我们报告了对高度r过程增强（r-II）恒星CS 29497-004的丰度分析，这是一颗非常贫金属的巨星，Teff = 5013 K，[Fe/H]=-2.85，其性质最初是在HERES项目过程中发现的。我们的分析是基于高信噪比，高分辨率（R~75000）的VLT/UVES光谱和MARCS模式大气的假设下，当地的热力学平衡，并获得了丰度测量共46个元素，其中31个是中子俘获元素。与目前已知的其他25颗r-II型恒星一样，CS 29497-004的重元素丰度模式与太阳系第二个r-过程元素丰度峰值模式非常匹配。我们确认我们以前的检测Th，并证明这颗星不表现出“锕系元素的提升”。铀也被探测到（log e（U）=-2.20+/-0.30），尽管有很大的测量误差，阻碍了它作为精密宇宙计时器的使用。结合这颗恒星现有的各种元素精密时计对，我们使用等待点近似模型的理论生产率得出平均年龄为12.2+/-3.7 Gyr（Kratz et al. 2007）。我们进一步探讨了高熵风模型（Farouqi et al. 2010）中不同的中子丰度（Y_e）所产生的产生率，并得出最佳拟合Y_e=0.447时的年龄为13.7+/-4.4 Gyr。U/Th核计时器被证实是最能适应理论生产率的，并得出16.5+：-6.6 Gyr的年龄。在CS 29497-004中也初步检测到铅（Pb），其水平与太阳r过程的比例一致，或者与该恒星纯r过程的理论预期一致。
英文摘要：
We report an abundance analysis for the highly r-process-enhanced (r-II) star CS 29497-004, a very metal-poor giant with Teff = 5013K and [Fe/H]=-2.85, whose nature was initially discovered in the course of the HERES project. Our analysis is based on high signal-to-noise, high-resolution (R~75000) VLT/UVES spectra and MARCS model atmospheres under the assumption of local thermodynamic equilibrium, and obtains abundance measurements for a total of 46 elements, 31 of which are neutron-capture elements. As is the case for the other 25 r-II stars currently known, the heavy-element abundance pattern of CS 29497-004 well-matches a scaled Solar System second peak r-process-element abundance pattern. We confirm our previous detection of Th, and demonstrate that this star does not exhibit an "actinide boost". Uranium is also detected (log e(U) =-2.20+/-0.30), albeit with a large measurement error that hampers its use as a precision cosmo-chronometer. Combining the various elemental chronometer pairs that are available for this star, we derive a mean age of 12.2+/-3.7 Gyr using the theoretical production ratios from waiting-point approximation models (Kratz et al. 2007). We further explore the high-entropy wind model (Farouqi et al. 2010) production ratios arising from different neutron richness of the ejecta (Y_e), and derive an age of 13.7+/-4.4 Gyr for a best-fitting Y_e=0.447. The U/Th nuclei-chronometer is confirmed to be the most resilient to theoretical production ratios and yields an age of 16.5+:-6.6 Gyr. Lead (Pb) is also tentatively detected in CS 29497-004, at a level compatible with a scaled Solar r-process, or with the theoretical expectations for a pure r-process in this star.
HE0144-4657: A Carbon-Enhanced Ultra Metal-Poor Star ([Fe/H] ~ -4.1) from the Helmi Stream Disrupted Dwarf Galaxy
NSF NOIRLab（美国国家光学红外天文科学实验室）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Department of Astronomy & Astrophysics, University of Chicago（芝加哥大学天文与天体物理系）；Randolph School（兰道夫学校）；Zentrum für Astronomie der Universität Heidelberg, Landessternwarte（海德堡大学天文中心，州立天文台）
Chemical Abundances in the Metal-Poor Globular Cluster ESO 280-SC06: A Formerly Massive, Tidally Disrupted Globular Cluster
University of Chicago（芝加哥大学）；Syracuse University（雪城大学）；University of New South Wales（新南威尔士大学）；University of Toronto（多伦多大学）；Carnegie Institution for Science（卡内基科学促进会）；University of Florida（佛罗里达大学）
Metal-Poor Stars Observed with the Magellan Telescope I. Constraints on Progenitor Mass and Metallicity of AGB Stars Undergoing s-Process Nucleosynthesis
The Gaia-ESO Survey: A new approach to chemically characterising young open clusters II. Abundances of the neutron-capture elements Cu, Sr, Y, Zr, Ba, La, and Ce
X-ray stellar feedback in low-metallicity starbursts: Insights from the template starburst galaxy ESO 338-IG04 and its halo
Institute for Physics and Astronomy, University of Potsdam（波茨坦大学物理与天文学研究所）；Department of Physics, University of Arkansas（阿肯色大学物理系）；Arkansas Center for Space and Planetary Sciences, University of Arkansas（阿肯色大学阿肯色空间与行星科学中心）；Department of Astronomy, The Oskar Klein Centre, Stockholm University（斯德哥尔摩大学奥斯卡·克莱因中心天文学系）；Centro de Astrobiología (CAB), INTA–CSIC（西班牙国家航空航天技术研究所-西班牙国家科学研究委员会天体生物学中心）；Department of Astronomy, U. Wisconsin-Madison（威斯康星大学麦迪逊分校天文学系）；ESA, ESAC（欧洲空间局欧洲空间应用与技术中心）
通过研究低金属licity恒星burst星系ESO 338-IG04，发现X射线源对电离光子预算的影响，并预测He II λ4686发射的亮度。
Tracing the early Milky Way thin disc with the Gaia-ESO Survey
Institute of Theoretical Physics and Astronomy, Faculty of Physics, Vilnius University（维尔纽斯大学物理学院理论物理与天体物理研究所）；INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze（佛罗伦萨大学物理与天文学系）
The T-GEX project. I. Stealth UV-bright Sun-like stars in the Galaxy as candidate contributors to the UV upturn
Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所 - 阿切尔奇天文台）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文中心）；Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo（圣保罗大学天文、地球物理与大气科学研究所）
High Resolution (<100pc) Ionization Structures in the ISM of AGN ESO~137-G34
Astronomical Observatory of the Jagiellonian University（雅盖隆大学天文台）；NASA-Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；Newcastle University（纽卡斯尔大学）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理学研究所）
