标题： 早期型Hα发射线星目录和58个从LAMOST DR7新确认的Herbig Ae/Bes 显示英文标题

标题： A catalog of early-type Hα emission line stars and 58 newly confirmed Herbig Ae/Bes from LAMOST DR7

摘要： 我们从LAMOST DR7中得到了一个早期类型发射线星的目录，其中包括25,886颗恒星的30,048条光谱，其中3,922颗有Simbad记录。 该样本是使用K-最近邻和随机森林方法获得的，并进行了人工检查。 光谱根据H$\alpha$发射线轮廓分为3种形态类型（10个子类型）。 一些受星云发射线（如HII区）污染的光谱在目录中被标记出来。 我们还提供了一个包含101颗恒星的特定子目录，这些恒星通过计算恒星风或吸积流速度（基于P Cygni或反向P Cygni轮廓）确定，其中74%的恒星速度低于400km/s。 更重要的是，利用已知Herbig Ae/Be星（HAeBes）和经典Ae/Be星（CAeBes）的两个颜色-颜色图（H-K，K-W1）和（H-K，J-H），我们提出了一个更新的准则来区分HAeBes和CAeBes。 根据该准则，我们从样本中选择了201个HAeBes候选者和5,547个CAeBes候选者。 我们通过使用WISE图像和LAMOST光谱确认了201个HAeBes中的66个，并呈现了一个特定的HAeBe子目录，其中58个是新识别的。 此外，WISE颜色（W1-W2，W1-W3，W1-W4）显示了我们确认的HAeBes与已知HAeBes之间的分布一致性。 大多数确认的66个HAeBes位于热端主序星的下边缘，而约77%的距离超过1Kpc，这扩大了远距离已知HAeBes的数量。 显示英文摘要

摘要： We derive a catalog of early-type emission-line stars including 30,048 spectra of 25,886 stars from LAMOST DR7, in which 3,922 have Simbad records. The sample is obtained using K-Nearest Neighbor and Random Forest methods and visually inspected. The spectra are classified into 3 morphological types (10 subtypes) based on H$\alpha$ emission line profiles. Some spectra contaminated by nebula emission lines such as from HII regions are flagged in the catalog. We also provide a specific sub-catalog of 101 stars with the stellar wind by calculating stellar wind or accretion flow velocities based on P Cygni or inverse P Cygni profiles, in which 74\% of them having velocities below 400km/s. More important, with two color-color diagrams (H-K, K- W1) and (H-K, J-H) of a collection of known Herbig Ae/Be stars (HAeBes) and classical Ae/Be stars (CAeBes), we propose an updated criterion to separate HAeBes from CAeBes. By the criterion, we select 201 HAeBes candidates and 5,547 CAeBes candidates from the sample. We confirmed 66 of the 201 HAeBes by using both WISE images and LAMOST spectra and present a specific HAeBe sub-catalog, in which 58 are newly identified. In addition, the WISE colors (W1-W2, W1- W3, and W1-W4) show the distribution consistency between our confirmed HAeBes and that of the known HAeBes. Most of the 66 confirmed HAeBes locate in the lower edge of the main sequence of hot end in the HR diagram, while the distances of about 77\% exceed 1Kpc, which enlarges the number of far distant known HAeBes.