类星体红移分布△ln（1＋z）＝0．205周期性的一种解释

根据红移定义１＋ｚ＝λｉ／λ０ｉ，我们认为类星体红移分布ｌｎ（１＋ｚ）周期性受两个因素影响。首先，决定类星体红移的主要线（如Ｌα１２１６，ＣＩＶ１５４９，ＣＩＩＩ１９０９，ＭｇＩＩ２７９８，ＮｅＶ３４２６，ＯＩＩ３７２７，ＮｅＩＩＩ３８６８，Ｈγ４３４０，Ｈβ４８６１，ＯＩＩＩ５００７）固有波长可能构成０．２０５的周期性；另外，这些谱线的观测波长进入一定光学窗口对红移有一定限制，在一定条件下，它正好在某些红移出现峰值，并与ｌｎ（１＋ｚ）＝０．２０５预言峰值一致。我们还在这两个基本考虑下进行模拟取样，发现有明显周期性，定量上证实了我们的基本考虑。本文是类星体红移分布的一种解释，它能说明为什么统计分布不同样品能得到不同的结论。进而，我们认为红移分布周期性不能成为内禀红移观点的观测支持。     

类星体色指数随红移的变化

本文讨论了类星体各光谱特征对其色指数的影响以及色指数随红移的变化．随着红移的增加，位于Ｌｙα发射线短波方向的各种吸收特征进入了可见光区，内禀的幂律谱和发射线强度的分布对类星体色指数及其弥散的影响将是次要的，各种吸收系统的作用将改变类星体色指数随红移变化的趋势，其中，Ｌｙｍａｎ系限吸收系统的影响最大。利用ＩＵＥ观测的类星体光谱求得色指数随红移的变化，对上述结果进行了验证。     

类星体红移分布的高频周期

本文对Ｖｅｒｏｎ－Ｃｅｔｔｙ和Ｖｅｒｏｎ类星体表中３１９７颗红移精度为０．００１的类星体做了红移分布的周期性分析。结果表明：类星体红移值在几个方向上存在高频波动的周期性分布，且置信度水平较高。根据我们的分析，这种周期性不可能完全是由于选择效应引起的。因此，类星体在大尺度上的分布很可能具有大约５０Ｍｐｃ的周期涨落。     

类星体色指数随红移的变化

本文讨论了类星体各光谱特征对其色指数的影响以及色指数随红移的变化，随着红移的增加，位于Ｌｙａ发射线短波方向的各种吸收特征进入了可见光区，内禀的禀的幂律谱和发射线强度的分布对类星体色指数及其弥散的影响将是次要的，各种吸收系统的作用将改变类星体色指数随红移变化的趋势，其中，Ｌｙｍａｎ系限吸收系统的影响最大，利用ＩＵＥ观测的类星体光谱求得色指数随红移的变化，对上述结果进行了验证。     

类星体红移分布的高频叶期

本对Ｖｅｒｏｎ－Ｃｅｔｔｙ和Ｖｅｒｏｎ类星体表中３１９７颗红移精度为０．００１的类星体做了红移分布的周期性分布。结果表明：类星体红移植在几个方向上存在高频波动的周期性分布，且置信度水平较高。根据我们的分析，这种周期性不可能完全是由于选择效应引起的。因此，类星体在大尺度上的分布很可能具有大约５０Ｍｐｃ的周期涨落。     

类星体HⅠ谱线的切仑柯夫红移与线强比I(Lyα)/I(Hβ)的关系

在切仑柯夫线发射理论的框架下,本文统一地讨论了类星体HI谱线的切合柯夫红移与线强比I(Lyα)/I(Hβ)之间的内在关系。忽略类星体宽线区气云外层光薄区中HI复合线的贡献,利用观测到的Lyα线相对于CIV线的相对红移,即切金柯夫红移,定出第二能级上粒子数布居R_2～0.02,利用观测的〈I(Hα)/I(Hβ)〉值定出参量x_β～14.0。在给定参量T～11000K时,HI的巴尔末线的切仑柯夫红移与线强比I(Lyα)/I(Hβ)同时与观测值相符甚佳,这对切仑柯夫线发射理论是一个有力的支持。     

跟类星体红移宇宙学解释相符合的证据

分析类星体吸收线红移和发射线红移的特征。我们从Hewitt和Burbidge（1993）的星表中选择了吸收线红称和发射线红移都同时提供的类星体，得到了包含401个对象的样本。这是至今对类星体红移研究的最大样本。我们从吸收线红移和发射线红移之间的关系图发现绝大多数（93．6％）对象的吸收线红移都小于相应的发射线红移。这个结论人们在20世纪70年代已经从很小的类星体样本（样本大小50左右）中得到。本文进一步支持了这个结论。它表明类星体红移确实是距离的指示器。这跟宇宙学对类星体红移的解释是一致的。     

