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Cosmic dust is a key tracer of structure formation and evolution in theuniverse. In active galactic nuclei (AGN) the origin and role of dust areuncertain. Here, we have studied dust in the X-ray bright and reddened type-1quasar IC 4329A, which exhibits an ionised AGN wind. We incorporatedhigh-resolution X-ray and mid-IR spectroscopy, combined with broad-bandcontinuum modelling, to investigate the properties of dust in this AGN. We usednew Chandra HETGS observations taken in June 2017, as well as archival datafrom XMM-Newton, Swift, HST, Spitzer, IRAS, and Herschel for ourIR-optical-UV-X-ray modelling. Two distinct components of dust in IC 4329A arefound. One component is in the interstellar medium (ISM) of the host galaxy,and the other is a nuclear component in the AGN torus and its associated wind.The emitting dust in the torus is evident in mid-IR emission (9.7 and 18 micronfeatures), while dust in the wind is present through both reddening and X-rayabsorption (O, Si, and Fe edge features). The gas depletion factors into dustfor O, Si, and Fe are measured. We derive an intrinsic reddening E(B-V) ~ 1.0,which is most consistent with a grey (flat) extinction law. The AGN windconsists of three ionisation components. From analysis of long-term changes inthe wind, we determine limits on the location of the wind components. The twolowest ionisation components are likely carriers of dust from the AGN torus. Wefind that the dust in the nuclear component of IC 4329A is different from dustin the Milky Way. The dust grains in the AGN torus and wind are likely largerthan the standard Galactic dust, and are in a porous composite form (containingamorphous silicate with iron and oxygen). This can be a consequence of graincoagulation in the dense nuclear environment of the AGN.

Probing the nature and origin of dust in the reddened quasar IC 4329A with global modelling from X-ray to infrared