The Open Cluster Chemical Abundances and Mapping Survey. VII. APOGEE DR17 [C/N]-Age Calibration

Spoo T.; Tayar J.; Frinchaboy P.M.; Cunha K.; Myers N.; Donor J.; Majewski S.R.; Bizyaev D.; García-Hernández D.A.; Jönsson H.; Lane R.R.; Pan K.; Longa-Peña P.; Roman-Lopes A.

Publication

The Open Cluster Chemical Abundances and Mapping Survey. VII. APOGEE DR17 [C/N]-Age Calibration

Spoo T.; Tayar J.; Frinchaboy P.M.; Cunha K.; Myers N.; Donor J.; Majewski S.R.; Bizyaev D.; García-Hernández D.A.; Jönsson H.; Lane R.R.; Pan K.; Longa-Peña P.; Roman-Lopes A.

Publisher

AAS

Date

2022

Abstract

Large-scale surveys open the possibility to investigate Galactic evolution both chemically and kinematically; however, reliable stellar ages remain a major challenge. Detailed chemical information provided by high-resolution spectroscopic surveys of the stars in clusters can be used as a means to calibrate recently developed chemical tools for age-dating field stars. Using data from the Open Cluster Abundances and Mapping survey, based on the Sloan Digital Sky Survey/Apache Point Observatory Galactic Evolution Experiment 2 survey, we derive a new empirical relationship between open cluster stellar ages and the carbon-to-nitrogen ([C/N]) abundance ratios for evolved stars, primarily those on the red giant branch. With this calibration, [C/N] can be used as a chemical clock for evolved field stars to investigate the formation and evolution of different parts of our Galaxy. We explore how mixing effects at different stellar evolutionary phases, like the red clump, affect the derived calibration. We have established the [C/N]-age calibration for APOGEE Data Release 17 (DR17) giant star abundances to be log[Age(yr)]DR17=10.14(±0.08)+2.23(±0.19)[C/N], usable for 8.62?log(Age[yr])?9.82, derived from a uniform sample of 49 clusters observed as part of APOGEE DR17 applicable primarily to metal-rich, thin- and thick-disk giant stars. This measured [C/N]-age APOGEE DR17 calibration is also shown to be consistent with asteroseismic ages derived from Kepler photometry. © 2022. The Author(s). Published by the American Astronomical Society.