LAMOST光谱J152238.11+333136.1 P-Cygni轮廓分析  

P-Cygni Profile Analysis of the Spectrum: LAMOST J152238.11+333136.1

作　　者：屈彩霞 杨海峰[1] 蔡江辉[1] 荀亚玲[1] QU Cai-Xia;YANG Hai-feng;CAI Jiang-hui;XUN Ya-ling(School of Computer Science and Technology,Taiyuan University of Science and Technology,Taiyuan 030024,China)

机构地区：[1]太原科技大学计算机科学与技术学院,山西太原030024

出　　处：《光谱学与光谱分析》2020年第4期1304-1308,共5页Spectroscopy and Spectral Analysis

基　　金：国家自然科学基金项目(U1931209,U1731126,61602335);山西省重点研发计划项目(201803D121059)资助。

摘　　要：LAMOST一期巡天成功获取河外星系光谱超过150 000条,大样本光谱数据为探索奇异、稀有的天体从而完善现有的天体演化理论提供了必要的数据条件;而先进的信息技术为从海量的数据中挖掘这些珍稀样本提供了有效途径。针对采用基于DoPS的数据挖掘方法,从LAMOST DR5星系光谱数据获得的离群数据挖掘结果中,呈现出疑似P-Cygni轮廓特征的光谱J152238.11+333136.1进行了深入讨论。首先针对该光谱的基本信息、疑似P-Cygni轮廓特征以及相应的离群数据挖掘方法进行了简要表述,光谱在Hβ和[OⅢ]λ4860处呈现P-Cygni轮廓,在NeⅢλ3869和HeⅠλ5874处呈现反P-Cygni轮廓;其次,对该特征的真实性及其生成机制从以下4个角度展开讨论。(1)交叉同源观测。Sloan巡天2004年(相差11年)的同源观测,其光谱上并未呈现对应的特征,据推测可能是正在进行的演化活动或者光纤定位误差所致;(2)通过分析光谱质量、减天光残差等方法,分析P-Cygni特征是否为观测或数据处理所致。NeⅢλ3869和HeⅠλ5874处呈现反P-Cygni轮廓可信度较低;同时,通过比较目标光谱与超级天光,以及相邻光纤观测到的光谱在对应波长处的光谱特征,说明存在P-Cygni轮廓为减天光过程导致的可能性;(3)光谱子型差异。IRAS和WISE等近红外同源观测,显示其为Seyfert 2型星系,光学波段发射线强比[NⅡ]/Hα,[OⅢ]/Hβ显示其为HⅡ区,结合光学、红外测光图像特征,推测目标可能是两个星系进行并合活动;(4)从导致P-Cygni轮廓的物理机制的角度,分析了由星系并合触发外流、由恒星形成(爆发)电离气体触发的外流以及由Wolf-Rayet特征星系的超星风等原因引起的可能性。LAMOST first-tage regular survey has been successfully observed more than 150 000 galaxy spectra, which will provide necessary data for mining the precious and rare objects to improve the existing cosmogony theories. The advanced information technologies will provide effective tools to mine these rare samples from the vast amounts of spectral data. In this paper, the spectrum J152238.11+333136.1 is particularly chosen from LAMOST DR 5 by using the outlier mining method based on the DoPS method and intensively discussed the rare characteristics of P-Cygni profiles. Firstly, the basic information, the description of suspected P-Cygni profiles and the related data mining methods are introduced briefly. The P-Cygni shapes are shown in the wavelength of Hβ and [OⅢ]λ4860, and inverted P-Cygni shapes are shown in the wavelength of NeⅢλ3869 and HeⅠλ5874. Secondly, the authenticity of the feature and its generation mechanism are discussed from the following four perspectives.(1) Homologous observation. The homologous observation of Sloan survey in 2004(11 years before) did not present corresponding features on the spectrum, which might be due to ongoing evolutionary activities or fiber positioning errors;(2) By analyzing the spectral quality and reducing the residual of the skylight, it is analyzed whether the P-Cygni features are caused by observations or data processing. The inverted P-Cygni shapes in NeⅢλ3869 and HeⅠλ5874 have lower credibility. Meanwhile, by comparing the target spectrum with the super skylight, and the spectral characteristics of the spectrum observed by the adjacent fibers, the possibility that the P-Cygni profiles is caused by the sky background reduction process is illustrated;(3) Spectral sub-type differences. Near-infrared homologous observations such as IRAS and WISE showed that it is a Seyfert 2 galaxy. However, the emission line intensity ratio [NⅡ]/Hα, [OⅢ]/Hβ shows that it is HⅡ region. Considering the characteristics of optical and infrared photometry images, we inf

关 键 词：P-Cygni轮廓 OUTFLOWS 郭守敬望远镜(LAMOST) 离群特征 

分 类 号：P114.1[天文地球—天文学]