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A Secure W2 Detection of WD 0806-661B from CatWISE

Meisner, A. and Cushing, Michael C. and Cutri, R. and Eisenhardt, Peter R. and Faherty, J. and Fowler, J. W. and Garcia, N. and Gonzalez, A. H. and Jarrett, T. H. and Kirkpatrick, J. Davy and Koontz, R. and Mainzer, A. and Marchese, E. and Marocco, F. and Mobasher, B. and Schlegel, D. and Stanford, S. A. and Stern, D. and Teplitz, H. and Wright, E. L. (2018) A Secure W2 Detection of WD 0806-661B from CatWISE. Research Notes of the AAS, 2 (3). Art. No. 140. ISSN 2515-5172. https://resolver.caltech.edu/CaltechAUTHORS:20180810-095948868

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Abstract

The WD 0806-661 system consists of a DQ white dwarf primary at 19.26 pc (Gaia Collaboration et al. 2018) and an extremely cold common proper motion companion at 130'' separation (WD 0806-661B; Luhman et al. 2011). Given its absolute magnitude at Spitzer [4.5], the cold companion is presumed to be either a Y type brown dwarf or giant planet. At a projected physical separation of ~2500 au, WD 0806-661B represents the widest known definitively planetary-mass companion, and may provide important insights into the processes of star and planet formation. Unlike most Y dwarfs, WD 0806-661B has lacked a secure detection at 4.6 μm in the Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010) W2 channel. WD 0806-661B was reported as a low-significance detection in the WISE All-Sky Source Catalog (Cutri et al. 2012), with W2 = 17.68 ± 0.41 (J080715.32-661851.6, w2snr = 2.5). No detection of a WD 0806-661B counterpart is reported in the AllWISE Source Catalog, although the AllWISE Reject Table contains a low-significance positional match (J080715.34-661852.1) with W2 = 17.85 ± 0.41 (Cutri et al. 2013). Both the All-Sky and AllWISE Reject best-fit W2 magnitudes, if taken at face value, would make WD 0806-661B a very blue outlier among Y dwarfs in [4.5]−W2 color, given that the W2 and [4.5] magnitudes of known Y dwarfs generally agree to within ~0.1 mag.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/2515-5172/aad7c0DOIArticle
ORCID:
AuthorORCID
Meisner, A.0000-0002-1125-7384
Cushing, Michael C.0000-0001-7780-3352
Cutri, R.0000-0002-0077-2305
Faherty, J.0000-0001-6251-0573
Gonzalez, A. H.0000-0002-0933-8601
Jarrett, T. H.0000-0002-4939-734X
Kirkpatrick, J. Davy0000-0003-4269-260X
Marocco, F.0000-0001-7519-1700
Schlegel, D.0000-0002-5042-5088
Stern, D.0000-0003-2686-9241
Teplitz, H.0000-0002-7064-5424
Wright, E. L.0000-0001-5058-1593
Additional Information:© 2018 The American Astronomical Society. Received 2018 August 1; Accepted 2018 August 2; Published 2018 August 7. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. CatWISE is funded by NASA under Proposal No. 16-ADAP16-0077 issued through the Astrophysics Data Analysis Program, and uses data from the NASA-funded WISE and NEOWISE projects. This work has also been supported by Hubble Fellowship HST-HF2-51415.001-A, NASA ADAP grant NNH17AE75I, and has benefited from the Y Dwarf Compendium maintained by Michael Cushing at https://sites.google.com/view/ydwarfcompendium.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
NASA16-ADAP16-0077
NASA Hubble FellowshipHST-HF2-51415.001-A
NASANNH17AE75I
Issue or Number:3
Record Number:CaltechAUTHORS:20180810-095948868
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180810-095948868
Official Citation:A. Meisner et al 2018 Res. Notes AAS 2 140
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:88749
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:13 Aug 2018 15:37
Last Modified:16 Nov 2019 05:52

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