The GLEAM 4-Jy (G4Jy) Sample: I. Definition and the catalogue
Sarah V. White, Thomas M. O. Franzen, Chris J. Riseley, O. Ivy Wong, Anna D. Kapińska, Natasha Hurley-Walker, Joseph R. Callingham, Kshitij Thorat, Chen Wu, Pau… 展开作者
Sarah V. White, Thomas M. O. Franzen, Chris J. Riseley, O. Ivy Wong, Anna D. Kapińska, Natasha Hurley-Walker, Joseph R. Callingham, Kshitij Thorat, Chen Wu, Paul Hancock, Richard W. Hunstead, Nick Seymour, Jesse Swan, Randall Wayth, John Morgan, Rajan Chhetri, Carole Jackson, Stuart Weston, Martin Bell, Bi-Qing For, B. M. Gaensler, Melanie Johnston-Hollitt, André Offringa, Lister Staveley-Smith
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57 pages (30 MB in size), 23 figures, 16 tables, accepted for publication in PASA, and now updated to match the final proof. Full-resolution images will be used for the published version, available through the journal. To keep up-to-date regarding the G4Jy Sample, bookmark https://github.com/svw26/G4Jy
The Murchison Widefield Array (MWA) has observed the entire southern sky (Declination, $δ<$ 30 deg) at low radio-frequencies, over the range 72-231 MHz. These observations constitute the GaLactic and Extragalactic All-sky MWA (GLEAM) Survey, and we use the extragalactic catalogue (Galactic latitude, $|b| >$ 10 deg) to define the GLEAM 4-Jy (G4Jy) Sample. This is a complete sample of the 'brightest' radio-sources ($S_{\mathrm{151MHz}} >$ 4 Jy), the majority of which are active galactic nuclei with powerful radio-jets. Crucially, low-frequency observations allow the selection of such sources in an orientation-independent way (i.e. minimising the bias caused by Doppler boosting, inherent in high-frequency surveys). We then use higher-resolution radio images, and information at other wavelengths, to morphologically classify the brightest components in GLEAM. We also conduct cross-checks against the literature, and perform internal matching, in order to improve sample completeness (which is estimated to be $>$ 95.5%). This results in a catalogue of 1,863 sources, making the G4Jy Sample over 10 times larger than that of the revised Third Cambridge Catalogue of Radio Sources (3CRR; $S_{\mathrm{178MHz}} >$ 10.9 Jy). Of these G4Jy sources, 78 are resolved by the MWA (Phase-I) synthesised beam ($\sim$2 arcmin at 200 MHz), and we label 67% of the sample as 'single', 26% as 'double', 4% as 'triple', and 3% as having 'complex' morphology at $\sim$1 GHz (45-arcsec resolution). Alongside this, our value-added catalogue provides mid-infrared source associations (subject to 6-arcsec resolution at 3.4 micron) for the radio emission, as identified through visual inspection and thorough checks against the literature. As such, the G4Jy Sample can be used as a reliable training set for cross-identification via machine-learning algorithms. [Abstract abridged for arXiv submission.]
