SDSS IV MaNGA : star-formation driven biconical outflows in face-on galaxies

• Autor(a) principal: Bizyaev, D.
• Data de Publicação: 2022
• Outros Autores: Chen, Yan-Mei, Shi, Yong, Roy, Namrata, Riffel, Rogério, Riffel, Rogemar André, Fernández-Trincado, José Gregorio
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/254615
• topic: Galáxias; Formacao de estrelas; Cinemática; ISM : Jets and outflows; Galaxies : Interactions; Galaxies : ISM; Galaxies : kinematics and dynamics; Galaxies : Star formation; Galaxies : Structure

We find 132 face-on and low inclination galaxies with central star formation driven biconical gas outflows (FSFB) in the SDSS MaNGA (Mapping Nearby Galaxies at APO) survey. The FSFB galaxies show either double peaked or broadened emission line profiles at their centres. The peak and maximum outflow velocities are 58 and 212 km s−1, respectively. The gas velocity dispersion reveals a mild dependence on the central star formation surface density compatible with models of gas dispersion powered by the Jeansinstability in gas clumps or by gasturbulence dissipation. We estimate the gas outflow rate and conclude that the central gas depletion time does not depend on galactic mass. In turn, the ratio of the gas outflow rate to the gas consumption rate by the star formation is low in massive galaxies and high in low mass objects, while the star formation is a more rapid process of the gas consumption. We compare properties of the FSFB galaxies with a control sample of 375 comparison galaxies and find that the FSFB objects have high central concentration of star formation and also younger central stellar population with respect to their periphery. We analysed the environment of the galaxies and identified nearby satellites and elements of low surface brightness structure. We see that many tidal-enhanced features that can be assigned to early and intermediate stages of galactic interaction are much more frequent in the FSFB galaxies with respect to the comparison sample. We conclude that the gas should be replenished via the accretion from small satellites.