We present a comprehensive model to predict the rate of spectroscopic confusion in HI surveys, and demonstrate good agreement with the observable confusion in existing surveys. Generically the action of confusion on the HI mass function was found to be a suppression of the number count of sources below the `knee', and an enhancement above it. This results in a bias, whereby the `knee' mass is increased and the faint end slope is steepened. For ALFALFA and HIPASS we find that the maximum impact this bias can have on the Schechter fit parameters is similar in magnitude to the published random errors. On the other hand, the impact of confusion on the HI mass functions of upcoming medium depth interferometric surveys, will be below the level of the random errors. In addition, we find that previous estimates of the number of detections for upcoming surveys with SKA-precursor telescopes may have been too optimistic, as the framework implemented here results in number counts between 60% and 75% of those previously predicted, while accurately reproducing the counts of existing surveys. Finally, we argue that any future single dish, wide area surveys of HI galaxies would be best suited to focus on deep observations of the local Universe (z < 0.05), as confusion may prevent them from being competitive with interferometric surveys at higher redshift, while their lower angular resolution allows their completeness to be more easily calibrated for nearby extended sources.
XID+PRIMA, II: Stepping Through Hyperspectral Imaging to Deblend PRIMAger Beyond the Extragalactic Confusion Limit
University of Sussex（萨塞克斯大学）；Université de Strasbourg（斯特拉斯堡大学）；CNRS（法国国家科学研究中心）；Observatoire astronomique de Strasbourg（斯特拉斯堡天文台）；University of Maryland, College Park（马里兰大学帕克分校）；Aix Marseille Univ（艾克斯-马赛大学）；CNES（法国国家空间研究中心）；LAM（天体物理与行星实验室）；SRON Netherlands Institute for Space Research（荷兰空间研究所）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；The Open University（开放大学）；Ritter Astrophysical Research Center, Department of Physics & Astronomy, University of Toledo（托莱多大学里特天体物理研究中心）
Extragalactic archaeology through high-resolution integrated-light spectroscopy of globular clusters
Instituto de Astrofı́sica de Canarias（加那利天体物理学研究所）；Universidad de La Laguna（拉帕尔马大学）；Centre for Astrophysics and Supercomputing, Swinburne University（斯威本大学天文物理与超级计算中心）；Department of Astrophysics, University of Vienna（维也纳大学天体物理学系）；Department of Physics, Centre for Extragalactic Astronomy, Durham University（达勒姆大学河外天文中心物理系）；Department of Astrophysics/IMAPP, Radboud University（拉德堡德大学天体物理学/IMAPP系）
The VIMOS Public Extragalactic Redshift Survey (VIPERS). Unsupervised classification with photometric redshifts: a method to accurately classify large galaxy samples without spectroscopic information
The Herschel-ATLAS Data Release 2, Paper I. Submillimeter and Far-infrared Images of the South and North Galactic Poles: The Largest Herschel Survey of the Extragalactic Sky
Extragalactic background Light: a measurement at 400 nm using dark cloud shadow II. Spectroscopic separation of dark cloud's light, and results
在一个旨在测量河外背景光（EBL）的项目中，我们使用了暗云的阴影。我们用ESO VLT/FORS对高银纬暗云Lynds 1642的表面亮度进行了分光光度测量。论文I中给出了一个光谱，代表了云的不透明核心和云周围几个未被遮挡的位置之间的差异（Mattila等人，2017 a）。本论文的主题是分离的散射星光从乌云本身，这是唯一剩下的前景成分，在这种差异。虽然散射星光光谱具有典型的Fraunhofer线和在400 nm处的不连续性，这是典型的星系积分光，但EBL光谱是平滑的，没有这些特征。作为散射星光的模板，我们利用两个半透明位置的光谱。在400 nm处得到的EBL强度为$I_{\rm EBL} = 2.9\pm1.1$ $10^{-9}$ erg cm $^{-2}$ s $^{-1}$ sr $^{-1}$，或$11.6\pm4.4$ nW m $^{-2}$ sr $^{-1}$，表示2.6 $σ$检测;定标不确定性为+20%/-16%。在520 nm处，我们将2 $σ$上限设定为$I_{\rm EBL} \le$ 4.5 $10^{-9}$ erg cm $^{-2}$ s $^{-1}$ sr $^{-1}$ sr $^{-1}$或$\le$ 23.4 nW m $^{-2}$ sr $^{-1}$ +20%/-16%。我们在400 nm处的EBL值是星系积分光的$\ge 2$…
ALMA spectroscopic survey in the Hubble Ultra Deep Field: Continuum number counts, resolved 1.2-mm extragalactic background, and properties of the faintest dusty star forming galaxies
