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Coordinates: Sky map 18h 28m 31.10s, +26° 50′ 37.79″
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{{Sky|18|28|31.10|+|26|50|37.79|36.5}}
{{Sky|18|28|31.10|+|26|50|37.79|36.5}}
{{Short description|Rogue planet or brown dwarf in the constellation Lyra}}
{{Starbox begin
{{Starbox begin
| name=WISEPA J182831.08+265037.8}}
| name=WISEPA J182831.08+265037.8}}
{{Starbox image
{{Starbox image
| image = <div style="margin-left:-15px">[[Image:WISE 1828+2650.jpg|280px]]</div>
| image = [[Image:WISE 1828+2650.jpg|280px]]
| caption ={{longitem|WISE 1828+2650 is circled in the centre<br>''([[Infrared]] image from the [[Wide-field Infrared Survey Explorer|WISE]] space telescope)''.|style=margin:-15px -15px 6px -15px; font-size: 1.2em;}}
| caption ={{longitem|WISE 1828+2650 is circled in the centre<br>''([[Infrared]] image from the [[Wide-field Infrared Survey Explorer|WISE]] space telescope)''.}}
}}
}}
{{Starbox observe
{{Starbox observe
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| constell=[[Lyra]]
| constell=[[Lyra]]
| ra={{RA|18|28|31.10}}{{r|Kirkpatrick2011}}
| ra={{RA|18|28|31.10}}{{r|Kirkpatrick2011}}
| dec={{DEC|26|50|37.79}}{{r|Kirkpatrick2011}}}}
| dec={{DEC|26|50|37.79}}{{r|Kirkpatrick2011}}
}}
{{Starbox character
{{Starbox character
|class=&gt;Y2{{r|Beichman2013}}
|class=&gt;Y2V{{r|Beichman2013}}
|appmag_1_passband=J {{small|([[Mauna Kea Observatory|MKO]] filter system)}}
|appmag_1_passband=J {{small|([[Mauna Kea Observatory|MKO]] filter system)}}
|appmag_1=23.57 ± 0.35{{r|Kirkpatrick2011}}
|appmag_1=23.57 ± 0.35{{r|Kirkpatrick2011}}
|appmag_2_passband=H {{small|([[Mauna Kea Observatory|MKO]] filter system)}}
|appmag_2_passband=H {{small|([[Mauna Kea Observatory|MKO]] filter system)}}
|appmag_2=22.45 ± 0.08{{r|Beichman2013}}}}
|appmag_2=22.45 ± 0.08{{r|Beichman2013}}
}}
{{Starbox astrometry
{{Starbox astrometry
|prop_mo_ra={{nowrap|954 ± 11{{r|Beichman2013}}}}
|prop_mo_ra={{val|1016.5|0.8|fmt=commas}}
|prop_mo_dec={{nowrap|153 ± 12.5{{r|Beichman2013}}}}
|prop_mo_dec={{val|169.3|0.8}}
|pm_footnote=<ref name="Kirkpatrick2021"/>
|parallax=70
|parallax=100.3
|p_error=14
|p_error=2.0
|parallax_footnote={{r|Dupuy2013}}
|parallax_footnote=<ref name="Kirkpatrick2021"/>
}}
}}
{{Starbox detail
{{Starbox detail
|mass_mj={{nowrap|3–6 or 0.5–20{{r|Beichman2013}}}}
|mass_mj={{nowrap|3–6 or 0.5–20{{r|Beichman2013}}}}
|temperature=250–400{{r|Beichman2013}}
|temperature={{val|406|88}}<ref name="Kirkpatrick2021"/>
|age_gyr={{nowrap|2–4 or 0.1–10{{r|Beichman2013}}}}
|age_gyr={{nowrap|2–4 or 0.1–10{{r|Beichman2013}}}}
}}
}}
{{Starbox catalog
{{Starbox catalog
| names=[[Wide-field Infrared Survey Explorer|WISEPA]] J182831.08+265037.8{{r|Kirkpatrick2011}}<br>[[Wide-field Infrared Survey Explorer|WISEP]] J182831.08+265037.8{{r|Beichman2013}}<br>[[Wide-field Infrared Survey Explorer|WISEP]] J1828+2650{{r|Cushing2011}}<br>[[Wide-field Infrared Survey Explorer|WISE]] J1828+2650{{r|Kirkpatrick2011}}<br>[[Wide-field Infrared Survey Explorer|WISE]] 1828+2650{{r|Kirkpatrick2011}}}}
| names=[[Wide-field Infrared Survey Explorer|WISEPA]] J182831.08+265037.8{{r|Kirkpatrick2011}}<br>[[Wide-field Infrared Survey Explorer|WISEP]] J182831.08+265037.8{{r|Beichman2013}}<br>[[Wide-field Infrared Survey Explorer|WISEP]] J1828+2650{{r|Cushing2011}}<br>[[Wide-field Infrared Survey Explorer|WISE]] J1828+2650{{r|Kirkpatrick2011}}<br>[[Wide-field Infrared Survey Explorer|WISE]] 1828+2650{{r|Kirkpatrick2011}}
}}
{{Starbox reference
{{Starbox reference
|Simbad=NAME+WISEP+J1828%2B2650
|Simbad=WISE+J182831.08%2B265037.7
}}
}}
{{Starbox end}}
{{Starbox end}}


