Comparison of our Venus-twin MIR spectrum (opaque H₂SO₄ clouds) to other models. We show the flux received by an observer located 10 pc from the planet. The solid line is the MIR thermal emission spectrum of our model (calculated assuming the true values listed in Table 1). The gray-shaded region indicates the S/N = 10 LIFESIM uncertainty considered for our retrievals (see Sect. 2.3.1). The black-dashed line is the standard Venus emission spectrum from the NASA-GSFC Planetary Spectrum Generator (PSG, https://psg. gsfc.nasa.gov; Villanueva et al. 2018). The brown-dashed-dotted line is the MIR Venus spectrum from Arney & Kane (2018).