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--- author: - Pierre Barge - 'L. Ricci' - 'C. L. Carilli' - 'R. Previn-Ratnasingam' bibliography: - 'giant.bib' date: 'Version 0.1' title: Gap and rings carved by vortices in protoplanetary dust --- [Large-scale vortices in protoplanetary disks are thought to form and survive for long periods of time. Hence, they can significantly change the global disk evolution and particularly the distribution of the solid particles embedded in the gas, possibly explaining asymmetries and dust concentrations recently observed at sub-millimeter and millimeter wavelengths.]{} [We investigate the spatial distribution of dust grains using a simple model of protoplanetary disk hosted by a giant gaseous vortex. We explore the dependence of the results on grain size and deduce possible consequences and predictions for observations of the dust thermal emission at sub-millimeter and millimeter wavelengths.]{} [Global 2D simulations with a bi-fluid code are used to follow the evolution of a single population of solid particles aerodynamically coupled to the gas. Possible observational signatures of the dust thermal emission are obtained using simulators of ALMA and ngVLA observations. ]{} [We find that a giant vortex not only captures dust grains with Stokes number $St < 1$ but can also affect the distribution of larger grains (with $St \sim 1$) carving a gap associated to a ring composed of incompletely trapped particles. The results are presented for different particle size and associated to their possible signatures in disk observations.]{} [Gap clearing in the dust spatial distribution could be due to the interaction with a giant gaseous vortex and their associated spiral waves, without the gravitational assistance of a planet. Hence, strong dust concentrations at short sub-mm wavelengths associated with a gap and an irregular ring at longer mm and cm wavelengths could indicate the presence of an unseen gaseous vortex. ]{} Introduction ============ The trapping of solid particles in gaseous vortices and its consequences on planet formation is an issue investigated today by many authors. Vortices in protoplanetary disks can be produced by various mechanisms like inverse cascade in two-dimensional geometries or specific 2D/3D instabilities like the Rossby wave or the baroclinic instability.Three-dimensional studies have confirmed that such vortices can form and survive in spite of the elliptical instability that predominantly affects the core of the vortices [@Lesur2010; @Richard2013]. Ultimately, they can be depicted as quasi-2D structures with a nearly stationary evolution. In two-dimensional Keplerian flows, vortices are known to capture very effectively the solid particles embedded in the gas [@Barge95]. The trapping mechanism is so efficient that particle concentration can be strong enough for significant back-reaction of the solid particles onto the gas. Dust feedback makes possible the growth of instabilities like Rayleigh-Taylor [@chang2010], Kelvin-Helmoltz [@johansen2006], or streaming [@youdin2007]. In vortices, the confinement of the solid particles was recently addressed by @Fu2014 [@Raettig2015; @Crnkovic2015; @Baruteau2016; @Surville2016].\ Here, our paper focuses on the global distribution of the solid particles in a disk hosting a persistent gaseous vortex but does not study the detailed complex evolution inside the vortex core which will be addressed elsewhere. Our goal