Where is the Metallicity Ceiling to Form Carbon Stars? – A Scarcity of Carbon Stars in the Inner Disk of M31

Creators: Boyer, Martha L.; Girardi, L.; Marigo, P.; Williams, B. F.; Aringer, B.; Nowotny, W.; Rosenfield, P.; Dorman, C. E.; Guhathakurta, P.; Dalcanton, J. J.; Melbourne, J. L.; Olsen, K. A. G.; Weisz, D. R.

Others:: Kerschbaum, F.; Wing, R. F.; Hron, J.

Abstract

We have used a novel technique involving near-infrared colors from the Hubble Space Telescope to distinguish C stars from M stars in a field in M31. The resulting C/M ratio is much lower than other estimates in M31.

Additional Information

© 2015 Astronomical Society of the Pacific. This work was supported by the NASA Postdoctoral Program at the GSFC, administered by ORAU through a contract with NASA, and by NASA through HST grant numbers GO-12862 and GO-12055 from the STScI, which is operated by AURA, Inc., under NASA contract NAS5-26555. PM and LG acknowledge support from Progetto di Ateneo 2012, University of Padova, ID: CPDA125588/12. This research was funded in part by the Austrian Science Fund (FWF): P21988-N16.

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