The identification of new Herbig Ae/Be stars from LAMOST DR7

Abstract

Herbig Ae/Be stars (HAeBes) are critical tracers of intermediate- and high-mass star formation, yet their census remains incomplete compared to low-mass young stellar objects like T-Tauri stars. To expand the known population, we systematically searched for HAeBes in LAMOST DR7 low-resolution spectra. Following Sun et al., we applied Uniform Manifold Approximation and Projection (UMAP) for dimensionality reduction and Support Vector Machine (SVM) classification, identifying $\sim$240,000 spectra with potential H$\alpha$ emission. After removing contaminants (non-stellar objects, extragalactic sources, CVs, and Algol systems) and restricting to B/A-type stars, we obtained 1,835 candidates through 2MASS/WISE visual inspection. Spectral energy distribution analysis confirmed 143 sources with infrared excess ($J$-band or longer wavelengths), including 92 known HAeBes. From the remaining 51 candidates, we classified 26 with strong infrared excess as new HAeBes. Color-index analysis of confirmed HAeBes and classical Ae/Be stars (CAeBes) revealed that the $(K-W1{)}_0$ vs. $(W2-W3{)}_0$ diagram effectively separates these populations: CAeBes predominantly occupy $(K-W1{)}_0\le 0.5$ and $(W2-W3{)}_0\le 1.1$, while other regions trace transition disks ($(K-W1{)}_0<0.5$ and $(W2-W3{)}_0>1.1$), globally depleted disks ($(K-W1{)}_0>0.5$ and $(W2-W3{)}_0<1.1$), and Class I/Flat/II HAeBes ($(K-W1{)}_0>0.5$ and $(W2-W3{)}_0>1.1$). More importantly, the HAeBes exhibit a clear evolutionary gradient on this diagram, with those in the Class III, Class II, Flat-SED, and Class I evolutionary stages being effectively distinguished by concentric ellipses that are roughly centered at (0,0) with semi-major axes of $a$=1.5, $a$=3.0, and $a$=4.0, and a semi-major to semi-minor axis ratio of 1.6:1.

arXiv comment22 pages, 11 figures. Accepted by the Astronomical Journal

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