A catalogue of early-type emission-line stars and H{\alpha} line profiles from LAMOST DR2

TL;DR

This paper presents a comprehensive catalogue of over 11,000 spectra of early-type emission-line stars from LAMOST DR2, classifies their Hα line profiles, and analyzes their physical properties and classifications.

Contribution

It provides a large, newly discovered dataset of early-type emission-line stars, categorizes their Hα profiles, and links spectral features to physical star types and phenomena.

Findings

Identified 9,752 new early-type emission-line spectra.

Classified Hα profiles into five morphological categories.

Separated stars into physical types like Be stars, Herbig Ae/Be stars, and binaries.

Abstract

We present a catalogue including 11,204 spectra for 10,436 early-type emission-line stars from LAMOST DR2, among which 9,752 early-type emission-line spectra are newly discovered. For these early-type emission-line stars, we discuss the morphological and physical properties from their low-resolution spectra. In this spectral sample, the H$\alpha$ emission profiles display a wide variety of shapes. Based on the H$\alpha$ line profiles, these spectra are categorized into five distinct classes: single-peak emission, single-peak emission in absorption, double-peak emission, double-peak emission in absorption, and P-Cygni profiles. To better understand what causes the H$\alpha$ line profiles, we divide these objects into four types from the view of physical classification, which include classical Be stars, Herbig Ae/Be stars, close binaries and spectra contaminated by HII regions. The majority of Herbig Ae/Be stars and classical Be stars are identified and separated using the (H-K, K-W1) color-color diagram. We also discuss thirty one binary systems as listed in SIMBAD on-line catalogue and identify 3,600 spectra contaminated by HII regions after cross matching with positions in the Dubout-Crillon catalogue. A statistical analysis of line profiles versus classifications is then conducted in order to understand the distribution of H$\alpha$ profiles for each type in our sample. Finally, we also provide a table of 172 spectra with FeII emission lines and roughly calculate stellar wind velocities for seven spectra with P-Cygni profiles.