Evolution of the Stellar Mass–Metallicity Relation. I. Galaxies in the z ∼ 0.4 Cluster Cl0024

Abstract

We present the stellar mass-stellar metallicity relationship (MZR) in the galaxy cluster Cl0024+1654 at z∼0.4 using full-spectrum stellar population synthesis modeling of individual quiescent galaxies. The lower limit of our stellar mass range is M * =10 9.7 M e , the lowest galaxy mass at which individual stellar metallicity has been measured beyond the local universe. We report a detection of an evolution of the stellar MZR with observed redshift at 0.037±0.007 dex per Gyr, consistent with the predictions from hydrodynamical simulations. Additionally, we find that the evolution of the stellar MZR with observed redshift can be explained by an evolution of the stellar MZR with the formation time of galaxies, i.e., when the single stellar population (SSP)-equivalent ages of galaxies are taken into account. This behavior is consistent with stars forming out of gas that also has an MZR with a normalization that decreases with redshift. Lastly, we find that over the observed mass range, the MZR can be described by a linear function with a shallow slope (The slope suggests that galaxy feedback, in terms of mass-loading factor, might be mass-independent over the observed mass and redshift range.

The GOGREEN survey: post-infall environmental quenching fails to predict the observed age difference between quiescent field and cluster galaxies at z > 1

“…We note that these studies all use different methodologies: Gallazzi et al (2005) and Gallazzi et al (2014) relied on line indices, Choi et al (2014) use full spectrum SPS modelling for continuum-corrected co-added spectra, while use full spectrum SPS modelling of spectroscopy and photometry, more similar to our own procedure. Although not shown in Figure B1, Leethochawalit et al (2018) study the MZR with respect to [Fe/H] for quiescent galaxies at z∼0.4 using spectral modelling, and recover values consistent with the highest density (purple) region in our plot (see their figure 7). Interestingly, Kriek et al (2019) measure the metallicity of three massive quiescent galaxies at z∼1.4, using high-resolution spectroscopy to measure absorption lines, Figure B1.…”

The Origin of r-process Enhanced Metal-poor Halo Stars In Now-destroyed Ultra-faint Dwarf Galaxies

“…10 relation based on the z=0 relation determined by Kirby et al (2013) for dwarf galaxies: This z=0 relation is combined with the redshift evolution found by Ma et al (2016) from hydrodynamical simulations: Δ[Fe/H]=0.67 [e −0.5 z −1]. This redshift evolution is consistent with observations (Leethochawalit et al 2018). For the destroyed subhalos that are sufficiently massive to form stars after reionization, we use the redshift of their destruction (z dest ) as the redshift at which to determine their mean metallicity.…”

Revisiting the Planet Mass and Stellar Metallicity Relation for Low-Mass Exoplanets Orbiting GKM Class Stars

“…The inclination (i) is randomly distributed so that it has no impact on the statistical analysis. From Figure 3, we can see that stellar mass increases approximately linearly with stellar metallicity for this group of low-mass exoplanets, a result that is supported by recent studies [17,18]. To show that this massmetallicity correlation does not explain the exponential law trend; we assume a perfect linear correlation between stellar mass and stellar metallicity and perform a linear regression to compute K 1 , in terms of metallicity.…”