An Empirical Measurement of the Initial-Final Mass Relation with Gaia White Dwarfs

Abstract

We use data from Gaia DR2 to constrain the initial-final mass relation (IFMR) for field stars with initial masses $0.9\lesssim m_{\mathrm{in}}/M_{\odot }\lesssim 8$. Precise parallaxes have revealed unprecedented substructure in the white dwarf (WD) cooling sequence on the color-magnitude diagram (CMD). Some of this substructure stems from the diversity of WD atmospheric compositions, but the CMD remains bimodal even when only spectroscopically-confirmed DA WDs are considered. We develop a generative model to predict the CMD for DA WDs as a function of the initial mass function (IMF), stellar age distribution, and a flexibly parameterized IFMR. We then fit the CMD of 1100 bright DA WDs within 100 pc, for which atmospheric composition and completeness are well-understood. The resulting best-fit IFMR flattens at $3.5\lesssim m_{\mathrm{in}}/M_{\odot }\lesssim 5.5$, producing a secondary peak in the WD mass distribution at $m_{\mathrm{WD}}\sim 0.8M_{\odot }$. Our IFMR is broadly consistent with weaker constraints obtained from binaries and star clusters in previous work but represents the clearest observational evidence obtained to date of theoretically-predicted non-linearity in the IFMR. A visibly bimodal CMD is only predicted for mixed-age stellar populations: in single-age clusters, more massive WDs reach the bottom of the cooling sequence before the first lower-mass WDs appear. This may explain why bimodal cooling sequences have thus far evaded detection in cluster CMDs.

7 pages, 4 figures. Accepted to ApJL

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