Comparison of the apparent fluxes of β Pictoris b (yellow squares) to best fitted fluxes (horizontal barres) generated from synthetic spectra. Bottom: comparison to AMES-Cond (green; T_eff = 1400 K,log g = 3.5,andR = 1.89 R_Jup), AMES-Dusty (pink; T_eff = 1700 K, log g = 3.5, and R = 1.22 R_Jup), and BT-Cond2012 (blue; T_eff = 1800 K,log g = 4.0,andR = 1.16 R_Jup) synthetic fluxes/spectra. Middle: comparison to BT-Settl 2012 models at solar metallicity (gold; T_eff = 1700 K,log g = 3.5,and R = 1.29 R_Jup), to BT-Settl 2012 models with [M/H] = + 0.5 dex (blue; T_eff = 1600 K,log g = 4.5,and R = 1.43 R_Jup), and to BT-Settl 2010 (red; T_eff = 1600 K,log g = 3.5,andR = 1.61 R_Jup) synthetic fluxes at solar metallicity. The corresponding model spectra smoothed at the resolution of the NB_4.05 filter are also shown. Top: comparison to DRIFT-PHOENIX spectra (T_eff = 1700 K,log g = 4.0,andR = 1.38 R_Jup) with solar metallicity (M/H = 0.0, orange), metal-enriched (M/H = +0.5, dark red), and metal-depleted (M/H = –0.5, brown) atmospheres.