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The ionospheres of Jupiter's icy moons have been observed by in situ plasma measurements and radio science. However, their spatial structures have not yet been fully characterized. To address this, we developed a new ray tracing method for modeling the radio occultation of the ionospheres using Jovian auroral radio sources. Applying our method to Jovian auroral radio observations with the Galileo spacecraft, we derived the electron density of the ionosphere of Ganymede and Callisto. For Ganymede's ionosphere, we found that the maximum electron density on the surface was 76.5–288.5 cm−3in the open magnetic field line regions and 5.0–20.5 cm−3in the closed magnetic field line region during the Galileo Ganymede 01 flyby. The difference in the electron density distribution was correlated with the accessibility of Jovian magnetospheric plasma to the atmosphere and surface of the moons. These results indicated that electron‐impact ionization of the Ganymede exosphere and sputtering of the surface water ice were effective for the producing Ganymede's ionosphere. For Callisto's ionosphere, we found that the densities were approximately 350 and 12.5 cm−3on the night side hemisphere during Callisto 09 and 30 flybys, respectively. These results combined with previous observations indicated that atmospheric production through sublimation controlled the ionospheric density of Callisto. This method is also applicable to upcoming Jovian radio observation data from the Jupiter Icy Moon Explorer, JUICE. We developed a ray tracing method for Jupiter's icy moon ionospheric occultation of Jovian auroral radio sourcesThe ionospheric density of Ganymede is associated with electron‐impact ionization and atmospheric production via ion sputteringThe Ionospheric density of Callisto is associated with atmospheric production by solar illumination on its surface We developed a ray tracing method for Jupiter's icy moon ionospheric occultation of Jovian auroral radio sources The ionospheric density of Ganymede is associated with electron‐impact ionization and atmospheric production via ion sputtering The Ionospheric density of Callisto is associated with atmospheric production by solar illumination on its surface

The Jovian high‐latitude radio emissions produced by Jupiter's magnetosphere extend from a few kilohertz to 40 MHz. Part of the decametric (DAM) emissions are driven by the Galilean moon Io (Io‐DAM). As UV aurorae have been detected at the footprint of Europa and Ganymede, we expect that these moons drive Jovian radio emissions as well. To check this assumption, we used the ExPRES simulation code (Exoplanetary and Planetary Radio Emissions Simulator) to predict dynamic spectrum (time‐frequency spectograms) of the radio emissions controlled by the four Galilean moons. Then we compared the simulations to the Voyager/PRA and Cassini/RPWS radio observations of Jupiter (1979, and between 2000 and 2003, respectively). We present the first clear evidence for the existence of decametric emissions controlled by Europa and Ganymede. Their statistical analysis allows us to describe the average properties of the Europa‐DAM and Ganymede‐DAM emissions such as their spectrum, temporal variability, and occurrence as a function of moon phase and subobserver's longitude. Detection of Jupiter decametric emissions controlled by Europa and GanymedeAverage properties of the Europa‐DAM emissions (spectral, temporal variability, maximal occurrences, and active longitudes)Average properties of the Ganymede‐DAM emissions (spectral, temporal variability, maximal occurrences, and active longitudes)

We conduct a survey of electrostatic electron cyclotron harmonic (ECH) emissions observed at Saturn by the radio and plasma wave science investigation on board the Cassini spacecraft. These emissions are known to be effective at interacting with electrons in the terrestrial inner magnetosphere, producing electron scattering into the loss cone and acceleration (cf. Horne and Thorne, 2000; Thorne et al., 2010). At Saturn ECH emission occurs with high probability and at strong intensity near the magnetic equator, outside the Enceladus torus in the range ~5 < L < ~10. Inside the inner boundary of the torus, ECH emissions are also observed near the equator and at higher latitude. Intensity levels of ECH emission are comparable to those observed at Earth, higher than Saturn chorus and Z‐mode emission, and are likely to scatter electrons into the loss cone as at Earth. ECH waves are particularly intense and extend to higher harmonics within some plasma injection regions. We present results for a survey of over 8 years of Saturn data for fundamental and up to three harmonics of fce, the electron cyclotron frequency. Saturn ECH wave intensity is binned in L, latitude, and local timeMedian distributions are much more ordered than mean distributionsPlasma injection and anomalous emission regions can have significant ECH wave intensity

