The TYPHOON Stellar Population Synthesis Survey. I. The Young Stellar Population of the Great Barred Spiral NGC 1365

• Published in: The Astrophysical journal Vol. 960; no. 1; pp. 83 - 94
• Main Authors: Sextl, Eva, Kudritzki, Rolf-Peter, Burkert, Andreas, Ho, I-Ting, Zahid, H. Jabran, Seibert, Mark, Battisti, Andrew J., Madore, Barry F., Rich, Jeffrey A.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01-01-2024; IOP Publishing
• Subjects: Active galactic nuclei; Astrophysics; Barred spiral galaxies; Chemical evolution; Extinction; Galaxies; Galaxy chemical evolution; Line spectra; Luminosity; Metal content; Metallicity; Spatial distribution; Spiral galaxies; Star & galaxy formation; Star formation; Starburst galaxies; Stars; Stellar populations; Stellar winds; Supernova; Synthesis; Typhoons
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad08b3

Abstract
We analyze TYPHOON long-slit-absorption line spectra of the starburst barred spiral galaxy NGC 1365 obtained with the Progressive Integral Step Method covering an area of 15 kpc
2
. Applying a population synthesis technique, we determine the spatial distribution of ages and metallicities of the young and old stellar populations together with star formation rates, reddening, extinction, and the ratio
R
V
of extinction to reddening. We detect a clear indication of inside-out growth of the stellar disk beyond 3 kpc characterized by an outward increasing luminosity fraction of the young stellar population, a decreasing average age, and a history of mass growth, which was finished 2 Gyr later in the outermost disk. The metallicity of the young stellar population is clearly super solar but decreases toward larger galactocentric radii with a gradient of −0.02 dex kpc
−1
. On the other hand, the metal content of the old population does not show a gradient and stays constant at a level roughly 0.4 dex lower than that of the young population. In the center of NGC 1365, we find a confined region where the metallicity of the young population drops dramatically and becomes lower than that of the old population. We attribute this to the infall of metal-poor gas, and additionally, to interrupted chemical evolution where star formation is stopped by active galactic nuclei and supernova feedback and then after several gigayears resumes with gas ejected by stellar winds from earlier generations of stars. We provide a simple model calculation as support for the latter.