论文标题
通过独立分析，在金星大气中没有膦的证据
No evidence of phosphine in the atmosphere of Venus by independent analyses
论文作者
论文摘要
最近，基于毫米波无线电观测值（Greaves etal。2020）及其重新分析（Greaves etal。2021a/b），最近报道了金星大气中磷酸（PH3）的检测。在这方面，我们进行了独立的重新分析，确定了光谱数据解释中的几个问题。结果，我们确定了在金星大气中（> 75 km，在云层上方）中对PH3的敏感上限，这些限制与G2020和G2021A/B中的发现相差。该测量值针对的是266.944513 GHz的PH3（j = 1-0）的基本第一轮旋转过渡，该测量在2017年6月与James Clerk Maxwell望远镜（JCMT）观察到，该速度于2017年6月在2019年3月的Atacama大型毫米/毫米阵列（Atray（Alma）靠近Atacama大型毫米/毫米阵列。 266.943329 GHz（距PH3线仅1.3 km/s），代表了潜在的污染源。 G2020中介绍的JCMT和ALMA数据的光谱分辨率与两条线的频率分离相当。此外，确定的光谱特征是宽度几km/s，因此不允许对PH3和SO2的候选光谱线的不同光谱分离。我们介绍我们执行的辐射转移建模，然后依次讨论ALMA和JCMT分析。
The detection of phosphine (PH3) in the atmosphere of Venus has been recently reported based on millimeter-wave radio observations (Greaves et al. 2020), and its re-analyses (Greaves et al. 2021a/b). In this Matters Arising we perform an independent reanalysis, identifying several issues in the interpretation of the spectroscopic data. As a result, we determine sensitive upper-limits for PH3 in Venus' atmosphere (>75 km, above the cloud decks) that are discrepant with the findings in G2020 and G2021a/b. The measurements target the fundamental first rotational transition of PH3 (J=1-0) at 266.944513 GHz, which was observed with the James Clerk Maxwell Telescope (JCMT) in June 2017 and with the Atacama Large Millimeter/submillimeter Array (ALMA) in March 2019. This line's center is near the SO2 (J=309,21-318,24) transition at 266.943329 GHz (only 1.3 km/s away from the PH3 line) which represents a potential source of contamination. The JCMT and ALMA data, as presented in G2020, are at spectral resolutions comparable to the frequency separation of the two lines. Moreover, the spectral features identified are several km/s in width, and therefore do not permit distinct spectroscopic separation of the candidate spectral lines of PH3 and SO2. We present the radiative transfer modelling we have performed and then discuss the ALMA and JCMT analyses in turn.
