studies, with average peak intensities approaching 10<sup>-2</sup> nT<sup>2</sup>, as also found by Galileo on the dayside. Auroral hiss and probably Z-mode are observed at higher latitudes. Jovian chorus emissions near an equatorial source region are more broad-banded than terrestrial chorus, and are coincident with a broad-banded electron distribution of free energy and strong electron scattering to large pitch angles. Intense whistler mode within a young plasma injection region is also observed, similar to injections in Saturn's magnetosphere. Future study of wave particle interactions within the chorus source region will be important. Possible Z-mode emission at significant intensity levels is observed in Jupiter’s inner magnetosphere, more intense, but not unlike Z-mode observed at Saturn.</p> <p><strong>Key Points</strong></p> <ul> <li>Jupiter whistler-mode & Z-mode intensity is binned in f, M, Magnetic latitude, and MLT</li> <li>Chorus emission coincident with electron scattering in source region</li> <li>Narrowband Z-mode emission likely observed at higher frequencies</li> </ul>
The High-Latitude Extension of Jupiter's Io Torus: Electron Densities Measured by Juno Waves
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics, <a href="https://doi.org/10.1029/2021JA029195">10.1029/2021JA029195</a></p> <p><strong>Abstract</strong></p> <p>We present Jovian electron densities measured by the Juno Waves instrument at high-latitudes on magnetic field lines threading the Io torus using the first 29 orbits of the Juno mission. We infer electron densities from characteristic frequency cutoffs and resonances in plasma wave spectra. There are often times when more than one of the characteristic frequency of the plasma can be identified, whose consistency provides more credibility to the plasma density estimates. The majority of density measurements are on magnetic field lines threading the Io torus and intersecting Jupiter's ionosphere between Io's M-shell and the auroral main oval, but there is evidence of density dropouts near and within the auroral oval, which may be important in auroral particle acceleration. Sharp density gradients are found near the inner edge of the Io torus region. These observations demonstrate the extension of elevated Io torus densities along field lines to higher latitudes. </p> <p><strong>Key Points</strong></p> <ul> <li>We present Jovian electron densities at high-latitudes on magnetic field lines connected to the Io torus and plasma sheet</li> <li>Sharp density gradients are found near the inner edge of the Io torus M-shell</li> <li>Our densities are consistent with partial electron densities measured by Juno's Jovian Auroral Distributions Experiment</li> </ul>
Dataset for Widespread occurrence of lava lakes on Io observed from Juno by A. Mura et al.
<div>This database provides supplementary information for the Article:</div> <div>Widespread occurrence of lava lakes on Io observed from Juno</div> <div>by Alessandro Mura, Federico Tosi, Francesca Zambon, Rosaly M. C. Lopes, Pete J. Mouginis-Mark, Jani Radebaugh, Alberto Adriani, Scott Bolton, Julie Rathbun, Andrea Cicchetti, Davide Grassi, Raffaella Noschese, Giuseppe Piccioni, Christina Plainaki, Roberto Sordini, Giuseppe Sindoni</div> <div> </div> <div>The data can be read with MATLAB. Each file name has the following convention:</div> <div> </div> <div>[Name of patera] _ [BAND] _ [ORBIT] _ [FILE]</div> <div>The data is a structure with the following fields:</div> <div> </div> <div> DATA.dat= calibrated data frame</div> <div> DATA.SCLK_SCI = SCLK time</div> <div> DATA.SCI_GeometryEpoch = ASCII time, not for geometry calibration</div> <div> DATA.File_Name_ACQ = PDS name</div> <div> DATA.File_Name_EGSE= EGSE name</div> <div> DATA.Name_cube= Cube name</div> <div> </div> <div>Each file may contain more than one frame. Each frame is 256 lines x 432 columns, and contains the calibrated band radiance in the L (lines 1 to 128) and M (lines 129 to 256) bands). Geometry can be obtained via the SPICE software by using the proper SCET time.</div> <div>The SCET can be obtained with cspice_scs2e from the provided SCLK_SCI field.</div> <div> </div> <div>The names of the Patera are the same as in the article with the following exceptions:</div> <div> </div> <div>Kibero is Unknown 03</div> <div>Dingir P. is Unknown 04</div> <div>JR055 is Unknown 02</div> <div>JR230 is Unknown 05 </div> <div>JR229 is Unknown 06 </div> <div>Hatchawa P. is Unknown 17</div> <div>JR207 is Unknown 16 </div> <div> </div> <div>Along with the data, we provide images of the frame (radiance in log scale). Data from Orbit 60 and 62 has been obtained from a test session occurred after a problem with the dark current electronics of JIRAM. Because the background level was not available, it has been obtained from images where Io was not in the field of view, and subtracted from the others. </div>
