Age-divided mean stellar populations from full spectrum fitting as the simplified star formation and chemical evolution history of a galaxy:methodology and reliability

• Published in: Monthly Notices of the Royal Astronomical Society
• Main Authors: Lee, Joon Hyeop, Pak, Mina, Jeong, Hyunjin, Oh, Sree
• Format: Article in Journal/Newspaper
• Language: English
• Published: 2023
• Subjects: galaxies: abundances; galaxies: evolution; galaxies: formation; galaxies: stellar content; sami
• Online Access: https://researchers.mq.edu.au/en/publications/680fcfbc-34a4-4909-afbb-cebbe983f5d8; https://doi.org/10.1093/mnras/stad814; http://www.scopus.com/inward/record.url?scp=85160291355&partnerID=8YFLogxK; http://purl.org/au-research/grants/arc/CE170100013

We introduce a practical methodology for investigating the star formation and chemical evolution history of a galaxy: age-divided mean stellar populations (ADPs) from full spectrum fitting. In this method, the mass-weighted mean stellar populations and mass fractions (f mass ) of young and old stellar components in a galaxy are separately estimated, which are divided with an age cut (selected to be 10 9.5 yr ≈3.2 Gyr in this paper). To examine the statistical reliability of ADPs, we generate 10 000 artificial galaxy spectra, each of which consists of five random simple stellar population components. Using the Penalized PiXel-Fitting (ppxf) package, we conduct full spectrum fitting to the artificial spectra with noise as a function of wavelength, imitating the real noise of Sydney-Australian Astronomical Observatory Multi-object Integral field spectrograph (SAMI) galaxies. As a result, the Δ(= output - input) of age and metallicity appears to significantly depend on not only signal-to-noise ratio (S/N), but also luminosity fractions (f lum ) of young and old components. At given S/N and f lum , Δ of young components tends to be larger than Δof old components; e.g. σ(Δ[M/H]) ∼0.40 versus 0.23 at S/N = 30 and f lum = 50 per cent. The age-metallicity degeneracy appears to be insignificant, but Δlog(age/yr) shows an obvious correlation with Δfmass for young stellar components (R∼ 0.6). The impact of dust attenuation and emission lines appears to be mostly insignificant. We discuss how this methodology can be applied to spectroscopic studies of the formation histories of galaxies, with a few examples of SAMI galaxies.