The high frequency limit (HFL) of the Saturnian Kilometric Radiation (SKR) can probe the deepest SKR sources, closest to Saturn's ionosphere. In this study, we determined and analyzed the SKR HFL throughout the entire Cassini Saturn orbital tour. The maximum frequency of the northern SKR, whose distribution peaks at ∼625 kHz, is shifted by +100 to +200 kHz from the distribution of southern SKR HFL, consistent with the magnetic field offset toward the northern hemisphere at Saturn. The uniformly observed SKR HFL in the vicinity of Saturn suggests a broad extent and beaming of the SKR source. When the observer is confined to certain locations, the rotational modulation of the SKR HFL is clearly observed. This modulation feature of the SKR HFL is statistically established and analyzed in this study. The modulation of HFL is best observed at mid‐latitudes between 10° and 40° and at almost all local times. We perform a simulation that suggests that the modulation of HFL requires the superposition of a “clock” like and a rotating source behavior. By comparing the derived HFL modulation using different longitudes with variable and fixed rotation periods, we can exclude the existence of a magnetic anomaly that was proposed in a previous study based on the Voyager data. The calculation of the least‐square periodogram confirms that the modulation observed in HFL is similar to the ones previously detected at Saturn. Auroral radio emission from Saturn, namely the Saturn Kilometric Radiation (SKR), is generated along high latitude magnetic field lines via the resonance between energetic electrons and a wave's electric field. The first work on the high frequency limit (HFL) of SKR dates back to 1991. Using data from the Voyager Saturn fly‐by, scientists found an asymmetry when the HFL is organized by the longitude of the Sun. Based on this asymmetry, a hypothesis about the existence of a magnetic anomaly in Saturn's magnetic field was proposed, which was a novel and breakthrough discovery at that time, but the later Cassini measurements did not confirm this magnetic anomaly. Cassini's expedition around Saturn with 13‐yr continuous measurements provided an opportunity to re‐study the HFL of SKR. The long‐term statistics allow us to exclude the magnetic anomaly hypothesis and instead attribute the asymmetry to a modulation which is introduced by an ionospheric/magnetospheric current system at Saturn. A simulation suggests that both temporal and spatial effects play a role to a certain degree. The average frequency and visibility of the HFL are also discussed. These new results provide new insights into the studies of cyclotron maser‐related radio emissions. The high frequency limit (HFL) of Saturn Kilometric Radiation is obtained during the 13‐yr Cassini missionThe average HFL is found to be above and below 600 kHz in the northern and southern hemisphere, respectivelyA rotational modulation of HFL is verified statistically and by simulation, which excludes a magnetic field anomaly The high frequency limit (HFL) of Saturn Kilometric Radiation is obtained during the 13‐yr Cassini mission The average HFL is found to be above and below 600 kHz in the northern and southern hemisphere, respectively A rotational modulation of HFL is verified statistically and by simulation, which excludes a magnetic field anomaly

We study 10 years (1995–2004 inclusive) of auroral kilometric radiation (AKR) radio emission data from the Wind spacecraft to examine the link between AKR and terrestrial substorms. We use substorm lists based on parameters including ground magnetometer signatures and geosynchronous particle injections as a basis for superposed epoch analyses of the AKR data. The results for each list show a similar, clear response of the AKR power around substorm onset. For nearly all event lists, the average response shows that the AKR power begins to increase around 20 min prior to expansion phase onset, as defined by the respective lists. The analysis of the spectral parameters of AKR bursts show that this increase in power is due to an extension of the source region to higher altitudes, which also precedes expansion phase onset by 20 min. Our observations show that the minimum frequency channel that observes AKR at this time, on average, is 60 kHz. AKR visibility is highly sensitive to observing spacecraft location, and the biggest radio response to substorm onset is seen in the 21:00–03:00 hr local time sector. Substorms are an energetic disturbance to the magnetic environment of the Earth. They represent the driving of the terrestrial magnetosphere by particles from the Sun and the subsequent response in various parts of this environment, in both its inner and outer boundaries. These effects are mostly constrained to the nightside of Earth, and can be observed by both ground‐based and remote sensing instruments. In this work, we select auroral kilometric radiation (AKR) observations from 10 years (from 1995 to 2004 inclusive) of radio data from the Wind/WAVES instrument, and compare this with lists of substorm expansion phase onsets that are derived from various observational signatures. After accounting for visibility of the radio sources, we show that the AKR response correlates with the size/strength of the substorm, based on the sensitivity of the list. Our results show that the AKR source region tends to increase in size along magnetic field lines while the emission intensifies, using a longer data set to corroborate previous results. Auroral kilometric radiation (AKR) observations made over 10 years are compared with four event lists of substorm onsets using superposed epoch analysesOn average, AKR power increases and source region extends to higher altitudes in the 20 min prior to onsetThe occurrence of AKR power at higher altitudes is sensitive to the substorm size Auroral kilometric radiation (AKR) observations made over 10 years are compared with four event lists of substorm onsets using superposed epoch analyses On average, AKR power increases and source region extends to higher altitudes in the 20 min prior to onset The occurrence of AKR power at higher altitudes is sensitive to the substorm size

