Project 1640 observations of the white dwarf HD 114174 B
Abstract
We present the first near infrared spectrum of the faint white dwarf companion HD 114174 B, obtained with Project 1640. Our spectrum, covering the Y, J and H bands, combined with previous TaRgetting bENchmark-objects with Doppler Spectroscopy (TRENDS) photometry measurements, allows us to place further constraints on this companion. We suggest two possible scenarios; either this object is an old, low-mass, cool H atmosphere white dwarf with T_(eff) ∼ 3800 K or a high-mass white dwarf with T_(eff) > 6000 K, potentially with an associated cool (T_(eff) ∼ 700 K) brown dwarf or debris disc resulting in an infrared excess in the L΄ band. We also provide an additional astrometry point for 2014 June 12 and use the modelled companion mass combined with the radial velocity and direct imaging data to place constraints on the orbital parameters for this companion.
Additional Information
© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 May 10. Received 2017 April 28; in original form 2017 February 2. Published: 15 May 2017. We thank Tim Pearce, Grant Kennedy and Matthew Kenworthy for their helpful discussions concerning the astrometry of HD 114174 B. We also thank Simon Hodgkin for his input concerning the data reduction and calibration of our data for this object and the referee for their detailed and helpful comments. P1640 is funded by National Science Foundation grants AST-0520822, AST-0804417 and AST-0908484. In addition, part of this work was performed under a contract with the California Institute of Technology funded by NASA through the Sagan Fellowship Program and part of the research in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). EB is supported by an STFC studentship, JA is supported by the Laboratory for Physical Sciences, College Park and MD, through the National Physical Science Consortium graduate fellowship programme. JC was supported by the US National Science Foundation under award no. 1009203. RN was funded by the Swedish Research Council's International Postdoctoral grant no. 637-2013-474. JRC acknowledges support from NASA Origins Grant NNX13AB03G and the NASA Early Career programme. The members of the Project 1640 team are also grateful for support from the Cordelia Corporation, Hilary and Ethel Lipsitz, the Vincent AstorFund, Judy Vale, Andrew Goodwin and an anonymous donor. This paper is based on observations obtained at the Hale Telescope, Palomar Observatory. This research made use of the Washington Double Star Catalogue maintained at the US Naval Observatory, the SIMBAD data base, operated by the CDS in Strasbourg, France, NASA's Astrophysics Data System and data from ESA's Gaia mission. Facilities: Hale (Project 1640).Attached Files
Published - Bacchus_2017p4796.pdf
Submitted - 1705.11030.pdf
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Additional details
- Eprint ID
- 81033
- Resolver ID
- CaltechAUTHORS:20170831-140837359
- AST-0520822
- NSF
- AST-0804417
- NSF
- AST-0908484
- NSF
- NASA/JPL/Caltech
- Science and Technology Facilities Council (STFC)
- Laboratory for Physical Sciences
- National Physical Science Consortium
- AST-1009203
- NSF
- 637-2013-474
- Swedish Research Council
- NNX13AB03G
- NASA
- Cordelia Corporation
- Hilary and Ethel Lipsitz
- Vincent Astor Fund
- Judy Vale
- Andrew Goodwin
- NASA Sagan Fellowship
- Created
-
2017-08-31Created from EPrint's datestamp field
- Updated
-
2021-11-15Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC), Astronomy Department