Open Access
Table A.1
Comparison of major SOAP versions by core capabilities and modeling details.
| Version | Input | AR Modeling | Planet | Star |
|---|---|---|---|---|
| SOAP (Boisse et al. 2012) | CCF (model) | ARs’ RV impact modeled by local CCFs with brightness contrast relative to the photosphere, Doppler-shifted by stellar rotation. The same contrast applies to flux variation. | No | Local flux weighted by linear limb-darkening law, adjusted for stellar properties. |
| SOAP-T (Oshagh et al. 2013) | CCF (model) | Inherited from SOAP | Yes | Includes planetary transits and occultations of ARs. |
| SOAP 2.0 (Dumusque et al. 2014) | CCF (Observed + model) | Includes inhibition of convective blueshift in ARs (FTS), limb brightening for faculae, and realistic spot/plage contrast ratios (Planck distribution). | No | Flux weighted by quadratic limb-darkening law; observational convective blueshift suppression. |
| SOAP 3.0 (Akinsanmi et al. 2018; Serrano et al. 2020) | CCF (Observed + model) | Inherits SOAP 2.0 AR modeling. | Yes | Simulates transits of ringed planets and their occultation of ARs; stellar surface with differential rotation. |
| SOAP-GPU (Zhao & Dumusque 2023) | Observed spectra (solar) Synthetic spectra (PHNX) | Quiet photosphere, spots, and faculae modeled using PHNX synthetic spectra at each μ angle. Direct mapping of the ARs. | No | GPU-based full-disk spectral synthesis; injects disk-position-dependent bisector profiles. |
| SOAPv4 (Cristo et al. 2024; This work) | CCF (Observed + model) Observed spectra (IAG, FTS, generic) Synthetic spectra (PHNX, TS, generic) | Inherits SOAP 2.0 AR modeling for CCF; adds spectral modeling. | Yes | Simulates spectral time-series including transmission spectra (POLDS), Doppler shadow profiles line-by-line or full spectrum, and activity impact on line profiles. |
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