Join us September 16 from 3-5 PM ET on Webex for the 2024 Planetary Science Early Career Award Showcase, featuring talks from selected investigators from ROSES-2024. Speakers will highlight projects […]
astronomy
![RMS vs bin-size of the residuals from our TTV fits (see Section 4.1). The four panels show the 2x2 different reduction-likelihood pairings considered in this work. The two jitter treatments find binning behavior worse than that expected from pure Gaussian noise (dashed line), and instead have a slope of ∼ − 1/3, similar to other NIRSpec PRISM results (e.g. Kipping et al. 2025). The inclusion of a GP to absorb time-correlated noise greatly reduces the slopes, as again expected.-- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/09/JWST-Excludes.png?resize=1200%2C720&ssl=1)
Posted inExoplanets, -moons, -comets
JWST Excludes Exomoons Down to 0.1 Earth Radii Around a Rocky, Temperate Exoplanet
[astro-ph.EP] To date, even with JWST, it has not been possible to test for exomoons as small as the Moon. Only two reported searches for exomoons around bound planets have […]
Posted inExoplanets, -moons, -comets
The Metallicity Of Giant Exoplanets Around Low-mass Stars And How Ariel Can Help
[astro-ph.EP] Giant planets orbiting low-mass stars represent a unique population of giant planets that can be studied to constrain planet formation theory. Surveys of transiting giant exoplanets around M-dwarfs (GEMS) […]
![Zoomed-in 12CO J = 3 − 2 channel maps. Contours are 3, 6 and 10σ. The isovelocity contours are calculated with a flat surface. The planet locations are marked with white dots. The beam is given in the bottom right corner while the velocity of the channel is provided in the bottom left corner. Fig. F.5 shows the channel maps over the full extent of the disk.-- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/09/Mapping.png?resize=1200%2C717&ssl=1)
Posted inExoplanets, -moons, -comets
Mapping the WISPIT2 Planet-Hosting Cavity at Sub-Hill-Radius scales
[astro-ph.EP] We present new deep, very high angular resolution observations of the sub-mm continuum (19×13 mas) and 12CO (67×52 mas) emission from the disk surrounding the planet host WISPIT2. Our […]
Posted inSETI & Technosignatures
Identifying Casual SETI Transmissions And Ultra-Faint RFI With Cumulant Imaging
[astro-ph.IM] Techniques for identifying radio beacons transmitted by extra-terrestrial civilizations are well advanced.
Posted inUncategorized
Multi-Wavelength Post-Perihelion Polarimetry of Interstellar Comet 3I/ATLAS
[astro-ph.EP] We present new post-perihelion polarimetric observations of the third discovered interstellar object, 3I/ATLAS (C/2025 N1; hereafter 3I), obtained using FORS2 at the Very Large Telescope, ALFOSC at the Nordic […]
![Planets that will be observed with MIRI in transit, in JWST Cycles 1-5. As mentioned in section 5, we see a wide variety of planet sizes and equilibrium temperatures. The currently published planets are shown in black dots, and listed in Table 1 and Figure 1. We have ommitted the white dwarf planet WD 1856 b (Teq = 160K, Rp = 10.2R⊕, cycle 4), as well as the disintergrating planets K2-22 b (see section 2.1) and BD+05 4868 A b (Teq = 1820K, unknown Rp, cycle 4). -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/09/A-Homogeneous.png?resize=1200%2C720&ssl=1)
Posted inExoplanets, -moons, -comets
A Homogeneous Survey Of JWST MIRI Transmission Spectra Of 10 Exoplanets
[astro-ph.EP] The launch of JWST has enabled unprecedented atmospheric characterization of exoplanets. In particular, the JWST-MIRI instrument in the mid-infrared enables probing of molecular species that are harder to detect […]
![The separation of β Pictoris b and β Pictoris c from the star in terms of their Hill sphere. β Pictoris b has a longer orbital period (∼20 yr), with a Hill sphere primary transit at MJD ∼58000 and a Hill sphere radius of 1.1 au. β Pictoris c has a shorter orbital period (∼3.3 yr), with two primary transits at MJD 58195+11 −20 and 59415+8 −8 and a secondary transit at 58707+3 −7 . The § Hill sphere radius is approximately 0.3 au. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/09/The-Hill.png?resize=1200%2C712&ssl=1)
Posted inBeta Pictoris
The Hill Sphere Transits of Beta Pictoris c and The Search for Another 1981-like Event
[astro-ph.EP]. Beta Pictoris is a young and nearby planetary system hosting an edge-on debris disk and at least three gas-giant planets. Their circumplanetary environments could host exomoons and rings, a […]
![Schematic of the flow-map encoder–operator–decoder architecture used to emulate chemical kinetics. The encoder maps the current normalized input state (and global parameters) to a latent space. The latent dynamics operator evolves this latent state using the time step and global parameters, and the decoder reconstructs the predicted future normalized species state. Optional residual connections can be applied in latent space and/or on the normalized model outputs.-- astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/09/Accelerating.png?resize=1200%2C718&ssl=1)
Posted inExoplanets, -moons, -comets
Accelerating Chemical Kinetics For Exoplanet Atmospheres Using Neural Networks
[astro-ph.EP] Observations increasingly reveal the coupled radiative, chemical, and dynamical processes that shape exoplanet atmospheres. Interpreting these atmospheres requires models that can capture this complexity.
![Sky maps with locations of star clusters with exoplanets and candidate objects. The upper graph is centred on the Galactic centre, while the lower one is centred on the Galactic Anticenter.-- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/09/Exoplanets-in.png?resize=1200%2C719&ssl=1)
Posted inExoplanets, -moons, -comets
Exoplanets In Star Clusters
[astro-ph.EP] The field of exoplanetary research is rapidly evolving, thanks to TESS and Kepler/K2. With the latest data release, Gaia DR3, Gaia has transformed the study of star clusters.