# J-PLUS: the impact of bars on quenching time-scales in nearby green valley disc galaxies

## TL;DR

This study develops a method using J-PLUS and GALEX data to estimate star formation quenching timescales in green valley galaxies and finds that barred galaxies tend to quench more slowly, indicating bars as markers of gradual quenching.

## Contribution

The paper introduces a new empirical approach to measure quenching timescales using specific J-PLUS filters and correlates these timescales with galaxy morphology, particularly bars.

## Key findings

- J-PLUS colours are sensitive to star formation history.
- Quenching timescales from the new method agree with spectral index estimates.
- Barred galaxies tend to quench star formation more slowly.

## Abstract

In a framework where galaxies mostly migrate on the colour-magnitude diagram from star-forming to quiescent, the green valley is considered a transitional galaxy stage. The details of the processes that drive galaxies from star-forming to passive systems still remain unknown. We developed a method that estimates empirically the star formation quenching times-scales of green valley galaxies, assuming an exponential decay model of the SFH and through a combination of narrow and broad bands from J-PLUS and GALEX. We correlate these quenching time-scales with the presence of bars. We find that the J-PLUS colours F0395-g and F0415-g are sensitive to different SFH, showing, a clear correlation with the Dn(4000) and H-delta,A spectral indices. We find that quenching time-scales obtained with our new approach are in agreement with those determined using spectral indices. We also find that galaxies with high bar probability tend to quench their star formation slowly. We conclude that: 1) J-PLUS filters can be used to measure quenching timescales in nearby green valley galaxies; and 2) the resulting star formation quenching time-scales are longer for barred green valley galaxies. Considering that the presence of a bar indicates that more violent processes (e.g., major mergers) are absent in host galaxies, we conclude that the presence of a bar can be used as a morphological signature for slow star formation quenching.