In this paper we present a photometric and spectroscopic study of the nearby galaxy cluster Abell 0671 (A671) with 15 intermediate-band filters in the Beijing-Arizona-Taiwan-Connecticut (BATC) system and the Sloan Digital Sky Survey (SDSS) data. The photometric redshift technique is applied to the galaxy sample for further membership determination. After the color-magnitude relation is taken into account, 97 galaxies brighter than h_batc=19.5 mag are selected as new member galaxies. Based on the enlarged sample of cluster galaxies, spatial distribution, dynamics of A671 are investigated. The substructures of A671 are well shown by the sample of bright members, but it appears less significant based on the enlarged sample, which is mainly due to larger uncertainties in the light-of-sight velocities of the newly-selected faint members. The SDSS r-band luminosity function of A671 is flat at faint magnitudes, with the faint end slope parameter alpha=-1.12. The SDSS spectra allow us to investigate the star formation history of bright cluster galaxies, and the galaxies in the core region are found to be older than those in the outskirts. No environmental effect is found for metallicities of the early-type galaxies (ETGs). The positive correlation between age and stellar mass supports the downsizing scenario. By comparing ETG absorption-line indices with the state-of-art stellar population models, we derive the relevant parameters of simple stellar population (such as age, [Fe/H], [Mg/Fe], [C/Fe], [N/Fe], and [Ca/Fe]). The ETGs at cluster center tend to have smaller hb indices, indicating that central ETGs are likely to be older. The distribution of total metallicity indicator, [MgFe]', does not show any environmental effects. The relations between the simple stellar population parameters and velocity dispersion in A671 are in good agreement with previous studies.
Hubble Frontier Field Photometric Catalogues of Abell 370 and RXC J2248.7-4431: Multiwavelength photometry, photometric redshifts, and stellar properties
A New Perspective on Galactic Evolution: Studying the Outskirts of the Abell S1063 Galaxy Cluster
Università di Salerno（萨莱诺大学）；INAF – Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；INFN – Gruppo Collegato di Salerno - Sezione di Napoli（意大利国家核物理学院萨莱诺协作组-那不勒斯分部）；INAF – IASF Milano（意大利国家天体物理研究所米兰天文与空间物理研究所）；Dipartimento di Fisica dell’Università degli Studi di Trieste – Sezione di Astronomia（的里雅斯特大学物理系天文学分部）；INAF – Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；Institute of Cosmology and Gravitation, University of Portsmouth（朴茨茅斯大学宇宙学与引力研究所）
The ALMA Frontier Fields Survey III: 1.1 mm Emission Line Identifications in Abell 2744, MACSJ0416.1-2403, MACSJ1149.5+2223, Abell 370, and Abell S1063
迄今为止，大多数对星系亚毫米发射线的研究都是针对具有已知红移的源，其中线的频率受到很好的限制。最近的盲线扫描规避了光谱红移的要求，这可能代表了选择偏差。我们的目标是检测连续谱定向观测中存在的发射线。这些谱线的探测提供了光谱红移和星系的性质。我们进行搜索的发射线在ALMA观测的五个前沿领域集群和评估我们的检测的可靠性，通过关联线候选人与检测到的星系在深近红外成像。我们发现26个显着的发射线候选人，与观测到的线通量之间的0.2-4.6 Jy km s $^{-1}$和速度色散（FWHM）的25-600 km s $^{-1}$。这些候选者中有九个位于近红外光源附近，提高了它们的可靠性;在六种情况下，观察到的线频率和强度与预期一致，因为光度红移和星系对应物的属性。我们提出了红移的鉴定，放大率和分子气体的估计与确定线的星系。我们发现，这些候选人中的两个可能起源于星暴星系，其中之一是水母星系，而另外两个是一致的主序星星系的基础上，在其耗尽时间。这项工作突出的程度，偶然发射线可以发现在大型镶嵌连续观测时，深辅助数据。然而，高显著性线检测的低数量证实了这样的调查不如盲线扫描那样最佳。我们强调，蒙特卡罗模拟应用来评估线检测的意义，因为使用负噪声遭受随机性和招致更大的不确定性。
The ALMA Frontier Fields Survey - II. Multiwavelength Photometric analysis of 1.1mm continuum sources in Abell 2744, MACSJ0416.1-2403 and MACSJ1149.5+2223
S-PLUS Clusters And Large-scale Environments (SCALE): I. A catalog of known clusters and groups in DR5 and a pilot study of Abell 4038
Universidade de São Paulo（圣保罗大学）；Universidade Federal do Rio de Janeiro（里约热内卢联邦大学）；Universidade Estadual de Santa Cruz（圣克鲁斯州立大学）；Universidad de Talca（塔尔卡大学）；Universidad Andrés Bello（安德烈斯·贝略大学）；CONICET-UNLP（阿根廷国家科学研究委员会-拉普拉塔国立大学）；U. Nacional de La Plata（拉普拉塔国立大学）
Validating the ICCF-Cut Method with Simultaneous Photometric and Spectroscopic H$α$ Reverberation Mapping of NGC 4151 and UGC 3374
Peking University（北京大学）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences（中国科学院天体结构与演化重点实验室）；Center for Astronomical Mega-Science, Chinese Academy of Sciences（中国科学院国家天文台）；Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences（中国科学院射电天文与技术重点实验室）
