A emissão do gás da região de linhas estreitas em galáxias Seyfert próximas

• Main Author: Santos, Izabel Cristina Freitas dos
• Publication Date: 2017
• Format: Doctoral thesis
• Language: por
• Source: Manancial - Repositório Digital da UFSM
• Download full: http://repositorio.ufsm.br/handle/1/14629
• topic: Galáxias ativas; Galáxias Seyfert; Mrk 6; Mrk 79; Mrk 348; Mrk 607; Mrk 1058; Galaxies active; Seyfert galaxies; Mrk 6; Mrk 79; Mrk 348; Mrk 607; Mrk 1058; CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA

The Active Galactic Nuclei (AGNs) show high luminosities ( 109 L ) and emit energy from the accretion disk around the central Supermassive Black Hole (SMBH). The Narrow Line Region (NLR) is the only AGN structure spatially resolved in the optical by current telescopes. It shows extensions typically of a few hundred of parsecs and is formed by low density gaseous clouds (≈10³cm⁻³). In this work, we used data obtained with the Integral Field Unit (IFU) of the Gemini Multi-Object Spectrograph (GMOS) instrument of the Gemini North telescope, to study the gas distribution, excitation and kinematics in the NLR of five nearby Seyfert galaxies (Mrk 6, Mrk 79, Mrk 348, Mrk 607 e Mrk 1058). The data cover the inner 3:005 5:000 – corresponding to physical scales in the range (0,6 to 0,9) (1,5 to 2,2) kpc2 at the galaxy – at a spatial resolution ranging from 110 to 280 pc with a spectral coverage of 4300 – 7100 Å and spectral resolution of ≈ 90 kms⁻¹. We fitted the line profiles at each spaxel by Gaussian curves using adapted versions of the PROFIT routine and constructed maps for the flux distributions, kinematics and intensity line-ratios for the galaxies of our sample. The gas excitation is Seyfert-like over the whole field-of-view in all galaxies. However, we can see ionization gradients of the gas that are correlated with the highest velocities dispersion regions and we have interpreted them as being due to nuclear outflows that reach line-of-sight velocities up to ≈200 kms⁻¹. Bipolar outflows are observed in Mrk 348 and Mrk 79, while in Mrk 1058 only the blueshifted part is clearly observed.