  We report the results of observations of p-mode oscillations in the G0
subgiant star HD 35833 in both radial velocities and photometry with NEID and
TESS, respectively. We achieve separate, robust detections of the oscillation
signal with both instruments (radial velocity amplitude $A_{\rm
RV}=1.11\pm0.09$ m s$^{-1}$, photometric amplitude $A_{\rm phot}=6.42\pm0.60$
ppm, frequency of maximum power $\nu_{\rm max} = 595.71\pm17.28$ $\mu$Hz, and
mode spacing $\Delta \nu = 36.65\pm0.96$ $\mu$Hz) as well as a non-detection in
a TESS sector concurrent with the NEID observations. These data shed light on
our ability to mitigate the correlated noise impact of oscillations with radial
velocities alone, and on the robustness of commonly used asteroseismic scaling
relations. The NEID data are used to validate models for the attenuation of
oscillation signals for exposure times $t<\nu_{\rm max}^{-1}$, and we compare
our results to predictions from theoretical scaling relations and find that the
observed amplitudes are weaker than expected by $>4\sigma$, hinting at gaps in
the underlying physical models.
