Analysis of Multi-Wavelength Data for 30 Galactic Emission-Line Stars with Dusty Envelopes

We selected 30 stars with V-band brightnesses of 11-16 mag, visual color-indices B-V of approximately 1.3 mag or less, and large near-IR color-indices (J-H and H-K of approximately 0.7 mag or greater) to search for the presence of the B[e] phenomenon. Spectroscopic observations confirmed the presence of emission lines previously detected in 11 stars of the sample and revealed them in 4 other stars for the first time. Spectral energy distributions (SEDs) in the optical and IR spectral regions were analyzed and compared with theoretical SEDs. The fundamental parameters were estimated using the SED fits corrected for the interstellar and circumstellar (CS) extinction and Gaia DR3 distance measurements. Properties of 14 objects previously classified as pre-main-sequence stars were reevaluated. The B[e] phenomenon was found in 16 objects, most of which exhibit observed properties of FS CMa type objects, a still small group of Galactic stars or binary systems with predominantly hot CS dust. Properties of 2 objects (IRAS 06237+0020 and IRAS 19156-0935) are consistent with those of Proto-Planetary Nebulae at early phases of this evolutionary stage. The nature and evolutionary status of 11 sample objects remain uncertain and require further investigation.