A Spectroscopic Census of Cluster White Dwarfs from DESI, LAMOST, and SDSS
Abstract
Gaia has substantially expanded the sample of candidate white dwarfs (WDs) in open clusters, but many remain without spectroscopic characterization. We leverage the increasingly extensive archives of large public spectroscopic surveys to identify 62 candidate cluster WDs with available spectra from DESI, LAMOST, and SDSS. After discarding sources with very low S/N and unreliable host clusters, 44 candidates remain, including 37 non-magnetic DA WDs, of which 15 had not previously been characterized in the literature for cluster studies. We find that nine are consistent with single-star origins in their proposed host clusters, increasing the combined cluster DA initial--final mass relation (IFMR) sample to 132 WDs. All lie within 2σ of the best-fit IFMR from the most comprehensive recent cluster WD sample, suggesting these additions do not require recalibrating the empirical IFMR. One is a likely Hyades tidal-tail WD, providing further evidence that dynamical dispersal helps explain the long-standing WD deficit in the nearest cluster. We further compare WDs with spectra from multiple surveys. Among seven Praesepe WDs observed by both DESI and SDSS, DESI gives higher WD masses in six cases, with a mean difference of 0.067 M⊙, while the inferred progenitor masses differ by as much as 0.459 M⊙. More broadly, nine of ten single-star cluster DAs with DESI spectra lie above the empirical IFMR, with a mean final-mass residual of 0.06±0.04 M⊙. These results show that survey-dependent differences can strongly affect cluster WD parameters, and should be considered when combining heterogeneous spectroscopy in empirical IFMR studies.
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BibTeX
@misc{miller2026spectroscopic,
title = {{A Spectroscopic Census of Cluster White Dwarfs from DESI, LAMOST, and SDSS}},
author = {David R. Miller and Jeremy Heyl and Huahui Yan and Chengyuan Li and Pier-Emmanuel Tremblay},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.14166},
eprint = {2610.14166},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.14166},
}
RIS
TY - UNPB
TI - A Spectroscopic Census of Cluster White Dwarfs from DESI, LAMOST, and SDSS
AU - David R. Miller
AU - Jeremy Heyl
AU - Huahui Yan
AU - Chengyuan Li
AU - Pier-Emmanuel Tremblay
PY - 2026
DA - 2026/10/09
PB - arXiv
DO - 10.48550/arxiv.2610.14166
UR - https://arxiv.org/abs/2610.14166
AB - Gaia has substantially expanded the sample of candidate white dwarfs (WDs) in open clusters, but many remain without spectroscopic characterization. We leverage the increasingly extensive archives of large public spectroscopic surveys to identify 62 candidate cluster WDs with available spectra from DESI, LAMOST, and SDSS. After discarding sources with very low S/N and unreliable host clusters, 44 candidates remain, including 37 non-magnetic DA WDs, of which 15 had not previously been characterized in the literature for cluster studies. We find that nine are consistent with single-star origins in their proposed host clusters, increasing the combined cluster DA initial--final mass relation (IFMR) sample to 132 WDs. All lie within 2σ of the best-fit IFMR from the most comprehensive recent cluster WD sample, suggesting these additions do not require recalibrating the empirical IFMR. One is a likely Hyades tidal-tail WD, providing further evidence that dynamical dispersal helps explain the long-standing WD deficit in the nearest cluster. We further compare WDs with spectra from multiple surveys. Among seven Praesepe WDs observed by both DESI and SDSS, DESI gives higher WD masses in six cases, with a mean difference of 0.067 M_⊙, while the inferred progenitor masses differ by as much as 0.459 M_⊙. More broadly, nine of ten single-star cluster DAs with DESI spectra lie above the empirical IFMR, with a mean final-mass residual of 0.06±0.04 M_⊙. These results show that survey-dependent differences can strongly affect cluster WD parameters, and should be considered when combining heterogeneous spectroscopy in empirical IFMR studies.
ER -