[abridged] Stars are thought to be formed predominantly in clusters. The clusters are formed following a cluster initial mass function (CMF) similar to the stellar initial mass function (IMF). Both the IMF and the CMF favour low-mass objects. The numerous low-mass clusters will lack high mass stars. If the integrated galactic initial mass function originates from stars formed in clusters, the IGIMF could be steeper than the IMF. We investigate how well constrained this steepening is and how it depends on the choice of sampling method and CMF. We compare analytic sampling to several implementations of random sampling of the IMF, and different CMFs. We implement different IGIMFs into GALEV to obtain colours and metallicities for galaxies. Choosing different ways of sampling the IMF results in different IGIMFs. Depending on the lower cluster mass limit and the slope of the cluster mass function, the steepening varies between very strong and negligible. We find the size of the effect is continuous as a function of the power-law slope of the CMF, if the CMF extends to masses smaller than the maximum stellarmass. The number of O-stars detected by GAIA might help in judging on the importance of the IGIMF effect. The impact of different IGIMFs on integrated galaxy photometry is small, within the intrinsic scatter of observed galaxies. Observations of gas fractions and metallicities could rule out at least the most extreme sampling methods. As we still do not understand the details of star formation, one sampling method cannot be favoured over another. Also, the CMF at very low cluster masses is not well constrained observationally. These uncertainties need to be taken into account when using an IGIMF, with severe implications for galaxy evolution models and interpretations of galaxy observations.
Spectrum Syntheses of High Resolution Integrated Light Spectra of Galactic Globular Clusters
本文给出了银河系球状星团47 Tuc、M3、M13、NGC 7006和M15的高分辨积分光谱中Mg、Na和Eu三种元素的光谱合成，以及太阳和大角星光谱的定标合成。铁丰度的目标集群也来自集成光等效宽度分析。在仔细考虑原子和分子光谱特征后，这五个球状星团光谱中的线轮廓非常合适，提供的精度水平优于相同积分光谱的等效宽度分析，并且与单个恒星分析的精度相当。来自5528和5711 A Mg I线、6154和6160 A Na I线以及6645 A Eu II线的积分光丰度落在单个恒星的观测范围内;然而，这些积分光丰度并不总是与文献中的平均丰度一致。用第二个参数簇M3、M13和NGC 7006进行的测试表明，假设不正确的水平分支形态可能对这些Mg、Na和Eu丰度只有很小的影响（< 0.06 dex）。因此，这些测试表明，集成的光谱合成可以应用于未解决的球状星团在很宽的范围内的金属丰度和水平分支形态。这种高精度的综合光谱合成对于解释其他星系周围球状星团系统的化学丰度是有价值的。
A spectroscopic map of the Galactic centre: Integrated light and dynamical modelling
University of Vienna（维也纳大学）；SDB Science-driven Business Ltd.（SDB科学驱动商业有限公司）；Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa（里斯本大学空间与天体物理研究所）
利用DYNAMITE代码对银河系中心内~3 pc x 66 pc区域的恒星视线运动学进行三轴轨道动力学建模，成功恢复Sgr A*质量并约束质量分布和轨道分布。
A new catalog of homogenised absorption line indices for Milky Way globular clusters from high-resolution integrated spectroscopy
我们对24个银河系球状星团进行了综合光谱分析。从一个核心半径的光谱观察到每个集群与高波长分辨率~2.0 A的FWHM。结合Puzia et al.（2002）和Schiavon et al.（2005）的两个现有数据集，我们构建了一个包含53个银河系球状星团的Lick光谱指数的大型数据库，这些球状星团具有广泛的金属丰度范围，-2.4 < [Fe/H] < 0.1，以及各种水平分支形态。经验指数到金属丰度的转换关系提供了20舔指数用于推导金属丰度的远程，未解决的恒星系统。
Deciphering the radio star formation correlation on kpc scales II. The integrated infrared-radio continuum and star formation - radio continuum correlations
Prescriptions for the stochasticity effect on the integrated X-ray luminosity of star-forming galaxies:Implications for selecting star-forming galaxies and AGN in X-ray surveys
University of Crete（克里特大学）；Foundation for Research and Technology-Hellas（希腊研究与技术基金会）；Max-Planck-Institut für Extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（ICE，CSIC））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院（IEEC））
Candidates for the most [$O_{III}$] $\lambda5007$-luminous planetary nebula in the Milky Way. I. Integrated light properties of NGC 6572, NGC 6884, and M 1-71
Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦阿斯特罗物理研究所）；Institut für Physik und Astronomie, Universität Potsdam（波茨坦大学物理与天文学研究所）；Deutsches Zentrum für Astrophysik (DZA)（德国天体物理学中心）；European Southern Observatory（欧洲南方天文台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）