Analysis of Whistler-Mode and Z-Mode Emission in the Juno Primary Mission
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics, <a href="https://doi.org/10.1029/2021JA029885">10.1029/2021JA029885</a></p> <p><strong>Key Points:</strong></p> <ul> <li>Jovian whistler-mode chorus and Z-mode intensity distributions are surveyed and analyzed at the end of the Juno primary mission</li> <li>Bursty low frequency whistler mode emission implies electrons energies exceeding 100 keV</li> <li>Jovian whistler mode chorus and Z-mode intensity are parametrically fit to frequency, M-shell, and mag-latitude.</li> </ul> <p><strong>Abstract</strong></p> <p>At the end of the Juno primary mission we report observations of whistler mode chorus and Z-mode emission. The Juno orbits are evolving and much better coverage of the whistler mode chorus source region has resulted since the earlier surveys. Bursty chorus emission extending to ~30° latitude and to frequencies less than the lower hybrid frequency near the source region imply high electron energies (>100 keV). Average chorus intensity levels peak at ~10<sup>-3</sup> nT<sup>2</sup> near M-shell of 8-9 and magnetic latitude of ~5°. Z-mode emission is identified at higher latitudes generally near and inward of the Io torus with intensity levels as much as two orders of magnitude higher than Z-mode emissions observed at Saturn. Inferred source regions for the Z-mode are consistent with the inner edge of the Io torus and with auroral field lines that may also support Jovian kilometric and decametric emission. Parametric fitting functions are evaluated for both whistler mode chorus and Z-mode, describing wave intensity as a function of frequency, magnetic latitude, and M-shell. Both whistler mode and Z-mode waves may have significant impact on electron scattering and acceleration at Jupiter as recent models indicate.</p>
Juno Stellar Reference Unit (SRU) image data from Juno's G34 Ganymede flyby on 7 June 2021
<p>This is the Juno Stellar Reference Unit (SRU) image data from Juno's G34 Ganymede flyby on 7 June 2021. The image is discussed in the paper, "Surface features of Ganymede revealed in Jupiter-shine by Juno's Stellar Reference Unit," published in AGU Geophysical Research Letters.</p>
Data for Magnetosphere-Ionosphere-Thermosphere Coupling Study at Jupiter Based on Juno's First 30 Orbits and Modeling Tools
<p>Data used in the code associated to the manuscript "Magnetosphere-Ionosphere-Thermosphere Coupling Study at Jupiter Based on Juno’s First 30 Orbits and Modeling Tools", by Al Saati et al. (2022, Journal of Geophysical Research - Space Physics, https://doi.org/10.1029/2022JA030586). Please read the documentation associated with the corresponding code.</p>
Data for, Energetic Electrons near Europa from Juno JEDI data, 10.1029/2023GL105598
<p>Juno/JEDI data are widely available at the PDS. Some data for the figures specific to the paper cited below are included. A formula sheet for deriving the reported quantities in the paper is provided, based on the work of Thomsen and Van Allen. Paranicas, C., et al. (2023), Energetic electrons near Europa from Juno JEDI data, Geophysical Research Letters, 50, e2023GL105598. https://doi.org/10.1029/2023GL105598. </p>
Corresponding Dataset of Advanced Water Vapor Radiometer Data for Juno Gravity Science
<p><br> Corresponding Dataset of Advanced Water Vapor<br> Radiometer Data for Juno Gravity Science<br> Troposphere Calibrations<br> README FILE<br> Dustin Buccino<br> August 24, 2021<br> Jet Propulsion Laboratory<br> California Institute of Technology</p> <p>=============================================================================<br> INTRODUCTION<br> =============================================================================</p> <p> This dataset contains high rate data collected by the Advanced Water<br> Vapor Radiometer (AWVR) at the Deep Space Network's Goldstone Complex in <br> California. This dataset is provided in order to supplement the submitted<br> article to the "Radio Science" journal</p> <p> Buccino, D.R., et al (2021), Performance of Earth Troposphere <br> Calibration Measurements with the Advanced Water Vapor Radiometer <br> for the Juno Gravity Science Investigation, Radio Science, submitted<br> October 2021.