Kupfer, ThomasBauer, Evan B.Burdge, Kevin B.Bellm, Eric C.Bildsten, LarsFuller, JimHermes, James J.Kulkarni, Shrinivas R.Prince, Thomas A.van Roestel, JanDekany, RichardDuev, Dmitry A.Feeney, MichaelGiomi, MatteoGraham, Matthew J.Kaye, StephenLaher, Russ R.Masci, Frank J.Porter, MichaelRiddle, ReedShupe, David L.Smith, Roger M.Soumagnac, Maayane T.Szkody, PaulaWard, Charlotte2020-04-092020-04-092019Thomas Kupfer, Evan B Bauer, Kevin B Burdge, Eric C Bellm, Lars Bildsten, Jim Fuller, J.J. Hermes, Shrinivas R Kulkarni, Thomas A Prince, Jan van Roestel, Richard Dekany, Dmitry A Duev, Michael Feeney, Matteo Giomi, Matthew J Graham, Stephen Kaye, Russ R Laher, Frank J Masci, Michael Porter, Reed Riddle, David L Shupe, Roger M Smith, Maayane T Soumagnac, Paula Szkody, Charlotte Ward. "A New Class of Large-amplitude Radial-mode Hot Subdwarf Pulsators." The Astrophysical Journal, Volume 878, Issue 2, pp. L35 - L35. https://doi.org/10.3847/2041-8213/ab263c2041-8213https://hdl.handle.net/2144/40091Using high-cadence observations from the Zwicky Transient Facility at low Galactic latitudes, we have discovered a new class of pulsating, hot compact stars. We have found four candidates, exhibiting blue colors (g − r ≤ −0.1 mag), pulsation amplitudes of >5%, and pulsation periods of 200–475 s. Fourier transforms of the light curves show only one dominant frequency. Phase-resolved spectroscopy for three objects reveals significant radial velocity, T eff, and log(g) variations over the pulsation cycle, which are consistent with large-amplitude radial oscillations. The mean T eff and log(g) for these stars are consistent with hot subdwarf B (sdB) effective temperatures and surface gravities. We calculate evolutionary tracks using MESA and adiabatic pulsations using GYRE for low-mass, helium-core pre-white dwarfs (pre-WDs) and low-mass helium-burning stars. Comparison of low-order radial oscillation mode periods with the observed pulsation periods show better agreement with the pre-WD models. Therefore, we suggest that these new pulsators and blue large-amplitude pulsators (BLAPs) could be members of the same class of pulsators, composed of young ≈0.25–0.35 M ⊙ helium-core pre-WDs.p. L35en-US© 2019. The American Astronomical Society. All rights reserved.AsteroseismologyStars: oscillationsStars: variables: generalWhite dwarfsAstronomy & astrophysicsAstronomical and space sciencesArticle10.3847/2041-8213/ab263c477797