We present a coherent multi-band modelling of the CO Spectral Energy Distribution of the local Seyfert Galaxy NGC7130 to assess the impact of the AGN activity on the molecular gas .
We take advantage of all the available data from X-ray to the sub-mm , including ALMA data .
The high-resolution ( \sim { 0.2 } ^ { " } ) ALMA CO ( 6-5 ) data constrain the spatial extension of the CO emission down to \sim 70 pc scale .
From the analysis of the archival Chandra and NuSTAR data , we infer the presence of a buried , Compton-thick AGN of moderate luminosity , L _ { 2 - 10 keV } { \sim } 1.6 { \times } 10 ^ { 43 } erg s ^ { -1 } .
We explore photodissociation and X-ray-dominated regions ( PDRs and XDRs ) models to reproduce the CO emission .
We find that PDRs can reproduce the CO lines up to J { \sim } 6 , however , the higher rotational ladder requires the presence of a separate source of excitation .
We consider X-ray heating by the AGN as a source of excitation , and find that it can reproduce the observed CO Spectral Energy Distribution .
By adopting a composite PDR+XDR model , we derive molecular cloud properties .
Our study clearly indicates the capabilities offered by current-generation of instruments to shed light on the properties of nearby galaxies adopting state-of-the art physical modelling .