</p> <p> ******************************************************************<br> * ANY USERS OF JUNO GRAVITY SCIENCE DATA ARE HIGHLY ENCOURAGED *<br> * TO INSTEAD REFER TO THE OFFICIAL ARCHIVE ON THE NASA PLANETARY *<br> * DATA SYSTEM. THIS SUPPLEMENTAL DATA SET DOES NOT CONTAIN ANY *<br> * GRAVITY SCIENCE DATA; IT ONLY CONTAINS HIGHER RATE AWVR DATA *<br> ******************************************************************</p> <p> Additional Juno Gravity Science Data may be found at the Planetary Data<br> System:</p> <p> Buccino, D. R. (2016). Juno jupiter gravity science raw data set <br> V1.0, JUNO-J-RSS-1 JUGR-V1.0, NASA planetary data system (PDS). <br> Retrieved from https://atmos.nmsu.edu/PDS/data/jnogrv_1001/<br> </p> <p>=============================================================================<br> ARCHIVE INFORMATION<br> =============================================================================</p> <p> This archive contains several data types, located within subdirectories.<br> <br> ROOT<br> `- PJ03/<br> <br> This directory contains all PJ-03 related data, including<br> path delay, path delay rate, calibration values, and frequency<br> residuals.<br> <br> `- PJ06/<br> <br> This directory contains all PJ-06 related data, including<br> path delay, path delay rate, and calibration values.<br> <br> `- PJ08/<br> <br> This directory contains all PJ-08 related data, including<br> path delay, path delay rate, and calibration values.<br> <br> `- ADEV/<br> <br> This directory contains troposphere scintillation Allan deviations<br> from each perijove. Files are named using the start time of the file,<br> in YYYYMMDDHHMM format, where YYYY is the year, MM is the month,<br> DD is the day of month, HH is the hour, and MM is the minute.<br> <br> `- STATS/<br> <br> This directory contains the Juno perijove frequency residual <br> statistics. Only one file is present in this directory.</p> <p>=============================================================================<br> FILE FORMAT<br> =============================================================================</p> <p> This dataset contains two separate file formats as described below.<br> ASCII plain-text files are given with the "*.txt" extension and the<br> comma-separated text files are given with the "*.csv" extension.</p> <p><br> TXT FILES<br> -------------------------------------------------------------------------</p> <p> The ASCII plain-text files are human-readable, space-delimited<br> text files. Each column is defined by a header row which provides<br> a description of each column. Additional comments may be optionally<br> specified by starting a row with the character "#".</p> <p> CSV FILES<br> -------------------------------------------------------------------------</p> <p> The Comma-Separated Value (CSV) files are plain-text files. Values in<br> each data file are separated using a comma ",". Each column is defined <br> by a header row which provides a description of each column.</p> <p><br> =============================================================================<br> FIGURE REPRODUCTION<br> =============================================================================</p> <p> This section will describe the data that are used to produce the figures<br> in the article that describes this dataset.</p> <p> FIGURE 1<br> -------------------------------------------------------------------------</p> <p> Figure 1 is a photograph and is not included in this dataset.</p> <p> FIGURE 2<br> -------------------------------------------------------------------------</p> <p> Figure 2 is produced using files within the "PJ03", "PJ06", and "PJ08"<br> directories.<br> <br> The first row of subfigures are produced by plotting the final three <br> columns of "pjXX_bt_zenith.txt" as a function of time.<br> <br> The second row of subfigures are produced by plotting the path delay<br> componets as a function of time from the "pjXX_pd_awvr.txt" and <br> "pjXX_pd_tsac.txt" data files.</p> <p><br> FIGURE 3<br> -------------------------------------------------------------------------</p> <p> Figure 3 is produced using files within the "PJ03", "PJ06", and "PJ08"<br> directories.<br> <br> The first row of subfigures are produced by plotting the last column<br> of "pjXX_freq_awvr.txt" and "pjXX_freq_tsac.txt".<br> <br> The second row of subfigures are produced by differencing the values.<br> <br> FIGURE 4<br> -------------------------------------------------------------------------</p> <p> Figure 4 is produced using files within the "ADEV" directory.