A Multiwavelength Consensus on the Main Sequence of Star-Forming Galaxies at z~2
G. Rodighiero, A. Renzini, E. Daddi, I. Baronchelli, S. Berta, G. Cresci, A. Franceschini, C. Gruppioni, D. Lutz, C. Mancini, P. Santini, G. Zamorani, J. Silver… 展开作者
G. Rodighiero, A. Renzini, E. Daddi, I. Baronchelli, S. Berta, G. Cresci, A. Franceschini, C. Gruppioni, D. Lutz, C. Mancini, P. Santini, G. Zamorani, J. Silverman, D. Kashino, P. Andreani, A. Cimatti, H. Dominguez Sanchez, E. Le Floch, B. Magnelli, P. Popesso, F. Pozzi
We compare various star formation rate (SFR) indicators for star-forming galaxies at $1.4<z<2.5$ in the COSMOS field. The main focus is on the SFRs from the far-IR (PACS-Herschel data) with those from the ultraviolet, for galaxies selected according to the BzK criterion. FIR-selected samples lead to a vastly different slope of the SFR-stellar mass ($M_*$) relation, compared to that of the dominant main sequence population as measured from the UV, since the FIR selection picks predominantly only a minority of outliers. However, there is overall agreement between the main sequences derived with the two SFR indicators, when stacking on the PACS maps the BzK-selected galaxies. The resulting logarithmic slope of the SFR-{$M_*$} relation is $\sim0.8-0.9$, in agreement with that derived from the dust-corrected UV-luminosity. Exploiting deeper 24$μ$m-Spitzer data we have characterized a sub-sample of galaxies with reddening and SFRs poorly constrained, as they are very faint in the $B$ band. The combination of Herschel with Spitzer data have allowed us to largely break the age/reddening degeneracy for these intriguing sources, by distinguishing whether a galaxy is very red in B-z because of being heavily dust reddened, or whether because star formation has been (or is being) quenched. Finally, we have compared our SFR(UV) to the SFRs derived by stacking the radio data and to those derived from the H$α$ luminosity of a sample of star-forming galaxies at $1.4<z<1.7$. The two sets of SFRs are broadly consistent as they are with the SFRs derived from the UV and by stacking the corresponding PACS data in various mass bins.
A Correlation between Star Formation Rate and Average Black Hole Accretion in Star-forming Galaxies (Proceeding of IAUS304: Multiwavelength AGN Surveys and Studies)
A Multiwavelength Study of ELAN Environments (AMUSE$^2$): Detection of a dusty star-forming galaxy within the enormous Lyman $α$ nebula at $z=2.3$ sheds light on its origin
我们在$z=2.28$对射电宁静类星体UM 287及其周围进行ALMA观测。UM 287与一个伴星一起被认为在为周围巨大的Ly $α$星云（ELAN）提供动力方面发挥了重要作用，该星云被称为Slug ELAN，其端到端大小为450物理kpc。除了类星体，我们还探测到一个新的尘埃恒星形成星系（DSFG），被称为鼻涕虫DSFG，在2毫米连续谱中具有与CO（4-3）一致的单一发射线。段塞-DSFG位于距离UM 287东南100 kpc的投影距离处，相对于UM 287，系统速度差为$-360\pm30$ km s $^{-1}$，这表明它可能是段塞ELAN的动力来源。仔细模拟的SED和动力学分析发现，Slug-DSFG和UM 287出现低的气体分数和气尘比，这表明由于主机质量晕的环境效应。此外，我们的凯克长缝光谱揭示了来自Slug-DSFG的显著的Ly $α$发射，以及Ly $α$尾部，该尾部开始于Slug-DSFG的位置和速度，并向南延伸，预计长度约为100 kpc。支持各种分析估计，我们建议，Ly PDMATHAMN尾巴是一个结果的蛞蝓DSFG经历冲压压力剥离。被剥离的气体质量估计约为10 $^9$ M $_\odot$，这有助于形成致密的暖/冷气体储层，据信这有助于为Ly $α$的异常亮度提供动力。
A Multiwavelength Study of ELAN Environments (AMUSE$^2$): Ubiquitous dusty star-forming galaxies associated with enormous Ly$α$ nebulae on megaparsec scales
A Multiwavelength Assessment Disfavoring the X-ray Binary Origin of He III Regions in Metal-Poor Star-Forming Dwarf Galaxies
University of Nevada, Reno（内华达大学雷诺分校）；Nevada Center for Astrophysics（内华达天体物理中心）；INAF - Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都天文台）；The University of Sydney（悉尼大学）；Greenhill Observatory（格林希尔天文台）；University of Michigan（密歇根大学）；Université de Strasbourg（斯特拉斯堡大学）；Catholic University of America（美国天主教大学）
Multiwavelength radio observations of a Brightest Cluster Galaxy at z=1.71: Detection of a modest Active Galactic Nucleus and evidence for extended star formation
