Extended Data Fig. 1: Comparing the limitations found in all-baseline data.
From: Reply to: No evidence of phosphine in the atmosphere of Venus from independent analyses
Top: (y-offsets for clarity only) ‘JAO/Berkeley-CASA’ whole planet spectrum, digitised from Villanueva et al.1 and converted to flux-density using the standard Venus model of ref. 2. The overlaid red-dashed curve is our radiative transfer model for PH3, scaled for a fixed 1 ppb abundance, as a guide to detection limits. Bottom: our equivalent whole-planet spectrum following similar processing (Supplementary Information) and subtracting a 2nd-order polynomial as in ref. 1.
