Revised spectroscopic parameters of SH$^+$ from ALMA and IRAM 30 m observations
Holger S. P. Müller, Javier R. Goicoechea, José Cernicharo, Marcelino Agúndez, Jérôme Pety, Sara Cuadrado, Maryvonne Gerin, Gaelle Dumas, Edwige Chapillon
Hydrides represent the first steps of interstellar chemistry. Sulfanylium (SH$^+$), in particular, is a key tracer of energetic processes. We used ALMA and the IRAM 30 m telescope to search for the lowest frequency rotational lines of SH$^+$ toward the Orion Bar, the prototypical photo-dissociation region illuminated by a strong UV radiation field. On the basis of previous $Herschel$/HIFI observations of SH$^+$, we expected to detect emission of the two SH$^+$ hyperfine structure (HFS) components of the $N_J = 1_0 - 0_1$ fine structure (FS) component near 346 GHz. While we did not observe any lines at the frequencies predicted from laboratory data, we detected two emission lines, each $\sim$15 MHz above the SH$^+$ predictions and with relative intensities and HFS splitting expected for SH$^+$. The rest frequencies of the two newly detected lines are more compatible with the remainder of the SH$^+$ laboratory data than the single line measured in the laboratory near 346 GHz and previously attributed to SH$^+$. Therefore, we assign these new features to the two SH$^+$ HFS components of the $N_J = 1_0 - 0_1$ FS component and re-determine its spectroscopic parameters, which will be useful for future observations of SH$^+$, in particular if its lowest frequency FS components are studied. Our observations demonstrate the suitability of these lines for SH$^+$ searches at frequencies easily accessible from the ground.
IRAM 04191+1522: a compact proto-brown dwarf binary candidate
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；European Southern Observatory（欧洲南方天文台）；Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México（墨西哥国立自治大学无线电天文学与天体物理研究所）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS（波尔多大学天体物理实验室）；Department of Physics, Maynooth University（梅努斯大学物理系）
Monitoring of 3C 286 with ALMA, IRAM, and SMA from 2006 to 2025: Stability, Synchrotron Ages, and Frequency-Dependent Polarization Attributed to Core-Shift
该研究通过 ALMA、IRAM 和 SMA 对射电类星体 3C 286 进行多频监测，发现其总流量长期稳定，偏振 EVPA 随波长平方呈幂律旋转，法拉第旋转随频率增加，归因于锥形喷流中的核位移效应。
ALMA Observations of the Spatial Distribution of three C$_2$H$_4$O$_2$ Isomers towards Sgr B2(N)
C $_2$ H $_4$ O $_2$异构体以前主要通过涉及单皿和阵列测量的不同观测集进行了研究。2013年对IRAM 30 m观测进行了唯一一次使用统一观测集的尝试（Belloche等人，2013年）。在这项研究中，我们提出了一个密集和严格的光谱和形态分析的C $_2$ H $_4$ O $_2$异构体对Sgr B2（N）的干涉仪，ALMA波段3的观测。我们提出了一种定量选择方法，它自动化的最不受污染的过渡的测定，并允许我们报告发现以前未检测到的过渡的三种异构体。随着最少的污染过渡，高空间分辨率毫米地图的C $_2$ H $_4$ O $_2$异构体显示，HCOOCH $_3$和CH $_2$ OHCHO每个显示两个不同的速度分量，而只有一个速度分量的CH $_3$ COOH的解决。此外，与CH $_2$ OHCHO和CH $_3$ COOH不同，HCOOCH $_3$的分布从连续谱发射扩展并偏移，对于它们，低速分量被发现是紧凑的并且集中在Sgr B2（N）的连续谱发射峰。这些C $_2$ H $_4$ O $_2$异构体的不同形态表明，HCOOCH $_3$在化学过程中与CH $_2$ OHCHO和CH $_3$ COOH有显著差异，它们显示出相似的空间分布。
ALMA [CI]$^{3}P_{1}-^{3}P_{0}$ observations of NGC6240: a puzzling molecular outflow, and the role of outflows in the global $α_{\rm CO}$ factor of (U)LIRGs
From Grism to IFU: Revising the Redshift and Nature of the Massive Dusty Galaxy S1 with JWST and ALMA
University of Geneva（日内瓦大学）；University of Sussex（萨塞克斯大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Université Paris-Saclay, Université Paris Cité（巴黎萨克雷大学、巴黎西岱大学）；Leiden University（莱顿大学）