'''WISE 1828+2650''' (full designation '''WISEPA J182831.08+265037.8''') is a [[brown dwarf]] or [[rogue planet]]{{r|Beichman2013}} of [[spectral class]] &gt;Y2,{{r|Beichman2013}} located in constellation [[Lyra]] at approximately 47 [[light-year]]s from [[Earth]].{{r|Dupuy2013}} It is the "archetypal member" of the Y spectral class.{{r|Cushing2011}}
'''WISE 1828+2650''' (full designation '''WISEPA J182831.08+265037.8''') is a possibly binary{{r|Cushing2021}} [[brown dwarf]] or [[rogue planet]]{{r|Beichman2013}} of [[spectral class]] &gt;Y2,{{r|Beichman2013}} located in the constellation [[Lyra]] at approximately 32.5 [[light-year]]s from [[Earth]].<ref name="Kirkpatrick2021"/> It is the "archetypal member" of the Y spectral class.{{r|Cushing2011}}


== History of observations ==
== History of observations ==
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=== Discovery ===
=== Discovery ===


'''WISE 1828+2650''' was discovered in 2011 from data collected by NASA's 40&nbsp;cm (16&nbsp;in) [[Wide-field Infrared Survey Explorer]] (WISE) [[space telescope]] at infrared wavelength. WISE 1828+2650 has two discovery papers: ''Kirkpatrick et al. (2011)'' and ''Cushing et al. (2011)'', however, basically with the same authors and published nearly simultaneously.{{r|Kirkpatrick2011|Cushing2011}}
WISE 1828+2650 was discovered in 2011 from data collected by NASA's 40&nbsp;cm (16&nbsp;in) [[Wide-field Infrared Survey Explorer]] (WISE) [[space telescope]] at infrared wavelength. WISE 1828+2650 has two discovery papers: Kirkpatrick et al. (2011) and Cushing et al. (2011), however, basically with the same authors and published nearly simultaneously.{{r|Kirkpatrick2011|Cushing2011}}


