2026-06-04T20:13:48Zivo://CDS.VizieR/J/A+A/709/A382026-05-19T14:14:26ZJ.A_AIVOAPAH across the Orion BarJWST observations of the Orion Bar have revealed rich and diverse Polycyclic Aromatic Hydrocarbon (PAH) emission. These observations allow for the first time a comprehensive characterisation of the charge state and size of the PAH population on morphologically resolved PDR scales, properties closely linked to physical conditions of their inhabiting environments. We investigate the evolution of the PAH population's charge state and size across key physical zones in the Orion Bar, which include the HII region, the atomic PDR (APDR), and three bright HI/H_2_ dissociation fronts (DF1, DF2, and DF3). We connect changes in PAH charge and size as probed by empirical emission proxies with the varying physical properties of their surrounding environments. Utilising the NASA Ames PAH Infrared Spectroscopic Database (PAHdb) and the pyPAHdb spectral modelling tool, we analysed the MIRI-MRS observations of the Orion Bar from the "PDRs4All" JWST Early Release Science Program. Decomposition and modelling was performed on the 5-15um spectrum across the entire JWST mosaic, as well as on the weighted average spectra of the five key physical zones. pyPAHdb modelling reveals the fractional contribution of the different PAH charge states and sizes to the total PAH emission across the Orion Bar. Cationic PAH emission peaks in the APDR region, where neutral PAHs have minimal contribution. Emission from neutral PAHs peaks in the HII region that consists of emission from a face-on PDR associated to the background OMC-1 molecular cloud, and in the molecular cloud regions past DF2. PAH anions are observed deep within the DF2 and DF3 zones. Small and medium sized PAHs make up ~70% of the PAH emission across the mosaic, with the peak of the small PAH emission found between the DF2 and DF3 zones. The average PAH size in the Orion Bar ranges between ~60-74N_C_ . The modelling reveals regions of top-down PAH formation at the ionisation front, and bottom-up PAH formation within the molecular cloud region. The PAH ionisation parameter gamma ranges between ~2-9x10^4^. Intensity ratios which are empirical tracers of PAH ionisation (I_6.2_ /I_11.2_, I_7.7_ /I_11.2_, I_8.6_ /I_11.2_) scale well with gamma in regions encompassing edge-on or face-on PDR emission, but their correlation weakens within the molecular cloud zone. Modelling of the 5-15um PAH spectrum with pyPAHdb achieves comprehensive characterization of the net contribution of neutral and cationic PAHs across different environments, whereas empirical PAH proxy intensity ratio tracers can be highly variable and unreliable outside regions dominated by PDR emission. The derived average PAH size in the different physical zones is consistent with a view of PAHs being more extensively subjected to ultraviolet processing closer to the ionisation front, and less affected within the molecular cloud.h-ii-regionsinterstellar-mediuminfrared-astronomyobservational-astronomyhttps://dc.g-vo.org/rr/q/lp/custom/CDS.VizieR/J/A+A/709/A38https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/709/A382026A&A...709A..38Mhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/709/A38Maragkoudakis A.Boersma C.Peeters E.Allamandola J.L.Temi P.,Esposito J.V.Bregman D.J.Ricca A.Alarcon F.Berne O.Buragohain M.,Cami J.Canin A.Chown R.Dartois E.Fuente F.Goicoechea J.R.,Habart E.Kannavou O.Khan B.Lai T.S.-Y.Onaka T.Van De Putte D.,Schroetter I.Sidhu A.Tielens A.G.G.M.Trahin B.Zhang Y.CDS2026https://cds.unistra.fr/vizier-org/licences_vizier.htmlCDS support team <cds-question@unistra.fr>DatasetAstroObjectsastronomy