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The detection of phosphine (PH3) in the atmosphere of Venus has been recentlyreported based on millimeter-wave radio observations (Greaves et al. 2020), andits re-analyses (Greaves et al. 2021a/b). In this Matters Arising we perform anindependent reanalysis, identifying several issues in the interpretation of thespectroscopic data. As a result, we determine sensitive upper-limits for PH3 inVenus' atmosphere (>75 km, above the cloud decks) that are discrepant with thefindings in G2020 and G2021a/b. The measurements target the fundamental firstrotational transition of PH3 (J=1-0) at 266.944513 GHz, which was observed withthe James Clerk Maxwell Telescope (JCMT) in June 2017 and with the AtacamaLarge Millimeter/submillimeter Array (ALMA) in March 2019. This line's centeris near the SO2 (J=309,21-318,24) transition at 266.943329 GHz (only 1.3 km/saway from the PH3 line) which represents a potential source of contamination.The JCMT and ALMA data, as presented in G2020, are at spectral resolutionscomparable to the frequency separation of the two lines. Moreover, the spectralfeatures identified are several km/s in width, and therefore do not permitdistinct spectroscopic separation of the candidate spectral lines of PH3 andSO2. We present the radiative transfer modelling we have performed and thendiscuss the ALMA and JCMT analyses in turn.

No evidence of phosphine in the atmosphere of Venus by independent analyses