*[[J. Davy Kirkpatrick|Kirkpatrick]] ''et al.'' presented discovery of 98 new found by WISE [[brown dwarf]] systems with components of [[spectral type]]s M, L, T and Y, among which also was WISE 1828+2650 — coolest of them.{{r|Kirkpatrick2011}}<ref name="note 1" group="~">These 98 brown dwarf systems are only among first, not all brown dwarf systems, discovered from data, collected by WISE: six discoveries were published earlier (however, also listed in Kirkpatrick et al. (2011)) in Mainzer et al. (2011) and Burgasser et al. (2011), and the other discoveries were published later.</ref>
*[[J. Davy Kirkpatrick|Kirkpatrick]] ''et al.'' presented discovery of 98 new found by WISE [[brown dwarf]] systems with components of [[spectral type]]s M, L, T and Y, among which also was WISE 1828+2650 – coolest of them.{{r|Kirkpatrick2011}}<ref name="note 1" group="~">These 98 brown dwarf systems are only among first, not all brown dwarf systems, discovered from data, collected by WISE: six discoveries were published earlier (however, also listed in Kirkpatrick et al. (2011)) in Mainzer et al. (2011) and Burgasser et al. (2011), and the other discoveries were published later.</ref>
*Cushing ''et al.'' presented discovery of seven brown dwarfs — one of T9.5 type, and six of Y-type — first members of the Y spectral class, ever discovered and spectroscopically confirmed, including "archetypal member" of the Y spectral class — WISE 1828+2650.{{r|Cushing2011}} These seven objects are also the faintest seven of 98 brown dwarfs, presented in ''Kirkpatrick et al. (2011)''.{{r|Kirkpatrick2011}}
*Cushing ''et al.'' presented discovery of seven brown dwarfs – one of T9.5 type, and six of Y-type – first members of the Y spectral class, ever discovered and spectroscopically confirmed, including "archetypal member" of the Y spectral class – WISE 1828+2650.{{r|Cushing2011}} These seven objects are also the faintest seven of 98 brown dwarfs, presented in Kirkpatrick et al. (2011).{{r|Kirkpatrick2011}}


== Distance ==
== Distance ==


Currently the most accurate distance estimate of WISE 1828+2650 is a [[trigonometric parallax]], measured using [[Spitzer Space Telescope]] and published in 2013 by Trent Dupuy and Adam Kraus: 0.070 ± 0.014 [[arcsecond|arcsec]], corresponding to a distance 14.3{{±|3.6|2.4}} pc, or 46.6{{±|11.6|7.8}} ly.{{r|Dupuy2013}}
Currently the most accurate distance estimate of WISE 1828+2650 is a [[trigonometric parallax]], published in 2021 by Kirkpatrick ''et al.'': {{val|100.3|2.0|ul=mas}}, corresponding to a distance of {{val|10.0|0.2|ul=pc}}, or {{val|32.5|0.6|ul=ly}}.<ref name="Kirkpatrick2021"/>


{| class="wikitable" style="text-align: center; width: 600px;"
{| class="wikitable" style="text-align: center; width: 600px;"
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| align=left |Kirkpatrick et al. (2011)<br>&nbsp;{{small|(Table 6)}} || &ndash; || ''&lt;9.4'' || ''&lt;30.7'' || {{r|Kirkpatrick2011}}
| align=left |Kirkpatrick et al. (2011)<br>&nbsp;{{small|(Table 6)}} || &ndash; || ''&lt;9.4'' || ''&lt;30.7'' || {{r|Kirkpatrick2011}}
|-
|-
| align=left |Beichman et al. (2013)<br>&nbsp;{{small|(according Kirkpatrick et al. (2012))}} || 122 ± 13 || 8.2{{±|1.0|0.8}} || 26.7{{±|3.2|2.6}} || {{r|Kirkpatrick2012}}
| align=left |Beichman et al. (2013)<br>&nbsp;{{small|(according to Kirkpatrick et al. (2012))}} || 122 ± 13 || 8.2{{±|1.0|0.8}} || 26.7{{±|3.2|2.6}} || {{r|Kirkpatrick2012}}
|-
|-
| align=left style="padding: 20px 2px;" |Beichman et al. (2013) || 90 ± 9.5<ref name="note 3" group="~">According Dupuy & Kraus (2013), this measurement uncertainty is likely underestimated.</ref> || 11.2{{±|1.3|1.0}} || 36.5{{±|4.2|3.3}} || {{r|Beichman2013}}
| align=left style="padding: 20px 2px;" |Beichman et al. (2013) || 90 ± 9.5<ref name="note 3" group="~">According to Dupuy & Kraus (2013), this measurement uncertainty is likely underestimated.</ref> || 11.2{{±|1.3|1.0}} || 36.5{{±|4.2|3.3}} || {{r|Beichman2013}}
|-
|-
| align=left style="padding: 15px 3px;" |Dupuy & Kraus (2013) || '''70 ± 14'''<ref name="note 4" group="~">Relative parallax.</ref> || '''14.3{{±|3.6|2.4}}''' || '''46.6{{±|11.6|7.8}}''' || {{r|Dupuy2013}}
| align=left style="padding: 15px 3px;" |Dupuy & Kraus (2013) || 70 ± 14<ref name="note 4" group="~">Relative parallax.</ref> || 14.3{{±|3.6|2.4}} || 46.6{{±|11.6|7.8}} || {{r|Dupuy2013}}
|-
| align=left style="padding: 15px 3px;" | Beichman et al. (2014) || 106 ± 7 || 9.4{{±|0.7|0.6}} || 30.8{{±|2.2|1.9}} || {{r|Beichman2014}}
|-
| align=left style="padding: 15px 3px;" | Kirkpatrick et al. (2021) || '''{{val|100.3|2.0}}''' || '''{{val|10.0|0.2}}''' || '''{{val|32.5|0.6}}''' || {{r|Kirkpatrick2021}}

