Searching for Spectroscopic Signatures of Ongoing Quenching in SDSS Galaxies

TL;DR

This study analyzes spectroscopic data from SDSS galaxies to investigate ongoing quenching of star formation, confirming some trends but finding limitations in conclusively detecting systematic quenching processes, with indications consistent with models suggesting a quenching timescale of about 500 Myr.

Contribution

It introduces the SFR$_{79}$ parameter for large galaxy samples and assesses its effectiveness in detecting ongoing quenching in SDSS galaxies, expanding previous findings.

Findings

Confirmed trends of star formation in SDSS galaxies.

Identified limitations in observational data and calibration for detecting quenching.

Found plausible signs of ongoing quenching consistent with models.

Abstract

In this paper we estimate the "star formation change parameter", SFR$_{79}$, which characterizes the current SFR relative to the average during the last 800 Myr, for $\sim$ 300'000 galaxies selected from the Sloan Digital Sky Survey (SDSS). The goals are to examine, in a much larger and independent sample, the trends previously reported in a sample of star-forming MaNGA galaxies, and also to search for spectroscopic signatures of ongoing quenching in the so-called "Green Valley", which is generally believed to contain galaxies that are migrating from the star-forming (SF) population to the quenched population of galaxies. Measuring SFR$_{79}$ for our large sample of SDSS galaxies, we first confirm the basic results of SF galaxies published by Wang & Lilly. We then discuss in detail the calibration and meaning of SFR$_{79}$ for galaxies that are well below the SFMS and establish the expected statistical signature of systematic ongoing quenching from modelling the z$\sim$0 quenching rate of the SF population. We conclude that it is not possible at present to establish unambiguous observational evidence for systematic ongoing quenching processes, due to limitations both in the noise of the observational data, in particular in the measurements of H$\delta$ absorption, and in the calibration of SFR$_{79}$, as well as biases introduced by the necessity of selecting objects with significant H$\alpha$ emission. We do however see plausible indications of ongoing quenching, which are quantitatively consistent with expectations from "growth+quenching" models of galaxy evolution and a typical e-folding timescale for quenching of $\sim500$ Myr.