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

Witold Maciejewski  James Binney 《Monthly notices of the Royal Astronomical Society》2001,323(4):831-838

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.  相似文献   

M31的观测与研究进展     

孙振娜  侯金良  常瑞香  陈力 《天文学进展》2004,22(2):163-178

介绍了本星系群中最大的旋涡星系M31(仙女星系)的基本观测性质。与银河系结构类似，M31的基本成分包括：核、核球、盘和晕。对以上各个成分的观测和研究进展分别作了综述，重点是盘的星族成分和恒星形成历史，以及球状星团的分布和晕的形成历史。同时与银河系的各种观测特征和形成机制作了详细的比较。  相似文献   

Characterization of a chalcopyrite from Brazil by Mössbauer spectroscopy and other physicochemical techniques     

W. N. Mussel  E. Murad  J. D. Fabris  W. S. Moreira  J. B. S. Barbosa  C. C. Murta  W. P. Abrahão  J. W. V. De Mello  V. K. Garg 《Physics and Chemistry of Minerals》2007,34(6):383-387

We studied a chalcopyrite from a Cu ore deposit in Rio Grande do Sul, Brazil, by Mössbauer spectroscopy at room temperature and 110 K. Supporting methods to check for sample purity and to characterize further sample properties were slow-scanning X-ray powder diffraction and optical and microprobe analyses of polished sections of selected grains. Chemical analyses obtained using a scanning electron microscope equipped with an energy-dispersive X-ray spectrometer showed the sample to consist of homogeneous and essentially stoichiometric chalcopyrite (CuFeS₂). Mössbauer spectra taken at both the above temperatures consist of asymmetric magnetically ordered patterns with unequal intensities of the line pairs 1–6 and 2–5, pointing to the existence of non-equivalent or multiple Fe sites. Least-squares fittings evidenced that the resonance intensity ratio of subspectrum with lower quadrupole shift (indicative of a more symmetric environment) to that with higher shift is 69:31, at room temperature, and 68:32, at 110 K. Rietveld refinement of the XRD data indicates the existence of tetragonal [a = 0.52855(1) and c = 1.0412(1) nm] and cubic [a ₀ = 0.5273(2) nm] modifications in a proportion of 74:26, in good agreement with the Mössbauer data. The saturation magnetization of the sample was 32.7 J/(T kg), confirming the oxidation state of Fe as trivalent and pointing to little to no spin canting.  相似文献   

自动推算室内接入点坐标算法   总被引：2，自引：1，他引：1  

郑加柱  高业何敏 《测绘通报》2018,(2):21-24,29

随着基于位置服务的应用与发展,室外和室内定位技术都得到了飞速发展。特别是在WiFi定位技术的不断完善下,室内定位技术有了广泛的应用,但是,WiFi定位技术的两种定位方式均需预先知道室内网络接入点的精确坐标,这一要求无法满足一些紧急情况下的定位需求。因此,本文提出了一种基于M估计的自动推算室内接入点坐标算法。该算法借助在室内外交界处同时获取卫星定位信息和WiFi信号的RSSI信息,巧用分段RSSI测距算法提高长距离RSSI测距精度,结合残差绝对和最小的M估计改进距离交会定位算法,最终推算出室内接入点的三维坐标,实现自动化推算过程。试验结果表明：该方法的定位精度比常规距离交会最小二乘算法提高了50%,能够快速实时较精确地推算室内接入点的坐标,进一步完善了WiFi定位技术。  相似文献   

中国大陆7级以上地震频次场时空异常特征     

罗国富  屠泓为  丁风和  马禾青  杨明芝 《地震》2022,42(1):181-196

本文以地震频次作为地震活动的变量, 通过自然正交函数展开方法, 计算中国大陆7级以上强震前的地震活动频次场, 提取出强震前时间因子和空间等值线的异常。 结果表明, 强震前时间因子出现超过均方差的高值或低值异常, 异常多数分布在频次场的前4个典型场, 具有多分量特点, 第1个典型场异常贡献率最大(占总场40%～60%), 绝大部分强震前5～8年出现长期异常, 部分强震前1～2年出现中期异常, 少数强震前3月出现短临异常的特征。 区域频次等值线出现的高梯度旋涡区域是异常危险区, 等值线值大于0.9且具有活动构造的危险区往往是强震的发震位置。 另外, 地震频次场与传统方法的区域地震活动频次(3月)震例对比, 表明频次场时间因子异常具有自己的独特优越性和缺陷, 并讨论了这些方法的差异性。  相似文献   

基于遥感的上海地区雾霾监测研究     

戴羊羊  李成范  周时强  赵俊娟  尹京苑 《测绘工程》2015,(12):29-32

以中分辨率成像光谱仪(MODIS)遥感数据为数据源,综合利用6S传输模型与NASA V5.2算法对2013年12月4日至8日上海地区雾霾污染进行了连续性监测,并对其形成原因进行分析。结果表明,此次雾霾污染主要是由本地生产和外地迁移来源共同作用形成,上海地区气溶胶光学厚度在12月6日达到最大,雾霾污染区域逐渐从上海地区的西北向东南扩散,污染等级也逐渐降低。  相似文献   