关于类星体宇宙学红移的新证据和新认识

自对类星体红移解释发生激烈争论以来,近7、8年新的观测证据、统计分析和理论解释,都是有利于宇宙学红移解释的。它们包括: a)与类星体红移相等但光学光度弱得很多的成协星系的系统观测和结果; b)引力透镜事例的发现和解释; c)标准烛光化后获得的视星等-红移关系; d)标准宇宙模型下解释了类星体发射线红移分布; e)射电子源间最大角径θ与红移图上上包络线的存在; f)理论上给出了可能的产能机制和传能过程,并获得新的观测证据。但是与类星体红移不等的星系成协事例,仍有待深入观测和进一步研究。     

新发现的一颗Z=1.66类星体

本文作者用北京天文台兴隆站２．１６米望远镜及卡焦ＣＣＤ摄谱仪，观测到一颗红移为１．６６的类星体，讨论了该望远镜卡焦摄谱系统的总体光效率。     

跟类星体红移宇宙学解释相符合的证据

分析类星体吸收线红移和发射线红移的特征。我们从Hewitt和Burbidge ( 1 993 )的星表中选择了吸收线红移和发射线红移都同时提供的类星体 ,得到了包含 4 0 1个对象的样本。这是至今对类星体红移研究的最大样本。我们从吸收线红移和发射线红移之间的关系图发现绝大多数 ( 93 .6% )对象的吸收线红移都小于相应的发射线红移。这个结论人们在 2 0世纪 70年代已经从很小的类星体样本 (样本大小 50左右 )中得到。本文进一步支持了这个结论。它表明类星体红移确实是距离的指示器。这跟宇宙学对类星体红移的解释是一致的     

A trend in the gaps in redshift distribution of QSOs

Analysis of gaps in the emission line redshift distribution of 537 QSOs shows a single definite trend in the distribution of the gaps. The trend is similar for radio-quiet objects, radio sources and all QSO's taken together. However, the trend does not suggest any periodicity in redshifts in any of the three cases.     

Are quasar redshifts randomly distributed?

A statistical analysis of possible clumping (not periodicity) of emission line redshifts of QSO's shows the available data to be compatible with random fluctuations of a smooth, nonclumped distribution. This result is demonstrated with Monte Carlo simulations as well as with the Kolmogorov-Smirnov test. It is in complete disagreement with the analysis by Varshni, which is shown to be incorrect.     

Emission line redshift distribution of QSOs

This paper is the second one of a series of papers on the redshift distribution of QSOs. In this paper, we shall study the influence of the selection effect in the identification of emission lines on the redshift distribution of QSOs more thoroughly than the previous paper (Zhouet al., 1983). If we assume that the QSO's redshift is cosmological, adopt the standard model, and consider the selection effect due to the redshift identification, the limiting apparent magnitude in the observation and the evolutionary effect of QSOs, we can compute the emission line redshift distribution for the so-called optically selected QSOs discovered by objective prism, grating prism technique alone, the QSOs discovered by positional methods or by colour technique and for whole QSOs, respectively (see Figures 6, 11, 12). The results of computation agree with the observations very well, especially for optically selected QSOs; the computational distribution has almost the same shape with the observational one. For this kind of the QSOs the computational distribution may give the positions and heights of all these observed peaks. The correlation coefficient between the calculated and observed distributions is larger than 0.95. It shows that (a) the peaks and dips in the redshift distribution of QSOs are mainly caused by the selection effect in the redshift identification, and (b) the redshift of QSOs is cosmological.     

Periodicity in quasar redshifts or selection effects?

Peaks at high redshifts in individual samples of quasars can be explained as due to selection effects. It is concluded that peaks in quasar redshift distribution do not obey any generalformula that can constitute a periodicity, even though individual samples may favour some redshifts of smaller values, viz. z < 1.     

The distribution of galaxy pair redshifts

High signal to noise neutral hydrogen observations of a complete sample of 132 galaxy pairs show a velocity difference distribution which decreases monotonically from zero. There is no strong indication of redshift periodicity for the entire sample and no indication at all for a subset of 79isolated galaxy pairs. In addition, when redshifts are corrected for the solar motion around the Galactic Center there is no indication of a redshift periodicity of 37.6 km s^–1 in V for galaxy pairs (as suggested by Guthrie and Napier 1996).     

