Astrobiology4- Page

HCl was detected in the Martian atmosphere by the NOMAD and ACS spectrometers aboard the ExoMars TGO. Photochemical models show that using gas-phase chemistry alone is insufficient to reproduce these

Time evolution of abundances of some notable metal-bearing species in the hot cores. — astro-ph.GA Metal-bearing species in diffuse or molecular clouds are often overlooked in astrochemical modeling except for

RGZ EMU user interface and its 3-step workflow setup. The first 2 steps (in blue color) of the workflow is compulsary, while the third (in green color) is optional. —

EWs for the K i lines in the J band vs. NIR spectral type for M dwarfs in our sample. The figure elements are the same as in Figure 3.

Multi-layered pipeline for identifying bacterium/archaeon pairs with similar genomic signatures. Layer 1: Five selected non-parametric clustering methods identify clusters of organisms with similar genomic signatures. The clusters containing both bacteria

Planetary growth timescales in an irradiated disc, for different fragmentation velocities (vfrag = 1 m/s in the left panel, vfrag = 10 m/s in the right panel). The black dotted

Flux contamination from nearby sources in the photometry of a TESS Object of Interest, TOI-4479. Left: heat map with the pixel-by-pixel flux fraction coming from TOI-4479 in sector 41. The

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

Final MCRDI data reductions for TWA 7 in the F200W (left) and F444W (right) filters. Both images are rotated with North up, and the + represents the star location. Each