We present the detection of bright [CII] emission in the z=4.76 submillimetre galaxy LESS J033229.4-275619 using the Atacama Pathfinder EXperiment. This represents the highest redshift [CII] detection in a submm selected, star-formation dominated system. The AGN contributions to the [CII] and far-infrared (FIR) luminosities are small. We find an atomic mass derived from [CII] comparable to the molecular mass derived from CO. The ratio of the [CII], CO and FIR luminosities imply a radiation field strength G_0~10^3 and a density ~10^4 cm^-3 in a kpc-scale starburst, as seen in local and high redshift starbursts. The high L_[CII]/L_FIR=2.4x10^-3 and the very high L_[CII]/L_CO(1-0) ~ 10^4 are reminiscent of low metallicity dwarf galaxies, suggesting that the highest redshift star-forming galaxies may also be characterised by lower metallicities. We discuss the implications of a reduced metallicity on studies of the gas reservoirs, and conclude that especially at very high redshift, [CII] may be a more powerful and reliable tracer of the interstellar matter than CO.
Shock-Enhanced C+ Emission and the Detection of H2O from Stephan's Quintet's Group-Wide Shock using Herschel
我们首次用赫歇尔光谱探测到了[OI]63和[CII]158微米的精细结构跃迁，以及斯蒂芬五重奏中35 x 15 kpc^2的受激星系际暗条中的一条para-H2O谱线。这条暗条被认为是当一个高速入侵者与星团内气体碰撞时形成的。PACS光谱仪的观测提供了宽（> 1000 km s^-1）的发光[CII]谱线轮廓以及较暗的[OI] 63微米发射的证据。SPIRE FTS观测揭示了细丝中几个位置的p-H2O（111-000）跃迁的水发射，但没有其他分子线。H2O谱线很窄，可能与密度较大的中速气体经历最强的冲击加热有关。[CII]/PAH（tot）和[CII]/FIR比率太大，无法通过PDR中的正常光电加热来解释。也可以排除HII区激发或X射线/宇宙射线加热。观测结果得出的结论是，大部分分子气体是扩散和温暖的。我们建议，[CII]，[OI]和暖H2线的发射是由一个湍流级联，其中的动能从星系碰撞与IGM耗散到小尺度和低速度，通过冲击和湍流涡旋。低速磁震可以帮助解释[CII]/[OI]比值和观察到的相对较高的[CII]/H2比值。发现[CII]发射可以增强，在大规模的湍流区域的碰撞环境中的影响的解释[CII]发射在高z星系。
Euclid: A UV-faint quasar in a highly luminous star-forming host galaxy at $z \approx 7.7$
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚空间科学与天体物理观测台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Hamburger Sternwarte, University of Hamburg（汉堡大学汉堡天文台）；INAF-Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；INAF-IASF Milano（意大利国家天体物理研究所米兰天文科学与技术研究所）；Institut für Theoretische Physik, University of Heidelberg（海德堡大学理论物理研究所）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）
When galaxies burst: enhanced shot-noise for line-intensity mapping in the JWST era
Ben-Gurion University of the Negev（内盖夫本-古里安大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Cosmic Frontier Center, The University of Texas at Austin（德克萨斯大学奥斯汀分校宇宙前沿中心）；Tel-Aviv University（特拉维夫大学）
Probing the Interstellar Medium of z~1 Ultra-luminous Infrared Galaxies through Interferometric Observations of CO and Spitzer Mid-infrared Spectroscopy
Evidence for inefficient dust production in a massive, metal-rich galaxy at $z=7.13$ uncovered by JWST and ALMA
Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；DTU Space, Technical University of Denmark（丹麦技术大学空间研究所）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；Centre for Astrophysics Research, University of Hertfordshire（赫特福德大学天体物理研究中心）；Department of Physics, University of Surrey（萨里大学物理系）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文系）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理与空间研究所）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）
