RETURN TO [Log-]NORMALCY: RETHINKING QUENCHING, THE STAR FORMATION MAIN SEQUENCE, AND PERHAPS MUCH MORE

• Published in: The Astrophysical journal 2016-11, Vol.832 (1), p.7
• Main Authors: Abramson, Louis E., Gladders, Michael D., Dressler, Alan, Oemler, Augustus, Poggianti, Bianca, Vulcani, Benedetta
• Format: Article
• Language: English
• Subjects: Astronomical models; Astrophysics; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; Computer simulation; COMPUTERIZED SIMULATION; CORRELATIONS; DENSITY; Downsizing; GALACTIC EVOLUTION; GALAXIES; galaxies: evolution; galaxies: formation; galaxies: luminosity function, mass function; galaxies: star formation; Initial conditions; LUMINOSITY; MASS; QUENCHING; Spatial data; Star & galaxy formation; STAR EVOLUTION; Star formation; Star formation rate; STARS; Stars & galaxies; Stellar evolution; Stellar mass
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/0004-637X/832/1/7

ABSTRACT Knowledge of galaxy evolution rests on cross-sectional observations of different objects at different times. Understanding of galaxy evolution rests on longitudinal interpretations of how these data relate to individual objects moving through time. The connection between the two is often assumed to be clear, but we use a simple "physics-free" model to show that it is not and that exploring its nuances can yield new insights. Comprising nothing more than 2094 loosely constrained lognormal star formation histories (SFHs), the model faithfully reproduces the following data it was not designed to match: stellar mass functions at the slope of the star formation rate/stellar mass relation (the SFR "Main Sequence") at the mean of low-mass galaxies at "fast-" and "slow-track" quenching; downsizing; and a correlation between formation timescale and similar to results from simulations that provides a natural connection to bulge growth. We take these findings-which suggest that quenching is the natural downturn of all SFHs affecting galaxies at rates/times correlated with their densities-to mean that: (1) models in which galaxies are diversified on Hubble timescales by something like initial conditions rival the dominant grow-and-quench framework as good descriptions of the data; or (2) absent spatial information, many metrics of galaxy evolution are too undiscriminating-if not inherently misleading-to confirm a unique explanation. We outline future tests of our model but stress that, even if ultimately incorrect, it illustrates how exploring different paradigms can aid learning and, we hope, more detailed modeling efforts.