![Assuming the presence of two companions, the orbital evolution of the HD 216595 system for 500 years from the best-fit orbit: (a) orbits of the system, (b) the evolution of the semi-major axes, and (c) the evolution of the eccentricities. Blue color indicates the inner companion and black color is the outer companion. -- [astro-ph.SR]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/A-Search-for.png?resize=1200%2C652&ssl=1)
[astro-ph.SR] Detecting planetary companions around evolved stars, particularly asymptotic giant branch (AGB) stars, is challenging due to intrinsic stellar variability such as surface convection, pulsations, and mass loss, which can […]
Astronomy & Telescopes
![Simulated light curve for a periodic laser beacon at fpulse = 413 Hz at d = 15 pc observed with a Dtel = 1 m telescope at a cadence of 10 µs. The upper panels show a short segment of the noiseless pulse signal (left) and the corresponding signal including the estimated noise contributions (right). The bottom panel shows the integrated folded pulse profile after combining 108 pulses, resulting in an expected SNR of approximately 5.99. -- [astro-ph.IM]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/The-Interstellar-Laser.png?resize=1200%2C716&ssl=1)
Posted inSETI & Technosignatures
The Interstellar Laser Beacons Hypothesis and the Cosmic Lighthouses Project
[astro-ph.IM] In this paper, we argue that in a realistic, resource-limited scenario senders whose intent is to maximize successful communication at the lowest cost will utilize very long-lived, pulsed beacons.
![DFT-computed anharmonic absorption spectra of 1-cyanonaphthalene in its neutral (1-CNN0 , top panel), cation (1-CNN+ , middle panel), and anion (1-CNN− , bottom panel) charge states. The calculated vibrational transitions are convolved with a Lorentzian profile using a FWHM of 4 cm−1 to simulate realistic spectral profiles. Numerical labels near the major peaks represent their respective wavelengths. Key vibrational bands, including the CN stretch at ∼ 4.4–4.6 µm and the CH stretch at ∼ 3.2–3.3 µm, are explicitly highlighted.-- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/Anharmonic-Infrared-Emission.png?resize=1200%2C718&ssl=1)
Posted inAstrochemistry
Anharmonic Infrared Emission Of Cyano-Substituted Polycyclic Aromatic Hydrocarbon Molecules: Cyanonaphthalenes As A Case Study
[astro-ph.GA] Recent detections of cyano-substituted polycyclic aromatic hydrocarbons (cyano-PAHs) highlight them as key tracers of nitrogen heterocycles in the interstellar medium (ISM).
Posted inExoplanets, -moons, -comets
New Exomoon Detection Challenges Cosmic Labels
[ESO] Observations made with the European Southern Observatory’s Very Large Telescope (ESO’s VLT) have revealed evidence for a moon-like object in the CD-35 2722 system. Unlike moons in our Solar […]
Posted inAstronomy & Telescopes, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Mapping, Geodesy, Cartography, Bathymetry
Mapping Alien Continents: Achieving Optical VLBI For Exoplanet Imaging
[NIAC / NASA] The scientific goal of the proposed work will be reconstructing the image, i.e. resolving surface features, of an Earth-like exoplanet around a nearby star as seen in […]
![Conservative CW mitigation demonstrated on a fully synthetic wideband radio dataset with realistic detector features. (a) Frequency spectrum before and after mitigation. Red shaded regions indicate the three cataloged anthropogenic CW tones at 137, 405, and 450 MHz (representing satellite downlinks, weather balloon telemetry, and South Pole station communications, respectively). These tones are removed via least-squares time-domain sine subtraction as described in the text. The orange dotted line marks an uncataloged narrowband feature at 285 MHz that is successfully preserved. (b) Time domain trace of the same waveform shown in panel (a), zoomed in to show the effect of mitigation around an injected nanosecond-scale broadband transient (dashed black line). The raw simulated trace before mitigation (light red line) is heavily obscured by CW interference. After subtraction of the cataloged tones, the mitigated trace (solid green line) shows significantly reduced coherent CW contamination, successfully recovering the underlying broadband impulsive signal and preserving both its original shape and temporal structure. -- [astro-ph.IM]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/Methodological-Synergies.png?resize=1200%2C720&ssl=1)
Posted inSETI & Technosignatures
Methodological Synergies Between Technosignature And UHE Neutrino Searches
[astro-ph.IM] Radio technosignature searches and radio-based ultra-high energy (UHE) neutrino experiments address different scientific questions, but share a closely related data analysis problem: identifying rare signals of unknown morphology within […]
![Semimajor axis distribution of captured ISOs in three simulations, each with stellar mass M⋆ = 0.7 M⊙ and impact parameter b = 3000 au, but with velocity at infinity v∞ = 1, 3, and 10 km/s. -- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/interstellar.png?resize=1200%2C717&ssl=1)
Posted inInterstellar
Interstellar Objects During Stellar Encounters
[astro-ph.EP] As they orbit within the Galaxy, stars swim through a vast population of interstellar objects (ISOs).
Posted inBiosignatures & Paleobiology
Substrate-Agnostic 3x: Biosignatures, Technosignatures, Ecologies
[physics.gen-ph] Substrate-agnostic perspectives are currently attracting increased attention. For example, it has become customary to refer to agnostic biosignatures to reflect the range of alternative extraterrestrial biospheres and to account […]
![Gas-phase abundance evolution of CH3OH, CH3CHO, CH3OCHO, and CH3OCH3 in the representative warm-up model with Tmax = 200 K. The shaded rectangles indicate the observed abundance ranges derived in this work. The gray vertical band marks the time interval, (1.25–1.42) × 106 yr, over which the model abundances overlap most closely with the observed ranges for the four species. -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/Molecule-dependent.png?resize=1200%2C720&ssl=1)
Posted inAstrochemistry
Molecule-dependent Abundance Behavior of Oxygen-bearing Complex Organics in High-Mass Star-Forming Regions: A Uniform 50-source Survey
[astro-ph.GA] We present a uniform IRAM-30m survey analysis of four oxygen-bearing complex organic molecules (COMs), methanol (CH3OH), acetaldehyde (CH3CHO), methyl formate (CH3OCHO), and dimethyl ether (CH3OCH3), toward 50 high-mass star-forming […]
![(Left) The aperture assumed in these simulations. Furthermore, the stellar radius is assumed to be 0.03 λ/D, and the planet is assumed to be at 1 λ/D in the positive X direction. Middle) The single-moded measurement shown in the pupil plane (top) and focal plane (bottom) obtained by using the highest information mode from the calculation of the SLD, denoted here as SLD Mode 0. Right) The single-moded measurement shown in the pupil and focal planes as calculated using a classical numerical optimization. Pupil plane extents are from -0.5 to 0.5 (with an aperture diameter normalized to 1), while focal plane extents are from -5 λ/D to 5λ/D. Both of these methods are described in Ref. 13, and achieve ηs ≈ 1 × 10−9 , with ηp at 1 λ/D of approximately 19%, and a maximum ηp of 73% at 1.8 λ/D. -- [astro-ph.IM]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/07/Optimal-mode-sorting.png?resize=1200%2C717&ssl=1)
Posted inAstronomy & Telescopes
Optimal Mode-sorting Coronagraphy: Limits Of Single-moded Measurements For The Habitable Worlds Observatory
[astro-ph.IM] Conventional coronagraph architectures struggle to reach the theoretical limit of exoplanet detection at close working angles. Spatial mode-sorting is capable of reaching the theoretical limit, which previous work has […]