2021ApJ...907L..27A

Recently published Atacama Large Millimeter Array (ALMA) observations suggest the presence of 20 ppb PH₃ in the upper clouds of Venus. This is an unexpected result, as PH₃ does not have a readily apparent source and should be rapidly photochemically destroyed according to our current understanding of Venus atmospheric chemistry. While the reported PH₃ spectral line at 266.94 GHz is nearly colocated with an SO₂ spectral line, the nondetection of stronger SO₂ lines in the wideband ALMA data is used to rule out SO₂ as the origin of the feature. We present a reassessment of wideband and narrowband data sets derived from these ALMA observations. The ALMA observations are re-reduced following both the initial and revised calibration procedures discussed by the authors of the original study. We also investigate the phenomenon of apparent spectral line dilution over varying spatial scales resulting from the ALMA antenna configuration. A 266.94 GHz spectral feature is apparent in the narrowband data using the initial calibration procedures, but this same feature cannot be identified following calibration revisions. The feature is also not reproduced in the wideband data. While the SO₂ spectral line is not observed at 257.54 GHz in the ALMA wideband data, our dilution simulations suggest that SO₂ abundances greater than the previously suggested 10 ppb limit would also not be detected by ALMA. Additional millimeter, submillimeter, and infrared observations of Venus should be undertaken to further investigate the possibility of PH₃ in the Venus atmosphere.