海岸线及其测绘技术探讨   总被引：1，自引：0，他引：1  

于彩霞  许军  黄文骞  卢岩  林林 《测绘工程》2015,(7):1-5

海岸线是人类所使用的最古老的边界线之一,然而,由于其动态特征,加之当今社会对海岸带的需求越来越多,这条边界线的位置存在争议,因而,如何使用客观手段测绘海岸线尤为重要。文中针对海岸线定义及其位置确定不明确的现状,指出海岸线定义存在的问题,给出完善定义的意见;分析海岸线常规的测绘方法,探讨海岸线精确测绘的新方法和技术。  相似文献   

陕北奥陶纪盐盆马五6时期东、西部盐坳沉积环境对比研究     

樊馥  张永生  郑绵平  苏奎  邢恩袁 《地质学报》2015,89(11):2141-2151

陕北奥陶纪盐盆位于鄂尔多斯盆地伊陕斜坡东部。研究表明:马五6亚期,盐盆存在"两坳一隆"的构造格局,即东、西部盐坳和中部隆起,东、西部盐坳在钾矿化情况、溴氯系数反映的水体咸化趋势方面初步显示了陕北盐盆东、西部沉积环境的差异。本文通过东、西部盐坳典型钻井马五6层位沉积学分析,揭示了马五6时期东、西部盐坳在水体深度变化、浓缩趋势、含钾量、淡化层段厚度、陆源物质输入方面均存在差异。其中,西部盐坳受海水影响大,水体变浅且持续淡化,泥质分布反映陆源物质贡献少,对钾盐的沉积与保存均十分不利。而东部盐坳受海水影响小,与西部盐坳水体联通性差,在马五6时期环境更为封闭,具体表现为淡化夹层分布数量少、厚度薄的特征;水体持续变深并浓缩咸化;泥质夹层较多,反映了相较于西部,陆源物质对其影响更大,上述特点为钾盐沉积提供了有利的地球化学条件及可容空间。东、西部盐坳沉积环境对比表明东部盐坳对成钾更为有利。  相似文献   

Masses of the local group and of the M81 group estimated from distortions in the local velocity field     

I. D. Karachentsev  O. G. Kashibadze 《Astrophysics》2006,49(1):3-18

Based on high precision measurements of the distances to nearby galaxies with the Hubble telescope, we have determined the radii of the zero velocity spheres for the local group, R₀ = 0.96±0.03Mpc, and for the group of galaxies around M 81/M 82, 0.89±0.05Mpc. These yield estimates of M_T = (1.29±0.14)· 10¹² M_⊙ and (1.03±0.17)· 10¹² M_⊙, respectively, for the total masses of these groups. The R₀ method allows us to determine the mass ratios for the two brightest members in both groups, as well. By varying the position of the center of mass between the two principal members of a group to obtain minimal scatter in the galaxies on a Hubble diagram, we find mass ratios of 0.8:1.0 for our galaxy and Andromeda and 0.54:1.00 for the M82 and M81 galaxies, in good agreement with the observed ratios of the luminosities of these galaxies. __________ Translated from Astrofizika, Vol. 49, No. 1, pp. 5–22 (February 2006).  相似文献   

Unravelling the mystery of the M31 bar     

E. Athanassoula  Rachael Lynn Beaton 《Monthly notices of the Royal Astronomical Society》2006,370(3):1499-1512

The inclination of M31 is too close to edge-on for a bar component to be easily recognized and is not sufficiently edge-on for a boxy/peanut bulge to protrude clearly out of the equatorial plane. Nevertheless, a sufficient number of clues allow us to argue that this galaxy is barred. We use fully self-consistent N -body simulations of barred galaxies and compare them with both photometric and kinematic observational data for M31. In particular, we rely on the near-infrared photometry presented in a companion paper. We compare isodensity contours to isophotal contours and the light profile along cuts parallel to the galaxy major axis and offset towards the north, or the south, to mass profiles along similar cuts on the model. All these comparisons, as well as position–velocity diagrams for the gaseous component, give us strong arguments that M31 is barred. We compare four fiducial N -body models to the data and thus set constraints on the parameters of the M31 bar, as its strength, length and orientation. Our 'best' models, although not meant to be exact models of M31, reproduce in a very satisfactory way the main relevant observations. We present arguments that M31 has both a classical and a boxy/peanut bulge. Its pseudo-ring-like structure at roughly 50 arcmin is near the outer Lindblad resonance of the bar and could thus be an outer ring, as often observed in barred galaxies. The shape of the isophotes also argues that the vertically thin part of the M31 bar extends considerably further out than its boxy bulge, that is, that the boxy bulge is only part of the bar, thus confirming predictions from orbital structure studies and from previous N -body simulations. It seems very likely that the backbone of M31's boxy bulge is families of periodic orbits, members of the x₁-tree and bifurcating from the x₁ family at its higher order vertical resonances, such as the x1v3 or x1v4 families.  相似文献