SDSS和FIRST巡天中的射电活动星系核

发布时间：2017-12-31 17:22

本文关键词：SDSS和FIRST巡天中的射电活动星系核　出处：《中国科学技术大学》2010年博士论文　论文类型：学位论文

【摘要】： 活动星系核的统一模型认为,拥有同样结构的活动星系核属于同一“父类”,不同的观测特征只是由于观测视角不同。当视线被尘埃环遮挡时,一个活动星系核会表现为窄线源(Ⅱ型),未被遮挡时表现为宽线源(Ⅰ型)。对于射电活动星系核来说,在视线接近于喷流轴时表现为平谱的射电致密源,远离喷流轴则表现为陡谱的射电延展源。活动星系核的结构可能依赖于中央引擎的内禀参数,比如光度、黑洞质量、爱丁顿比率等。这些参数可影响活动星系核的吸积盘、宽线区、尘埃环、喷流等结构和性质,从而决定活动星系核属于哪一种统一模型的“父类”。本论文利用SDSS光学巡天和FIRST射电巡天数据,详细考虑了各种选择效应,通过对不同的观测类型(致密／延展射电源,Ⅰ型／Ⅱ型射电源)的统计研究,讨论了射电活动星系核的统一模型对内禀参数的依赖。第一章首先介绍了活动星系核的观测特性与基本结构,重点介绍了射电喷流和射电瓣。然后介绍了活动星系核的分类：根据窄发射线强度比(BPT诊断图)分为Seyfert、LINER和Seyfert+HⅡ混合型活动星系核,根据宽发射线出现与否分为Ⅰ型和Ⅱ型活动星系核；根据射电光度或射光比,活动星系核分为射电强和射电宁静；在射电强源中根据射电形态可分为致密和延展源；在射电延展源中分出FRⅠ和FRⅡ型源。随后介绍了统一模型,以及统一模型对本征参数的可能依赖关系,包括吸积盘、尘埃环、宽线区和射电喷流,与吸积率光度、黑洞质量、爱丁顿比率等内禀参数的关系。我还介绍了活动星系的两种吸积模式“类星体模式”(QSO mode)和“射电模式”(radio mode),以及“射电模式”对寄主星系和星系团演化的反馈作用。第二章中,我介绍了对于射光比的双峰分布的争论；讨论了光学、射电探测极限等选择效应对射电光度和射光比统计结果的影响。然后介绍了使用SDSS DR3数据和FIRST射电巡天数据来匹配、选取射电类星体样本的过程。我的光学选SDSS-FIRST射电强类星体样本包括3641个射电光度高于1023 WHz-1的纯光学选射电类星体,其中包括859个射电延展源和2782个致密源。我对样本进行了统计分析,讨论了由FIRST的表面亮度探测极限引起的不完备性。我发现在3 mJy水平之上,由于FIRST的小光斑原因而漏掉的弥散射电辐射对样本的完备性影响不大。我也讨论了仅由匹配半径寻找光学源射电对应体造成的选择效应,发现只用2″的匹配半径会造成-16.8%的源流量被低估或者完全被漏掉。我在限定的红移和光学探测极限bin之内进行统计研究,发现尽管延展源与致密源光学光度很相近,延展源的射电光度要明显高于致密源。这一结果提示我们,致密源可能是内禀射电弱或射电中等的源。当它们的喷流轴接近我们视线时,类星体的射电辐射会由于集束效应被显著放大,使得内禀射电较弱的类星体仍然可以被探测到,并表现为致密射电形态；当喷流轴远离我们视线时,这些内禀射电弱类星体则可能落在探测极限之外。在第三章中,我使用Ⅰ型射电活动星系核的比例讨论了射电强活动星系核的尘埃覆盖因子与各种参数的关系。我首先介绍了尘埃环与宽线区对参数的依赖,以及在讨论这种依赖关系中可能遇到的选择效应。随后我介绍了我的射电强活动星系核样本的选取过程。我通过SDSS DR4光谱数据与FIRST巡天的射电源匹配,得到了997个红移z0.35且射电功率P1.4GHz1023 W Hz-1的光学选射电强活动星系核,包括711个Ⅱ型活动星系核,和286个I型活动星系核。我通过选择函数的方法修正了证认和探测Ⅰ型和Ⅱ型源过程中产生的选择效应。在限定的参数空间内,我讨论了Ⅰ型源比例f1对活动星系核内禀参量的可能依赖关系。结果发现：经过消光改正后,f1不随[OⅢ]光度增加而增大。这个结果不支持“尘埃环内径随光度增加后退”模型,而是支持高／低两种吸积率模式的模型。此外,我发现f1在M(?)～108M(?)附近上升了约10%,这很可能与星系尺度的尘埃消光有关。最后一章是全文的总结和后续工作展望。
[Abstract]:As a unified model of active galactic nuclei, have the same structure of active galactic nuclei belong to the same parent, observing the different characteristics of the different perspective. Just because of the observation when the line of sight by dust ring shielding, an AGN appears narrow line source (type II), not blocked performance wide line source (type I). For radio AGN, close to the jet axis in sight for compact radio source spectrum, away from the axis of jet stream is shown as the radio extended source steep spectrum. The structure of active galactic nuclei may depend on the central engine of the intrinsic parameters, such as luminosity, black hole the quality of the Eddington ratio. These parameters can affect the accretion disk of active galactic nuclei, broad line region, dust ring, jet structure and properties, so as to determine the active galactic nuclei which belong to a unified model of the "parent". This paper uses SDSS and FIRST optical inspection day radio patrol All kinds of selection effects are considered in detail. Based on the statistical study of different observation types (dense / extended radio source, type I / II radio sources), the dependence of the unified model of radio active galactic nuclei on intrinsic parameters is discussed.
The first chapter introduces the observational characteristics of active galactic nuclei and the basic structure, introduces the radio jets and the radio lobes. Then this paper introduces the classification of AGNs: according to the narrow emission line intensity ratio (BPT diagnosticdiagram) is divided into Seyfert, LINER and Seyfert+H II hybrid Galaxy nuclear activities, according to the broad emission lines appear divided into type I and type II active galactic nuclei; according to the radio luminosity than light or radiation, AGN is divided into radio and radio quiet; in radio loud sources according to the radio morphology can be divided into dense and extended source; the separation of FR I and FR II type radio source in the extended source. Then introduce the unified model and unified model of the intrinsic parameters may depend on the relationship, including the accretion disc, dust ring, broad line region and radio jets, and the accretion rate of black hole mass, luminosity, intrinsic parameters in the Eddington ratio relationship. I also introduced active galaxies The two accretion modes are "QSO mode" and "radio mode" (radio mode), and the feedback effect of radio modes on the evolution of host galaxies and clusters.