The Kolmogorov-Smirnov test for three redshift distributions of long gamma-ray bursts in the Swift Era

We investigate redshift distributions of three long burst samples, with the first sample containing 131 long bursts with observed redshifts, the second including 220 long bursts with pseudo-redshifts calculated by the variability-luminosity relation, and the third including 1194 long bursts with pseudo-redshifts calculated by the lag-luminosity relation, respectively. In the redshift range 0-1 the Kolmogorov-Smirnov probability of the observed redshift distribution and that of the variability-luminosity relation is large. In the redshift ranges 1-2, 2-3, 3-6.3 and 0-37, the Kolmogorov-Smimov probabilities of the redshift distribution from lag-luminosity relation and the observed redshift distri-bution are also large. For the GRBs, which appear both in the two pseudo-redshift burst samples, the KS probability of the pseudo-redshift distribution from the lag-luminosity relation and the observed reshifi distribution is 0.447, which is very large. Based on these results, some conclusions are drawn: I) the V-Liso relation might be more believable than the τ-Liso relation in low redshift ranges and the τ-Liso relation might be more real than the V-Liso relation in high redshift ranges; ii) if we do not consider the redshift ranges, the τ-Liso relation might be more physical and intrinsical than the V-Liso relation.     

The power spectrum of the Lyman-α clouds

We investigate the clustering properties of 13 QSO lines of sight in flat space, with average redshifts from z ≈2 to 4. We estimate the 1D power spectrum and the integral density of neighbours, and discuss their variation with respect to redshift and column density. We compare the results with standard CDM models, and estimate the power spectrum of Lyman- α clustering as a function of both redshift and column density. We find that (a) there is no significant periodicity or characteristic scale; (b) the clustering depends on both column density and redshift; (c) the clustering increases linearly only if at the same time the H  i column density decreases strongly with redshift. The results remain qualitatively the same, assuming an open cosmological model.     

Astronomical redshifts of highly ionized regions

Astronomical or cosmological redshifts are an observable property of extragalactic objects and have historically been wholly attributed to the recessional velocity of that object. The question of other, or intrinsic, components of the redshift has been highly controversial since it was first proposed. This paper investigates one theoretical source of intrinsic redshift that has been identified. The highly ionized regions of Active Galactic Nuclei (AGN) and Quasi-Stellar Objects (QSO) are, by definition, plasmas. All plasmas have electromagnetic scattering characteristics that could contribute to the observed redshift. To investigate this possibility, one region of a generalized AGN was selected, the so called Broad Line Region (BLR). Even though unresolvable with current instrumentation, physical estimates of this region have been published for years in the astronomical literature. These data, selected and then averaged, are used to construct an overall model that is consistent with the published data to within an order of magnitude. The model is then subjected to a theoretical scattering investigation. The results suggest that intrinsic redshifts, derivable from the characteristics of the ambient plasma, may indeed contribute to the overall observed redshift of these objects.     

Ejections of quasars at relativistic speeds from nearby galaxies: Ejection mechanism and selection effects

It has become part of the conventional wisdom of quasar research that quasars cannot be objects ejected from nearby galaxies. The reasons are summarized in Burbidge & Burbidge (1967) and they include: (1) in quasar spectra only redshifts, and no blueshifts, are observed, contrary to expectation in a local Doppler interpretation of quasar line shifts; (2) the energy requirements for relativistically moving quasars seem excessive and the ejection mechanism is unknown. In. this work we show that the first problem could be explained via some powerful selection effects, and that the second problem does not exist in the relativistic slingshot process of ejecting black holes. Consequently one cannot exclude the possibility that at least some of the quasar-galaxy associations of large redshift differentials discussed by Arp and Sulentic are real and that the redshift differences are due to high speeds of ejected quasars     

Evidence for Intrinsic Redshifts in Normal Spiral Galaxies

The Tully–Fisher Relationship (TFR) is utilized to identify anomalous redshifts in normal spiral galaxies. Three redshift anomalies are identified in this analysis: (1) several clusters of galaxies are examined, in which late type spirals have significant excess redshifts relative to early-type spirals in the same clusters; (2) galaxies of morphology similar to ScI galaxies are found to have a systematic excess redshift relative to the redshifts expected if the Hubble Constant is 72 km s⁻¹ Mpc⁻¹; (3) individual galaxies, pairs, and groups are identified which strongly deviate from the predictions of a smooth Hubble flow. These redshift deviations are significantly larger than can be explained by peculiar motions and TFR errors. It is concluded that the redshift anomalies identified in this analysis are consistent with previous claims for large non-cosmological (intrinsic) redshifts.