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The chemical abundances in the Galactic Centre from the atmospheres of Red Supergiants

AutorDavies, Ben; Origlia, Livia; Kudritzki, Rolf-Peter; Figer, Don F.; Rich, R. MIchael; Najarro, Francisco
Palabras claveGalaxy: center
Galaxy: evolution
Stars: Evolution
Stars: late-type
Fecha de publicaciónmar-2009
EditorAmerican Astronomical Society
CitaciónAstrophysical Journal 694(1): 46-55 (2009)
ResumenThe Galactic center (GC) has experienced a high degree of recent star-forming activity, as evidenced by the large number of massive stars currently residing there. The relative abundances of chemical elements in the GC may provide insights into the origins of this activity. Here, we present high-resolution H-band spectra of two red supergiants (RSGs) in the GC (IRS 7 and VR 5-7), and in combination with spectral synthesis we derive abundances for Fe and C, as well as other α-elements Ca, Si, Mg Ti, and O. We find that the C depletion in VR 5-7 is consistent with the predictions of evolutionary models of RSGs, while the heavy depletion of C and O in IRS 7's atmosphere is indicative of deep mixing, possibly due to fast initial rotation and/or enhanced mass loss. Our results indicate that the current surface Fe/H content of each star is slightly above solar. However, comparisons to evolutionary models indicate that the initial Fe-to-H ratio was likely closer to solar, and has been driven higher by H depletion at the stars' surface. Overall, we find α-to-Fe ratios for both stars, which are consistent with the thin Galactic disk. These results are consistent with other chemical studies of the GC, given the precision to which abundances can currently be determined. We argue that the GC abundances are consistent with a scenario in which the recent star-forming activity in the GC was fueled by either material traveling down the Bar from the inner disk, or from the winds of stars in the inner bulge—with no need to invoke top-heavy stellar initial mass functions to explain anomalous abundance ratios.
Descripción23 pages, 4 figures, 2 tables.-- Pre-print archive.
Versión del editorhttp://dx.doi.org/10.1088/0004-637X/694/1/46
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