Molecular envelopes around carbon stars - Interferometric observations andmodels of HCN and CN emission

We have observed four carbon stars (W Ori, RW LMi [CIT6], Y CVn, and LP And [IRC+40540]) in the HCN(J = 1 --> 0) line and three of them (RW LMi, Y CVn , and LP And) also in the CN(N = 1 --> 0) line using the IRAM interferomete r on Plateau de Bure. The HCN brightness distributions are centred on the s tellar positions suggesting a photospheric origin of this molecule. We see the expected structure of a hollow CN brightness distribution outside that of the HCN emitting region (in particular, for RW LMi and LP And). We have used a non-LTE radiative transfer code, based on the Monte Carlo method, to model the circumstellar HCN and CN line emissions. We have, in addition to the interferometer data, used also multi-transition single dish data as constraints. The results are qualitatively, and in mos t cases also quantitatively, consistent with a simple photodissociation mod el, in which HCN is produced in the stellar atmosphere, while the observed CN is formed in the circumstellar envelope due to the photodissociation of HCN. The most notable discrepancy is the low CN/HCN peak abundance ratios, approximate to0.16, obtained for those objects with the best observational constraints. These are lower by at least a factor of two compared to the re sults of also more elaborate chemical models. Some of our modelling discrep ancies, e.g., the weakness of the model HCN(J = 1 --> 0) intensities, are a ttributed to a too crude treatment of the radiative excitation in the inner region of a circumstellar envelope, and to a lack of knowledge of the dens ity structure and kinematics in the same region. We find it particularly di fficult to model the circumstellar line emissions towards RW LMi, and suspe ct that this is due to, e.g., a mass loss rate that has varied with time an d/or a non-spherical envelope. The HCN and CN brightness maps suggest the l atter. Furthermore, we have obtained interferometric data towards RW LMi in also t he HNC(J = 1 --> 0), HC3N(J = 10 --> 9), HC5N(J = 34 --> 33) and SiS(J = 5 --> 4) lines. The HNC, HC3N, and HC5N molecules appear to be distributed in a shell, while the SIS emission is clearly confined to regions close to th e star. The HCN(J = 1 --> 0), HNC(J = 1 --> 0), and HC3N(J = 10 --> 9) line s show the effect that the peak bright-ness position varies systematically with the velocity. We attribute this to a large-scale asymmetry in the enve lope. We also find that some of the spectra obtained towards the map centre are highly asymmetric, with the redshifted emission being significantly st ronger than the blueshifted emission.