JWST Observations of the Enigmatic Y-Dwarf WISE 1828+2650. I. Limits to a Binary Companion
The Y-dwarf WISE 1828+2650 is one of the coldest known brown dwarfs with an effective temperature of ∼300 K. Located at a distance of just 10 pc, previous model-based estimates suggest WISE1828+2650 has a mass of ∼5–10 M J , making it a valuable laboratory for understanding the formation, evolution,...
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| Veröffentlicht in: | The Astrophysical journal 2023-05, Vol.948 (2), p.92 |
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| creator | De Furio, Matthew Lew, Ben Beichman, Charles Roellig, Thomas Bryden, Geoffrey Ciardi, David Meyer, Michael Rieke, Marcia Greenbaum, Alexandra Leisenring, Jarron Llop-Sayson, Jorge Ygouf, Marie Albert, Loic Boyer, Martha Eisenstein, Daniel Hodapp, Klaus Horner, Scott Johnstone, Doug Kelly, Doug Misselt, Karl Rieke, George Stansberry, John Young, Erick |
| description | The Y-dwarf WISE 1828+2650 is one of the coldest known brown dwarfs with an effective temperature of ∼300 K. Located at a distance of just 10 pc, previous model-based estimates suggest WISE1828+2650 has a mass of ∼5–10
M
J
, making it a valuable laboratory for understanding the formation, evolution, and physical characteristics of gas giant planets. However, previous photometry and spectroscopy have presented a puzzle, with the near impossibility of simultaneously fitting both the short- (0.9–2.0
μ
m) and long-wavelength (3–5
μ
m) data. A potential solution to this problem has been the suggestion that WISE 1828+2650 is a binary system whose composite spectrum might provide a better match to the data. Alternatively, new models being developed to fit JWST/NIRSpec, and MIRI spectroscopy might provide new insights. This article describes JWST/NIRCam observations of WISE 1828+2650 in six filters to address the binarity question and to provide new photometry to be used in model fitting. We also report adaptive optics imaging with the Keck I0 m telescope. We find no evidence for multiplicity for a companion beyond 0.5 au with either JWST or Keck. Companion articles will present low- and high-resolution spectra of WISE 1828 obtained with both NIRSpec and MIRI. |
| doi_str_mv | 10.3847/1538-4357/acbf1e |
| format | Article |
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M
J
, making it a valuable laboratory for understanding the formation, evolution, and physical characteristics of gas giant planets. However, previous photometry and spectroscopy have presented a puzzle, with the near impossibility of simultaneously fitting both the short- (0.9–2.0
μ
m) and long-wavelength (3–5
μ
m) data. A potential solution to this problem has been the suggestion that WISE 1828+2650 is a binary system whose composite spectrum might provide a better match to the data. Alternatively, new models being developed to fit JWST/NIRSpec, and MIRI spectroscopy might provide new insights. This article describes JWST/NIRCam observations of WISE 1828+2650 in six filters to address the binarity question and to provide new photometry to be used in model fitting. We also report adaptive optics imaging with the Keck I0 m telescope. We find no evidence for multiplicity for a companion beyond 0.5 au with either JWST or Keck. Companion articles will present low- and high-resolution spectra of WISE 1828 obtained with both NIRSpec and MIRI.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/acbf1e</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Adaptive optics ; Astrophysics ; Binary stars ; Brown dwarfs ; Gas giant planets ; Infrared spectroscopy ; James Webb Space Telescope ; Optics ; Photometry ; Physical properties ; Planetary evolution ; Planets ; Spectroscopy ; Spectrum analysis ; Theoretical models ; Visual binary stars ; Y dwarfs</subject><ispartof>The Astrophysical journal, 2023-05, Vol.948 (2), p.92</ispartof><rights>2023. The Author(s). Published by the American Astronomical Society.</rights><rights>2023. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c416t-a837375492168a67ae19d1211c242995059c23b5fb4107b5247c442c5ef070843</citedby><cites>FETCH-LOGICAL-c416t-a837375492168a67ae19d1211c242995059c23b5fb4107b5247c442c5ef070843</cites><orcidid>0000-0003-1227-3084 ; 0000-0003-1487-6452 ; 0000-0002-0834-6140 ; 0000-0001-7591-2731 ; 0000-0003-2303-6519 ; 0000-0002-5741-3047 ; 0000-0002-5627-5471 ; 0000-0003-4850-9589 ; 0000-0002-6730-5410 ; 0000-0002-7162-8036 ; 0000-0003-0475-9375 ; 0000-0002-6773-459X ; 0000-0002-6395-4296 ; 0000-0003-0786-2140 ; 0000-0001-9886-6934 ; 0000-0002-7893-6170 ; 0000-0003-2434-5225 ; 0000-0003-1863-4960 ; 0000-0002-2929-3121 ; 0000-0002-3414-784X ; 0000-0001-5966-837X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/acbf1e/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,776,780,860,2096,27901,27902,38867,53842</link.rule.ids></links><search><creatorcontrib>De