<br> <br> Each individual file within the "ADEV" directory contains the Allan <br> deviation. Each Allan deviation is plotted on a log-log scale and is<br> color-mapped to the calendar date. The file naming convention gives<br> the calendar date of data collection, with the filenames starting with<br> YYYYMMDD, where YYYY is 4-digit year, MM is 2-digit month, and DD is<br> 2-digit day of month in UTC time.</p> <p> FIGURE 5<br> -------------------------------------------------------------------------</p> <p> Figure 5 is produced using files within the "PJ03" directory. The<br> frequency residual from the "pj03_resid_awvr.csv" and<br> "pj03_resid_tsac.csv" is simply plotted as a function of time.<br> <br> FIGURE 6<br> -------------------------------------------------------------------------</p> <p> Figure 6 is produced using files within the "STATS" directory. This <br> directory contains a single file, "AWVR_stats_jul2021_v3.csv" and<br> contains the root-mean-square of the frequency residuals from Juno <br> perijove passes. The root-mean-square of the frequency residuals<br> are plotted using a bar plot and the percent improvement is plotted <br> with a scatterplot.<br> </p> <p>=============================================================================<br> ACKNOWLEDGMENTS<br> =============================================================================</p> <p>This work was carried out at the Jet Propulsion Laboratory, <br> California Institute of Technology, under contract with the National <br> Aeronautics and Space Administration. Government sponsorship acknowledged.</p> <p>=============================================================================<br> PRIMARY POINT OF CONTACT<br> =============================================================================</p> <p>Dustin Buccino<br> Jet Propulsion Laboratory<br> Planetary Radar and Radio Sciences<br> (818) 393 - 1072<br> Dustin.R.Buccino@jpl.nasa.gov</p> <p>=============================================================================<br> ACRONYMS AND ABBREVIATIONS<br> =============================================================================</p> <p> ASCII American Standard Code for Information Interchange<br> DOY Day of year<br> DSN Deep Space Network<br> JPL Jet Propulsion Laboratory<br> NAIF Navigation Ancillary Information Facility<br> NASA National Aeronautics and Space Administration<br> PDS Planetary Data System<br> RS Radio Science<br> RSS Radio Science Subsystem<br> SIS Software Interface Specification<br> TXT Text file<br> UTC Universal Time, Coordinated<br> </p>
Survey and Analysis of Whistler- and Z-mode Emission in the Juno Extended Mission
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics.</p> <p><strong>Key Points:</strong></p> <ul> <li> <p>Whistler mode lower and upper band chorus intensities are surveyed in the extended Juno mission, increasing orbital coverage.</p> </li> <li> <p>Z-mode intensity distributions are re-analyzed with improved plasma density evaluations.</p> </li> <li> <p>Mixed Z-mode, O-mode, and W-mode emission challenges discrete mode identification.</p> </li> </ul> <p><strong>Abstract</strong></p> <p>Whistler mode and Z-mode waves may have significant impact on electron scattering and acceleration at Jupiter as recent stochastic models indicate. New observations of these waves in the Juno extended mission expand the orbital coverage from previous surveys, extending especially to smaller radial distances near the magnetic equator, and to extended ranges of dusk-side magnetic local time. M-shells transiting the Io torus and the orbit of Europa are recognized as a significant source region for whistler mode lower and upper band chorus emission with intensity peaks near 9 R<sub>j</sub>. Ganymede is a significant source of intense whistler mode chorus confined to the local moon environment. New Z-mode observations now extend from a few kHz to over 80 kHz. Inferred source regions for Z-mode are consistent with the outer edge of the Io torus and with auroral field lines that may also support broadband kilometric or decametric emission.</p> <ul> </ul>
Corresponding Dataset for "Measurements of Europa's Ionosphere from Juno's close flyby"
