Astrobiology160- Page

Galactic-scale properties of the sample. We plot against sin(|b|) EB−V (top left), N(HI) (top right), N(H2) = N(HCO+ )/3 × 10−9 (bottom left), and WCO, the line profile integral of

Keith Cowing Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻 Follow on

Analysis & Data Overview. (a) Top Left: Systematic-corrected signal image, for which a model fit is retrieved, which is shown in the central panel. Top Right: Spatially-flattened spectral profile of

The HHZ (blue shaded regions) and dark HHZ (red shaded regions) around a 0.12M⊙ star for a 7M⊕, 1.7R⊕ hycean planet with tidal quality factor Q = 2. The low-opacity

Spectra showing local sources of RFI that consistently affect the Parkes UWL bandpass. The UWL receiver records two polarisations which are represented by the colours red and blue, respectively, in

LP 791-18 d, illustrated here, is an Earth-size world about 86 light-years away. The gravitational tug from a more massive planet in the system, shown as a blue dot in

NASA’s Mars rover Curiosity acquired this image of the “Altadena” drill hole using its Mast Camera (Mastcam) on June 8, 2025 — Sol 4564, or Martian day 4,564 of the

NASA’s New Horizons spacecraft captured this image of Pluto’s surface shrouded in atmospheric haze. (Credit: NASA/JHUAPL/SwRI) The first observations of Pluto by NASA’s James Webb Space Telescope (JWST) reveal dramatic

Red dwarf stars are more favorable for transiting planet atmosphere characterization. The main way we observe exoplanet atmospheres today is via transiting planets. The planet transit signal is the planet-to-star