2002/02/18 by M. Contini, M. Radovich, P. Rafanelli +1 · 16 citations
Physics and Astronomy · #Active galactic nucleus #Astronomy and Astrophysical Research #Emission spectrum #Galaxies: Formation, Evolution, Phenomena #Galaxy #Line (geometry) #Shock wave #Spectral line #Stars #Stellar, planetary, and galactic studies #Supernova #astro-ph
paper · pdf · doi:10.1086/340287
published in The Astrophysical Journal 572(1), 124-139 (IOP Publishing) · 36 pages +10 figures PostScript To appear in The Astrophysical Journal
arxiv created 2002/02/18 · openalex publication_date 2002/06/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Detailed modeling of the different regions of NGC 7130 is presented, accounting for its composite nature of an active galactic nucleus (AGN) and a starburst galaxy. Shock waves, created by stellar winds from hot massive stars and by supernova ejecta, are evident in the continuum and line spectra emitted from the clouds. Therefore, the SUMA code, which accounts consistently for photoionization and shocks, is adopted in model calculation. The results show that the nuclear region is dominated by gas ionized by a power-law radiation flux from the active center (AC). High-velocity ( V s = 1000 km s -1 ) clouds, which account for the broad FWHM component of the line profile, are found close to the AC and are characterized by a high dust-to-gas ratio (>10 -12 , while the dust-to-gas ratio is about 10 -14 throughout the galaxy). Massive stars with temperatures of (5-7) × 10 4 K photoionize and heat the gas in the outer regions, and old star population ( T * = 3000 K) background radiation contributes to the fit of the continuum in the optical-near-IR range. The AGN-starburst connection is discussed on the basis of model results, considering, particularly, the distribution of densities and velocities throughout the galaxy.