Clear first harmonic emissions of Saturn Kilometric Radiation are discovered during the Cassini Grand Finale orbits. Both ordinary (O) and extraordinary (X) mode fundamental emissions accompanied by X mode harmonics are observed. Analysis shows that the frequency ratio between the fundamental and harmonic emissions is 2.01 ± 0.08, and the harmonic emissions display weaker intensities than the fundamental, by 30–40 dB for the X‐X (fundamental‐harmonic) type harmonic and 10–30 dB for the O‐X type harmonic. The intensity relations between the two types of harmonics, that is, O‐X and X‐X show different patterns that we attribute to different conditions of emission at the source. Direction‐finding results shows that the fundamental and harmonic emissions are plausibly generated in the same source region. In agreement with previous studies at Earth, the generation of the two types of harmonics can be attributed to the cyclotron maser instability operating with different plasma density and electron energy distributions in the source region. Auroral radio emission from Saturn, namely the Saturn Kilometric Radiation (SKR), is generated along high latitude magnetic field lines via the resonance between energetic electrons and wave's electric field. This resonance mechanism is called the cyclotron maser instability. Theoretical and observational studies of the same emission at Earth, called the Auroral Kilometric Radiation (AKR), have shown that the emissions near the harmonic frequency could be generated simultaneously with the fundamental AKR emission. However, no study of SKR harmonic emissions has been reported to date. This paper focuses on searching for the possible harmonic emissions of SKR by using the data measured by the radio experiment onboard the Cassini Spacecraft. Several clear harmonic emissions are found, and their characteristics are analyzed. Based on the circular polarization, two different types of harmonic emissions are identified. We find that the harmonic emissions have a frequency two times that of the fundamental emissions, but a much weaker intensity. The analysis of the source location of simultaneous fundamental and harmonic emissions suggests that they originate from the same source region. These new features of SKR observed in Saturn's magnetosphere provide new insights to the studies of cyclotron maser‐related radio emissions. X mode first harmonics of Saturn Kilometric Radiation (SKR) associated with X/O mode fundamental emissions are identifiedSKR 1st harmonic occurs at frequencies very close to twice the fundamental emissions and, display weaker intensitiesDirection‐finding analysis is consistent with harmonic and fundamental emissions from the same source but affected by large uncertainties X mode first harmonics of Saturn Kilometric Radiation (SKR) associated with X/O mode fundamental emissions are identified SKR 1st harmonic occurs at frequencies very close to twice the fundamental emissions and, display weaker intensities Direction‐finding analysis is consistent with harmonic and fundamental emissions from the same source but affected by large uncertainties

