Extended Data Fig. 3: The IMF power-law index as a function of [M/H] measured with different methods and different stellar models.
From: Stellar initial mass function varies with metallicity and time
![Extended Data Fig. 3: The IMF power-law index as a function of [M/H] measured with different methods and different stellar models.](http://media.springernature.com/full/springer-static/esm/art%3A10.1038%2Fs41586-022-05488-1/MediaObjects/41586_2022_5488_Fig6_ESM.jpg?as=webp)
a, The red filled rectangles are derived by all stars with the hierarchical Bayesian model considering the exponential Galactic disk profile. The filled stars denote the values of α derived directly from the observed densities of stars in the |z| range from 100 to 250 pc. b, The IMF power-law slope as a function of [M/H] based on various stellar models and empirical MLR, respectively. The red filled rectangles are derived by PARSEC, and the black rectangles are derived by Dartmouth56. The blue rectangles denote the values of α from the empirical mass–luminosity relation48. Error bars represent 1σ uncertainty.
