Cinemática do gás ionizado e molecular quente na região central da rádio galáxia 3C 293

• Ano de defesa: 2026
• Autor(a) principal: Mellos, Maitê Silvana de Zorzi de
• Tipo de documento: Dissertação
• Tipo de acesso: Acesso aberto
• Idioma: por
• Instituição de defesa: Universidade Federal de Santa Maria; Brasil; UFSM; Programa de Pós-Graduação em Física; Centro de Ciências Naturais e Exatas
• Palavras-chave em Português: Núcleos ativos de galáxias; Cinemática de galáxias; Rádio galaxia; Active galactic nuclei; Galaxy kinematics; Radio galaxy; CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA
• Link de acesso: http://repositorio.ufsm.br/handle/1/39038

Active Galactic Nuclei (AGN) play a key role in the evolutionary life of their host galaxies, mainly through the transfer of energy and momentum to the interstellar medium via radiation, winds, and jets. In low-luminosity AGN, the interaction with the host galaxy is often dominated by the mechanical action of jets, which are capable of interacting with the gas and drive outflows. In this context, the radio galaxy 3C 293 constitutes an excellent laboratory for studying the interplay between these processes, as it exhibits a high concentration of molecular gas in its central region, hosts a Low-Ionization Nuclear Emission-line Region (LINER) AGN, and presents an inner jet extending over ∼ 4.5 kpc that propagates through the gas in the galaxy disk. In this work, we use observations of 3C 293 obtained with the James Webb Space Telescope/Near-Infrared Spectrograph to map the emission, extinction, and kinematics of the ionized and warm molecular gas, as well as the stellar kinematics, within the central 3×3 kpc2 region of the galaxy. Our results indicate that the stellar velocity field is well described by a rotating disk model, with the kinematic center displaced by approximately 0.5 arcsec from the nucleus, defined as the position of the continuum peak. The warm molecular gas is traced by the H2 2.12 µm emission line, while the ionized gas by [Fe II] 1.64 µm and Paα. From Gaussian fitting of the emission lines, we identify three distinct kinematic components: a narrow one associated with the rotating disk, with velocity dispersion of ∼ 100 km s−1 ; a broad component associated with an outflow, presenting velocity dispersion of ∼ 250 km s−1 ; and a broader component associated with a faster ionized outflow, exhibiting velocity dispersion of ∼ 640 km s−1 . Extinction maps reveal high AV values for all components, spatially coincident with dust lanes seen in optical images. In addition to the disk and outflows components, inflows along the dust lanes are detected in H2 gas, with a mass inflow rate of M˙ in ≃ 4 × 10−4 M⊙ yr−1 , which is lower than the AGN accretion rate. For the outflows, we derive peak mass-outflow rates of 0.08 ± 0.02 M⊙ yr−1 for the molecular gas and 6.5 ± 1.7 M⊙ yr−1 for the ionized gas. The observed outflow is likely driven by the interaction between the radio jet and the interstellar medium, exhibiting a kinetic power of 5.7% of the jet power, enough to suppress star formation.