Narrow-band CCD photometry of giant H ii regions

We have obtained accurate CCD narrow-band Hβ and Hα photometry of giant H  ii regions (GEHRs) in M33, NGC 6822 and M101. Comparison with previous determinations of emission-line fluxes shows large discrepancies; their probable origins are discussed. Combining our new photometric data with global velocity dispersion ( σ ) derived from emission linewidths, we review the     relation. A re-analysis of the properties of the GEHRs included in our sample shows that age spread and the superposition of components in multiple regions introduce a considerable spread in the regression. Combining the information available in the literature regarding ages of the associated clusters, evolutionary footprints on the interstellar medium, and kinematical properties of the knots that build up the multiple GEHRs, we find that a subsample – which we refer to as young and single GEHRs – do follow a tight relation in the     plane.     

Hubble Space Telescope photometry of globular clusters in the Sombrero galaxy

We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the 'Sombrero' (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the >99 per cent confidence level, with peaks at     and     . The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ∼2 pc with the red ones being ∼30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.     

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.     

M31的观测与研究进展

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。     

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

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.     

自动推算室内接入点坐标算法

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。     

2022年1月8日青海门源6.9级地震的震源区结构特征和b值意义初探

2022年1月8日1时45分青海省门源县发生M_S6.9地震.本文基于青藏高原东北缘水平分辨率为0.3°的地震层析成像结果,获取了震源周边区域的地壳浅部构造信息,包括波速、泊松比以及估计的裂隙密度和饱和率的空间分布.结果表明:此次门源M_S6.9地震发生在P波和S波波速剧烈变化的区域,靠近高速体的边缘.泊松比和饱和率同样都显示,门源M_S6.9地震发生在高低值变化的过渡区.地震活动参数分析显示,震前冷龙岭断裂带的震源周边区域显示出了低b值、较低的a值和高a/b值的特征,与龙门山—岷山构造带强震之前的情况类似.裂隙密度在冷龙岭断裂两侧呈现出显著差异,北侧高于南侧,这可能是震后现场科考发现的断裂带地表破裂北侧高于南侧的构造成因.     

2022年门源MS6.9地震震区三维速度与发震机制研究

2022年1月8日,青海省门源县发生M_S6.9地震。使用青海、甘肃等区域数字台网所观测到的2009年1月1日—2022年2月8日间青海门源及周边地区(36°～39°N,101°～104°E)14 869次地震事件的地震观测资料,基于双差成像(TomoDD)方法进行重定位分析,结果表明：门源及周边地区地震震源深度较浅,主要集中在5～15 km深度范围,其中10 km附近分布最多。推断该深度区域为门源及周边地区的主要孕震区。基于地震重定位结果和主震区三维速度结构分别对2016年门源M_S6.4地震和此次地震序列的发震机理进行分析对比,发现两次地震都位于高速异常体边缘,速度结构与断裂、地震序列吻合较好。2022年门源地震位于高速体的西端末梢位置,是该高速体受青藏高原东北缘顺时针应力作用导致的滑动产生的走滑型地震。     

以门源M6.9地震为契机的祁连带中东段地震热红外异常区域特征研究

以中国静止气象卫星亮温资料为数据基础,使用小波变换和功率谱估计法研究2022年1月8日门源M6.9地震前的热辐射异常,并对祁连带中东段以往震例的热辐射异常作回溯性研究。门源6.9级地震的热辐射异常发展过程可分为3个阶段：初始演化阶段、增强持续阶段、减弱消失阶段。面积最大时强辐射区的面积约为8万km~2,地震发生在其西北部。相对功率谱峰值为平均值的17倍,地震发生在峰值后82天。大面积、高强度的热辐射状态持续时间长是此次异常的显著特点。祁连带中东段的几次地震前均出现过热辐射异常,其特征可为该区震情判定不断积累经验,以期形成可作为判定指标的区域震例库。     

2022年门源MS 6.9地震序列特征及强余震判定

2022年1月8日青海门源发生M_S 6.9地震,基于青海地震台网对此次地震序列时空演化特征进行分析。结果表明,门源地震序列的空间展布整体上呈西段NWW、东段SE向的带状分布,且序列衰减较缓慢。另外,基于同一构造历史地震类比、h值、等待时间法等进行分析,认为门源M_S 6.9地震序列为主—余型;根据祁连地震带中东段5级以上地震最大余震发震时间统计和震级差特征分析认为,门源M_S 6.9地震的最大余震已经发生,即2022年1月12日18时20分的M_S 5.2地震。