We study the spatially resolved physical properties of the Cosmic Snake arc in MACS J1206.2-0847 and the arc in Abell 0521 (A521). These are two strongly lensed galaxies at redshifts $z=1.036$ and $z=1.044$. We used observations of the Hubble Space Telescope (HST) and the Atacama Large Millimeter/submillimeter Array (ALMA). The former gives access to the star formation rate (SFR) and stellar mass ($M_\star$), and the latter to the H$_2$ molecular gas mass ($M_{\mathrm{mol}}$). HST and ALMA observations have similar angular resolutions of $0.15^{\prime \prime}-0.2^{\prime \prime}$, which with the help of strong gravitational lensing enable us to reach spatial resolutions down to $\sim 30\,\mathrm{pc}$ and $\sim 100\,\mathrm{pc}$ in these two galaxies, respectively. These resolutions are close to the resolution of observations of nearby galaxies. We study the radial profiles of SFR, $M_\star$, and $M_{\mathrm{mol}}$ surface densities of these high-redshift galaxies and compare the corresponding exponential scale lengths with those of local galaxies. We find that the scale lengths in the Cosmic Snake are about $0.5\,\mathrm{kpc}-1.5\,\mathrm{kpc}$, and they are 3 to 10 times larger in A521. This is a significant difference knowing that the two galaxies have comparable integrated properties. These high-redshift scale lengths are nevertheless comparable to those of local galaxies, which cover a wide distribution. The particularity of our high-redshift radial profiles is the normalisation of the $M_{\mathrm{mol}}$ surface density profiles ($ΣM_{\mathrm{mol}}$), which are offset by up to a factor of 20 with respect to the profiles of $z=0$ counterparts. The SFR surface density profiles are also offset by the same factor as $ΣM_{\mathrm{mol}}$, as expected from the Kennicutt-Schmidt law.
Infrared Galaxies in the Field of the Massive Cluster Abell S1063: Discovery of a Luminous Kiloparsec-Sized HII Region in a Gravitationally Lensed IR-Luminous Galaxy at $z=0.6$
An ALMA sub-kiloparsec test of the Kennicutt--Schmidt relation in a strongly lensed dusty star-forming galaxy at $z\sim2.78$
Universidad de Valparaíso（瓦尔帕莱索大学）；Millenium Nucleus for Galaxies (MINGAL)（星系千年核（MINGAL））；STAR Institute（STAR研究所）；Université Côte d’Azur（蔚蓝海岸大学）；University of Florida（佛罗里达大学）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）；Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE)（国家天体物理学、光学和电子学研究所）；Universidad Central de Chile（智利中央大学）
LEGGOS: A Shocking Lack of Evidence for Shocks at sub-kiloparsec Scales at 2 < z < 4
The Pennsylvania State University（宾夕法尼亚州立大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；University of Maryland, Baltimore County（马里兰大学巴尔的摩分校）；International Space Science Institute（国际空间科学研究所）；University of Washington（华盛顿大学）
Kiloparsec view of a typical star-forming galaxy when the Universe was $\sim$1 Gyr old II. Regular rotating disk and evidence for baryon dominance on galactic scales
我们提出了一个运动学分析的主序星星系HZ 4在$z=5.5$。我们的研究是基于深，空间分辨观测的[CII] 158 PDMATHAMN米过渡与阿塔卡马大型毫米/亚毫米阵列（ALMA）。从盘形态的综合分析，二维速度结构，和一维速度和速度色散剖面的正演模拟，我们得出结论，HZ 4有一个规则的旋转盘到位。HZ 4的本征速度频散很高（$σ_{0}=65.8^{+2.9}_{-3.3}$ km s $^{-1}$），自转速度与本征速度频散之比为$V_{\rm rot}/σ_{0}=2.2$。这些值是一致的预期从增加$σ_{0}$和减少$V_{\rm rot}/σ_{0}$的红移的函数观测到的主序星星系高达$z\approx4$的趋势。星系演化模型表明，在HZ 4中观察到的高水平湍流只有在除了恒星反馈之外，圆盘内还有气体的径向传输时才能实现。最后，我们发现HZ 4是星系尺度上的重子支配（$\lesssim2\times R_{\rm e}$），暗物质分数在一个有效半径为$f_{\rm DM}(R_{\rm e})=0.41^{+0.25}_{-0.22}$。这个值与在可能是HZ 4后代的较低红移星系中发现的暗物质部分相当：大质量（$M_{\star}\approx10^{11}~M_{\odot}$），在$z\sim2$的恒星形成星系，以及在$z\approx0$的被动早期类型星系。
VENUS: A Strongly Lensed Clumpy Galaxy at $z\sim11-12$ behind the Galaxy Cluster MACS J0257.1-2325
Institute for Cosmic Ray Research, The University of Tokyo（宇宙线研究所，东京大学）；Department of Physics, Graduate School of Science, The University of Tokyo（东京大学理学研究科物理学系）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；Cosmic Frontier Center, The University of Texas at Austin（德克萨斯大学奥斯汀分校前沿宇宙学中心）；David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学戴维·A·邓普天文学与天体物理学系）；Dunlap Institute for Astronomy and Astrophysics（邓普天文学与天体物理研究所）；National Astronomical Observatory of Japan（日本国立天文台）；Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies)（SOKENDAI（高级研究大学院大学）天文学科学系）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo（东京大学 Kavli宇宙物理数学研究所（WPI））
The large-scale kinematics of young stars in the Milky Way disc: first results from SDSS-V
University of North Florida（北佛罗里达大学）；University of Toronto（多伦多大学）；KU Leuven（荷语鲁汶大学）；Universidad de La Serena（拉塞雷纳大学）；University of Colorado Boulder（科罗拉多大学博尔德分校）；University of Virginia（弗吉尼亚大学）；Chalmers University of Technology（查尔姆斯理工大学）；New Mexico State University（新墨西哥州立大学）；Moscow State University（莫斯科国立大学）；Texas Christian University（得克萨斯基督教大学）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Princeton University（普林斯顿大学）
NOEMA3D: Resolving radial gas flows in disk galaxies at z~1.1-1.6 with high-resolution CO observations
Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）；Departments of Physics and Astronomy, University of California, Berkeley（加州大学伯克利分校物理与天文学系）；Institut de Radioastronomie Millimétrique (IRAM)（毫米波射电天文研究所）；Max-Planck-Institut für Astrophysik (MPA)（马克斯·普朗克天体物理研究所）；Department of Physics and Astronomy “Augusto Righi”, University of Bologna（博洛尼亚大学“奥古斯托·里吉”物理与天文学系）；INAF – Astrophysics and Space Science Observatory of Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）
Spatially Resolved AGN Ionization and Star Formation at Cosmic Noon with JWST/JEMS
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；NSF NOIRLab（美国国家科学基金会NOIR天文台）；International Gemini Observatory/NSF NOIRLab（国际Gemini天文台/美国国家科学基金会NOIR天文台）；Department of Astronomy, University of Wisconsin-Madison（威斯康星大学麦迪逊分校天文学系）；Kavli Institute for Cosmology, Cambridge（剑桥卡弗里宇宙学研究所）