|-
|-
| colspan=5 style="font-size: 0.85em; background-color: #f2f2f2; padding: 6px 0 4px 4px; text-align: left;" | Non-trigonometric distance estimates are marked in ''italic''. The most precise estimate is marked in '''bold'''.
| colspan=5 style="font-size: 0.85em; background-color: #f2f2f2; padding: 6px 0 4px 4px; text-align: left;" | Non-trigonometric distance estimates are marked in ''italic''. The most precise estimate is marked in '''bold'''.
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== Proper motion ==
== Proper motion ==


WISE 1828+2650 has proper motion of about 966 milliarcseconds per year.{{r|Beichman2013}}
WISE 1828+2650 has a proper motion of {{val|1030.5|1.1|fmt=commas}} milliarcseconds per year.<ref name="Kirkpatrick2021"/>


{| class="wikitable" style="width: 600px; text-align: center;"
{| class="wikitable" style="width: 600px; text-align: center;"
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| align=left | Kirkpatrick et al. (2011) || 1084 || 84 || 1078 ± 327 || 118 ± 409 || {{r|Kirkpatrick2011}}
| align=left | Kirkpatrick et al. (2011) || 1084 || 84 || 1078 ± 327 || 118 ± 409 || {{r|Kirkpatrick2011}}
|-
|-
| align=left | Beichman et al. (2013) || '''966''' || '''81''' || '''954 ± 11''' || '''153 ± 12.5''' || {{r|Beichman2013}}
| align=left | Beichman et al. (2013) || 966 || 81 || 954 ± 11 || 153 ± 12.5 || {{r|Beichman2013}}
|-
|-
| align=left | Dupuy & Kraus (2013) || 1034 ± 15 || 80.4 ± 0.9 || 1020 ± 15 || 173 ± 16 || {{r|Dupuy2013}}
| align=left | Dupuy & Kraus (2013) || 1034 ± 15 || 80.4 ± 0.9 || 1020 ± 15 || 173 ± 16 || {{r|Dupuy2013}}
|-
| align=left | Beichman et al. (2014) || '''1039''' || '''80.4''' || '''1024 ± 7''' || '''174 ± 6''' || {{r|Beichman2014}}
|-
|-
| colspan=6 style="font-size: 0.85em; background-color: #f2f2f2; padding: 6px 0 4px 4px; text-align: left;" |The best estimate is marked in '''bold'''.
| colspan=6 style="font-size: 0.85em; background-color: #f2f2f2; padding: 6px 0 4px 4px; text-align: left;" |The best estimate is marked in '''bold'''.
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== Physical properties ==
== Physical properties ==


