Mars craterfill deposits showing varying intensities and topographies (cross sections). Crater locations are shown in Figure 2A. (A) Thin and laterally restricted fill with deposits concentrated in the southwestern region

Radius evolution for a metal-enriched planet (Z=0.1) as computed with our approach (square points) versus the planetsynth models of M¨uller & Helled (2021) (solid curves; note that they employ a

Schematic showing the reset approach applied for the close-in four-planet system. The left graphic shows “exaggerated” orbits of the four planets after the encounter when they are on slightly eccentric,

Scatter plot of Laromatic/LIR as a function of LIR for the AGNdominated (red circles) and AGN-SF-composite galaxies (red triangles). The gray circles show the relationship for the SFG sample. —

Simulated PRIMA/FIRESS spectrum of the PAH emission based on the model spectrum for a galaxy with log(LIR/L⊙)= 13.6 in Fig.7(b) for selective redshifts (z = 3, 5, 7, 10). In