Red Supergiants as Cosmic Abundance Probes: Massive Star Clusters in M83 and the Mass–Metallicity Relation of Nearby Galaxies

Journal Article · Sun Oct 01 04:00:00 EDT 2017 · Astrophysical Journal

DOI:https://doi.org/10.3847/1538-4357/AA89ED· OSTI ID:22875740

Davies, Ben; Lardo, Carmela; Beasor, Emma; Bastian, Nate ^[1]; Kudritzki, Rolf-Peter ^[2]; Bergemann, Maria ^[3]; Plez, Bertrand ^[4]; Evans, Chris ^[5]; Patrick, Lee R. ^[6]

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1. Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park ic2, 146 Brownlow Hill, Liverpool L3 5RF (United Kingdom)
2. Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)
3. Max-Planck Institute for Astronomy, D-69117, Heidelberg (Germany)
4. Laboratoire Univers et Particules de Montpellier, Université de Montpellier 2, CNRS, F-34095 Montpellier (France)
5. UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ (United Kingdom)
6. Instituto de Astrofsica de Canarias, E-38205 La Laguna, Tenerife (Spain)

We present an abundance analysis of seven super star clusters in the disk of M83. The near-infrared spectra of these clusters are dominated by red supergiants, and the spectral similarity in the J-band of such stars at uniform metallicity means that the integrated light from the clusters may be analyzed using the same tools as those applied to single stars. Using data from VLT/KMOS, we estimate metallicities for each cluster in the sample. We find that the abundance gradient in the inner regions of M83 is flat, with a central metallicity of [Z]=0.21±0.11 relative to a solar value of Z {sub ⊙} = 0.014, which is in excellent agreement with the results from an analysis of luminous hot stars in the same regions. Compiling this latest study with our other recent work, we construct a mass–metallicity relation for nearby galaxies based entirely on the analysis of RSGs. We find excellent agreement with the other stellar-based technique—that of blue supergiants—as well as with temperature-sensitive (“auroral” or “direct”) H ii-region studies. Of all the H ii-region strong-line calibrations, those that are empirically calibrated to direct-method studies (N2 and O3N2) provide the most consistent results.

• OSTI ID: 22875740
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 847; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
CALIBRATION
GALACTIC EVOLUTION
GALAXIES
INFRARED SPECTRA
MASS
METALLICITY
STAR CLUSTERS
STARS