  We present new optical transmission spectra for two hot Jupiters: WASP-25b (M
= 0.56~M$_J$; R = 1.23 R$_J$; P =~3.76 days) and WASP-124b (M = 0.58~M$_J$; R =
1.34 R$_J$; P = 3.37 days), with wavelength coverages of 4200 - 9100\AA\ and
4570 - 9940\AA, respectively. These spectra are from the ESO Faint Object
Spectrograph and Camera (v.2) mounted on the New Technology Telescope (NTT) and
Inamori-Magellan Areal Camera & Spectrograph on Magellan Baade. No strong
spectral features were found in either spectra, with the data probing 4 and 6
scale heights, respectively. \texttt{Exoretrievals} and \texttt{PLATON}
retrievals favor stellar activity for WASP-25b, while the data for WASP-124b
did not favor one model over another. For both planets the retrievals found a
wide range in the depths where the atmosphere could be optically thick
($\sim0.4\mu$ - 0.2 bars for WASP-25b and 1.6 $\mu$ -- 32 bars for WASP-124b)
and recovered a temperature that is consistent with the planets' equilibrium
temperatures, but with wide uncertainties (up to $\pm$430$^\circ$K). For
WASP-25b, the models also favor stellar spots that are $\sim$500-3000$^\circ$K
cooler than the surrounding photosphere. The fairly weak constraints on
parameters are owing to the relatively low precision of the data, with an
average precision of 840 and 1240 ppm per bin for WASP-25b and WASP-124b,
respectively. However, some contribution might still be due to an inherent
absence of absorption or scattering in the planets' upper atmospheres, possibly
because of aerosols. We attempt to fit the strength of the sodium signals to
the aerosol-metallicity trend proposed by McGruder et al. 2023, and find
WASP-25b and WASP-124b are consistent with the prediction, though their
uncertainties are too large to confidently confirm the trend.