The Grism Lens-Amplified Survey from Space (GLASS). IV. Mass reconstruction of the lensing cluster Abell 2744 from frontier field imaging and GLASS spectroscopy
The merger history of the complex cluster Abell 1758: a combined weak lensing and spectroscopic view
We present a weak-lensing and dynamical study of the complex cluster Abell 1758 (A1758, z = 0.278) supported by hydrodynamical simulations. This cluster is composed of two main structures, called A1758N and A1758S. The Northern structure is composed of A1758NW & A1758NE, with lensing determined masses of 7.90_{-1.55}^{+1.89} X 10^{14} M_ \odot and 5.49_{-1.33}^{+1.67} X 10^{14} M_ \odot , respectively. They show a remarkable feature: while in A1758NW there is a spatial agreement among weak lensing mass distribution, intracluster medium and its brightest cluster galaxy (BCG) in A1758NE the X-ra…
The Spectroscopic and Photometric Study of a Star Cluster Sample in Andromeda Halo
CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台光学天文重点实验室）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；South-Western Institute For Astronomy Research, Yunnan University（云南大学西南天文研究所）；Xi’an Jiaotong-Liverpool University（西交利物浦大学）
A Redshift Survey of the Nearby Galaxy Cluster Abell 2199: Comparison of the Spatial and Kinematic Distributions of Galaxies with the Intracluster Medium
Color Dispersion as an Indicator of Stellar Population Complexity: Insights from the Pixel Color-Magnitude Diagrams of 32 Bright Galaxies in Abell 1139 and Abell 2589
Weak lensing and spectroscopic analysis of the nearby dissociative merging galaxy cluster Abell 3376
The galaxy cluster Abell~3376 is a nearby (z=0.046) dissociative merging cluster surrounded by two prominent radio relics and showing an X-ray comet-like morphology. The merger system is comprised of the subclusters A3376W & A3376E. Based on new deep multi-wavelength large-field images and published redshifts, we bring new insights about the history of this merger. Despite the difficulty of applying the weak lensing technique at such low redshift, we successfully recovered the mass distribution in the cluster field. Moreover, with the application of a two-body model, we have addressed the dyna…
The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma
基于对星系团Abell 2029和后发座星系团的广泛红移观测，我们测量了整个星系团成员星系的光度函数和恒星质量函数。最重要的是，我们测量的速度色散函数（VDFs）的静态成员。MMT/Hectospec红移调查的星系在A2029确定982光谱成员，838名成员，我们得出的中心速度色散的光谱。后发座是唯一一个被调查得如此密集的星团。A2029和Coma的LF、SMF和VDF基本相同。簇的SMF与模拟一致。静止星系的A2029和后发星系的速度色散比场星系的速度色散有一个明显更陡的斜率$\lesssim 100$ km s $^{-1}$。在速度色散$\gtrsim 250$ km s $^{-1}$时，星系团VDFs也超过了磁场。星系团VDF和场VDF之间的差异是对模拟和宇宙结构形成的潜在重要测试。
Quasi-simultaneous Spectroscopic and Multi-band Photometric Observations of Blazar S5 0716+714 during 2018-2019
为了研究$γ$射线耀变体S5 0716+714的短时间尺度光学变率，利用云南天文台丽江天文台2.4 m光学望远镜，于2018年11月至2019年3月进行了准同时光谱和多波段光度观测。所观察到的光谱与幂律$F_λ=Aλ^{-α}$（光谱指数$α>0$）很好地拟合。在$\dotα$、$\dot{A}$、$\dot{A}/A$、$\dot{F_{\rmλ}}$和$\dot{F_{\rmλ}}/F_{\rmλ}$之间发现的相关性与更亮时更蓝（BWB）的趋势一致。\textbf{The same case is for colors, magnitudes, color variation rates, and magnitude variation rates of photometric observations.} $α$的变异导致$F_{\rmλ}$的变异。此外，颜色变化导致幅度变化。观测数据主要分布在坐标系的I（+，+）和III（-，-）象限。光谱和光度观测均表明S50716 +714具有BWB行为。观测到的BWB可以用激波喷流模型来解释，它的出现可能取决于观测频率范围相对于同步加速器峰值频率的相对位置，例如，在峰值频率的左边。\textbf{Fractional variability amplitudes are $F_{\rm{var}}\sim 40\%$ for both…
An Enhanced Catalog of Gaia DR3 Galaxy Candidates with Spectroscopic and Machine-Learning Photometric Redshifts
Seoul National University（首尔大学）；SNU Astronomy Research Center, Seoul National University（首尔大学天文研究中心）；Institute for Data Innovation in Science, Seoul National University（首尔大学数据科学创新研究所）
Measuring galaxy environment with the synergy of future photometric and spectroscopic surveys
我们利用低分辨率光谱学和光度红移之间的协同作用，研究环境对星系演化的影响，从空间的无缝光谱调查。作为一个测试案例，我们考虑未来的欧几里得深调查（~ 40度$^2$），它结合了一个无狭缝光谱调查有限的H $α$通量$\geq5\times 10^{-17}$ erg cm $^{-2}$ s $^{-1}$和测光调查有限的H波段（$H\leq26$）。我们使用欧几里德星系模拟目录，在其中我们锚定的光度红移可用的光谱红移的三维星系分布。然后，我们估计的局部密度对比度的计数对象的半径从1到10 h $^{-1}$ Mpc的红移范围0.9<z<1.8的圆柱形细胞。我们比较这个密度场与一个模拟目录中计算的深度相同的欧几里德深调查（H=26），但没有红移测量误差。我们发现，我们的方法成功地从低密度环境（最后从第一个五分之一的密度分布），在低红移和大细胞的效率更高：低密度区域的分数错误的高密度峰是<1%的所有尺度和红移探索，但1小时$^{-1}$ Mpc的尺度，这是几个百分点。这些结果表明，我们可以有效地研究环境中的光度样本，如果光谱信息是一个较小的样本的对象，稀疏采样相同的体积。我们证明，这些研究是可能的欧几里得深调查，即在红移范围内的环境影响是不同于在本地宇宙中观察到的，从而为星系演化模型提供了新的约束。