Auroral Kilometric Radiation (AKR) is the strongest terrestrial radio emission, and emanates from the same electron acceleration regions from which particles precipitate into the ionosphere, exciting the aurorae and other phenomena. As such, AKR is a barometer for the state of solar wind ‐ magnetosphere ‐ ionosphere coupling. AKR is anisotropically beamed in a hollow cone from a source region generally found at nightside local times, meaning that a single source region cannot be viewed from all local times in the magnetosphere. In radio data such as dynamic spectra, AKR is frequently observed simultaneously to other radio emissions which can have a similar intensity and frequency range, making it difficult to automatically detect. Building on a previously published pipeline to extract AKR emissions from Wind/WAVES data, in this paper a novel automated AKR burst detection technique is presented and applied to Wind/WAVES data. Over a five year interval, about 5000 AKR bursts are detected with median burst length ranging from about 30 to 60 min. During detected burst windows, higher solar wind velocity is observed, and the interplanetary magnetic field clock angle is observed to tend toward BZ< 0, BY< 0, when compared with the entire statistical interval. Additionally, higher geomagnetic activity is observed during burst windows at polar, high and equatorial latitudes. Auroral Kilometric Radiation (AKR) is a terrestrial radio emission which is excited by the same electrons which enhance the aurorae. Due to a combination of complex beaming, and the statistical position of the source region, an AKR event cannot be observed at all positions in the Earth's magnetosphere. A combination of different radio emissions are simultaneously observed in the radio data, including both AKR and non‐AKR sources. Building on previous work, in this paper individual AKR burst events are automatically detected from Wind/WAVES data over a five year interval. About 5000 events are detected over the interval, during which the observed geomagnetic activity was higher. Higher solar wind velocity and differences in the morphology of the interplanetary magnetic field are also observed during burst windows, both of which are known to excite magnetospheric dynamics. A novel technique has been developed to detect individual Auroral Kilometric Radiation bursts in Wind/WAVES dataWhen the technique is applied to 2000–2004 data, about 5000 bursts are detected with median duration 30–60 minDuring burst windows, higher solar wind velocity, more negative IMF BZand greater geomagnetic activity is observed A novel technique has been developed to detect individual Auroral Kilometric Radiation bursts in Wind/WAVES data When the technique is applied to 2000–2004 data, about 5000 bursts are detected with median duration 30–60 min During burst windows, higher solar wind velocity, more negative IMF BZand greater geomagnetic activity is observed

We investigate the beaming of 11 Io‐Jupiter decametric (Io‐DAM) emissions observed by Juno/Waves, the Nançay Decameter Array, and NenuFAR. Using an up‐to‐date magnetic field model and three methods to position the active Io Flux Tube (IFT), we accurately locate the radiosources and determine their emission angle θfrom the local magnetic field vector. These methods use (a) updated models of the IFT equatorial lead angle, (b) ultraviolet (UV) images of Jupiter's aurorae, and (c) multi‐point radio measurements. The kinetic energy Ee−of source electrons is then inferred from θin the framework of the Cyclotron Maser Instability. The precise position of the active IFT achieved from methods (b and c) can be used to test the effective plasma density of the Io torus. Simultaneous radio/UV observations reveal that multiple Io‐DAM arcs are associated with multiple UV spots and provide the first direct evidence of an Io‐DAM arc associated with a trans‐hemispheric beam UV spot. Multi‐point radio observations probe the Io‐DAM sources at various altitudes, times and hemispheres. Overall, θvaries a function of frequency (altitude), by decreasing from 75°−80° to 70°−75° over 10−40 MHz with slightly larger values in the northern hemisphere, and independently varies as a function of time (or longitude of Io). Its uncertainty of a few degrees is dominated by the error on the longitude of the active IFT. The inferred values of Ee−also vary as a function of altitude and time. For the 11 investigated cases, they range from 3 to 16 keV, with a 6.6 ± 2.7 keV average. The auroral decametric emissions of Jupiter induced by Io (Io‐DAM) are radiated along high latitude magnetic field lines at large aperture angles from the local magnetic field vector, forming a thin hollow cone. In this study, we determine the emission angle θof 11 cases of Io‐DAM emissions observed by Juno/Waves, the Nançay Decameter Array and the NenuFAR radiotelescope with an up‐to‐date magnetic field model and three different methods aimed at minimizing the uncertainty on θ. These methods accurately position the active Io magnetic Flux Tube (IFT) which hosts the decametric radiosources by using (a) models of the active IFT, (b) ultraviolet images of Jupiter's aurorae, and (c) multi‐point radio measurements. most notably, we found that θvaries within 70°–80° as a function of the source altitude along the field line and independently as a function of time. Assuming that the Io‐DAM emissions are driven by the Cyclotron Maser Instability from energetic electrons, we infer from the measured θthe kinetic energy Ee−of the source electrons accelerated by the Io‐Jupiter interaction. The obtained values of Ee−also depend on altitude and time and vary between 3 and 16 keV, with a ∼6.5 keV average, in agreement with Juno in situ measurements. We derive the Io‐decametric emission angle θfrom Juno, Nançay Decameter Array, and NenuFAR data using 3 methods to locate the radio sourcesθ(f) decreases from 75°−80° to 70°−75° over 10–40 MHz and varies both as a function of frequency (or altitude) and time (or longitude of Io)The inferred electron energies amplifying Io‐decametric waves range from 3 to 16 keV also vary as a function of altitude and time We derive the Io‐decametric emission angle θfrom Juno, Nançay Decameter Array, and NenuFAR data using 3 methods to locate the radio sources θ(f) decreases from 75°−80° to 70°−75° over 10–40 MHz and varies both as a function of frequency (or altitude) and time (or longitude of Io) The inferred electron energies amplifying Io‐decametric waves range from 3 to 16 keV also vary as a function of altitude and time