Furio, Matthew</creatorcontrib><creatorcontrib>Lew, Ben</creatorcontrib><creatorcontrib>Beichman, Charles</creatorcontrib><creatorcontrib>Roellig, Thomas</creatorcontrib><creatorcontrib>Bryden, Geoffrey</creatorcontrib><creatorcontrib>Ciardi, David</creatorcontrib><creatorcontrib>Meyer, Michael</creatorcontrib><creatorcontrib>Rieke, Marcia</creatorcontrib><creatorcontrib>Greenbaum, Alexandra</creatorcontrib><creatorcontrib>Leisenring, Jarron</creatorcontrib><creatorcontrib>Llop-Sayson, Jorge</creatorcontrib><creatorcontrib>Ygouf, Marie</creatorcontrib><creatorcontrib>Albert, Loic</creatorcontrib><creatorcontrib>Boyer, Martha</creatorcontrib><creatorcontrib>Eisenstein, Daniel</creatorcontrib><creatorcontrib>Hodapp, Klaus</creatorcontrib><creatorcontrib>Horner, Scott</creatorcontrib><creatorcontrib>Johnstone, Doug</creatorcontrib><creatorcontrib>Kelly, Doug</creatorcontrib><creatorcontrib>Misselt, Karl</creatorcontrib><creatorcontrib>Rieke, George</creatorcontrib><creatorcontrib>Stansberry, John</creatorcontrib><creatorcontrib>Young, Erick</creatorcontrib><title>JWST Observations of the Enigmatic Y-Dwarf WISE 1828+2650. I. Limits to a Binary Companion</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>The Y-dwarf WISE 1828+2650 is one of the coldest known brown dwarfs with an effective temperature of ∼300 K. Located at a distance of just 10 pc, previous model-based estimates suggest WISE1828+2650 has a mass of ∼5–10
M
J
, making it a valuable laboratory for understanding the formation, evolution, and physical characteristics of gas giant planets. However, previous photometry and spectroscopy have presented a puzzle, with the near impossibility of simultaneously fitting both the short- (0.9–2.0
μ
m) and long-wavelength (3–5
μ
m) data. A potential solution to this problem has been the suggestion that WISE 1828+2650 is a binary system whose composite spectrum might provide a better match to the data. Alternatively, new models being developed to fit JWST/NIRSpec, and MIRI spectroscopy might provide new insights. This article describes JWST/NIRCam observations of WISE 1828+2650 in six filters to address the binarity question and to provide new photometry to be used in model fitting. We also report adaptive optics imaging with the Keck I0 m telescope. We find no evidence for multiplicity for a companion beyond 0.5 au with either JWST or Keck. 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M
J
, making it a valuable laboratory for understanding the formation, evolution, and physical characteristics of gas giant planets. However, previous photometry and spectroscopy have presented a puzzle, with the near impossibility of simultaneously fitting both the short- (0.9–2.0
μ
m) and long-wavelength (3–5
μ
m) data. A potential solution to this problem has been the suggestion that WISE 1828+2650 is a binary system whose composite spectrum might provide a better match to the data. Alternatively, new models being developed to fit JWST/NIRSpec, and MIRI spectroscopy might provide new insights. This article describes JWST/NIRCam observations of WISE 1828+2650 in six filters to address the binarity question and to provide new photometry to be used in model fitting. We also report adaptive optics imaging with the Keck I0 m telescope. We find no evidence for multiplicity for a companion beyond 0.5 au with either JWST or Keck. Companion articles will present low- and high-resolution spectra of WISE 1828 obtained with both NIRSpec and MIRI.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/acbf1e</doi><tpages>14</tpages><orcidid>https://orcid.org/0000-0003-1227-3084</orcidid><orcidid>https://orcid.org/0000-0003-1487-6452</orcidid><orcidid>https://orcid.org/0000-0002-0834-6140</orcidid><orcidid>https://orcid.org/0000-0001-7591-2731</orcidid><orcidid>https://orcid.org/0000-0003-2303-6519</orcidid><orcidid>https://orcid.org/0000-0002-5741-3047</orcidid><orcidid>https://orcid.org/0000-0002-5627-5471</orcidid><orcidid>https://orcid.org/0000-0003-4850-9589</orcidid><orcidid>https://orcid.org/0000-0002-6730-5410</orcidid><orcidid>https://orcid.org/0000-0002-7162-8036</orcidid><orcidid>https://orcid.org/0000-0003-0475-9375</orcidid><orcidid>https://orcid.org/0000-0002-6773-459X</orcidid><orcidid>https://orcid.org/0000-0002-6395-4296</orcidid><orcidid>https://orcid.org/0000-0003-0786-2140</orcidid><orcidid>https://orcid.org/0000-0001-9886-6934</orcidid><orcidid>https://orcid.org/0000-0002-7893-6170</orcidid><orcidid>https://orcid.org/0000-0003-2434-5225</orcidid><orcidid>https://orcid.org/0000-0003-1863-4960</orcidid><orcidid>https://orcid.org/0000-0002-2929-3121</orcidid><orcidid>https://orcid.org/0000-0002-3414-784X</orcidid><orcidid>https://orcid.org/0000-0001-5966-837X</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Adaptive optics Astrophysics Binary stars Brown dwarfs Gas giant planets Infrared spectroscopy James Webb Space Telescope Optics Photometry Physical properties Planetary evolution Planets Spectroscopy Spectrum analysis Theoretical models Visual binary stars Y dwarfs |
| title | JWST Observations of the Enigmatic Y-Dwarf WISE 1828+2650. I. Limits to a Binary Companion |
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