Potential signatures of proto-planets embedded in their natal protoplanetary disk are radial gaps or cavities in the continuum emission in the IR-mm wavelength range. ALMA observations are now probing spatially resolved rotational line emission of CO and other chemical species. These observations can provide complementary information on the mechanism carving the gaps in dust and additional constraints on the purported planet mass. We post-process 2D hydrodynamical simulations of planet-disk models, where the dust densities and grain size distributions are computed with a dust evolution code. The simulations explore different planet masses ($1\,M_{\rm J}\leq M_{\rm p}\leq15\,M_{\rm J}$) and turbulent parameters. The outputs are post-processed with the thermo-chemical code DALI, accounting for the radially and vertically varying dust properties as in Facchini et al. (2017). We obtain the gas and dust temperature structures, chemical abundances, and synthetic emission maps of both thermal continuum and CO rotational lines. This is the first study combining hydro simulations, dust evolution and chemistry to predict gas emission of disks hosting massive planets. All radial intensity profiles of the CO main isotopologues show a gap at the planet location. The ratio between the location of the gap as seen in CO and the peak in the mm continuum at the pressure maximum outside the orbit of the planet shows a clear dependence on planet mass. Due to the low dust density in the gaps, the dust and gas components can become thermally decoupled, with the gas being colder than the dust. The gaps seen in CO are due to a combination of gas temperature dropping at the location of the planet, and of the underlying surface density profile. In none of the models is a CO cavity observed, only CO gaps, indicating that one single massive planet is not able to explain the CO cavities observed in transition disks.
Dust continuum emission and the upper limit fluxes of sub-millimeter water lines of the protoplanetary disk around HD 163296 observed by ALMA
本文利用阿塔卡玛大型毫米/亚毫米波阵列（ALMA），分析了Herbig Ae星HD 163296周围原行星盘的亚毫米波正H $_{2}$ $^{16}$ O 321 GHz、paraH $_{2}$ $^{18}$ O 322 GHz和HDO 335 GHz谱线的上限通量。这些水线被认为是最好的候选亚毫米线定位的H $_{2}$ O雪线的位置，在我们以前的模式计算的基础上。我们比较了上限通量与我们的模式计算的值与尘埃排放，我们约束的线发射区域和尘埃不透明度的观测。我们的结论是，如果高水蒸气丰度区的外缘和水雪线的位置也超过8 au，则毫米尘埃不透明度值将大于2.0 cm $^{2}$ g $^{-1}$。此外，如果mm尘埃不透明度为2.0 cm $^{2}$ g $^{-1}$，则水雪线的位置将在20 au以内。未来的观测尘埃连续辐射在更高的角分辨率和亚毫米水线与更长的观测时间需要澄清的详细结构和位置的H $_{2}$ O雪线在磁盘中面。
The MESAS Project: ALMA observations of the F-type stars $γ$ Lep, $γ$ Vir A, and $γ$ Vir B
由于缺乏大多数光谱类型的数据，在亚毫米到厘米波长范围内的恒星光谱仍然没有得到很好的限制。一个准确的表征恒星发射在这一制度是需要测试恒星大气模型，也是必不可少的揭示与未解决的星周碎片的排放。我们目前的ALMA观测的三个附近，主序星，碎片少，F-型恒星$γ$ Lep，$γ$ Vir A，和$γ$ Vir B在0.87和1.29毫米。我们使用这些数据来约束半经验大气模型。我们讨论了这些恒星的大气结构，探索潜在的短期变化，以及对碎片盘研究的潜在影响。这些结果是正在进行的活动的一部分，以获得长波长观测的碎片贫星，题为测量恒星大气层的发射在亚毫米/毫米波长（MESAS）。
Resolving the terrestrial planet-forming region of HD 172555 with ALMA: I. Post-impact dust distribution
Trinity College Dublin, the University of Dublin（都柏林三一学院，都柏林大学）；Malaghan Institute of Medical Research（马拉甘医学研究所）；University of Exeter（埃克塞特大学）；Space Science Institute（太空科学研究所）；University of Arizona（亚利桑那大学）；University of Cambridge（剑桥大学）；Towson University（陶森大学）
Observations of highly inclined disks with ALMA. Results from 12CO gas and continuum observations
Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学）；Astronomy Department, University of California Berkeley（加州大学伯克利分校天文学系）；Astronomy Unit, Department of Physics and Astronomy, Queen Mary University of London（伦敦大学玛丽女王学院物理与天文学系天文学单元）；Institute of Astronomy, University of Cambridge（剑桥大学天文研究所）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
Revealing Callisto's Near Subsurface Thermophysical Properties with ALMA Calibration Data
Lunar and Planetary Laboratory, University of Arizona（亚利桑那大学月球与行星实验室）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理科学系）；Division of Geological and Planetary Sciences, California Institute of Technology（加州理工学院地质与行星科学部）；School of Public and International Affairs, Princeton University（普林斯顿大学公共与国际事务学院）；National Radio Astronomy Observatory（国家射电天文台）
