Introduction: When lacking polarimetric observations, the Bright Points (BPs) visible in the G-band at 430 nm are commonly used as tracers for magnetic fields. Methods: Observations presented in this paper were taken on October 11, 2005 at the German Vacuum Tower Telescope and involved the Tenerife Infrared Polarimeter (TIP) at 1.5 micron, the Telecentric Etalon Solar Spectrometer (TESOS) in the Fe I spectral line at 557.6 nm, and a speckle setup in G-band. The area scanned by TIP was 75''x33'' and covered a pore surrounded by network. The TIP spectra were inverted with the SIR (Stokes Inversion based on Response functions) code to retrieve the magnetic field vector. Results: We find that G-band BPs are not cospatial with the central part of the flux concentrations. Even at the small heliocentric angle of 12 degree, the BPs appear projected on the limb side walls of the granules (Fig. 1), whereas the fields are concentrated in the intergranular lanes. Discussion: Our findings indicate that the G-band Bright Points are a result of the "hot wall effect". The downward shift of the optical depth scale in the presence of magnetic fields allows to see deeper and hotter layers, where CH dissociates, in the granules next to the field concentrations. Thus, information drawn from the observations of BPs cannot be used to conclude on the actual variation of the magnetic field structure, as only the outer parts of the flux concentrations are seen in the BPs. Figure 1. Non-cospatiality of BPs and field concentrations. Top row, left to right: line-core intensity, LOS velocity (range =+/- 1 km/s), magnetic flux , polarity, LOS velocity from the inversion (range =+/- 1.5 km/s), field azimuth. Bottom row, left to right: polarization degree, G-band intensity, continuum intensity at 1.5 micron, BP mask, field strength, field inclination. The white arrow in the G-band image denotes the limb direction, the cross marks the center of the 6.7 x 6.7 Mm field-of-view shown.