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We model the broad emission lines present in the optical, UV and X-rayspectra of Mrk 509, a bright type 1 Seyfert galaxy. The broad lines weresimultaneously observed during a large multiwavelength campaign, using theXMM-Newton-OM for the optical lines, HST-COS for the UV lines andXMM-Newton-RGS and Epic for the X-ray lines respectively. We also used FUSEarchival data for the broad lines observed in the far-ultra-violet. The goal isto find a physical connection among the lines measured at different wavelengthsand determine the size and the distance from the central source of the emittinggas components. We used the "Locally optimally emission Cloud" (LOC) modelwhich interprets the emissivity of the broad line region (BLR) as regulated bypowerlaw distributions of both gas density and distances from the centralsource. We find that one LOC component cannot model all the linessimultaneously. In particular, we find that the X-ray and UV lines likely mayoriginate in the more internal part of the AGN, at radii in the range~5x10^{14}-3x10^{17} cm, while the optical lines and part of the UV lines maylikely be originating further out, at radii ~3x10^{17}-3x^{18} cm. These twogas components are parametrized by a radial distribution of the luminositieswith a slope gamma of ~1.15 and ~1.10, respectively, both of them covering atleast 60% of the source. This simple parameterization points to a structuredbroad line region, with the higher ionized emission coming from closer in,while the emission of the low-ionization lines is more concentrated in theoutskirts of the broad line region.

Multiwavelength campaign on Mrk 509 XV. A global modeling of the broad emission lines in the Optical, UV and X-ray bands