scholarly journals Variability in the stellar initial mass function at low and high mass: three-component IMF models

2004 ◽  
Vol 354 (2) ◽  
pp. 367-374 ◽  
Author(s):  
B. G. Elmegreen
Keyword(s):  
Mass Function ◽  
Initial Mass Function ◽  
High Mass ◽  
Initial Mass ◽  
Stellar Initial Mass Function

scholarly journals THE HIGH-MASS STELLAR INITIAL MASS FUNCTION IN M31 CLUSTERS

2015 ◽  
Vol 806 (2) ◽  
pp. 198 ◽  
Author(s):  
Daniel R. Weisz ◽  
L. Clifton Johnson ◽  
Daniel Foreman-Mackey ◽  
Andrew E. Dolphin ◽  
Lori C. Beerman ◽  
...  
Keyword(s):  
Mass Function ◽  
Initial Mass Function ◽  
High Mass ◽  
Initial Mass ◽  
Stellar Initial Mass Function

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

2021 ◽  
Vol 923 (1) ◽  
pp. 120
Author(s):  
Fu-Heng Liang ◽  
Cheng Li ◽  
Niu Li ◽  
Shuang Zhou ◽  
Renbin Yan ◽  
...  
Keyword(s):  
Mass Function ◽  
Initial Mass Function ◽  
High Mass ◽  
Initial Mass ◽  
Spectral Fitting ◽  
Wide Range ◽  
Bayesian Evidence ◽  
Stellar Initial Mass Function ◽  
Binary Evolution ◽  
The Imf

Abstract 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.

scholarly journals Is the stellar initial mass function universal?

2016 ◽  
Vol 57 (2) ◽  
pp. 2.32-2.36 ◽  
Author(s):  
Ignacio Ferreras ◽  
Francesco La Barbera ◽  
Alexandre Vazdekis
Keyword(s):  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Stellar Initial Mass Function
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