Figure 4 from An Ancient Extrasolar System with Five Sub-Earth-size Planets

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An Ancient Extrasolar System with Five Sub-Earth-size Planets

Authors: T. L. Campante, T. Barclay, J. J. Swift, D. Huber, V. Zh. Adibekyan, W. Cochran, C. J. Burke, H. Isaacson, E. V. Quintana, G. R. Davies, V. Silva Aguirre, D. Ragozzine, R. Riddle, C. Baranec, S. Basu, W. J. Chaplin, J. Christensen-Dalsgaard, T. S. Metcalfe, T. R. Bedding, R. Handberg, D. Stello, J. M. Brewer, S. Hekker, C. Karoff, R. Kolbl, N. M. Law, M. Lundkvist, A. Miglio, J. F. Rowe, N. C. Santos, C. Van Laerhoven, T. Arentoft, Y. P. Elsworth, D. A. Fischer, S. D. Kawaler, H. Kjeldsen, M. N. Lund, G. W. Marcy, S. G. Sousa, A. Sozzetti, and T. R. White

Campante et al. 2015 The Astrophysical Journal 799 170.

Provider: AAS Journals

Caption: Figure 4.

[Ti/Fe] abundance ratio vs. [Fe/H] in the low-metallicity regime. Kepler-444 is denoted by a blue star. Blue triangles represent the Kepler planet-candidate host stars of Adibekyan et al. (2012a) with available titanium abundances. Black dots correspond to stars without planetary companions observed in the context of the HARPS GTO planet search program. The dashed line marks the fiducial chemical separation between the thin and thick disks (below and above the line, respectively; Adibekyan et al. 2012a) based solely on the HARPS GTO sample.

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