Seminário será apresentado pelo pós-doutorando da Instituto de Astronomía de la Universidade Nacional Autónoma de México (UNAM), Eduardo Alberto Duarte Lacerda
Demais autores: Sebastián F. Sánchez, Roberto Cid Fernandes, Carlos López-Cobá, Carlos Espinosa-Ponce, Lluís Galbany
Resumo: With new observations from the CALIFA survey, we perform a comparison between the physical properties of AGN hosts and their non-active counterparts. The CALIFA survey provides data with excellent spatial and spectral resolutions to this goal. Firstly we choose the candidates to host an AGN.
They are selected analysing their central 3″ x 3″ region (approximately the radius of the spatial PSF FWHM). This election is made based on the analysis of very well-known excitation diagrams: [NII]/Hα, [SII]/Hα and [OI]/Hα vs [OIII]/Hβ together with a cut in the equivalent width of Hα. For the Type-I AGN hosts classification we search for those with best signal-to-noise on the fit of a broad component of Hα.
About 4 per cent (33) of the 810 galaxies on our bona-fide sample are consider hosting a Type-I or TypeII AGN. We found that the AGN hosts have morphology type mostly between Sa to Sbc galaxies, are more massive and with intermediate mean stellar ages (between SFG and RG). They are systems with more central stellar surface density and with a peak of 0.4 for the distribution of central velocity-tovelocity dispersion (v/σ) ratio, that means that are more supported by pressure. We found that the AGN hosts are between the so-called green-valley and the star-forming main sequence at most majority of the analysed diagrams.