PDRs4All
J. R. Goicoechea, J. Pety, S. Cuadrado, Olivier Berné, E. Dartois, M. Gerin, C. Joblin, Jacek Kłos, F. Lique, T. Onaka, E. Peeters, A. G. G. M. Tielens, Felipe Alarcón, Émeric Bron, J. Cami, Amélie Canin, E. Chapillon, Ryan Chown, A. Fuente, E. Habart, Olga Kannavou, Franck Le Petit, Miriam G. Santa-Maria, Ilane Schroetter, Ameek Sidhu, Boris Trahin, Dries Van De Putte, Marion Zannese
Abstract
The infrared emission from polycyclic aromatic hydrocarbons (PAHs), along with emission from atomic carbon and simple hydrocarbons, is a robust tracer of the interaction between stellar far-UV (FUV) radiation and molecular clouds. We present subarcsecond-resolution ALMA mosaics of the Orion Bar photodissociation region (PDR) in [C I ] 609 μm ( 3 P 1 − 3 P 0 ), C 2 H ( N = 4−3), and C 18 O ( J = 3−2) emission lines complemented by JWST images of H 2 and aromatic infrared band (AIB) emission. We interpreted the data using up-to-date PDR and radiative transfer models, including high-temperature C 2 H (X 2 Σ + )- o / p -H 2 and C ( 3 P)- o / p -H 2 inelastic collision rate coefficients (we computed the latter up to 3000 K). The rim of the Bar shows very corrugated and filamentary structures made of small-scale H 2 dissociation fronts (DFs). The [C I ] 609 μm emission peaks very close (≲ 0.002 pc) to the main H 2 -emitting DFs, suggesting the presence of gas density gradients. These DFs are also bright and remarkably similar in C 2 H emission, which traces “hydrocarbon radical peaks” characterized by very high C 2 H abundances, reaching up to several ×10 −7 . The high abundance of C 2 H and of related hydrocarbon radicals, such as CH 3 , CH 2 , and CH, can be attributed to gas-phase reactions driven by elevated temperatures, the presence of C + and C, and the reactivity of FUV-pumped H 2 . The hydrocarbon radical peaks roughly coincide with maxima of the 3.4/3.3 μm AIB intensity ratio, which is a proxy for the aliphatic-to-aromatic content of PAHs. This implies that the conditions triggering the formation of simple hydrocarbons also favor the formation (and survival) of PAHs with aliphatic side groups, potentially via the contribution of bottom-up processes in which abundant hydrocarbon radicals react in situ with PAHs. Ahead of the DFs, in the atomic PDR zone (where [H] ≫ [H 2 ]), the AIB emission is the brightest, but small PAHs and carbonaceous grains undergo photo-processing due to the stronger FUV field. Our detection of trace amounts of C 2 H in this zone may result from the photoerosion of these species. This study provides a spatially resolved view of the chemical stratification of key carbon carriers in a PDR. Overall, both bottom-up and top-down processes appear to link simple hydrocarbon molecules with PAHs in molecular clouds; however, the exact chemical pathways and their relative contributions remain to be quantified.