Heliophysics data analysis often involves combining diverse science measurements, many of them captured as time series. Although there are now only a few commonly used data file formats, the diversity in mechanisms for automated access to and aggregation of such data holdings can make analysis that requires intercomparison of data from multiple data providers difficult. The Heliophysics Application Programmer's Interface (HAPI) is a recently developed standard for accessing distributed time series data to increase interoperability. The HAPI specification is based on the common elements of existing data services, and it standardizes the two main parts of a data service: the request interface and the response data structures. The interface is based on the REpresentational State Transfer (REST) or RESTful architecture style, and the HAPI specification defines five required REST endpoints. Data are returned via a streaming format that hides file boundaries; the metadata is detailed enough for the content to be scientifically useful, e.g., plotted with appropriate axes layout, units, and labels. Multiple mature HAPI‐related open‐source projects offer server‐side implementation tools and client‐side libraries for reading HAPI data in multiple languages (IDL, Java, MATLAB, and Python). Multiple data providers in the US and Europe have added HAPI access alongside their existing interfaces. Based on this experience, data can be served via HAPI with little or no information loss compared to similar existing web interfaces. Finally, HAPI has been recommended as a COSPAR standard for time series data delivery. The Heliophysics Application Programmer's Interface (HAPI) specification allows data providers to use a standard set of conventions for returning data in response to a URL‐based request. This specification was developed because no standard exists. Data providers use incompatible conventions so that automated access to and aggregation of data requires users to write custom code for each data provider. The benefit to the user is that software libraries for many common languages have been developed to read HAPI data; if a data provider serves data using the HAPI specification, the user does not need to write additional code to access the data. The starting point for using and learning more about HAPI is http://hapi-server.org/. HAPI was developed because there are many nonstandard approaches to serving Heliophysics time series dataHAPI provides a standard specification that will simplify data accessSoftware libraries for downloading data from HAPI servers in many commonly used programming languages are available HAPI was developed because there are many nonstandard approaches to serving Heliophysics time series data HAPI provides a standard specification that will simplify data access Software libraries for downloading data from HAPI servers in many commonly used programming languages are available

Auroral Kilometric Radiation (AKR) is terrestrial radio emission that originates in particle acceleration regions along magnetic field lines, coinciding with discrete auroral arcs. AKR viewing geometry is complex due to the confinement of the source regions to nightside local times (LTs) and the anisotropy of the beaming pattern, so observations are highly dependent on spacecraft viewing position. We present a novel, empirical technique that selects AKR emission from observations made with the spin‐axis aligned antenna of the Wind/WAVES instrument, based on the rapidly varying amplitude of AKR across spacecraft spin timescales. We apply the technique to Wind/WAVES data during 1999 day of year 227–257, when the Cassini spacecraft flew past Earth and provided an opportunity to observe AKR from two remote locations. We examine the AKR flux and power, with observations made from LTs of 1700–0300 hr having an average power up to 104Wsr‐1larger than those on the dayside and an increasing AKR power observed at higher magnetic latitudes. We perform a linear cross‐correlation between the Wind AKR power and the spacecraft magnetic latitude, showing positive then negative correlation as Wind travels from the Northern to Southern magnetic hemisphere. Statistically significant diurnal modulations are found in the whole 30‐day period and in subsets of the data covering different local time sectors, indicative of a predominantly geometrical effect for remote AKR viewing. The reproduction of well‐known features of the AKR verifies the empirical selection and shows the promise of its application to Wind/WAVES observations. Auroral Kilometric Radiation (AKR) is naturally occurring radio emission from the Earth's Northern and Southern polar regions, which becomes more intense as the aurora brightens. In this work, we examine data from the Wind spacecraft WAVES instrument from a 30‐ day interval in 1999 when a second spacecraft, Cassini, was also flying near Earth and measuring the AKR from a different viewpoint. In this work, we select the AKR using an empirical measure of the variability observed by the WAVES instrument, and compare the distribution and time profile of AKR intensity. Comparing measurements of this radio emission from different spacecraft positions help us to understand how the AKR is best viewed and illustrate the constrained beaming of the emission. This information is important for anyone wanting to attempt to interpret measurements of the AKR. Novel, empirically based method to extract Auroral Kilometric Radiation (AKR) from Wind/WAVES is presented and applied to observations made during the Cassini flybySelected data show a distribution of AKR power with expected longitudinal and latitudinal visibility constraintsDiurnal temporal modulation observed, suggesting the dominance of a geometric viewing effect and agreeing with previous AKR observations Novel, empirically based method to extract Auroral Kilometric Radiation (AKR) from Wind/WAVES is presented and applied to observations made during the Cassini flyby Selected data show a distribution of AKR power with expected longitudinal and latitudinal visibility constraints Diurnal temporal modulation observed, suggesting the dominance of a geometric viewing effect and agreeing with previous AKR observations

