We observed Jupiter four times over a full rotation (10 hrs) with the upgraded Karl G. Jansky Very Large Array (VLA) between December 2013 and December 2014. Preliminary results at 4-17 GHz were presented in de Pater et al. (2016); in the present paper we present the full data set at frequencies between 3 and 37 GHz. Major findings are: (i) the radio-hot belt at 8.5--11$^\circ$N latitude, near the interface between the North Equatorial Belt (NEB) and the Equatorial Zone (EZ) is prominent at all frequencies (3--37 GHz). Its location coincides with the southern latitudes of the NEB (7--17$^{\circ}$ N). (ii) Longitude-smeared maps reveal belts and zones at all frequencies at latitudes $\lesssim |20^\circ|$. The lowest brightness temperature is in the EZ near a latitude of 4$^\circ$N, and the NEB has the highest brightness temperature near 11$^\circ$N. The bright part of the NEB increases in latitudinal extent (spreads towards the north) with deceasing frequency, i.e., with depth into the atmosphere. In longitude-resolved maps, several belts, in particular in the southern hemisphere, are not continuous along the latitude line, but broken into small segments as if caused by an underlying wave. (iii) Model fits to longitude-smeared spectra are obtained at each latitude. These show a high NH$_3$ abundance (volume mixing ratio $\sim 4 \times 10^{-4}$) in the deep ($P>8-10$ bar) atmosphere, decreasing at higher altitudes due to cloud formation (e.g., in zones), or dynamics in combination with cloud condensation (belts). In the NEB ammonia gas is depleted down to at least the 20 bar level with an abundance of $1.75 \times 10^{-4}$. (iv) Using the entire VLA dataset, we confirm that the planet is extremely dynamic in the upper layers of the atmosphere, at $P<$2--3 bar, i.e., at the altitudes where clouds form. [Abridged]
Cloud and ammonia vertical profiles in the equatorial atmosphere of Jupiter determined from visible to near-IR observations made by VLT/MUSE, Cassini/VIMS, IRTF/SpeX and Juno/JIRAM
University of Oxford（牛津大学）；Universidad del País Vasco UPV/EHU（巴斯克大学）；Istituto Nazionale di Astrofisica（意大利国家天体物理研究所）
A second visit to Eps Ind Ab with JWST: new photometry confirms ammonia and suggests thick clouds in the exoplanet atmosphere of the closest super-Jupiter
Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；University of Texas at Austin（德克萨斯大学奥斯汀分校）；Space Telescope Science Institute（太空望远镜科学研究所）；Heidelberg University（海德堡大学）；Leiden University（莱顿大学）
Simultaneous retrieval of orbital phase resolved JWST/MIRI emission spectra of the hot Jupiter WASP-43b: evidence of water, ammonia and carbon monoxide
Juno Microwave Radiometer Observations Reveal A Warmer Polar Atmosphere on Jupiter
University of Michigan（密歇根大学）；University of Leicester（莱斯特大学）；Weizmann Institute of Science（魏茨曼科学研究所）；Université Côte d’Azur（蔚蓝海岸大学）；University of Houston（休斯顿大学）；Aeolis Research（埃俄利斯研究公司）；INAF-Istituto di Astrofisica e Planetologia Spaziali（意大利国家天体物理研究所空间天体物理学与行星科学研究所）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
JWST Reveals Varied Origins Between Jupiter's Irregular Satellites
University of Maryland（马里兰大学）；Johns Hopkins University Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）；Space Telescope Science Institute（太空望远镜科学研究所）；Northern Arizona University（北亚利桑那大学）
