  X-ray- and EUV- (XEUV-) driven photoevaporative winds acting on
protoplanetary disks around young T-Tauri stars may crucially impact disk
evolution, affecting both gas and dust distributions. We constrain the dust
densities in a typical XEUV-driven outflow, and determine whether these winds
can be observed at $\mu\mathrm{m}$-wavelengths in scattered and polarised
light. For an XEUV-driven outflow around a $M_* = 0.7\,\mathrm{M}_\odot$
T-Tauri star with $L_X = 2 \cdot 10^{30}\,\mathrm{erg/s}$, we find a dust
mass-loss rate $\dot{M}_\mathrm{dust} \lesssim 4.1 \cdot
10^{-11}\,\mathrm{M_\odot / yr}$ for an optimistic estimate of dust densities
in the wind (compared to $\dot{M}_\mathrm{gas} \approx 3.7 \cdot
10^{-8}\,\mathrm{M_\odot / yr}$). The synthesised scattered-light images
suggest a distinct chimney structure emerging at intensities $I/I_{\max} <
10^{-4.5}$ ($10^{-3.5}$) at $\lambda_\mathrm{obs} = 1.6$ ($0.4$)
$\mu\mathrm{m}$, while the features in the polarised-light images are even
fainter. Observations synthesised from our model do not exhibit clear features
for SPHERE IRDIS, but show a faint wind signature for JWST NIRCam under optimal
conditions. In conclusion, unambiguous detections of photoevaporative XEUV
winds launched from primordial disks are at least challenging with current
instrumentation; this provides a possible explanation as to why disk winds are
not routinely detected in scattered or polarised light.
