Ionized gas kinematics within the inner kiloparsec of the Seyfert galaxy NGC 1365

• Autor(a) principal: Lena, Davide
• Data de Publicação: 2016
• Outros Autores: Robinson, Andrew, Storchi-Bergmann, Thaisa, Couto, Guilherme dos Santos, Müller, Allan Schnorr, Riffel, Rogemar André
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/149994
• topic: Cinemática; Nucleo galatico; Galáxia NGC 1365; Galaxias seyfert; Gas ionizado; Black hole physics; Galaxies: active; Galaxies: individual: NGC 1365; Galaxies: kinematics and dynamics; Galaxies: nuclei; Galaxies: seyfert

We observed the nuclear region of the galaxy NGC 1365 with the integral field unit of the Gemini Multi Object Spectrograph mounted on the GEMINI-South telescope. The field of view covers 13 × 6 arcsec2(1173 × 541 pc2) centred on the nucleus, at a spatial resolution of 52 pc. The spectral coverage extends from 5600 to 7000 Å, at a spectral resolution R = 1918. NGC 1365 hosts a Seyfert 1.8 nucleus, and exhibits a prominent bar extending out to 100 arcsec (9 kpc) from the nucleus. The field of view lies within the inner Lindblad resonance. Within this region, we found that the kinematics of the ionized gas (as traced by [O I], [N II], Hα, and [S II]) is consistent with rotation in the large-scale plane of the galaxy.While rotation dominates the kinematics, there is also evidence for a fan-shaped outflow, as found in other studies based on the [OIII] emission lines. Although evidence for gas inflowing along nuclear spirals has been found in a few barred galaxies, we find no obvious signs of such features in the inner kiloparsec of NGC 1365. However, the emission lines exhibit a puzzling asymmetry that could originate from gas which is slower than the gas responsible for the bulk of the narrow-line emission.We speculate that it could be tracing gas which lost angular momentum, and is slowly migrating from the inner Lindblad resonance towards the nucleus of the galaxy.