S. Rodríguez
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View article: Zonal winds in Titan's middle atmosphere from a stellar occultation observed with Keck adaptive optics
Zonal winds in Titan's middle atmosphere from a stellar occultation observed with Keck adaptive optics Open
We present spatially resolved Keck/NIRC2 images of a stellar occultation by Titan on September 5, 2022 and compare them to predictions from concurrent ALMA observations and a suite of General Circulation Model (GCM) simulations. ALMA data …
View article: 3D Monte Carlo Radiative Transfer for Parameter Retrieval in Planetary Atmospheres
3D Monte Carlo Radiative Transfer for Parameter Retrieval in Planetary Atmospheres Open
Retrieving planetary atmospheric parameters from observational data is particularly challenging under large observation angles, in thick and highly scattering media (such as Titan and Venus), and in the presence of horizontal heterogeneiti…
View article: A new description of Titan’s aerosol optical properties from the analysis of VIMS Emission Phase Function observations
A new description of Titan’s aerosol optical properties from the analysis of VIMS Emission Phase Function observations Open
Introduction: The Huygens probe gave unprecedented information on the properties of Titan’s aerosols (vertical distribution, opacity as a function of wavelength, phase function, single scattering albedo) by in-situ measurements [1]. Being …
View article: Enceladus surface properties using Cassini/VIMS hyperspectral data
Enceladus surface properties using Cassini/VIMS hyperspectral data Open
Enceladus is one of the most intriguing icy moons of the solar system, exhibiting active cryovolcanism and continuous plume activity at its south pole [1]. The surface in this region is geologically young and frequently resurfaced by plume…
View article: Super-resolution maps of icy moons: Application to the Cassini-VIMS observations of Enceladus
Super-resolution maps of icy moons: Application to the Cassini-VIMS observations of Enceladus Open
The icy moons of the outer solar system (Ganymede, Enceladus, Titan, etc.) have been found in the forefront of planetary exploration, due to their diverse geomorphology coupled with numerous discoveries hinting to possible habitable condit…
View article: Preparing Dragonfly to Titan: Detection of Body Waves to Constrain Ice Shell Thickness
Preparing Dragonfly to Titan: Detection of Body Waves to Constrain Ice Shell Thickness Open
The NASA Dragonfly mission, selected in 2019 as the 4th mission of the New Frontiers mission program, is set to explore Saturn's largest moon, Titan, in the mid-2030s [1]. Titan remains a prime target for astrobiological research due to it…
View article: Inferring Discharge From River Geometry on Titan
Inferring Discharge From River Geometry on Titan Open
Titan's dense atmosphere, composed mainly of methane and nitrogen, maintains a methane cycle that shapes its surface. Like water on Earth, methane precipitation erodes Titan's surface, carving river networks at all latitudes, as revealed b…
View article: Calibration of MAJIS (Moons And Jupiter Imaging Spectrometer). I. On-ground setup description and characterization
Calibration of MAJIS (Moons And Jupiter Imaging Spectrometer). I. On-ground setup description and characterization Open
The visible and infrared Moon And Jupiter Imaging Spectrometer (MAJIS), aboard the JUpiter ICy Moons Explorer (JUICE) spacecraft, will characterize the composition of the surfaces and atmospheres of the Jupiter system. Prior to the launch,…
View article: Synthetic topography, roughness, albedo, and thermal inertia maps for mesoscale modeling on Titan
Synthetic topography, roughness, albedo, and thermal inertia maps for mesoscale modeling on Titan Open
Titan’s climate includes dynamic processes at multiple scales, ranging from local turbulence to global super-rotation. Several mesoscale models are currently being developed which will permit simulations of surface winds at kilometri…
View article: Evolution of Titan’s labyrinths through chemical erosion and hillslope transport
Evolution of Titan’s labyrinths through chemical erosion and hillslope transport Open
Introduction: First seen in the T39 Cassini RADAR SAR data in 2007, the high latitude labyrinth terrain on Titan consists in complex valleys that range from polygonal to linear features with morphological similarities with terrestrial kars…
View article: Titan’s Atmosphere in Late Northern Summer from JWST and Keck Observations
Titan’s Atmosphere in Late Northern Summer from JWST and Keck Observations Open
Saturn’s moon Titan is the only moon in the solar system with a dense atmosphere, composed largely of nitrogen (94.5–98.6%) and methane (5.5–1.4%). Due to the cold troposphere and surface (70–93 K) close to the trip…
View article: Eolian landforms and processes on Titan and role in material movement 
Eolian landforms and processes on Titan and role in material movement  Open
The surface of Titan is composed of varied geomorphic units indicative of a vivid depositional, erosional and tectonic history. Dominant at Titan's equatorial regions are vast eolian landscapes of dunes, sand sheets, yardangs and wind stre…
View article: Titan haze and mist layers observed by Nirpsec/JWST and comparison with inversions from VIMS/Cassini and Planetary Climate Model of Titan.
