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We carried out an optical polarimetric study in the direction of the RCW95star forming region in order to probe the sky-projected magnetic fieldstructure by using the distribution of linear polarization segments which seemto be well aligned with the more extended cloud component. A mean polarizationangle of $\theta=49.8^o\pm7.7^o$ was derived. Through the spectral dependenceanalysis of polarization it was possible to obtain the total-to-selectiveextinction ratio ($R_V$) by fitting the Serkowski function, resulting in a meanvalue of $R_V=2.93\pm0.47$. The foreground polarization component was estimatedand is in agreement with previous studies in this direction of the Galaxy.Further, near-infrared images from Vista Variables in the Via L\'actea (VVV)survey were collected to improve the study of the stellar population associatedwith the HII region. The Automated Stellar Cluster Analysis (ASteCA) algorithmwas employed to derive structural parameters for two clusters in the region,and a set of PAdova and TRieste Stellar Evolution Code (PARSEC) isochrones wassuperimposed on the decontaminated colour-magnitude diagrams (CMDs) to estimatean age of about 3 Myr for both clusters. Finally, from the near-infraredphotometry study combined with spectra obtained with the Ohio State InfraredImager and Spectrometer (OSIRIS) mounted at the Southern Astrophysics ResearchTelescope (SOAR) we derived the spectral classification of the main ionizingsources in the clusters associated with IRAS 15408$-$5356 and IRAS15412$-$5359, both objects classified as O4 V stars.

Optical Polarimetric and Near-Infrared Photometric Study of the RCW95 Galactic HII Region