2004/02/10 by J. Falcón‐Barroso, J. Falcón-Barroso, R. F. Peletier +16 · 4 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Bulge #Disc galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Hubble sequence #Milky Way #Photometry (optics) #Physics #Stars #Stellar kinematics #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2004.07704.x
published as Mon.Not.Roy.Astron.Soc. 350 (2004) 35 · 12 pages, 12 figures, accepted for publication in MNRAS
arxiv created 2004/02/10 · openalex publication_date 2004/04/21 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present SAURON integral‐field observations of the S0 galaxy NGC 7332. Existing broad‐band ground‐based and Hubble Space Telescope (HST) photometry reveals a double‐disc structure and a boxy bulge interpreted as a bar viewed close to edge‐on. The SAURON two‐dimensional stellar kinematic maps confirm the existence of the bar and inner disc but also uncover the presence of a cold counter‐rotating stellar component within the central 250 pc. The Hβ and [O iii] emission line maps show that the ionized gas has a complex morphology and kinematics, including both a component counter‐rotating with respect to the stars and a fainter corotating one. Analysis of the absorption line‐strength maps show that NGC 7332 is young everywhere. The presence of a large‐scale bar can explain most of those properties, but the fact that we see a significant amount of unsettled gas, together with a few peculiar features in the maps, suggests that NGC 7332 is still evolving. Interactions as well as bar‐driven processes must thus have played an important role in the formation and evolution of NGC 7332, and presumably of S0 galaxies in general.