Titan haze and mist layers observed by Nirpsec/JWST and comparison with inversions from VIMS/Cassini and Planetary Climate Model of Titan. Open
 The photochemical haze layer in the stratosphere above about 80 km and the condensation haze (hereafter, mist) in the lower stratosphere and troposphere completely cover Titan and play a dominant role in its climate. These hazes dete…
View article: A spherical and heterogeneous radiative transfer code for near-infrared remote sensing: application to Titan
A spherical and heterogeneous radiative transfer code for near-infrared remote sensing: application to Titan Open
The Cassini mission has gathered extensive near-infrared spectra and imagery of Titan, which pose challenges for analysis due to the significant scattering effects of its atmosphere with potential heterogeneous radiative properties. Tradit…
View article: Monitoring the performances of MAJIS from ground to flight calibration measurements
Monitoring the performances of MAJIS from ground to flight calibration measurements Open
 ESA’s Jupiter Icy Moons Explorer (JUICE) mission scientific payload includes a 2-channels (visible to near-infrared (VISNIR) and infrared (IR)) cryogenic imaging spectrometer instrument called the Moons And Jupiter Imaging Spec…
View article: Titan in Late Northern Summer from JWST and Keck Observations
Titan in Late Northern Summer from JWST and Keck Observations Open
Titan is an object of fascination for scientists researching the solar system, as a ‘terrestrial-like’ world with active meteorology and fluvial and lacustrine formations based on methane chemistry and condensation. The Cassini…
View article: Calibration of MAJIS (Moons And Jupiter Imaging Spectrometer). III. Spectral calibration
Calibration of MAJIS (Moons And Jupiter Imaging Spectrometer). III. Spectral calibration Open
The Moons And Jupiter Imaging Spectrometer (MAJIS) is the visible and near-infrared imaging spectrometer onboard the European Space Agency (ESA)’s Jupiter Icy Moons Explorer mission. Before its integration into the spacecraft, the instrume…
View article: Description of Martian Convective Vortices Observed by InSight and Implications for Vertical Vortex Structure and Subsurface Physical Properties
Description of Martian Convective Vortices Observed by InSight and Implications for Vertical Vortex Structure and Subsurface Physical Properties Open
Convective vortices (whirlwinds) and dust devils (dust‐loaded vortices) are one of the most common phenomena on Mars. They reflect the local thermodynamical structure of the atmosphere and are the driving force of the dust cycle. Additiona…
View article: Systematic catalog of Martian convective vortices observed by InSight
Systematic catalog of Martian convective vortices observed by InSight Open
Convective vortices (whirlwinds) and dust devils (dust-loaded vortices) are one of the most common phenomena on Mars, observable on a daily basis. They reflect the local thermodynamical structure of the atmosphere and are the driving force…
View article: Discussion on seismically triggered avalanches on Mars after the s1222a Marsquake
Discussion on seismically triggered avalanches on Mars after the s1222a Marsquake Open
Potential dust avalanches as aftermaths of the seismic event of S1222a detected by the SEIS/InSight seismometer are investigated. Orbital observations emphasize that the area around the estimated location shows rather flat topography with …
View article: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area Open
We present an analysis of Titan data acquired by the Cassini Visual and Infrared Mapping Spectrometer (VIMS) at the landing site of the Dragonfly mission, using a new version of our radiative transfer model for Titan, with significant upda…