tokens: scale height (Klahr Henning 1997; Pinilla et al. 2012; Testi et al. 2014; Johansen et al. 2014) . The regions in the disk midplane that correspond to the snowlines of major volatiles are particularly interesting. These may promote locally efficient grain growth through recondensation across the snowline or by changing the sticking properties of ice-coated grains and, in addition, the local release of volatiles from the ices may induce a local pressure bump that could trap large grains (e.g., Supulver Lin 2000; Wada et al. 2009; Ros Johansen 2013; Gundlach Blum 2015) . The dense regions of disk midplanes can be investigated at submillimeter and millimeter wavelengths, where the dust emission is more optically thin and can now be spatially resolved with present-day facilities, such as the Atacama Large Millimeter/submillimeter Array (ALMA) and the Karl G. Jansky Very Large Array (VLA). These facilities allow us to obtain sensitive and high angular resolution observations of the dust continuum and gas emission lines from protoplanetary disks and therefore study the radial variations of the physical parameters of the disk. Recent results include the study of the dust properties as a function of radius in disks (e.g., Guilloteau et al. 2011; Banzatti et al. 2011; Pérez et al. 2012, 2015; Menu et al. 2014; Tazzari et al. 2016) , and the clear identification of the CO snowline in nearby disks (Mathews et al. 2013; Qi et al. 2013, 2015) , through its effects on DCO and NH abundances. It is thus becoming possible to directly investigate the effect of the CO snowline on grain growth observationally. This snowline is thought to be one of the most important after that of water, because the CO abundance in protostellar ices is found to be about 3040% of HO (Öberg et al. 2011) . In this work we focus on the Herbig Ae star HD 163296, a bright and isolated object at a distance of parsec (van den Ancker et al. 1998) with a relatively massive disk (~0.1 M⊙: Qi et al. 2011; Isella et al. 2007) and an excellent prototype for gas- and dust-rich protoplanetary disks. An estimated age of 5 Myr was obtained from the comparison between H ipparcos astrometric measurements and pre-main sequence evolutionary models by van den Ancker et al. (1998) . The stellar parameters computed by Natta et al. (2004) are , , K. To study the dust properties in the protoplanetary disk around HD 163296, we re-analyse the ALMA science verification observations (de Gregorio-Monsalvo et al. 2013; Mathews et al. 2013; Rosenfeld et al. 2013) and for the first time discuss the continuum emission in Band 6, combined with new VLA observations from the Disks@EVLA collaboration. In Sect. 2 we describe the observational data, in Sect. 3 we report the main new results of our analysis, in Sect. 4 we present the result of our disk modeling, and in Sect. 5 we discuss the main implications for grain properties. Fig. 1 Continuum maps at different wavelengths, from the left : 850 m, 1.3 mm, and 9 mm, the
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