类星体发射线的应用—估算类星体中心黑洞质量
发布时间：2018-08-25 10:05
【摘要】：活动星系核是一类中央核区活动性很强的河外星系。这些星系显得比正常星系活跃，可以辐射出从射电到γ射线的全波段的电磁波。自上世纪60年代类星体被发现以来，又相继发现了许多具有类似特征的天体，都是河外星系，统称为活动星系核。 根据标准模型，黑洞-吸积盘模型，目前普遍认为类星体是由位于星系中心位置的超大质量黑洞和吸积盘构成。此外，还引入了宽线区和窄线区，以便解释发射线光谱。黑洞质量的大小对于帮助我们了解宇宙的早期以及超大质量黑洞的形成和演化有着重要的作用，也是类星体研究工作的一个基本问题。本文就是利用宽发射线的光度和谱线宽度来估算类星体中心黑洞质量，并把估算的结果与其他方法估算出的结果相比较，，看是否跟之前吴学兵等人提出的观点相吻合。 第一章介绍活动星系核的观测特征和分类，类星体的概述和发射线、类星体的黑洞-吸积盘模型。 第二章介绍了类星体中心黑洞质量的估算方法的来源以及改进和发展，然后针对吴学兵等人提出的连续谱的光度有可能被观测方向上的喷流污染，从而影响了黑洞质量的估算结果，造成偏大效果的观点，我们构建了一个基于RASS-SDSS-FIRST-GB6交叉认证过的射电陡谱源样本，此样本中包含了185个源。这些源的性质目录数据中已经给出了Shen等人利用连续谱估算得到的维里黑洞质量。我们利用数据中给出的这些源的Hβ,MgII,CIV宽发射线的光度和这些宽发射线相应的FWHM，通过相关经验公式的估算从而得到黑洞质量，然后用这些黑洞质量跟Shen的维里黑洞质量进行比较，发现通过CIV宽发射线估算得到的黑洞质量比维里质量要小，对于样本里的绝大多数源都如此，但同样的情况在通过Hβ,MgII宽发射线估算的黑洞质量跟维里黑洞质量的比较中并未出现。 第三章做了一个简单的总结和展望。
[Abstract]:Active galactic nuclei (AGNs) are a class of extragalactic galaxies with strong activity in the central nucleus region. These galaxies appear to be more active than normal galaxies, radiating full-band electromagnetic waves from radio to 纬-rays. Since the discovery of quasars in the 1960s, many objects with similar characteristics have been discovered, all of which are extragalactic, collectively known as active galactic nuclei (AGNs). According to the standard model, black hole accretion disk model, it is generally believed that quasars are composed of supermassive black holes and accretion disks located in the center of galaxies. In addition, broad and narrow line regions are introduced to explain the emission line spectrum. Black hole mass plays an important role in understanding the early universe and the formation and evolution of supermassive black holes. It is also a basic problem in quasar research. In this paper, the mass of a quasar central black hole is estimated by using the luminosity and spectral line width of the broad emission line, and the estimated results are compared with those obtained by other methods to see if it is consistent with the viewpoint put forward by Wu Xuebing et al. The first chapter introduces the observational characteristics and classification of active galactic nuclei, the overview and emission lines of quasars, and the black hole accretion disk model of quasars. In the second chapter, the source, improvement and development of the method for estimating the mass of a quasar central black hole are introduced, and then the luminosity of the continuous spectrum proposed by Wu Xuebing and others may be polluted by a jet in the observed direction. Therefore, we construct a radio steep-spectrum source sample based on RASS-SDSS-FIRST-GB6 cross-authentication, which contains 185 sources. The properties of these sources in the catalog data have been given by Shen et al., using continuous spectra to estimate the mass of the Wirelli black hole. We obtain the mass of black hole by using the luminosity of the H 尾 Mg-III CIV wide emission line given in the data and the FWHM, corresponding to these wide emission lines through the estimation of relevant empirical formulas, and then compare the mass of these black holes with those of Shen's Wirelli black hole. It is found that the mass of black hole estimated by the CIV wide emission line is smaller than that of the Wirelli mass, which is true for most of the sources in the sample. However, the same situation is not found in the comparison between the mass of black hole estimated by H 尾 -MgII wide emission line and the mass of Virie black hole. The third chapter makes a simple summary and prospect.
【学位授予单位】：广州大学
【学位级别】：硕士
【学位授予年份】：2012
【分类号】：P145.8
本文编号：2202550
[Abstract]:Active galactic nuclei (AGNs) are a class of extragalactic galaxies with strong activity in the central nucleus region. These galaxies appear to be more active than normal galaxies, radiating full-band electromagnetic waves from radio to 纬-rays. Since the discovery of quasars in the 1960s, many objects with similar characteristics have been discovered, all of which are extragalactic, collectively known as active galactic nuclei (AGNs). According to the standard model, black hole accretion disk model, it is generally believed that quasars are composed of supermassive black holes and accretion disks located in the center of galaxies. In addition, broad and narrow line regions are introduced to explain the emission line spectrum. Black hole mass plays an important role in understanding the early universe and the formation and evolution of supermassive black holes. It is also a basic problem in quasar research. In this paper, the mass of a quasar central black hole is estimated by using the luminosity and spectral line width of the broad emission line, and the estimated results are compared with those obtained by other methods to see if it is consistent with the viewpoint put forward by Wu Xuebing et al. The first chapter introduces the observational characteristics and classification of active galactic nuclei, the overview and emission lines of quasars, and the black hole accretion disk model of quasars. In the second chapter, the source, improvement and development of the method for estimating the mass of a quasar central black hole are introduced, and then the luminosity of the continuous spectrum proposed by Wu Xuebing and others may be polluted by a jet in the observed direction. Therefore, we construct a radio steep-spectrum source sample based on RASS-SDSS-FIRST-GB6 cross-authentication, which contains 185 sources. The properties of these sources in the catalog data have been given by Shen et al., using continuous spectra to estimate the mass of the Wirelli black hole. We obtain the mass of black hole by using the luminosity of the H 尾 Mg-III CIV wide emission line given in the data and the FWHM, corresponding to these wide emission lines through the estimation of relevant empirical formulas, and then compare the mass of these black holes with those of Shen's Wirelli black hole. It is found that the mass of black hole estimated by the CIV wide emission line is smaller than that of the Wirelli mass, which is true for most of the sources in the sample. However, the same situation is not found in the comparison between the mass of black hole estimated by H 尾 -MgII wide emission line and the mass of Virie black hole. The third chapter makes a simple summary and prospect.
【学位授予单位】：广州大学
【学位级别】：硕士
【学位授予年份】：2012
【分类号】：P145.8
【参考文献】
相关硕士学位论文 前2条
1 陈志福;SDSS类星体谱线的测量及其应用[D];广州大学;2011年
2 张春玲;FRIs和FRIIs星系观测性质的研究[D];广州大学;2010年
本文编号：2202550
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