Suh, HyewonHyewonSuhCivano, FrancescaFrancescaCivanoHasinger, GüntherGüntherHasingerLUSSO, ELISABETAELISABETALUSSOLANZUISI, GiorgioGiorgioLANZUISIMARCHESI, STEFANOSTEFANOMARCHESITrakhtenbrot, BennyBennyTrakhtenbrotALLEVATO, VIOLAVIOLAALLEVATOCAPPELLUTI, NicoNicoCAPPELLUTICapak, Peter L.Peter L.CapakElvis, MartinMartinElvisGriffiths, Richard E.Richard E.GriffithsLaigle, ClotildeClotildeLaigleLira, PaulinaPaulinaLiraRiguccini, LaurieLaurieRigucciniRosario, David J.David J.RosarioSalvato, MaraMaraSalvatoSchawinski, KevinKevinSchawinskiVIGNALI, CRISTIANCRISTIANVIGNALI2020-12-222020-12-2220170004-637Xhttp://hdl.handle.net/20.500.12386/29096We investigate the star formation properties of a large sample of ∼2300 X-ray-selected Type 2 Active Galactic Nuclei (AGNs) host galaxies out to z∼ 3 in the Chandra COSMOS Legacy Survey in order to understand the connection between the star formation and nuclear activity. Making use of the existing multi-wavelength photometric data available in the COSMOS field, we perform a multi-component modeling from far-infrared to near-ultraviolet using a nuclear dust torus model, a stellar population model and a starburst model of the spectral energy distributions (SEDs). Through detailed analyses of SEDs, we derive the stellar masses and the star formation rates (SFRs) of Type 2 AGN host galaxies. The stellar mass of our sample is in the range of 9< {log} {M}<SUB>{stellar</SUB>}/{M}<SUB>☉ </SUB>< 12 with uncertainties of ∼0.19 dex. We find that Type 2 AGN host galaxies have, on average, similar SFRs compared to the normal star-forming galaxies with similar M <SUB>stellar</SUB> and redshift ranges, suggesting no significant evidence for enhancement or quenching of star formation. This could be interpreted in a scenario, where the relative massive galaxies have already experienced substantial growth at higher redshift (z> 3), and grow slowly through secular fueling processes hosting moderate-luminosity AGNs.STAMPAenArticle10.3847/1538-4357/aa725c2-s2.0-85020877622000402560200003https://iopscience.iop.org/article/10.3847/1538-4357/aa725c2017ApJ...841..102SFIS/05 - ASTRONOMIA E ASTROFISICA