<p> Corresponding Dataset for "Radio Occultation Measurements of Europa's </p><p> Ionosphere from Juno's close flyby"<br> Marzia Parisi<br> September 29, 2023<br> Jet Propulsion Laboratory<br> California Institute of Technology</p><p>=============================================================================<br>INTRODUCTION<br>=============================================================================</p><p> This dataset contains processed radio science data and results of the<br>Juno Europa radio occultation. This dataset is provided in order to <br>supplement the submitted article to the "Geophysical Research Letters"<br>journal:</p><p> Parisi, M. et al. (2023 or 2024), Measurements of Europa's Ionosphere from Juno's close flyby, Geophysical Research <br> Letters, submitted September 2023.</p><p>Please note the raw data used in this analysis are not provided in this<br>supplementary dataset. The raw Juno Gravity Science Data may be found at <br>the Planetary Data System:</p><p> </p><p> Buccino, D. R. (2016). Juno jupiter gravity science raw data set <br> V1.0, JUNO-J-RSS-1 JUGR-V1.0, NASA planetary data system (PDS). <br> Retrieved from https://atmos.nmsu.edu/PDS/data/jnogrv_1001/<br> </p><p>=============================================================================<br>ARCHIVE INFORMATION<br>=============================================================================</p><p> This archive contains two files within the root directory.<br> <br> - JunoE45OccData_Ingress_v1.csv</p><p> This data file contains the INGRESS data relevant to the radio<br> occultation. The data is a timeseries of impact parameter, </p><p> the uncalibrated frequency residuals, the calibrated frequency residuals, </p><p> Total Electron Content, Electron density, 1-sigma electron density uncertainty (thermal only) </p><p> and 1-sigma electron density uncertainty (thermal+trajectory).</p><p> </p><p> - JunoE45OccData_Egress_v1.csv</p><p> This data file contains the EGRESS data relevant to the radio<br> occultation. The data is a timeseries of impact parameter, </p><p> the uncalibrated frequency residuals, the calibrated frequency residuals, </p><p> Total Electron Content, Electron density, 1-sigma electron density uncertainty (thermal only) </p><p> and 1-sigma electron density uncertainty (thermal+trajectory).</p><p> </p><p>=============================================================================<br>FILE FORMAT<br>=============================================================================</p><p> This dataset contains only a comma-separated text files which are<br>given with the "*.csv" extension.</p><p><br> CSV FILES<br> -------------------------------------------------------------------------</p><p> The Comma-Separated Value (CSV) files are plain-text files. Values in<br> each data file are separated using a comma ",". Each column is defined <br> by a header row which provides a description of each column.<br> </p><p>=============================================================================<br>ACKNOWLEDGMENTS<br>=============================================================================</p><p>This work was carried out at the Jet Propulsion Laboratory, <br>California Institute of Technology, under contract with the National <br>Aeronautics and Space Administration. Government sponsorship acknowledged.</p><p>AC, EG, LGC, PT and MZ are grateful to the Italian Space Agency for financial support through</p><p>Agreement No. 2018-25-HH.0 in the context of ESA's JUICE mission, and Agreement</p><p>No. 2017-40-H.1-2020, and its extension 2017-40-H.02020-13-HH.0, for ESA's BepiColombo</p><p>and NASA's Juno radio science experiments. EG is grateful to "Fondazione Cassa dei</p><p>Risparmi di Forl`ı" for financial support of his PhD fellowship. PS was supported by NASA</p><p>Contract NNM06AA75C from the Marshall Space Flight Center under subcontract 699054X</p><p>from Southwest Research Institute. </p><p><br>=============================================================================<br>PRIMARY POINT OF CONTACT<br>=============================================================================</p><p>Marzia Parisi </p><p>Jet Propulsion Laboratory<br>Planetary Radar and Radio Sciences<br>(818) 354 - 0463 </p><p>marzia.parisi@jpl.nasa.gov</p><p>=============================================================================<br>ACRONYMS AND ABBREVIATIONS<br>=============================================================================</p><p> ASCII American Standard Code for Information Interchange<br> DOY Day of year<br> DSN Deep Space Network<br> JPL Jet Propulsion Laboratory<br> NAIF Navigation Ancillary Information Facility<br> NASA National Aeronautics and Space Administration<br> PDS Planetary Data System<br> RS Radio Science<br> RSS Radio Science Subsystem<br> SIS Software Interface Specification<br> TXT Text file<br> UTC Universal Time, Coordinated</p>
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
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DANDI Archive for NWB datasets
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International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.