我们提出了一个深（1 $σ$ =13 $μ$ Jy）宇宙学1.2毫米连续谱图的基础上ASPECS，ALMA光谱调查在哈勃超深场的分析。在1弧分$^2$所涵盖的ASPECS，我们检测到9个源在$>3.5σ$的意义在1.2毫米。我们的ALMA-选择的样本有一个中位数红移$z=1.6\pm0.4$，只有一个星系检测到z $>$ 2内的调查区域。该值明显低于在较高通量密度截止和类似频率下选择的毫米样品中发现的值。大多数星系的恒星形成率与主序星相同，我们分别得到了恒星质量和恒星形成率的中值为$4.0\times10^{10}\ M_\odot$和$\sim40~M_\odot$ yr $^{-1}$。使用的尘埃排放作为示踪剂的ISM质量，我们推导出的耗尽时间，通常长于300万年，我们发现分子气体分数范围从$\sim$ 0.1到1.0。正如以前的研究所指出的，这些值比使用基于CO的ISM估计值低一个因子$\sim$ 2。1 mm的计数（校正保真度和完整性）与以前的研究，通常限于较亮的来源是一致的。我们的个人检测，我们恢复$55\pm4\%$的河外背景光（EBL）在1.2毫米测量的普朗克卫星，我们恢复$80\pm7\%$的EBL，如果我们包括明亮端的数量计数和额外的检测叠加。堆积的贡献主要是星系在$z\sim1-2$，与恒星质量（1-3）$\times$ 10 $^{10}$ M $_\odot…
Deep Extragalactic VIsible Legacy Survey (DEVILS): First Data Release Covering The D10 (COSMOS) Region
ICRAR, The University of Western Australia（西澳大利亚大学）；Department of Physics & Astronomy, McMaster University（麦克马斯特大学）；Jodrell Bank Centre for Astrophysics, University of Manchester（曼彻斯特大学）；Australian Astronomical Optics, Macquarie University（麦考瑞大学）；School of Physics & Astronomy, Monash University（莫纳什大学）；Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney（悉尼大学）；Astrophysics Group, School of Physics, University of Bristol（布里斯托大学）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Departamento de Astrofísica, Universidad de La Laguna (ULL)（拉帕尔马大学）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学）
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）
The NIRISS PASSAGE Spectroscopic Redshift Catalog in COSMOS
University of Minnesota, Twin Cities（明尼苏达大学双城分校）；California Institute of Technology（加州理工学院）；Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Stockholm University（斯德哥尔摩大学）
SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES). V. Confusion-limited Submillimeter Galaxy Number Counts at 450 $μ$m and Data Release for the COSMOS Field
Wide Area VISTA Extragalactic Survey (WAVES): Redshift-limited selection of targets for the Wide survey using decision-tree classification
Center for Theoretical Physics, Polish Academy of Sciences（波兰科学院理论物理中心）；ICRAR, The University of Western Australia（西澳大利亚大学星际与计算天体物理研究中心）；Tartu Observatory, University of Tartu（塔尔图大学塔尔图天文台）；Astronomy Centre, University of Sussex（萨塞克斯大学天文学中心）；European Southern Observatory（欧洲南方天文台）；Physics & Astronomy Department, University of Louisville（路易斯维尔大学物理与天文学系）
The VIMOS Public Extragalactic Redshift Survey (VIPERS). The complexity of galaxy populations at 0.4< z<1.3 revealed with unsupervised machine-learning algorithms
Deep Extragalactic VIsible Legacy Survey (DEVILS): SED Fitting in the D10-COSMOS Field and the Evolution of the Stellar Mass Function and SFR-$M_\star$ relation
JWST Advanced Deep Extragalactic Survey (JADES) Data Release 5: Photometrically Selected Galaxy Candidates at z > 8
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory - Astrophysics Group, University of Cambridge（剑桥大学卡文迪许实验室天体物理组）；Department of Astronomy and Astrophysics, University of California, Santa Cruz（加州大学圣克鲁兹分校天文学与天体物理学系）；Cosmic Dawn Center (DAWN)（宇宙黎明中心（DAWN））；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）
The Spitzer Data Fusion - A Far-Ultraviolet to Far-Infrared Multi-Wavelength Database in Spitzer Extragalactic Survey Fields
Inter-University Institute for Data Intensive Astronomy (IDIA), Department of Astronomy, University of Cape Town（开普敦大学数据密集型天文学校际研究所）；University of the Western Cape（西开普大学）；INAF - Istituto di Radioastronomia（意大利国家天体物理研究所射电天文台）
Extragalactic Planetary Nebulae (xPNe). Determining Distances out to 100 Mpc and the Renaissance of the PN Luminosity Function Method
ESO（欧洲南方天文台）；MPE（马克斯·普朗克地外物理研究所）；AIP（阿基米德研究所）；CAR, Univ. Hertfordshire（赫特福德大学计算与应用研究中心）；FINCA（图尔库天体物理学中心）；LMU（慕尼黑大学）；NSFʼs NOIRLab（美国国家科学基金会NOIR天文实验室）；Department of Astronomy & Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文与天体物理系）
The $\textit{NuSTAR}$ Extragalactic Surveys: Source Catalogs from the Extended $\textit{Chandra}$ Deep Field-South and the $\textit{Chandra}$ Deep Field-North
