The TRENDS High-contrast Imaging Survey. VII. Discovery of a Nearby Sirius-like White Dwarf System (HD 169889)
Abstract
Monitoring the long-term radial velocity (RV) and acceleration of nearby stars has been proven as an effective method for directly detecting binary and substellar companions. Some fraction of nearby RV trend systems are expected to be comprised of compact objects that likewise induce a systemic Doppler signal. In this paper, we report the discovery of a white dwarf (WD) companion found to orbit the nearby (π = 28.297 ± 0.066 mas) G9 V star HD 169889. High-contrast imaging observations using NIRC2 at the W. M. Keck Observatory and LMIRCam at the Large Binocular Telescope (LBT) Observatory uncover the (ΔH = 9.76 ± 0.16, ΔL' = 9.60 ± 0.03) companion at an angular separation of 0."8 (28 au). Thirteen years of precise Doppler observations reveal a steep linear acceleration in the RV time series and place a dynamical constraint on the companion mass of M ≥ 0.369 ± 0.010 M_⊙. This "Sirius-like" system adds to the census of WD companions suspected to be missing from surveys of in the solar neighborhood.
Additional Information
© 2018 The American Astronomical Society. Received 2018 May 7; revised 2018 July 11; accepted 2018 July 11; published 2018 August 29. The TRENDS high-contrast imaging program is supported in part by NASA Origins of Solar Systems grant NNX13AB03G. J.R.C. acknowledges support from the NASA Early Career Fellowship and NSF Career Fellowship. E.J.G. acknowledges support from the NSF graduate research fellowship program. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. 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 LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are: The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University, and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota, and University of Virginia. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper made use of WD cooling models from http://www.astro.umontreal.ca/~bergeron/CoolingModels/. We are deeply grateful for the vision and support of the Potenziani and Wolfe families.Attached Files
Published - Crepp_2018_ApJ_864_42.pdf
Accepted Version - 1807.06012.pdf
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Additional details
- Eprint ID
- 89300
- Resolver ID
- CaltechAUTHORS:20180830-090413303
- NASA
- NNX13AB03G
- NSF Graduate Research Fellowship
- W. M. Keck Foundation
- Created
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2018-08-30Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department