SDSS-IV MaNGA: Stellar M/L gradients and the M/L-colour relation in galaxies
arXiv:2108.05487 · doi:10.1093/mnras/stab2341
Abstract
The stellar mass-to-light ratio gradient in SDSS band of a galaxy depends on its mass assembly history, which is imprinted in its morphology and gradients of age, metallicity, and stellar initial mass function (IMF). Taking a MaNGA sample of 2051 galaxies with stellar masses ranging from to released in SDSS DR15, we focus on face-on galaxies, without merger and bar signatures, and investigate the dependence of the 2D on other galaxy properties, including -colour relationships by assuming a fixed Salpeter IMF as the mass normalization reference. The median gradient is (i.e., the is larger at the centre) for massive galaxies, becomes flat around and change sign to at the lowest masses. The inside a half light radius increases with increasing galaxy stellar mass; in each mass bin, early-type galaxies have the highest value, while pure-disk late-type galaxies have the smallest. Correlation analyses suggest that the mass-weighted stellar age is the dominant parameter influencing the profile, since a luminosity-weighted age is easily affected by star formation when the specific star formation rate (sSFR) inside the half light radius is higher than . With increased sSFR gradient, one can obtain a steeper negative . The scatter in the slopes of -colour relations increases with increasing sSFR, for example, the slope for post-starburst galaxies can be flattened to from the global value in the vs. diagram. Hence converting galaxy colours to should be done carefully, especially for those galaxies with young luminosity-weighted stellar ages, which can have quite different star formation histories.
arXiv comment12 pages, 10 figures. Accepted for publication in MNRAS
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