Wolf-Rayet Galaxies in SDSS-IV MaNGA. II. Metallicity Dependence of the High-mass Slope of the Stellar Initial Mass Function

Liang, Fu-Heng; Li, Cheng; Li, Niu; Zhou, Shuang; Yan, Renbin; Mo, Houjun; Zhang, Wei

doi:10.3847/1538-4357/ac2bff

Title: Wolf-Rayet Galaxies in SDSS-IV MaNGA. II. Metallicity Dependence of the High-mass Slope of the Stellar Initial Mass Function

Journal Article · 14 December 2021 · The Astrophysical Journal

DOI: https://doi.org/10.3847/1538-4357/ac2bff · OSTI ID:1983196

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Tsinghua Univ., Beijing (China); Univ. of Oxford (United Kingdom)
Tsinghua Univ., Beijing (China)
Univ. of Kentucky, Lexington, KY (United States)
Univ. of Massachusetts, Amherst, MA (United States)
Chinese Academy of Sciences (CAS), Beijing (China). National Astronomical Observatories

As hosts of living high-mass stars, Wolf-Rayet (WR) regions or WR galaxies are ideal objects for constraining the high-mass end of the stellar initial mass function (IMF). We construct a large sample of 910 WR galaxies/regions that cover a wide range of stellar metallicity (from Z ~ 0.001 to 0.03) by combining three catalogs of WR galaxies/regions previously selected from the SDSS and SDSS-IV/MaNGA surveys. We measure the equivalent widths of the WR blue bump at ~4650 Å for each spectrum. They are compared with predictions from stellar evolutionary models Starburst99 and BPASS, with different IMF assumptions (high-mass slope α of the IMF ranging from 1.0 to 3.3). Both singular evolution and binary evolution are considered. We also use a Bayesian inference code to perform full spectral fitting to WR spectra with stellar population spectra from BPASS as fitting templates. We then make a model selection among different α assumptions based on Bayesian evidence. These analyses have consistently led to a positive correlation of the IMF high-mass slope α with stellar metallicity Z, i.e., with a steeper IMF (more bottom-heavy) at higher metallicities. Specifically, an IMF with α = 1.00 is preferred at the lowest metallicity (Z ~ 0.001), and an Salpeter or even steeper IMF is preferred at the highest metallicity (Z ~ 0.03). These conclusions hold even when binary population models are adopted.

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Research Organization:: US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)

Sponsoring Organization:: National Key Research and Development Program of China; National Science Foundation of China (NSFC); USDOE Office of Science (SC)

OSTI ID:: 1983196

Journal Information:: The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 1 Vol. 923; ISSN 0004-637X

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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The Fifteenth Data Release of the Sloan Digital Sky Surveys: First Release of MaNGA-derived Quantities, Data Visualization Tools, and Stellar Library Aguado, D. S.; Ahumada, Romina; Almeida, Andrés The Astrophysical Journal Supplement Series, Vol. 240, Issue 2 https://doi.org/10.3847/1538-4365/aaf651	journal	January 2019

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