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JWST$'$s large aperture and wide wavelength coverage will enable it tocollect the highest quality transit spectra observed so far. For exoplanetaryatmospheres we expect to retrieve the abundance of the most abundant molecules,such as H$_2$O, CO, and CH$_4$. Other molecules, such as H$_2$S and PH$_3$,have been observed in Jupiter and Saturn but their chemistry and detectabilityin strongly irradiated planets is highly unknown. In this paper, we make thefirst effort to study their spectral features in solar composition atmospheres,and evaluate their detectability with JWST. We model the chemistry ofphosphorus and sulfur in solar composition atmospheres. Our model includes theeffect of vertical transport. Photochemistry effects are not included in ourcalculations. Using the abundance profiles, we model the JWST transmission andemission spectra for K=6.8 G-type star and for planets with cloud-free solarcomposition atmospheres. We find PH$_3$ is detectable at 3 sigma fromtransmission spectra of the simulated atmosphere with $T_{\rm eq}$ $<$ 500Kusing the NIRCam LW grism F444W mode with a total observing time of 28.8 hrs.H$_2$S is detectable at 3 sigma in the transmission and emission spectra forthe simulated planet with $T_{\rm eq}$ $>$ 1500K using the NIRCam LW grismF322W2 mode with a total observing time of 24.0 hrs. Our results specificallyhighlight the importance of including H$_2$S for future abundances retrievalwith JWST. The presence of clouds and hazes challenges the detections of PH$_3$and H$_2$S, but H$_2$S features are still expected to be present in theemission spectra.

Modeling synthetic spectra for transiting extrasolar giant planets: detectability of H$_2$S and PH$_3$ with JWST