使用亚毫米阵列（SMA）和亚毫米望远镜（SMT）观测到巴纳德1b（B1-b）核心中的两个亚毫米/毫米源B1-bN和B1-bS。SMA获得的1.1 mm连续谱图显示，这两个源包含空间紧凑的组件，这表明它们拥有原恒星。通过结合SMA和SMT数据获得N2 D+和N2 H + J=3-2图。N2 D+图清楚地示出了在连续体位置处的两个峰。N2 H+地图也在连续位置处达到峰值，但更多地由空间延伸的分量主导。在B1-bN和B1-bS位置处的N2 D +/N2 H+比率估计为约0.2。N_2D ~+/N_2H ~+比值与星前核演化晚期和0类原恒星演化早期的N_2D ~+/N_2H ~+比值相当。虽然B1-bN在N2 H+和N2 D+中很亮，但在H13 CO+中几乎看不到。这意味着含碳分子的消耗在B1-bN中是显著的。化学性质表明B1-bN比B1-bS与H13 CO+对应物处于较早的演化阶段。N2 H+和N2 D+线表明两个源的径向速度相差约0.9 km s-1。然而，沿B1-bN和B1-bS线的速度模式表明，这两个源不是由单一的旋转云形成的。B1-b核很可能由两个速度分量组成，每个分量都有一个非常年轻的源。
英文摘要：
Two submm/mm sources in the Barnard 1b (B1-b) core, B1-bN and B1-bS, have been observed with the Submillimeter Array (SMA) and the Submillimeter Telescope (SMT). The 1.1 mm continuum map obtained with the SMA reveals that the two sources contain spatially compact components, suggesting that they harbor protostars. The N2D+ and N2H+ J=3-2 maps were obtained by combining the SMA and SMT data. The N2D+ map clearly shows two peaks at the continuum positions. The N2H+ map also peaks at the continuum positions, but is more dominated by the spatially extended component. The N2D+/N2H+ ratio was estimated to be ~ 0.2 at the positions of both B1-bN and B1-bS. The derived N2D+/N2H+ ratio is comparable to those of the prestellar cores in the late evolutionary stage and the class 0 protostars in the early evolutionary stage. Although B1-bN is bright in N2H+ and N2D+, this source was barely seen in H13CO+. This implies that the depletion of carbon-bearing molecules is significant in B1-bN. The chemical property suggests that B1-bN is in the earlier evolutionary stage as compared to B1-bS with the H13CO+ counterpart. The N2H+ and N2D+ lines show that the radial velocities of the two sources are different by ~ 0.9 km s-1. However, the velocity pattern along the line through B1-bN and B1-bS suggests that these two sources were not formed out of a single rotating cloud. It is likely that the B1-b core consists of two velocity components, each of which harbors a very young source.
Protostellar Outflows at the EarliesT Stages (POETS). IX. Magnetohydrodynamic disk winds traced by SO and SO$_2$ in luminous protostars
INAF - Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；UK Astronomy Technology Centre, Royal Observatory Edinburgh（英国天文学技术中心爱丁堡皇家天文台）；Faculty of Physics, University of Duisburg-Essen（杜伊斯堡-埃森大学物理学院）；I. Physikalisches Institut, Universität zu Köln（科隆大学第一物理研究所）；Universidad Nacional Autónoma de México, Instituto de Radioastronomía y Astrofísica（墨西哥国立自治大学无线电天文学与天体物理研究所）；Department of Physics and Astronomy, McMaster University（麦克马斯特大学物理与天文学系）
Sub-millimeter wavelength protostellar accretion rate monitoring with AtLAST
Max-Planck-Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；Thüringer Landessternwarte Tautenburg（图林根州陶滕堡天文台）；NRC Herzberg Astronomy and Astrophysics Research Centre & University of Victoria（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究中心和维多利亚大学）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学卡尔·古斯塔夫·凯夫利天文学与天体物理学研究所）；University of Toledo（托莱多大学）；Finnish Centre for Astronomy with ESO（芬兰ESO天文学中心）；NTNU（挪威科技大学）
The ALMA Legacy survey of Class 0/I disks in Corona australis, Aquila, chaMaeleon, oPhiuchus north, Ophiuchus, Serpens (CAMPOS). I. Evolution of Protostellar disk radii
JOYS: Launch and destruction of dust in protostellar jets. The case of BHR71-IRS1 with JWST MIRI
Leiden University（莱顿大学）；INAF - Osservatorio Astronomico di Roma（罗马天文台国家天体物理研究所）；University of Helsinki（赫尔辛基大学）；Max-Planck-Institut für Extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；INAF-Osservatorio Astronomico di Capodimonte（卡波迪蒙特天文台国家天体物理研究所）；University of Virginia（弗吉尼亚大学）；Virginia Institute of Theoretical Astronomy（弗吉尼亚理论天文研究所）；Institut de Cienciès de l’Espai (ICE-CSIC)（空间科学研究所（西班牙高等科学研究委员会））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究所）；Université Paris-Saclay（巴黎萨克雷大学）
Q/W-band Observations toward Starless Cores in Orion (QWOSCO) I. Overview, Isotopologues, Isomers, and Complex Organics
Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；University of Helsinki（赫尔辛基大学）；Korea Astronomy and Space Science Institute（韩国天文学与空间科学研究所）；University of Science and Technology, Korea (UST)（韩国科学技术院）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）
The JCMT Transient Survey: Identifying Submillimetre Continuum Variability over Several Year Timescales Using Archival JCMT Gould Belt Survey Observations
Early Planet Formation in Embedded Disks (eDisk). XXIV: Systematic Investigation of Disk Structures based on Visibility Analysis
Academia Sinica Institute of Astronomy & Astrophysics（中央研究院天文及天文物理研究所）；Department of Astronomy, University of Illinois（伊利诺伊大学天文学系）；National Radio Astronomy Observatory（国家射电天文台）；Institute for Astronomy, University of Hawai‘i at Mānoa（夏威夷大学马诺阿分校天体物理研究所）；Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University（鹿儿岛大学理工学研究科物理学与天文学系）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）
Clustered star formation at early evolutionary stages. Physical and chemical analysis of the young star-forming regions ISOSS J22478+6357 and ISOSS J23053+5953
