In the standard cosmological model, the assembly of galaxies is primarily driven by the growth of their host dark matter halos. At the centre of these halos, however, baryonic processes take over, leading to the plethora of observed galaxy properties. The coupling between baryonic and dark matter physics is central to our understanding of galaxies, and yet, it remains a challenge for theoretical models and observations. Here, we demonstrate that measured ages, metallicities, stellar angular momentum, morphology and star formation rates are correlated with both stellar and halo mass. We find using dynamical modelling that at fixed stellar mass, CALIFA galaxies are younger, more metal-poor and rotationally supported and have higher star formation rates and later-type morphologies as their total mass increases, due to the independent measurements of the stellar and total masses. These results indicate that the formation of galaxies and, thus, their baryonic properties do not vary with stellar mass alone, with halo mass also playing an important role.

在标准宇宙学模型中，星系的聚集主要是由其宿主暗物质晕的增长驱动的。然而，在这些光晕的中心，重子过程占据主导地位，导致观察到大量的星系特性。重子物理和暗物质物理之间的耦合是我们理解星系的核心，然而，它仍然是理论模型和观测的一个挑战。在这里，我们证明测量的年龄、金属丰度、恒星角动量、形态和恒星形成率与恒星和晕质量相关。我们使用动力学模型发现，在固定的恒星质量下，CALIFA 星系更年轻，金属更贫乏，并且受到旋转支撑，并且随着总质量的增加，具有更高的恒星形成率和晚型形态，这是由于对恒星和总质量的独立测量。群众。这些结果表明，星系的形成及其重子特性并不仅随恒星质量而变化，晕质量也发挥着重要作用。