Strong spiral arms drive secular growth of pseudo bulges in disk galaxies

Abstract

Spiral-driven instabilities may drive gas inflow to enhance central star formation in disk galaxies. We investigate this hypothesis using the Sloan Digital Sky Survey (SDSS) in a sample of 2779 nearby unbarred star-forming main-sequence spiral galaxies. The strength of spiral arms is quantified by their average Fourier amplitude relative to the axisymmetric disk. The star formation properties in the central 1-3 kpc region were derived from the SDSS spectra. We show that galaxies with stronger spiral arms not only tend to have more intense central specific star formation rate (sSFR), larger Balmer absorption line index, and lower 4000-Å break strength, but also have enhanced central sSFR relative to sSFR measured for the whole galaxy. This link is independent of redshift, stellar mass, surface density, and concentration. There is a lack of evidence for strong spiral arms being associated with a significant fraction of starburst or post-starburst galaxies, implying that the spiral-induced central star formation is likely continuous rather than bursty. We also show that stronger spiral arms tend to have an increasing fraction of pseudo bulges, a relatively unchanged fraction of star-forming classical bulges, and a decreasing fraction of quenched classical bulges. Moreover, the concentration of galaxies hosting pseudo bulges mildly increases with stronger spiral arms, implying that spirals help pseudo bulges grow. The connection between spirals and the bulge type is partly attributed to the suppression of spirals by classical bulges and partly to the enhanced central star formation driven by spirals. We explain our results in a picture where spiral arms transport cold gas inward to trigger continuous central star formation, which facilitates the build-up of pseudo bulges. Spiral arms thus play a role in the secular evolution of disk galaxies.

Centrally Concentrated H i Distribution Enhances Star Formation in Galaxies

“…optical radius is critical for star formation in galaxies. The angular momentum of the gas can be redistributed by internal processes due to bars (e.g., Fanali et al 2015) and spiral arms (e.g., Yu et al 2021Yu et al , 2022b, and external processes such as minor mergers (e.g., Mihos & Hernquist 1994), major merger (e.g., Toomre & Toomre 1972;Barnes 2004;Larson et al 2016), and tidal interactions (e.g., Larson 2002).…”