Reanalyzing Cassini radio observations performed during Jupiter's flyby of 2000–2001, we study the internal (rotational) versus external (solar wind) control of Jupiter's radio emissions, from kilometer to decameter wavelengths, and the relations between the different auroral radio components. For that purpose, we build a database of the occurrence of Jovian auroral radio components bKOM, HOM, and DAM observed by Cassini, and then frequency‐longitude stacked plots of the polarized intensity of these radio components. Comparing the results obtained inbound and outbound, as a function of the Observer's or Sun's longitude, we find that HOM & DAM are dominantly rotation‐modulated (i.e., emitted from searchlight‐like sources fixed in Jovian longitude), whereas bKOM is modulated more strongly by the solar wind than by the rotation (i.e., emitted from sources more active within a given Local Time sector). We propose a simple analytical description of these internal and external modulations and evaluate its main parameters (the amplitude of each control) for HOM + DAM and bKOM. Comparing Cassini and Nançay Decameter Array data, we find that HOM is primarily connected to the decameter emissions originating from the dusk sector of the Jovian magnetosphere. HOM and DAM components form a complex but stable pattern in the frequency‐longitude plane. HOM also seems to be related to the “lesser arcs” identified by Voyager. bKOM consists of a main part above ∼40 kHz in antiphase with HOM occurrence, and detached patches below ∼80 kHz in phase with HOM. The frequency‐longitude patterns formed by DAM, HOM and bKOM remain to be modeled. We build synthetic frequency‐longitude maps of polarized Jovian auroral radio emissions, DAM, HOM, and bKOMJovian HOM and DAM are dominantly rotation‐modulated, bKOM dominantly solar wind‐modulatedHOM appears primarily connected to decameter sources from the dusk side of the Jovian magnetosphere We build synthetic frequency‐longitude maps of polarized Jovian auroral radio emissions, DAM, HOM, and bKOM Jovian HOM and DAM are dominantly rotation‐modulated, bKOM dominantly solar wind‐modulated HOM appears primarily connected to decameter sources from the dusk side of the Jovian magnetosphere

The observations from the Juno spacecraft in polar orbit of Jupiter provide for the first time a complete view of Jupiter's radio emissions from all latitudes. Characterizing the latitudinal distribution of radio emissions' occurrence and intensity is a useful step for elucidating their origin. Here, we analyze for that purpose the first 3 years of observations from the Waves experiment on the Juno spacecraft (mid‐2016 to mid‐2019). Two prerequisites for the construction of the latitudinal distribution of intensities for each Jovian radio component are (a) to work with absolute flux densities and (b) to be able to associate each radio measurement with a specific radio component. Accordingly, we develop a method to convert the Juno/Waves data in flux densities and then we build a catalog of all Jovian radio components over the first 3 years of Juno's orbital mission. From these, we derive occurrence and intensity distributions versus observer's latitude and frequency for each component; these will be the basis for future detailed studies and interpretations of each component's characteristics and origin. We build a processing pipeline of Juno/Waves data that include conversion to absolute flux densitiesWe build a catalog of all Jovian radio components over the first 3 years of Juno's orbital missionWe derive occurrence and intensity distributions versus observer's latitude and frequency for each component We build a processing pipeline of Juno/Waves data that include conversion to absolute flux densities We build a catalog of all Jovian radio components over the first 3 years of Juno's orbital mission We derive occurrence and intensity distributions versus observer's latitude and frequency for each component