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Theoretical models of grain growth predict dust properties to change as afunction of protoplanetary disk radius, mass, age and other physicalconditions. We lay down the methodology for a multi-wavelength analysis of(sub-)mm and cm continuum interferometric observations to constrainself-consistently the disk structure and the radial variation of the dustproperties. The computational architecture is massively parallel and highlymodular. The analysis is based on the simultaneous fit in the uv-plane ofobservations at several wavelengths with a model for the disk thermal emissionand for the dust opacity. The observed flux density at the differentwavelengths is fitted by posing constraints on the disk structure and on theradial variation of the grain size distribution. We apply the analysis toobservations of three protoplanetary disks (AS 209, FT Tau, DR Tau) for which acombination of spatially resolved observations in the range ~0.88mm to ~10mm isavailable (from SMA, CARMA, and VLA), finding evidence of a decreasing maximumdust grain size (a_max) with radius. We derive large a_max values up to 1 cm inthe inner disk between 15 and 30 AU and smaller grains with a_max~1 mm in theouter disk (R > 80AU). In this paper we develop a multi-wavelength analysisthat will allow this missing quantity to be constrained for statisticallyrelevant samples of disks and to investigate possible correlations with disk orstellar parameters.

astronomy and astrophysics

A multi-wavelength analysis for interferometric (sub-)mm observations of  protoplanetary disks: radial constraints on the dust properties and the disk  structure