2018/01/01 by Rogemar A. Riffel, C Hekatelyne, C. Hekatelyne +1
Chemistry · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Chemistry #Flux (metallurgy) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy rotation curve #Geometry #Kinematics #Line (geometry) #Meteorology #Milky Way #Outflow #Physics #Position angle #RADIUS #Rotation (mathematics) #Spectral line #Spectrograph #Stellar kinematics #Stellar, planetary, and galactic studies #Velocity dispersion #astro-ph.GA
paper · pdf · doi:10.1017/pasa.2018.31
Submitted to PASA, after include the referee's suggestions
openalex publication_date 2018/01/01 · arxiv created 2018/07/08 · openalex created_date 2018/07/19 · arxiv updated 2018/12/05 · openalex updated_date 2026/08/05
Abstract We use Gemini Multi-Object Spectrograph integral Field Unit observations of the inner 285 × 400 pc 2 region of the Seyfert 2 galaxy NGC 5643 to map the [S iii ]λ9069 emission line flux distribution and kinematics, as well as the stellar kinematics, derived by fitting the Ca ii λλλ8498,8542,8662 triplet, at a spatial resolution of 45 pc. The stellar velocity field shows regular rotation, with a projected velocity of 100 km s −1 and kinematic major axis along a position angle of –36°. A ring of low stellar velocity dispersion values (∼70 km s −1 ), attributed to young/intermediate age stellar populations, is seen surrounding the nucleus with a radius of 50 pc. We found that the [S iii ] flux distribution shows an elongated structure along the east–west direction and its kinematics is dominated by outflows within a bi-cone at an ionised gas outflow rate of 0.3 M ⊙ yr −1 . In addition, velocity slices across the [S iii ]λ9069 emission line reveal a kinematic component attributed to rotation of gas in the plane of the galaxy.