Alexandre Roman-LopesCarlos G. Román-ZúñigaMauricio TapiaJesús HernándezValeria Ramírez-PreciadoGuy S. StringfellowJason E. YbarraJinyoung Serena KimDante MinnitiKevin R. CoveyMarina KounkelGenaro SuárezBorissova, JuraJuraBorissovaD. A. García-HernándezOlga ZamoraJuan David Trujillo2025-12-072025-12-072019-03-0110.3847/1538-4357/ab03052-s2.0-85063583765https://cris-uv-2.scimago.es/handle/123456789/7704WOS:000460449000013Abstract In this work, we have applied a semi-empirical spectral classification method for OB-stars using the APOGEE spectrograph to a sample of candidates in the W3–W4–W5 (W345) complexes. These massive star-forming regions span over 200 pc across the Perseus arm and have a notorious population of massive stars, from which a large fraction are members of various embedded and young open clusters. From 288 APOGEE spectra showing H -band spectral features typical of O- and B-type sources, 46 probably correspond to previously unknown O-type stars. Therefore, we confirm that Br11–Br13 together with He ii λ 16923 (7–12) and He ii λ 15723 (7–13) lines contained in the APOGEE spectral bands are useful in providing spectral classification down to one spectral sub-class for massive stars in regions as distant as d ≈ 2 kpc. The large number of newly found O-type stars as well as the numerous intermediate-mass population confirm that W345 is a very efficient massive star factory, with an integral stellar population probably amounting several thousand solar masses.enacceso abiertoAstronomy And AstrophysicsSpace And Planetary Sciencearticle