Abundances of trace constituents in Jupiter's atmosphere inferred from Herschel/PACS observations

Abstract

On October 31, 2009, the Photodetector Array Camera and Spectrometer (PACS) on board the Herschel Space Observatory observed far-infrared spectra of Jupiter in the wavelength range between 50 and 220$\ as part of the program "Water and Related Chemistry in the Solar System". The spectra have an effective spectral resolution between 900 and 3500, depending on the wavelength and grating order. We investigate the disk-averaged chemical composition of Jupiter's atmosphere as a function of height using these observations. We used the Planetary Spectrum Generator (PSG) and the least-squares fitting technique to infer the abundances of trace constituents. The PACS data include numerous spectral lines attributable to ammonia (NH$_3$), methane (CH$_4$), phosphine (PH$_3$), water (H$_2$O), and deuterated hydrogen (HD) in the Jovian atmosphere and probe the chemical composition from $p 275$\,mbar to $p 900$\,mbar. From the observations, we infer an ammonia abundance profile that decreases from a mole fraction of $(1.7 $ at $p 900$\,mbar to $(1.7 $ at $p 275$\,mbar, following a fractional scale height of about $0.114$. For phosphine, we find a mole fraction of $(7.2 $ at pressures higher than $(550 100)$\,mbar and a decrease of its abundance at lower pressures following a fractional scale height of $(0.09 0.02)$. Our analysis delivers a methane mole fraction of $(1.49 $. Analyzing the HD $R(0)$ line at $112.1\ yields a new measurement of Jupiter's D/H ratio, $ D/H $. Finally, the PACS data allow us to put the most stringent $3 upper limits yet on the mole fractions of hydrogen halides in the Jovian troposphere. These new upper limits are $<1.1 $ for hydrogen fluoride (HF), $<6.0 $ for hydrogen chloride (HCl), $<2.3 $ for hydrogen bromide (HBr) and $<1.2 $ for hydrogen iodide (HI) and support the proposed condensation of hydrogen halides into ammonium halide salts in the Jovian troposphere.