Until the discovery of [[WISE 0855−0714]] in 2014 WISE 1828+2650 was considered as the coldest currently known brown dwarf or the first example of [[free-floating planet]] (it is not currently known if it is a brown dwarf or a free-floating planet).{{r|Beichman2013}} It has a temperature in the range {{Convert|250|–|400|K|C F}}{{r|Beichman2013}} and was initially estimated below 300 [[Kelvin|K]],{{r|Cushing2011}} or about {{convert|27|C|F|abbr=on}}. It has been assigned the latest known [[spectral class]] (&gt;Y2,{{r|Beichman2013}} initially estimated as &gt;Y0{{r|Cushing2011}}).
Until the discovery of [[WISE 0855−0714]] in 2014, WISE 1828+2650 was considered as the coldest currently known brown dwarf or the first example of [[free-floating planet]] (it is not currently known if it is a brown dwarf or a free-floating planet).{{r|Beichman2013}} It has a temperature in the range {{Convert|250|–|400|K|C F}}{{r|Beichman2013}} and was initially estimated below 300 [[Kelvin|K]],{{r|Cushing2011}} or about {{convert|27|C|F|abbr=on}}. It has been assigned the latest known [[spectral class]] (&gt;Y2,{{r|Beichman2013}} initially estimated as &gt;Y0{{r|Cushing2011}}).


The mass of WISE 1828+2650 is in the range {{Jupiter mass|Jup=y|link=y|0.5–20}} for ages of 0.1–10 [[Gigayear|Gyr]].{{r|Beichman2013}}
The mass of WISE 1828+2650 is in the range {{Jupiter mass|Jup=y|link=y|0.5–20}} for ages of 0.1–10 [[Gigayear|Gyr]].{{r|Beichman2013}} The high [[tangential velocity]] of WISE 1828+2650, characteristic of an old disk population, indicates a possible age of WISE 1828+2650 in the range 2–4 [[Gigayear|Gyr]], leading to a mass estimate of about {{Jupiter mass|Jup=y|link=y|3–6}}.{{r|Beichman2013}} This suggests that WISE 1828+2650 may be a free-floating planet rather than a brown dwarf, since it is below the lower mass limit for [[deuterium]] fusion ({{Jupiter mass|Jup=y|~13}}).


⚫
WISE 1828+2650 is similar in appearance to the other Y-type object [[WD 0806-661 B]]. WD 0806-661 B could have formed as a planet close to its primary, WD 0806-661 A, and later, when the primary became a [[white dwarf]] and lost most of its mass, have migrated into a larger orbit of 2500 [[astronomical unit|AU]], and similarity between WD 0806-661 B and WISE 1828+2650 may indicate that WISE 1828+2650 had formed in the same way.{{r|Beichman2013}}
High [[tangential velocity]] of WISE 1828+2650, characteristic of an old disk population, indicates possible age of WISE 1828+2650 in the range 2–4 [[Gigayear|Gyr]], leading to mass estimate of about {{Jupiter mass|Jup=y|link=y|3–6}}.{{r|Beichman2013}}<ref name="note 2" group="~">This may indicate that WISE 1828+2650 is more likely a free-floating planet, not a brown dwarf, since it is below the lower mass limit for brown dwarfs ({{Jupiter mass|Jup=y|~13}}, see [[brown dwarf]]).</ref>


