Spectroscopic study of the peculiar galaxy UGC 5119

We present the results of our study of the stellar kinematics in the elliptical galaxy UGC 5119, which has previously been suspected to be a polar-ring galaxy. We have detected a rapidly rotating disk in the central region (r ≤ 3.2 kpc) of the galaxy’s main body and found a radial velocity gradient along its minor axis (in the putative ring). We conclude that UGC 5119 is a medium-luminosity elliptical galaxy with a rapidly rotating disk component and a stellar (probably polar) ring. We have calculated the Lick indices of the Hβ, Mggb, Fe 5270, and Fe 5335 absorption lines and compared them with evolutionary synthesis models. Differences in the [Mg/Fe] ratios, metallicities, and ages of the stars have been found: the young stellar population with a solar [Mg/Fe] ratio and a high metallicity dominates in the circumnuclear region (r ≤ 1 kpc), while the old one with a low metal abundance dominates in the ring.     

融合点、对象、关键点等3种基元的点云滤波方法

基元是影响点云滤波精度和效率的关键因素之一。本文提出了一种基于多基元的三角网渐进加密(MPTPD)滤波方法。它包括点云分割、对象关键点提取、基于关键点的对象类别判别3个主要阶段,且3个阶段的基元分别为点、对象、关键点。使用了4景机载激光雷达和摄影测量点云数据对MPTPD、三角网渐进加密(TPD)、基于对象的三角网渐进加密(OTPD)3种滤波方法进行了性能测试。试验表明,MPTPD方法具有整体上最优的性能:在精度方面,MPTPD与OTPD两种方法的精度相当,MPTPD方法的一类误差I、总误差T比TPD的相应误差分别低约22.07%和8.44%;在效率方面,多数情况下TPD、MPTPD、OTPD方法的效率依次降低,且MPTPD的平均耗时是OTPD平均耗时的57.93%。     

The irregular galaxy Cassiopeia 1 – a new member of the Local group

A photometry in the V, R, I (Cousins) system has been performed for stars in the galaxy Cassiopeia 1. The resulting colour-agnitude (CM) diagram of Cas 1 reveals the existence of blue stars and the absence of red ones. From an analysis of the CM diagram of the galaxy it is concluded that A_v = 4.0 mag, and the distance modulus (m – M)_o = 24.5 mag, corresponding to a distance of 790 kpc. The visual magnitude of the galaxy is V = 14^m.62 (M_v = −13^m.8) and the colour index (V – R) = 0.89 mag. From the distance determination the galaxy Cassiopeia 1 is a member of the Local group.     

Photo—gravitational effects in the two—body problem

The effect of the radiation-pressure in the problem of the two bodies is analysed. It is found that such an effect is the same as that of reducing the stellar mass, m, by the factor p (0 ≤ p ≤ 1). The case p < 0 leads to stellar instability and, consequently, it is not considered here. The problem of the mass determination from spectroscopic observations is reviewed and an iterative method is recommended.     

Photographic photometry for stellar statistics with Tautenburg Schmidt telescope

Photometric properties of deep Tautenburg Schmidt plates in the UBV system over the whole field and over a wide range of stellar magnitudes are discussed. Different reduction models based on the calibration curve alone and with additional terms containing colour and plate coordinates are considered. With the filter-emulsion combinations used the Johnson UBV system can be reproduced quite well by the Tautenburg telescope. The accuracy of photometric data can be improved if geometrical terms are taken into account. For deep plates with a significant effect of background nebulosity a supplementary term is to be included in the reduction model. The polynomial coefficients vary in dependence on spectral bands and individual properties of each plate.     

面向对象空间数据组织与管理的初步实现

通过分析3种传统数据模型的特点,得出它们在管理地理复杂对象方面的局限性,从而引出了面向对象数据模型。本文利用面向对象数据模型中的各种操作,以基本地理对象为基础构建复杂地理对象,并且在VC 6.0平台上实现了面向对象几何数据模型。     

Stellar populations and dust in the galaxy NGC 2976, a low-luminosity member of the M81 group

Photographic UBV photometry of NGC 2976, a low-luminosity member of the central M81 group of galaxies, is presented. Young stars in the central disk determine the optical view and the classification of this Sc(pec) galaxy. It is surrounded by a halo of an old population which contains nearly all the mass and half the luminosity of the system. This halo has some properties typical of spheroidal dwarf galaxies: an exponential brightness profile, an ellipticity trend of the isophotes typical of low-mass systems, and mass and luminosity near the upper limit of typical dwarfs. In the central population I disk, star formation proceeds in dense associations scattered irregularly in a broad ringlike region of 1.2 kpc radius just inside the turnover of the rotation curve. This star formation episode may last since some 10⁸ a; it is possibly triggered by gas infall from the interstellar cloud generated during encounters between other group members in the central M81 group. A direct triggering by recent encounters is excluded since NGC 2976 is undisturbed in its outer parts.     

珠母贝人工繁育优化技术的研究

在室内水泥池分别进行了移池培育、不同种类附着器、光照强度、水流和冲洗对珠母贝附着幼虫变态和稚贝存活的研究,结果表明:附着密度为2.18个/cm~2±0.50个/cm~2时,移池培育,其变态幼虫密度为0.95个/cm~2±0.13个/cm~2,20 d稚贝存活密度0.41个/~2±0.08个/cm~2,移池培育显著提高附着幼虫变态和稚贝存活;附着板、附着绳、网片、小石块变态幼虫密度分别为0.70个/cm~2±0.08个/cm~2、1.38个/cm~2±0.15个/cm~2、0.97个/cm~2±0.12个/cm~2、1.04个/cm~2±0.28个/cm~2,稚贝存活密度分别为0.36个/cm~2±0.06个/cm~2、0.62个/cm~2±0.07个/cm~2、0.45个/cm~2±0.07个/cm~2、0.60个/cm~2±0.08个/cm~2,附着绳显著提高附着幼虫变态和稚贝存活;光照强度为300～600 lx时变态幼虫密度为0.87个/cm~2±0.07个/cm~2,20 d稚贝存活密度0.45个/cm~2±0.08个/cm~2,强光不利于幼虫的变态和稚贝存活;水流速为2.3 cm/s时变态幼虫密度为1.08个/cm~2±0.07个/cm~2,20 d稚贝存活密度0.87个/cm~2±0.07个/cm~2,冲洗的变态幼虫密度为1.64个/cm~2±0.19个/cm~2,20 d稚贝存活密度1.00个/cm~2±0.12个/cm~2,水流或冲洗显著提高附着幼虫变态和稚贝存活.