The Initial‐Final Mass Relation: Direct Constraints at the Low‐Mass End
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The initial-final mass relation represents a mapping between the mass of a white dwarf remnant and the mass that the hydrogen-burning main-sequence star that created it once had. The empirical relation thus far has been constrained using a sample of ~40 stars in young open clusters, ranging in initial mass from ~2.75 to 7 M ☉ , and shows a general trend that connects higher mass main-sequence stars with higher mass white dwarfs. In this paper, we present CFHT CFH12K photometric and Keck LRIS multiobject spectroscopic observations of a sample of 22 white dwarfs in two older open clusters, NGC 7789 ( t = 1.4 Gyr) and NGC 6819 ( t = 2.5 Gyr). We measure masses for the highest signal-to-noise ratio spectra by fitting the Balmer lines to atmosphere models and place the first direct constraints on the low-mass end of the initial-final mass relation. Our results indicate that the observed general trend at higher masses continues down to low masses, with M initial = 1.6 M ☉ main-sequence stars forming M final = 0.54 M ☉ white dwarfs. When added to our new data from the very old cluster NGC 6791, the relation is extended down to M initial = 1.16 M ☉ (corresponding to M final = 0.53 M ☉ ). This extension of the relation represents a fourfold increase in the total number of hydrogen-burning stars for which the integrated mass loss can now be calculated from empirical data, assuming a Salpeter initial mass function. The new leverage at the low-mass end is used to derive a purely empirical initial-final mass relation. The sample of white dwarfs in these clusters also shows several interesting systems that we discuss further: a DB (helium) white dwarf, a magnetic white dwarf, a DAB (mixed hydrogen/helium atmosphere or a double degenerate DA+DB) white dwarf(s), and two possible equal-mass DA double degenerate binary systems.
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Large populations of disk and halo white dwarfs will provide unprecedented constraints on their luminosity function, yielding independent ages for the Galactic disk and halo.
“These large populations of disk and halo white dwarfs will provide unprecedented constraints on the luminosity function of these stars, which will directly yield independent ages for the Galactic disk and halo”
From LSST: From Science Drivers to Reference Design and Anticipated Data Products (2019) · cites this paper as Kalirai et al. 2008
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- Authors
- Kalirai, J. S., Hansen, B. M. S., Kelson, D. D., Reitzel, D. B., Rich, R. M., & Richer, H. B.
- Affiliations
- University of California, Los Angeles (US)
- Carnegie Institution for Science (US)
- University of British Columbia (CA)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2008-03-20
- Volume
- 676
- Issue
- 1
- Pages
- 594-609
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2017540369
- Cited by
- 327
- References
- 77
- Citations by year
- 2026: 10 · 2025: 8 · 2024: 6 · 2023: 12 · 2022: 6 · 2021: 12 · 2020: 14 · 2019: 16 · 2018: 18 · 2017: 17 · 2016: 33 · 2015: 18 · 2014: 26 · 2013: 23 · 2012: 19
- FWCI
- 16.91
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Aeronautics and Space Administration (NAS 526555)
- W. M. Keck Foundation
- California Institute of Technology
- Space Telescope Science Institute (NAS5- 26555, 26555)
- Natural Sciences and Engineering Research Council of Canada
- Institut national des sciences de l'Univers
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Gamma-ray bursts and supernovae
- Keywords
- initial-final mass relation, white dwarfs, low-mass stars, open clusters, NGC 7789, NGC 6819, NGC 6791, white dwarf mass, stellar mass loss, Salpeter initial mass function, DB white dwarfs, magnetic white dwarfs, double degenerate binaries
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Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
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