Tracing 3D flows in Jupiter's Atmosphere: Multispectral Observations in February 2017

We will present results from near-simultaneous observations in three very different wavelength ranges, tracing both horizontal and vertical motions. The combined dataset will provide a coherent picture of the flow within discrete features such as 5-micron hot spots. The observations taken together can better constrain models of atmospheric flow, compared to the Galileo era, where some wavelengths were missing and observations were not simultaneous.We span a wide range of the spectrum. Images in reflected sunlight range from 225 to 889 nm, captured by the WFC3 instrument on Hubble, from 1 to 2 February 2017. Images in the thermal infrared were obtained at 4.7 microns with the NIRI instrument at Gemini North, on 2 and 5 February 2017, and high-resolution infrared spectroscopy at similar wavelengths was performed with Keck NIRSPEC on 5 and 6 February 2017. Spectral imaging was performed in the 1.2 to 1.7 cm range by the VLA, on 2 February 2017. These three data sets measure velocities in different ways.Our initial correlation of the multispectral dataset involves flow in a 5-micron hot spot (very similar in morphology to the one imaged by the Galileo Orbiter in Vasavada et al., 1998), found at a longitude of about 330 deg on UT 2017-02-02. At this longitude, Hubble imaging data provide coverage of the feature over three Jupiter rotations, enabling retrieval of two separate velocity fields, 10 hours apart. Both velocity fields show similar features to the Vasavada hot spot, particularly an anticyclonic circulation in the "oval cloud" to the southeast of the hot spot. The Gemini data confirm that the dark area in the Hubble imaging corresponds exactly to a region of high 5-micron emission, which is a sign of downward flow, as traced by low cloud opacity. The infrared spectroscopy will be inverted to measure NH3 and H2O gas abundance profiles. VLA data require much more calibration and processing, but eventually will reveal how locations of high ammonia abundance trace upwelling flow, a capability demonstrated by earlier observations by the VLA at this latitude (de Pater et al. 2016).