Toward a Unification of Star Formation Rate Determinations in the Milky Way and Other Galaxies

TL;DR

This paper consolidates various SFR estimates for the Milky Way, identifies discrepancies among different measurement methods, and discusses potential reasons and tests for reconciling these differences, aiming for a unified understanding of galactic star formation.

Contribution

It unifies Galactic SFR estimates by normalizing to the same IMF and models, and explores systematic differences among measurement techniques and their implications.

Findings

Galactic SFR estimates converge to 1.9 +/- 0.4 M_sun/yr after normalization.

Resolved stellar populations suggest higher SFRs than IR and radio diagnostics.

Milky Way's SFR measurements show slight deviations from expectations, indicating possible overestimation or calibration issues.

Abstract

The star formation rate (SFR) of the Milky Way remains poorly known, with often-quoted values ranging from 1 to 10 solar masses per year. This situation persists despite the potential for the Milky Way to serve as the ultimate SFR calibrator for external galaxies. We show that various estimates for the Galactic SFR are consistent with one another once they have been normalized to the same initial mass function (IMF) and massive star models, converging to 1.9 +/- 0.4 M_sun/yr. However, standard SFR diagnostics are vulnerable to systematics founded in the use of indirect observational tracers sensitive only to high-mass stars. We find that absolute SFRs measured using resolved low/intermediate-mass stellar populations in Galactic H II regions are systematically higher by factors of ~2-3 as compared with calibrations for SFRs measured from mid-IR and radio emission. We discuss some potential explanations for this discrepancy and conclude that it could be allayed if (1) the power-law slope of the IMF for intermediate-mass (1.5 M_sun < m < 5 M_sun) stars were steeper than the Salpeter slope, or (2) a correction factor was applied to the extragalactic 24 micron SFR calibrations to account for the duration of star formation in individual mid-IR-bright H II regions relative to the lifetimes of O stars. Finally, we present some approaches for testing if a Galactic SFR of ~2 M_sun/yr is consistent with what we would measure if we could view the Milky Way as external observers. Using luminous radio supernova remnants and X-ray point sources, we find that the Milky Way deviates from expectations at the 1-3 sigma level, hinting that perhaps the Galactic SFR is overestimated or extragalactic SFRs need to be revised upwards.