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Aims: We characterised the properties of the bar hosted in lenticular galaxyNGC 4277, which is located behind the Virgo cluster.  Methods: We measured the bar length and strength from the surface photometryobtained from the broad-band imaging of the Sloan Digital Sky Survey and wederived the bar pattern speed from the stellar kinematics obtained from theintegral-field spectroscopy performed with the Multi Unit SpectroscopicExplorer at the Very Large Telescope. We also estimated the co-rotation radiusfrom the circular velocity, which we constrained by correcting the stellarstreaming motions for asymmetric drift, and we finally derived the bar rotationrate.  Results: We found that NGC 4277 hosts a short ($R_{bar}=3.2^{+0.9}_{-0.6}$kpc), weak ($S_{bar}=0.21 \pm 0.02$), and slow ($R=1.8^{+0.5}_ {-0.3}$) bar andits pattern speed ($\Omega_{bar}=24.7\pm3.4$ km s$^{-1}$ kpc$^{-1}$) is amongstthe best-constrained ones ever obtained with the Tremaine-Weinberg (TW) methodwith relative statistical errors of $\sim0.2$.  Conclusions: NGC 4277 is the first clear-cut case of a galaxy hosting a slowstellar bar ($R>1.4$ at more than a 1$\sigma$ confidence level) measured withthe model-independent TW method. A possible interaction with the neighbourgalaxy NGC 4273 could have triggered the formation of such a slow bar and/orthe bar could be slowed down due to the dynamical friction with a significantamount of dark matter within the bar region.

A slow bar in the lenticular barred galaxy NGC 4277