Stringent upper limits of minor species at the cloud top of Venus: PH₃, HCN, and NH₃

¹ LESIA, Observatoire de Paris, PSL Université, CNRS, Sorbonne Université, Université de Paris, 92195 Meudon, France
² SwRI, Div. 15, San Antonio, TX 78228, USA
³ LATMOS/IPSL, UVSQ Université Paris-Saclay, Sorbonne Université, CNRS, 78280 Guyancourt, France
⁴ Denmark Technical University, 2800 Kongens Lyngby, Denmark
⁵ Kyoto Sangyo University, Kyoto 603-8555, Japan

^★ Corresponding author; therese.encrenaz@obspm.fr

Received: 13 July 2024
Accepted: 13 September 2024

Abstract

Aims. Following several reports announcing the detection or non-detection of minor species above the clouds of Venus, we have searched for other possible signatures of PH₃, HCN, and NH₃ in the infrared range.

Methods. Since 2012, we have performed ground-based observations of Venus in the thermal infrared at various wavelengths to monitor the behavior of SO₂ and H₂O at the cloud top. We have identified spectral intervals where transitions of PH₃ (around 955 cm⁻¹), HCN (around 747 cm⁻¹), and NH₃ (around 951cm⁻¹) are present.

Results. From the absence of any feature at these frequencies, we derive, on the disk-integrated spectrum, a 3-σ upper limit of 3 ppbv for the PH₃ mixing ratio, 0.5 ppbv for HCN, and 0.3 ppbv for NH₃, assuming that these species have a constant mixing ratio throughout the atmosphere. Maps of the Venus disk recorded at the center position of the lines show that there is no evidence for local detection anywhere over the Venus disk.

Conclusions. Our results bring new constraints on the maximum abundance of these species at the cloud top and in the lower mesosphere of Venus.