International Centre for Radio Astronomy Research, Curtin University（国际射电天文中心，科廷大学）；Australian SKA Regional Centre (AusSRC), Curtin University（澳大利亚SKA区域中心（AusSRC），科廷大学）；CSIRO Space and Astronomy（CSIRO空间与天文学）
GLEAM-300: The GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey at 300 MHz
International Centre for Radio Astronomy Research, Curtin University（国际无线电天文学研究中心，科廷大学）；SKA Observatory, SKA-Low Science Operations Centre（平方公里阵列射电望远镜天文台，SKA低频科学运行中心）
The GLEAM 4-Jy (G4Jy) Sample: IV. Multiwavelength data and analysis
South African Astronomical Observatory (SAAO)（南非天文台）；Rhodes University（罗德兹大学）；International Centre for Radio Astronomy Research (ICRAR), Curtin University（科廷大学国际射电天文研究中心）；University of Pretoria（比勒陀利亚大学）；Thüringer Landessternwarte（图林根州立天文台）；Univ. de Guanajuato（瓜纳华托大学）；Square Kilometre Array Observatory (SKAO)（平方公里阵列望远镜观测站）；CSIRO Space & Astronomy（联邦科学与工业研究组织空间与天文学部）；ICRAR, University of Western Australia（西澳大学国际射电天文研究中心）；National Radio Astronomy Observatory (NRAO)（美国国家射电天文台）；Netherlands Institute for Radio Astronomy (ASTRON)（荷兰射电天文研究所）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内克天文研究所）
The POlarised GLEAM Survey (POGS) II: Results from an All-Sky Rotation Measure Synthesis Survey at Long Wavelengths
低频线性极化射电源人口在很大程度上是未开发的。然而，低频偏振测量的复兴已经被平方公里阵列的探路者和先驱仪器所实现。在这第二篇论文中，来自极化银河系和河外全天空默奇森宽场阵列（MWA）调查-极化GLEAM调查，或POGS -我们提出了我们的全天空MWA第一阶段法拉第旋转测量调查的结果。我们的调查几乎涵盖了整个南部天空在12月范围$-82^{\circ}$到$+30^{\circ}$在分辨率之间约3和7弧分（取决于12月）使用的数据频率范围169 $-$ 231兆赫。我们进行了两次有针对性的搜索：第一次覆盖25，489平方度的天空，搜索河外极化源;第二次覆盖December $+30^{\circ}$以南的整个天空，搜索已知的恒星。我们共检测到517个源，200 MHz的线性极化的通量密度在9.9毫焦耳和1.7焦耳，其中33个是已知的射电望远镜。我们目录中的所有源的法拉第旋转测量范围为$-328.07$ rad m $^{-2}$至$+279.62$ rad m $^{-2}$。法拉第旋转测量与高频测量的结果大致一致，但精度通常提高了一个数量级以上，突出了低频极化测量准确研究银河系和河外磁场的能力。我们讨论我们的河外和已知的脉冲星源人口的属性，如何天空分布与银河系的功能，并确定少数新的脉冲星候选人在我们名义上的河外源人口。
The Alma catalogue of OB stars. III. A cross-match with Gaia DR3 and an extension based on new spectral classifications
Centro de Astrobiología. CSIC-INTA（天体生物学中心）；University of Vienna（维也纳大学）；Universidad Complutense de Madrid（马德里康普顿斯大学）；Universidad de La Serena（拉塞雷纳大学）；Alma College（阿尔玛学院）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Universidad de La Laguna（拉古纳大学）；Georgia College and State University（佐治亚州立大学）
Coma Cluster Ultra-Diffuse Galaxies Are Not Standard Radio Galaxies
通过SUBARU成像将后发座星系团超漫射星系目录（UDG，Yagi et al. 2016）中的成员与该星系团的极深射电连续巡天源目录（Miller et al. 2009）进行匹配，使用Karl G. Jansky甚大阵列（VLA）在以集群核心为中心的约1.19平方度的矩形区域内显示与随机一致的匹配。在这个矩形区域中的470个UDG和696个VLA射电源的重叠集合在25弧秒的间隔内找到33个匹配;将样本分成间隔为5弧秒、10弧秒、20弧秒和25弧秒的箱，找到1、4、17和11个匹配。基于泊松概率分布的分析模型估计，在这些相同的分离界限内随机预期匹配的数量为1.7，4.9，19.4和14.2，每个分别与观察值的95%泊松置信区间一致。将数据分为五个0.1度的聚类中心环，并分为四个分离箱，发现相同的结果。UDG与VLA源的随机匹配意味着UDG不是标准定义的射电星系。Miller等人（2009）在1.4 GHz处积分通量> 1 mJy的VLA源，没有SDSS星系匹配，与背景射电源的已知表面密度一致。我们简要地探讨了UDG附近一些未解决的VLA源可能是年轻的，紧凑的，明亮的，Ia型事件的超新星遗迹的可能性，可能在星团内的体积。
