http://arxiv.org/abs/2108.05487

The stellar mass-to-light ratio gradient in SDSS $r-$band $\nabla (M_/L_r)$ 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 $10^9$ to $10^{12}M_\odot$ released in SDSS DR15, we focus on face-on galaxies, without merger and bar signatures, and investigate the dependence of the 2D $\nabla (M_/L_r)$ on other galaxy properties, including $M_/L_r$-colour relationships by assuming a fixed Salpeter IMF as the mass normalization reference. The median gradient is $\nabla M_/L_r\sim -0.1$ (i.e., the $M_/L_r$ is larger at the centre) for massive galaxies, becomes flat around $M_\sim 10^{10} M_{\odot}$ and change sign to $\nabla M_/L_r\sim 0.1$ at the lowest masses. The $M_/L_r$ 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 $M_/L_r$ 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 $10^{-3} {\rm Gyr}^{-1}$. With increased sSFR gradient, one can obtain a steeper negative $\nabla (M_/L_r)$. The scatter in the slopes of $M_/L$-colour relations increases with increasing sSFR, for example, the slope for post-starburst galaxies can be flattened to $0.45$ from the global value $0.87$ in the $M_/L$ vs. $g-r$ diagram. Hence converting galaxy colours to $M_*/L$ should be done carefully, especially for those galaxies with young luminosity-weighted stellar ages, which can have quite different star formation histories.

Read this paper on arXiv…

J. Ge, S. Mao, Y. Lu, et. al.
Fri, 13 Aug 21
24/64

Comments: 12 pages, 10 figures. Accepted for publication in MNRAS