JWST observation with [[Mid-Infrared Instrument|MIRI]] detected [[water vapor]] (H<sub>2</sub>O), [[methane]] (CH<sub>4</sub>) and [[ammonia]] (NH<sub>3</sub>) in the atmosphere of WISE 1828+2650. The work detected a low amount of ammonia containing the [[Isotopes of nitrogen#Nitrogen-15|<sup>15</sup>N]] isotope when compared to ammonia containing the [[Isotopes of nitrogen#Nitrogen-14|<sup>14</sup>N]] isotope. The <sup>14</sup>NH<sub>3</sub>-to-<sup>15</sup>NH<sub>3</sub> ratio was measured as 670. This amount of <sup>15</sup>NH<sub>3</sub> is lower than in any [[List of Solar System objects|Solar System body]] and it is an indication that WISE 1828+2650 has formed like a [[star]] and not like a planet. Thus, this provides evidence that the object is a [[sub-brown dwarf|(sub-)brown dwarf]] and not a free-floating planet.<ref>{{Cite web |date=2023-11-07 |title=An ammonia trail to exoplanets |url=https://www.phys.ethz.ch/news-and-events/d-phys-news/2023/11/an-ammonia-trail-to-exoplanets.html |access-date=2023-11-07 |website=www.phys.ethz.ch |language=en}}</ref><ref name="Barrado2023"/> Another team used the [[NIRSpec]] instrument on JWST and detected water vapor, methane, ammonia, [[carbon monoxide]] (<sup>12</sup>CO), [[carbon dioxide]] (CO<sub>2</sub>) and [[hydrogen sulfide]] (H<sub>2</sub>S). These molecules are the major [[carbon]], [[nitrogen]], [[oxygen]], and [[sulfur]] bearing species in the atmosphere of WISE 1828+2650. The carbon-to-oxygen ratio (C/O ratio) is with 0.45±0.01 close to the solar ratio. The abundance of carbon, oxygen and sulfur is higher than the sun, but the abundance of nitrogen is likely similar to the sun.<ref name=":1">{{Cite journal |last1=Lew |first1=Ben W.P. |last2=Roellig |first2=Thomas |last3=Batalha |first3=Natasha E. |last4=Line |first4=Michael |last5=Greene |first5=Thomas |last6=Murkherjee |first6=Sagnick |last7=Freedman |first7=Richard |last8=Meyer |first8=Michael |last9=Beichman |first9=Charles |last10=De Oliveira |first10=Catarina Alves |last11=De Furio |first11=Matthew |last12=Johnstone |first12=Doug |last13=Greenbaum |first13=Alexandra Z. |last14=Marley |first14=Mark |last15=J. Fortney |first15=Jonathan |date=8 Feb 2024 |title=High-precision atmospheric characterization of a Y dwarf with JWST NIRSpec G395H spectroscopy: isotopologue, C/O ratio, metallicity, and the abundances of six molecular species |journal=The Astronomical Journal |volume=167 |issue=5 |page=237 |doi=10.3847/1538-3881/ad3425 |doi-access=free |arxiv=2402.05900|bibcode=2024AJ....167..237L }}</ref>
⚫
WISE 1828+2650 is similar in appearance to the other Y-type object [[WD 0806-661|WD 0806-661 B]]. WD 0806-661 B could have formed as a planet close to its primary, WD 0806-661 A, and later, when the primary became a [[white dwarf]] and lost most of its mass, have migrated into a larger orbit of 2500 [[astronomical unit|AU]], and similarity between WD 0806-661 B and WISE 1828+2650 may indicate that WISE 1828+2650 had formed in the same way.{{r|Beichman2013}}
{| class="wikitable"
|+Elemental Abundances of WISE 1828+2650<ref name=":1" />
![[Metallicity#Chemical abundance ratios|Normalized element abundance]]
!Abundance
([M/H]=0 is solar)
|-
|[C/H]
|{{Val|+0.24|0.01|0.02}}
|-
|[O/H]
|≥ {{Val|+0.34|0.01|0.02}}
|-
|[N/H]
|> {{Val|-0.31|0.02}}, might be +0.04
|-
|[S/H]
|{{Val|+0.14|0.03}}
|}