Testing the evolutionary pathways of galaxies and their supermassive black holes and the impact of feedback from Active Galactic Nuclei via large multiwavelength datasets
A Multiwavelength Study of ELAN Environments (AMUSE$^2$). Mass budget, satellites spin alignment and gas infall in a massive $z\sim3$ quasar host halo
系统地瞄准高红移类星体周围的扩展Ly $α$辐射导致发现了与多个活动星系核（AGN）相关的罕见而明亮的巨大Ly $α$星云（ELANe）。我们在这里启动了“ELAN环境的多波长研究”（AMUSE $^2$），重点关注$z\sim3$类星体SDSS J1040+1020（又名）周围的ELAN。神话般的伊兰我们报告了VLT/HAWK-I、APEX/LABOCA、JCMT/SCUBA-2、SMA/850 $μ$ m、ALMA/CO（5-4）和2 mm观测结果，并将它们与先前发表的VLT/MUSE数据进行了比较。通过连续谱和谱线探测，可以初步估计与ELAN有关的四个天体（三个活动星系核和一个Ly $α$发射体）的恒星形成率、尘埃、恒星和分子气体质量，从而确认类星体宿主是系统中最具恒星形成能力的（${\rm SFR}\sim500$ M $_\odot$ Y $^{-1}$）和大质量星系（$M_{\rm star}\sim10^{11}$ M $_{\odot}$），因此可以假定为中心星系。所有四个嵌入对象具有相似的分子气藏（$M_{\rm H_2}\sim10^{10}$ M $_{\odot}$），导致短的耗尽时间尺度。这一事实加上估计的暗物质晕总质量$M_{\rm DM}=(0.8-2)\times10^{13}$ M $_{\odot}$，意味着这个ELAN将演化成一个巨大的椭圆星系…
A Multiwavelength view of IC 860: What Is in Action inside Quenching Galaxies
我们提出了一个多波长的研究IC 860，附近的后星暴星系在早期阶段的过渡，从蓝色和恒星形成红色和静止。光学图像揭示了一个星系范围内的尘埃流出，起源于一个致密的核心。从CO位置-速度图和NaD吸收特征中，我们发现了分子和中性气相中多相流出的证据。我们将中性质量流出速率限制为约0.5 M $_{\odot}/$/年，总氢质量流出速率限制为约12 M $_{\odot}$ /年。两个外流成分似乎都无法逃离星系。我们还发现了最近合并的光学图像，CO的空间分布和运动学的证据，并在光发射线比，中红外特性和无线电光谱形状的证据掩埋AGN。在当前恒星形成速率下，分子气体库的耗尽时间为~7 Gyr，表明该星系可能长期停留在蓝色和红色序列之间的中间阶段。因此，恒星形成率显著下降（“淬灭”）和气体耗尽的时间尺度不一定相同。我们的分析支持淬火图片流出物有助于抑制恒星形成的干扰，而不是驱逐气体，并揭示了可能正在进行的活动，在类似的淬火星系。
PEARLS: NuSTAR and XMM-Newton Extragalactic Survey of the JWST North Ecliptic Pole Time Domain Field VI: Multiwavelength SED Analysis
Arizona State University（亚利桑那州立大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Center for Astrophysics | Harvard & Smithsonian（天体物理中心 | 哈佛与史密森尼学会）；University of Utah（犹他大学）
Detection of non-thermal radio emission components from the Orion Nebula: stellar jets, cloud collision or feedback from stellar winds?
Tata Institute of Fundamental Research (TIFR)（塔塔基础研究所）；Joint Astronomy Programme, Indian Institute of Science（印度科学学院联合天文学项目）；Department of Physics, Indian Institute of Science（印度科学学院物理系）；Department of Physics, New Mexico Institute of Mining and Technology（新墨西哥矿业理工学院物理系）；Department of Physics, IIT (BHU), Varanasi（瓦拉纳西印度理工大学（贝拿勒斯 Hindu 大学）物理系）；Department of Earth and Space Sciences, Indian Institute of Space Science and Technology（印度空间科学研究与技术学院地球与空间科学系）；Department of Physics and McGill Space Institute, McGill University（麦吉尔大学物理系与麦吉尔太空研究所）；Centre for Strings, Gravitation and Cosmology, Department of Physics, Indian Institute of Technology, Madras（马德拉斯印度理工大学物理系弦论、引力与宇宙学中心）
A Multiwavelength Evaluation of AGN in the Post-Starburst Phase
Johns Hopkins University（约翰斯·霍普金斯大学）；Texas A&M University（德克萨斯农工大学）；Space Telescope Science Institute（太空望远镜科学研究所）；AURA for ESA（欧洲空间局天文研究协调协会）；The College of New Jersey（新泽西学院）；Arizona State University（亚利桑那州立大学）；University of Waterloo（滑铁卢大学）
A multiwavelength overview of the giant spiral UGC 2885
University of Western Ontario（韦仕敦大学）；Northwestern University（西北大学）；Chalmers University of Technology（查尔姆斯理工大学）；University of Louisville（路易斯维尔大学）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；The SETI Institute（SETI研究所）
本文通过 CFHT、IRAM 30 米和 WISE 多波段观测研究巨型旋涡星系 UGC 2885，发现其金属丰度极高、分子气体含量约为普通恒星形成星系的 100 倍但恒星形成率相对较低，提出其经历多轮恒星形成周期并可能由分子棒抑制当前恒星形成。
Multiwavelength study of the Carina--Sagittarius Arm. I.Astrometric and photometric search for new open clusters in the 320$^ \circ $ $\le$ l $\le$ 325$^ \circ $ region
Facultad de Ciencias Astronómicas y Geofísicas, (UNLP)（拉普拉塔国立大学天文学与地球物理科学学院）；Instituto de Astrofísica La Plata, (CONICET - UNLP)（拉普拉塔天体物理研究所）；Facultad Regional Concepción del Uruguay, (UTN)（恩特雷里奥斯省康塞普西翁德尔乌拉圭区域学院）
Far-Infrared Star Formation Rates of Quasar Host Galaxies from Multiwavelength Spectral Energy Distribution Decomposition
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）；Leiden University（莱顿大学）；University of Groningen（格罗宁根大学）；University of Chinese Academy of Sciences (UCAS)（中国科学院大学）
