![[LEFT] Diagram of a pixel component from a microbolometer array showing the absorbing surface, electrically conducting bridge connecting the absorber to the readout electronics, and the mirrored surface below the absorber. [RIGHT] A digital render of the Enceladus Thermal Mapper instrument. The arrow shows the location of the filter assembly. -- [astro-ph.IM]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/Tailoring.png?resize=1200%2C606&ssl=1)
[astro-ph.IM]. We present the results of an initial study into the feasibility and design of the Enceladus Thermal Mapper (ETM) instrument, designed to provide detailed temperature data for Enceladus, an […]
Cassini
Posted inTitan
Detection Of Hydrocarbons In Titan Using High-resolution Cross-correlation Spectroscopy
[astro-ph.EP]. High-resolution cross-correlation spectroscopy (HRCCS) is a powerful technique for detecting molecules whose individual spectral lines are too weak to be identified directly, but its sensitivity is limited by the […]
![Longitude–height structure of the rotational component of the stationary s = 1 zonal wind anomaly, near the Huygens latitude band during Ls = 290◦–310◦ -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/Topographically.png?resize=1200%2C719&ssl=1)
Posted inTitan
Topographically Forced Stationary Waves Can Explain The Near-Surface Zonal Winds Observed By Huygens On Titan
[astro-ph.EP] Titan’s equatorial superrotation is associated with climatological retrograde (westward) near-surface winds at low latitudes, as consistently simulated by Titan general circulation models.
![A heterotrophic ecosystem enabled by fermentation on Enceladus. [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/Fermentation.png?resize=1200%2C720&ssl=1)
Posted inEnceladus
Fermentation Heterotrophy Can Reproduce Enceladus’s H2 And CH4 Under Limited Serpentinization
[astro-ph.EP] Saturn’s icy moon Enceladus is a prime target in the search for life beyond Earth. Abundant H2 and CH4 in Enceladus’s south-polar plume have been shown to be consistent […]
Posted inEnceladus
How Enceladus’ Ocean Spray Becomes Chemically Diverse Ice Grains
[Institute of Science Tokyo] Saturn’s icy moon Enceladus hides a global ocean beneath its frozen surface. From fractures near its south pole, material from this ocean is ejected into space […]
Posted inEnceladus
Enceladus Offers Clues In The Search For Extraterrestrial Life
[Free University Berlin] With a global ocean of liquid water below a thick crust of ice, Saturn’s moon Enceladus is one of the most promising places to search for life […]
Posted inTitan
Experimental Measurements of Benzene Ice Critical Saturation Ratios on Titan Tholins and Impact on the Microphysical Modeling of Titan’s South Polar Benzene Cloud
[The Planetary Science Journal] The Cassini Composite Infrared Spectrometer revealed the presence of a benzene (C6H6) ice cloud in Titan’s autumn south polar stratosphere following the northern spring equinox in […]
![Schematic diagram (not to scale) of the experimental apparatus used for benzene ice nucleation and growth studies (adapted from Dubois et al. (2021)). Pressure was measured with a capacitance manometer (P1) and an ion gauge (P2). The inset shows a top view of the cooled sample holder with the positions of the three K-type thermocouple gauges (red dots) used for temperature measurements. The ice sample formed on either or both sides of the silicon substrate/tholin sample (grey), which was in the path of the IR beam of the Thermo Fisher iS50. Infrared transmission spectra were collected with a liquid N2-cooled MCT/A detector. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/Experimental-Measurements.png?resize=1200%2C717&ssl=1)
Posted inTitan
Experimental Measurements of Benzene Ice Critical Saturation Ratios on Titan Tholins and Impact on the Microphysical Modeling of Titan’s South Polar Benzene Cloud
[astro-ph.EP] The Cassini Composite Infrared Spectrometer (CIRS) revealed the presence of a benzene (C6H6) ice cloud in Titan’s autumn south polar stratosphere, following the northern spring equinox in August 2009.
![Retrieved temperature, mixing ratios, and haze parameters from all three retrieval set ups. Left: Retrieved volume mixing ratios for all three retrieval cases shown at the approximate depth of the haze layer. Right: Haze opacity in dashed lines and temperature in solid lines as a function of pressure and altitude. Where available we show the Teanby et al. (2006) mixing ratios and temperature profile. Despite varying assumptions and haze schemes, all retrievals indicate a haze layer in approximately the same pressure location. Note that the POSEIDON haze location is inferred from the pressure contribution functions and is shown as a shaded region. - [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/Piercing-through.png?resize=1200%2C710&ssl=1)
Posted inExoplanets, -moons, -comets
Piercing Through The Haze: Characterizing Titan-like Terrestrial Exoplanets With JWST
[astro-ph.EP] As we enter a new era of using JWST to characterize exoplanet atmospheres, a top priority is defining observational needs and parameters in the search for life on an […]
Posted inAstrochemistry, Astrogeology, Biogeochemical Cycles & Geobiology, Biosignatures & Paleobiology, Enceladus, Habitable Zones, Icy Worlds, Status Report
Tidal Rock Grinding As A Source Of H2 On Enceladus
The Solar System hosts multiple potentially habitable environments, including the subsurface ocean beneath the icy crust of Saturn’s moon Enceladus.