The origin of [Fe ii] emission in NGC 4151

The centre of NGC 4151 has been observed in the J band with the SMIRFS integral field unit (IFU) on the UK Infrared Telescope. A map of [Fe  ii ] emission is derived, and compared with the distributions of the optical narrow-line region and radio jet. We conclude that, because the [Fe  ii ] emission is associated more closely with the visible narrow-line region than with the radio jet, it arises mainly through photoionization of gas by collimated X-rays from the Seyfert nucleus. The velocity field and strength with respect to Pa β are found to be consistent with this argument. The performance of the IFU is considered briefly, and techniques for observation and data analysis are discussed.     

二维太阳光谱观测方法和技术

经典的太阳光谱观测是一维的，它有很大的局限性。从５０年代起，天文工作者采用多种方法开展二维太阳光谱观测，已经研制出一系列仪器，建立完整的资料归算程序，取得优良成果。在二维观测资料的基础上，用理论方法推出深度分布，可以得出三维的立体图像，这会成为太阳研究的主要方法之一。     

Kinematics from spectroscopy with a wide slit: detecting black holes in galaxy centres

We consider long-slit emission-line spectra of galactic nuclei when the slit is wider than the instrumental point spread function, and the target has large velocity gradients. The finite width of the slit generates complex distributions of brightness at a given spatial point in the measured spectrum, which can be misinterpreted as coming from additional physically distinct nuclear components. We illustrate this phenomenon for the case of a thin disc in circular motion around a nuclear black hole (BH). We develop a new method for estimating the mass of the BH that exploits a feature in the spectrum at the outer edge of the BH's sphere of influence, and therefore gives higher sensitivity to BH detection than traditional methods. Moreover, with this method we can determine the BH mass and the inclination of the surrounding disc separately, whereas the traditional approach to BH estimation requires two long-slit spectra to be taken. We show that, with a given spectrograph, the detectability of a BH depends on the sense of rotation of the nuclear disc. We apply our method to estimate the BH mass in M84 from a publicly available spectrum, and recover a value four times lower than that published previously from the same data.     

CVN硬盘系统和软件相关处理在e-VLBI试验中的应用

介绍了中国VLBI网（CVN）的e-VLBI技术研究进展．CVN包括上海佘山、乌鲁木齐南山2个固定观测站和云南昆明的流动站，以及上海天文台的2台站硬件相关处理机。2003年上海天文台自行研制了基于PC技术的VLBI数据记录、回放系统，命名为CVN硬盘系统，并成功将其安置于CVN观测站和处理机系统。硬件处理机经过改造后，已能处理来自硬盘和原有磁带系统的数据．从2003年至今，中国VLBI网采用该硬盘系统进行了多次VLBI观测和e-VLBI试验。在CVN硬盘系统基础上，软件相关处理技术的研究也得以开展。软件相关处理原型程序已经被用于台站条纹检测、卫星条纹搜索和数据处理中。该软件获得的计算结果被成功用于国内第一个3台站卫星VLBI的延迟和延迟率闭合试验，以及国内首次利用VLBI数据进行的卫星定轨试验。除此之外，该软件还用作硬件处理机的条纹引导器。为适应未来“嫦娥”月球探测工程，CVN将扩展成含有4个观测站和2个相关处理机（硬件、软件）的实时VLBI网。今后，e-VLBI将被应用于月球卫星导航以及测地和天体物理的VLBI观测。     

HAXTEL: A Laue lens telescope development project for a deep exploration of the hard X-ray sky (> 60 keV)

A review of the HAXTEL project devoted to the development of a Laue lens telescope for hard X-/gamma-ray observation of the continuum spectra of celestial sources is presented. Main design properties, open issues, the status of the project and an example of multi-lens configuration with sensitivity expectations are discussed.     

基于测井频谱分析的松科二井登娄库组地层沉积速率研究

松辽盆地科学钻探工程松科二井获取了白垩纪陆相沉积资料, 其中连续、多参数、高分辨率的地球物理测井资料为研究松辽盆地地层的沉积速率变化规律提供了机会。本文利用GR、Th、K、Th/K多种测井数据, 采用天文旋回的方法来计算松科二井登娄库组地层的沉积速率, 并探讨影响地层沉积的主控因素。多种测井数据的频谱分析结果表明了登娄库组地层记录着米兰科维奇旋回信息, 这说明登娄库组沉积过程受天文轨道驱动力影响。Th测井数据对天文旋回信息的敏感性强, 综合考虑多种测井数据的测试结果获得了连续、相对准确的地层沉积速率。登娄库组地层沉积速率从下往上整体呈现为由高到低的趋势。 登二段至登三段时期地层沉积主要受盆地断陷活动控制, 地层整体具有高沉积速率特征, 最高达到 16.2 cm/ka。随后至登四段时期由于断陷活动逐渐减弱, 盆地向区域坳陷的构造格局转化, 登四段整体具有沉积速率较低的特征, 最低为5.9 cm/ka。该研究建立了松科二井登娄库组地层连续的沉积速率剖面, 为揭示松辽盆地由断陷活动过渡到坳陷活动的地质规律提供了测井证据。     

一种亮星识别算法及其在天文定向中的应用

基于全站仪对任意亮星的观测采样,提出了一种利用高度角序列和水平角速率进行联合匹配的任意亮星识别算法。通过引入天体地平坐标计算程序,算法可正确辨别行星和恒星。本文分析了任意亮星高度角和水平角速率的观测误差和计算误差,以此给出了匹配阈值条件的设定依据,并在此基础上制定了有效的匹配策略。仿真计算及实际观测试验均表明,该算法具有100%的识别成功率,远优于现有算法。将此算法应用于任意亮星天文定向,定向结果的内符合精度达到2″,外部检核精度达到1.6″。采用多颗任意亮星进行定向,可有效减弱由测站位置误差引入的定向系统误差,提高绝对定向精度。本文提出的天文定向适用于多云及雾霾天气。     

Digitization of sunspot drawings by Spörer made in 1861–1894

Most of our knowledge about the Sun's activity cycle arises from sunspot observations over the last centuries since telescopes have been used for astronomy. The German astronomer Gustav Spörer observed almost daily the Sun from 1861 until the beginning of 1894 and assembled a 33‐year collection of sunspot data covering a total of 445 solar rotation periods. These sunspot drawings were carefully placed on an equidistant grid of heliographic longitude and latitude for each rotation period, which were then copied to copper plates for a lithographic reproduction of the drawings in astronomical journals. In this article, we describe in detail the process of capturing these data as digital images, correcting for various effects of the aging print materials, and preparing the data for contemporary scientific analysis based on advanced image processing techniques. With the processed data we create a butterfly diagram aggregating sunspot areas, and we present methods to measure the size of sunspots (umbra and penumbra) and to determine tilt angles of active regions. A probability density function of the sunspot area is computed, which conforms to contemporary data after rescaling. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)