The Hi-GAL compact source catalogue -- II. The 360° catalogue of clump physical properties
D. Elia, M. Merello, S. Molinari, E. Schisano, A. Zavagno, D. Russeil, P. Mège, P. G. Martin, L. Olmi, M. Pestalozzi, R. Plume, S. E. Ragan, M. Benedettini, D. … 展开作者
D. Elia, M. Merello, S. Molinari, E. Schisano, A. Zavagno, D. Russeil, P. Mège, P. G. Martin, L. Olmi, M. Pestalozzi, R. Plume, S. E. Ragan, M. Benedettini, D. J. Eden, T. J. T. Moore, A. Noriega-Crespo, R. Paladini, P. Palmeirim, S. Pezzuto, G. L. Pilbratt, K. L. J. Rygl, P. Schilke, F. Strafella, J. C. Tan, A. Traficante, A. Baldeschi, J. Bally, A. M. di Giorgio, E. Fiorellino, S. J. Liu, L. Piazzo, D. Polychroni
We present the $360^\circ$ catalogue of physical properties of Hi-GAL compact sources, detected between 70 and 500 $μ$m. This release not only completes the analogous catalogue previously produced by the Hi-GAL collaboration for $-71^\circ \lesssim \ell \lesssim 67^\circ$, but also meaningfully improves it thanks to a new set of heliocentric distances, 120808 in total. About a third of the 150223 entries are located in the newly added portion of the Galactic plane. A first classification based on detection at 70 $μ$m as a signature of ongoing star-forming activity distinguishes between protostellar sources (23~per cent of the total) and starless sources, with the latter further classified as gravitationally bound (pre-stellar) or unbound. The integral of the spectral energy distribution, including ancillary photometry from $λ=21$ to 1100 $μ$m, gives the source luminosity and other bolometric quantities, while a modified black body fitted to data for $λ\geq 160\, μ$m yields mass and temperature. All tabulated clump properties are then derived using photometry and heliocentric distance, where possible. Statistics of these quantities are discussed with respect to both source Galactic location and evolutionary stage. No strong differences in the distributions of evolutionary indicators are found between the inner and outer Galaxy. However, masses and densities in the inner Galaxy are on average significantly larger, resulting in a higher number of clumps that are candidates to host massive star formation. Median behaviour of distance-independent parameters tracing source evolutionary status is examined as a function of the Galactocentric radius, showing no clear evidence of correlation with spiral arm positions.
The initial conditions of stellar protocluster formation. II. A catalogue of starless and protostellar clumps embedded in IRDCs in the Galactic longitude range 15<l<55
The Galactic Census of High- and Medium-mass Protostars. I. Catalogues and First Results from Mopra HCO+ Maps
高质量和中等质量原恒星普查（CHaMP）是第一个大规模的，无偏见的，均匀的映射调查，在亚秒差距尺度分辨率的90 GHz线发射从银河系中的大质量分子团。我们在HCO+ J=1-0线上展示了CHaMP调查区域（300°>l>280°）的第一张Mopra（ATNF）图，通常认为该图可以追踪密度高达10^11 m-3的气体。本文介绍了这次巡天的概况及其策略，描述了观测和数据处理的过程，给出了301个大质量分子团簇系综HCO+ J=1-0发射的矩图的完整目录。从这些地图，我们也得到的物理参数的团块，使用标准的分子光谱线分析技术。该分析产生以下性质范围：积分谱线强度1-30 K km s-1，峰值谱线亮度1-7 K，谱线宽度1-10 km s-1，积分谱线光度0.5-200 K km s-1 pc ^2，半高宽0.2-2.5 pc，平均投影轴比2，光学深度0.08-2，总表面密度30-3000 M{ \sun } pc-2，数密度0.2-30 x 10^9 m-3，质量15-8000 M{ \sun }，维里参数1-55，总气体压力0.3-700 pPa。我们发现CHaMP团簇不服从Larson型的尺寸-线宽关系。在这些团块中，存在大量亚热激发、弱发射（但很容易检测）的致密分子团块，证实了Narayanan等人的预测。（2008）。这些微弱发光的团块占银河系这一部分所有大质量团块的95%，分子…
Properties of Hi-GAL clumps in the inner Galaxy]{The Hi-GAL compact source catalogue. I. The physical properties of the clumps in the inner Galaxy ($-71.0^{\circ}< \ell < 67.0^{\circ}$)
ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- VII. A catalogue of SiO clumps from ACA observations
为了了解SiO发射的性质，我们对146个大质量恒星形成区的SiO（2-1）线进行了ACA观测，作为ALMA大质量恒星形成区（ATOMS）调查的三毫米观测的一部分。我们在128（87.7 $\%$）源中检测到SiO发射，并确定了171个SiO团块，其中105个在空间上与3 mm连续发射分离。大量的SiO线轮廓（60 $\%$）是非高斯的。SiO线的速度色散范围为0.3 - 5.43 km/s $^{-1}$。在63个源中，SiO团簇与H $_\rm{II}$区域相关联，其特征在于H 40 $α$发射。我们发现，68 $\%$（116）的SiO团块与强流出。流出源和非流出源的SiO线的中值速度离散度分别为1.91 km s $^{-1}$和0.99 km s $^{-1}$。这些结果表明，外流活动可以连接到强烈冲击气体。速度弥散和[SiO]/[H $^{13}$ CO $^+$ ]强度比与尘埃温度和粒子数密度没有任何相关性。我们发现SiO线光度和热光度之间存在正相关关系，这意味着更强的激波活动与更亮的原星系团有关。在$L_\rm{sio}$ / $L_\rm{bol}$中，与H $_\rm{II}$区缔合的SiO团簇显示出较陡的特征。SiO线光度和激波气体分数与光度质量比（$L_\rm{bol}/M$）所追踪的演化阶段没有明显的相关性。
Clumps in spiral galaxies at $z \lesssim 3$: Disentangling two spatial modes of star formation
Pulkovo Astronomical Observatory, Russian Academy of Sciences（俄罗斯科学院普尔科沃天文台）；Sternberg Astronomical Institute, Lomonosov Moscow State University（莫斯科国立大学斯滕伯格天文研究所）；Saint Petersburg State University（圣彼得堡国立大学）
A merger-driven scenario for clumpy galaxy formation in the epoch of reionization: Physical properties of clumps in the FirstLight simulation
The University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), UT Institute for Advanced Study, The University of Tokyo（宇宙物理与数学 Kavli 研究所（WPI），UT 高等研究院，东京大学）；Research Center for the Early Universe, School of Science, The University of Tokyo（东京大学理学部早期宇宙研究中心）
Testing the asteroseismic estimates of stellar radii with surface brightness-colour relations and {\it Gaia} DR3 parallaxes. II. Red giants and red clump stars from the {\it Kepler} catalogue
Galaxy classification: A machine learning analysis of GAMA catalogue data
University of Groningen（格罗宁根大学）；SRON Netherlands Institute for Space Research（荷兰空间研究所）；Leiden University（莱顿大学）；Polish Academy of Sciences（波兰科学院）；University of Louisville（路易斯维尔大学）
