CaltechAUTHORS
  A Caltech Library Service

A New Class of Large-amplitude Radial-mode Hot Subdwarf Pulsators

Kupfer, Thomas and Bauer, Evan B. and Burdge, Kevin B. and Bellm, Eric C. and Bildsten, Lars and Fuller, Jim and Hermes, J. J. and Kulkarni, Shrinivas R. and Prince, Thomas A. and van Roestel, Jan and Dekany, Richard and Duev, Dmitry A. and Feeney, Michael and Giomi, Matteo and Graham, Matthew J. and Kaye, Stephen and Laher, Russ R. and Masci, Frank J. and Porter, Michael and Riddle, Reed and Shupe, David L. and Smith, Roger M. and Soumagnac, Maayane T. and Szkody, Paula and Ward, Charlotte (2019) A New Class of Large-amplitude Radial-mode Hot Subdwarf Pulsators. Astrophysical Journal Letters, 878 (2). Art. No. L35. ISSN 2041-8213. http://resolver.caltech.edu/CaltechAUTHORS:20190617-135126883

[img] PDF - Published Version
See Usage Policy.

794Kb
[img] PDF - Submitted Version
See Usage Policy.

450Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20190617-135126883

Abstract

Using 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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/2041-8213/ab263cDOIArticle
https://arxiv.org/abs/1906.00979arXivDiscussion Paper
ORCID:
AuthorORCID
Kupfer, Thomas0000-0002-6540-1484
Bauer, Evan B.0000-0002-4791-6724
Bellm, Eric C.0000-0001-8018-5348
Fuller, Jim0000-0002-4544-0750
Kulkarni, Shrinivas R.0000-0001-5390-8563
Prince, Thomas A.0000-0002-8850-3627
Duev, Dmitry A.0000-0001-5060-8733
Graham, Matthew J.0000-0002-3168-0139
Laher, Russ R.0000-0003-2451-5482
Masci, Frank J.0000-0002-8532-9395
Riddle, Reed0000-0002-0387-370X
Shupe, David L.0000-0003-4401-0430
Soumagnac, Maayane T.0000-0001-6753-1488
Alternate Title:A new class of pulsating hot subdwarfs
Additional Information:© 2019 The American Astronomical Society. Received 2019 May 13; revised 2019 May 29; accepted 2019 June 1; published 2019 June 18. Based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. This work makes use of observations from the LCOGT network. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research was supported in part by the National Science Foundation through grants AST-1514737, ACI-1663688, and at the KITP by grant PHY-1748958. This research benefited from interactions that were funded by the Gordon and Betty Moore Foundation through Grant GBMF5076. Facilities: PO:1.2 m (ZTF) - , LCOGT (Spectral) - , Hale (DBSP - , Chimera) - , Keck:I (LRIS). - Software: Lpipe (Perley 2019), PyRAF (Bellm & Sesar 2016), Gatspy (VanderPlas & Ivezić 2015), Period04 (Lenz & Breger 2005), FITSB2 (Napiwotzki et al. 2004), MESA (Paxton et al. 2011, 2013, 2015, 2018), GYRE (Townsend & Teitler 2013), Matplotlib (Hunter 2007), Astropy (Astropy Collaboration et al. 2013, 2018), Numpy (Oliphant 2015).
Group:Infrared Processing and Analysis Center (IPAC), Zwicky Transient Facility
Funders:
Funding AgencyGrant Number
NSFAST-1440341
W. M. Keck FoundationUNSPECIFIED
NSFAST-1514737
NSFACI-1663688
NSFPHY-1748958
Gordon and Betty Moore FoundationGBMF5076
Subject Keywords:asteroseismology – stars: oscillations – stars: variables: general – white dwarfs
Record Number:CaltechAUTHORS:20190617-135126883
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190617-135126883
Official Citation:Thomas Kupfer et al 2019 ApJL 878 L35
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96475
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:17 Jun 2019 21:32
Last Modified:12 Jul 2019 21:47

Repository Staff Only: item control page