Stellar Population Gradients in ULIRGs: Implications for Gas Inflow Timescales

TL;DR

This study uses optical spectra of ULIRGs to measure star formation history and gas inflow timescales during mergers, revealing outer disk star formation decline and central continuous activity, informing galaxy evolution models.

Contribution

It provides empirical measurements of gas inflow timescales and star formation evolution in ULIRGs, improving understanding of merger-driven galaxy transformation.

Findings

Star formation declines in outer disks about 300-400 Myr ago.

Central regions show ongoing, continuous star formation.

Gas depletion proceeds from outer to inner regions during mergers.

Abstract

Using longslit, optical spectra of Ultraluminous Infrared Galaxies (ULIRGs), we measure the evolution in the star-formation intensity during galactic mergers. In individual galaxies, we resolve kpc scales allowing comparison of the nucleus, inner disk, and outer disk. We find that the strength of the Hbeta absorption line increases with the projected distance from the center of the merger, typically reaching about 9 Angstrom around 10 kpc. At these radii, the star formation intensity must have rapidly decreased about 300-400 Myr ago; only stellar populations deficient in stars more massive than Type A produce such strong Balmer absorption. In contrast, we find the star formation history in the central kpc consistent with continuous star formation. Our measurements indicate that gas depletion occurs from the outer disk inwards during major mergers. This result is consistent with merger-induced gas inflow and empirically constrains the gas inflow timescale. Numerical simulations accurately calculate the total amount of infalling gas but often assume the timescale for infall. These new measurements are therefore central to modeling merger-induced star formation and AGN activity.