摘要：Context.The cyanide radical CN is abundant in protoplanetary disks, with line fluxes often comparable to those of13CO. It is known to be sensitive to UV irradiation of the upper disk atmosphere, with models predicting ring-shaped emission.Aims.We seek to characterize the CN emission from 94 Class-II disks in the Lupus star-forming region, compare it to observations in other regions, and interpret our observations with a grid of models. The CN emission morphology is discussed for two primordial disks, Sz 71 and Sz 98, and is modeled in more detail.Methods.ALMA observed CNN= 3−2 in Lupus disks down to sensitivities better than previous surveys. Models constructed with the physico-chemical codeDALIare used to study the integrated fluxes of the disks and resolved emission of CN in disks without (dust) substructures.Results.CNN= 3−2 is bright, and detected in 38% of sources, but its disk-integrated flux is not strongly correlated to either13CO or continuum flux. Compared to pre-ALMA single-dish surveys, no significant difference in the CN flux distributions in Lupus and Taurus–Auriga is found, althoughρOphiuchus disks may be fainter on average. We find ring-shaped CN emission with peak radii of ~50 AU in two resolved disks.Conclusions.A large fraction of sources are faint in CN; only exponential gas surface density cutoffs atRc≤ 15 AU can reconcile observations with models. This is the first observational evidence of such a compact gas disk population in Lupus. Absolute intensities and the emission morphology of CN are reproduced byDALImodels without the need for any continuum substructure; they are unrelated to the CO snowline location. The observations presented here, together with the modeling of these rings, provide a new probe of the structure and conditions in disks, and particularly their incident UV radiation field, if disk size is determined from the data.
