HINOTORI I: The Nature of Rejuvenation Galaxies

TL;DR

This study constructs a large sample of rejuvenation galaxies, revealing their properties, star formation histories, and potential mechanisms, highlighting their role in ongoing cosmic star formation.

Contribution

The paper introduces the largest sample of rejuvenation galaxies and demonstrates a method to detect weak rejuvenation events using spectral energy distribution fitting.

Findings

Rejuvenation galaxies constitute about 10% of the sample.

Rejuvenation events contribute approximately 0.1% of stellar mass but 17% of current star formation.

RGs are more disk-like than quiescent galaxies, indicating morphology's role in rejuvenation.

Abstract

We present the HINOTORI (star formation History INvestigatiOn TO find RejuvenatIon) project to reveal the nature of rejuvenation galaxies (RGs), which are galaxies that restarted their star formation after being quiescent. As the first step of HINOTORI, we construct the largest RG sample with 1071 sources. We select these RGs from 8857 MaNGA (Mapping Nearby Galaxies at APO) survey galaxies by reconstructing their star formation histories with Prospector spectral energy distribution fitting code. Both optical spectral data and UV to IR photometric data are used for the fitting. Using mock data, we confirm that our method can detect weak rejuvenation events that form only about 0.1% of the total stellar mass with high completeness. The RGs account for ~10% of the whole sample, and rejuvenation events contribute on average only about 0.1% of the total stellar mass in those galaxies but 17% of the cosmic-star formation rate density today. Our RGs have a similar mass distribution to quiescent galaxies (QGs). However, the morphology of the RGs is more disk-like than QGs, suggesting that rejuvenation may occur selectively in disk-like QGs. Our results also suggest the possibility of multiple-time rejuvenation events in a single galaxy. Further spatially resolved analyses of integral field unit data and radio observations and comparisons to simulations are needed to identify the mechanism and the role of rejuvenation in galaxy evolution.