In the second chapter, I introduced the Shuangfeng light distribution of an argument is discussed; the optical, radio detection limit selection effect of light than the statistical results of the impact on the radio luminosity and radiation. Then introduced the use of SDSS DR3 data and FIRST radio survey data to match the process of selection of radio quasars in my sample. Optical SDSS-FIRST radio loud quasar sample including 3641 pure optical radio luminosity is higher than 1023 WHz-1 of the selected radio quasars, including 859 extended radio sources and 2782 compact source. I made a statistical analysis of samples, discusses the surface brightness caused by FIRST the detection limit is not complete. I found on the 3 the level of mJy, due to the small spot FIRST and disperse radio radiation effect on the completeness of missing samples. I also discussed the optical source radio counterpart caused only by the radius, choose to find We find that the source flow effect, only 2 "match radius will cause -16.8% underestimated or completely missed. I do statistical research within the redshift and optical limiting detection limit of bin, found that although the extended source and the compact source is very similar to the optical luminosity, radio luminosity extended source was higher than that of dense source. These results suggest that we, dense source may be intrinsic weak or moderate radio radio source. When the jet axis close to our line of sight, radio quasars will because the cluster effect is significantly enlarged, the intrinsic weak radio quasars can still be detected, and the performance of the compact radio form; when the jet axis away from in our view, these intrinsic weak radio quasars may fall on the detection limit.
In the third chapter, I use the type I radio AGN proportion discusses the relationship between radio loud active galactic nuclei in the dust covering factors and parameters. I first introduced the dust ring and the broad line region's dependence on the parameters, as well as the dependent selection effect may be encountered in the discussion of this relationship. Then I introduced. My radio loud AGNs are selected. I, through radio source SDSS DR4 spectral data and FIRST survey, 997 of the optical and radio power P1.4GHz1023 W z0.35 red Hz-1 selected radio loud AGN, including 711 type II active galactic nuclei, and 286 I type active galactic nuclei I choose. By modifying the effect of identification and detection of type I and type II source in the process of choice function method. In the parameter space defined, I discussed the source type ratio of F1 on the AGN intrinsic parameters can be Can dependence. The result showed that after extinction correction, F1 does not increase with increasing of [O III]. The photometric results do not support the "dust ring diameter with increasing luminosity back" model, but the support of high / low two accretion rate model. In addition, I found F1 in M (108M ~ (?) near?) increased by about 10%, which is likely to dust extinction and Galaxy scale.
The last chapter is the summary of the full text and the prospect of the follow-up work.

【学位授予单位】：中国科学技术大学
【学位级别】：博士
【学位授予年份】：2010
【分类号】：P145.9

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