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The brightness of faculae and network depends on the angle at which they areobserved and the magnetic flux density. Close to the limb, assessment of thisrelationship has until now been hindered by the increasingly lower signal inmagnetograms. This preliminary study aims at highlighting the potential ofusing simultaneous observations from different vantage points to betterdetermine the properties of faculae close to the limb. We use data from theSolar Orbiter/Polarimetric and Helioseismic Imager (SO/PHI), and the SolarDynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI), recorded at$\sim60^\circ$ angular separation of their lines of sight at the Sun. We usecontinuum intensity observed close to the limb by SO/PHI and complement it withthe co-observed $B_{\rm LOS}$ from SDO/HMI, originating closer to disc centre(as seen by SDO/HMI), thus avoiding the degradation of the magnetic fieldsignal near the limb. We derived the dependence of facular brightness in thecontinuum on disc position and magnetic flux density from the combinedobservations of SO/PHI and SDO/HMI. Compared with a single point of view, wewere able to obtain contrast values reaching closer to the limb and to lowerfield strengths. We find the general dependence of the limb distance at whichthe contrast is maximum on the flux density to be at large in line with singleviewpoint observations, in that the higher the flux density is, the closer theturning point lies to the limb. There is a tendency, however, for the maximumto be reached closer to the limb when determined from two vantage points. Wenote that due to the preliminary nature of this study, these results must betaken with caution. Our analysis shows that studies involving two viewpointscan significantly improve the detection of faculae near the solar limb and thedetermination of their brightness contrast relative to the quiet Sun.

Intensity contrast of solar network and faculae close to the solar limb, observed from two vantage points