SDSS-IV MaNGA: The Spatially Resolved Stellar Initial Mass Function in $\sim$400 Early-Type Galaxies

TL;DR

This study uses MaNGA data to measure spatial variations in the stellar initial mass function (IMF) in about 400 early-type galaxies, revealing a central bottom-heavy IMF that becomes more Milky Way-like outward, with implications for galaxy evolution.

Contribution

It provides the first detailed radial IMF gradient measurements in a large sample of early-type galaxies using optical and near-infrared features, demonstrating the impact of metallicity and mass on IMF variations.

Findings

Negative IMF gradients with bottom-heavy centers and Milky Way-like outskirts.

IMF-$\sigma$ relation within galaxies is steeper than the global relation.

Radial IMF gradient is consistent across different stellar population models.

Abstract

MaNGA provides the opportunity to make precise spatially resolved measurements of the IMF slope in galaxies owing to its unique combination of spatial resolution, wavelength coverage and sample size. We derive radial gradients in age, element abundances and IMF slope analysing optical and near-infrared absorption features from stacked spectra out to the half-light radius of 366 early-type galaxies with masses $9.9 - 10.8\;\log M/M_{\odot}$. We find flat gradients in age and [$\alpha$/Fe] ratio, as well as negative gradients in metallicity, consistent with the literature. We further derive significant negative gradients in the [Na/Fe] ratio with galaxy centres being well enhanced in Na abundance by up to 0.5 dex. Finally, we find a gradient in IMF slope with a bottom-heavy IMF in the centre (typical mass excess factor of 1.5) and a Milky Way-type IMF at the half-light radius. This pattern is mass-dependent with the lowest mass galaxies in our sample featuring only a shallow gradient around a Milky Way IMF. Our results imply the local IMF-$\sigma$ relation within galaxies to be even steeper than the global relation and hint towards the local metallicity being the dominating factor behind the IMF variations. We also employ different stellar population models in our analysis and show that a radial IMF gradient is found independently of the stellar population model used. A similar analysis of the Wing-Ford band provides inconsistent results and further evidence of the difficulty in measuring and modelling this particular feature.