=== Possible binarity ===
=== Possible binarity ===


Comparison between WISE 1828+2650 and WD 0806-661 B may suggest that WISE 1828+2650 is a system of two equal-mass objects. Observations with [[Hubble Space Telescope|Hubble Space Telescope (HST)]] and [[Keck Observatory|Keck-II]] [[laser guide star|LGS]]-[[adaptive optics|AO]] system had not revealed binarity, suggesting that if any such companion exists, it would have an orbit less than 0.5 [[astronomical unit|AU]], and no evidence for binarity yet exists.{{r|Beichman2013}}
Comparison between WISE 1828+2650 and WD 0806-661 B may suggest that WISE 1828+2650 is a system of two equal-mass objects. Observations with [[Hubble Space Telescope|Hubble Space Telescope (HST)]] and [[Keck Observatory|Keck-II]] [[laser guide star|LGS]]-[[adaptive optics|AO]] system had not revealed binarity, suggesting that if any such companion exists, it would have an orbit less than 0.5 [[astronomical unit|AU]], and no direct evidence for binarity yet exists.{{r|Beichman2013}} However, the spectrum of the system best fits a pair of brown dwarfs, each with an effective temperature of about 325 K and a mass of about {{Jupiter mass|5|link=y}}.<ref name=Cushing2021>{{cite journal|doi=10.3847/1538-4357/ac12cb|title=An Improved Near-infrared Spectrum of the Archetype Y Dwarf WISEP J182831.08+265037.8|year=2021|last1=Cushing|first1=Michael C.|last2=Schneider|first2=Adam C.|last3=Kirkpatrick|first3=J. Davy|last4=Morley|first4=Caroline V.|last5=Marley|first5=Mark S.|last6=Gelino|first6=Christopher R.|last7=Mace|first7=Gregory N.|last8=Wright|first8=Edward L.|last9=Eisenhardt|first9=Peter R.|last10=Skrutskie|first10=Michael F.|last11=Marsh|first11=Kenneth A.|journal=The Astrophysical Journal|volume=920|issue=1|page=20|arxiv=2107.00506|bibcode=2021ApJ...920...20C|s2cid=235694398 |doi-access=free }}</ref>

[[James Webb Space Telescope|JWST]] [[NIRCam]] imaging observations did not find a companion at a separation larger than 0.5 astronomical units.<ref name=":0">{{Cite journal |last1=De Furio |first1=Matthew |last2=Lew |first2=Ben |last3=Beichman |first3=Charles |last4=Roellig |first4=Thomas |last5=Bryden |first5=Geoffrey |last6=Ciardi |first6=David |last7=Meyer |first7=Michael |last8=Rieke |first8=Marcia |last9=Greenbaum |first9=Alexandra |last10=Leisenring |first10=Jarron |last11=Llop-Sayson |first11=Jorge |last12=Ygouf |first12=Marie |last13=Albert |first13=Loic |last14=Boyer |first14=Martha |last15=Eisenstein |first15=Daniel |date=2023-05-01 |title=JWST Observations of the Enigmatic Y-Dwarf WISE 1828+2650. I. Limits to a Binary Companion |journal=The Astrophysical Journal |volume=948 |issue=2 |pages=92 |doi=10.3847/1538-4357/acbf1e |arxiv=2302.12723 |bibcode=2023ApJ...948...92D |issn=0004-637X|doi-access=free }}</ref> [[NIRSpec]] low resolution prism observations cannot be explained with existing Sonora Bobcat models of planetary objects, neither single nor multiple.<ref>{{Cite journal |last1=Beichman |first1=Charles |last2=De Furio |first2=Matthew |last3=Roellig |first3=Thomas |last4=Lew |first4=Ben |last5=Greene |first5=Thomas |last6=Leisenring |first6=Jarron |last7=Misselt |first7=Karl |last8=Stansberry |first8=John |last9=Boyer |first9=Martha |last10=Rieke |first10=Marcia |last11=Meyer |first11=Michael |last12=Albert |first12=Loic |last13=Kelly |first13=Douglas |last14=Greenbaum |first14=Alexendra |last15=Bryden |first15=Geoffrey |date=2023-01-01 |title=JWST Observations of the Enigmatic Y Dwarf WISE 1828+2650 |journal=American Astronomical Society Meeting Abstracts |url=https://ui.adsabs.harvard.edu/abs/2023AAS...24134505B |volume=55 |issue=2 |pages=345.05|bibcode=2023AAS...24134505B }}</ref> The binary model fails to provide an improved fit for the existing photometric data.<ref name=":0" /> A newer analysis of the NIRSpec data compared radius determined with atmospheric retrieval framework CHIMERA and evolutionary model Sonora Bobcat. The CHIMERA radius for a single object ({{val|1.23|0.01}} {{Jupiter radius|link=true}}) compared with predicted radius from Sonora Bobcat (10 Gyrs, 33 {{Jupiter mass}},0.87 {{Jupiter radius}}) is too large for its age, which might be an indication that WISE 1828+2650 is an equal mass binary with both objects having a radius of 0.87 {{Jupiter radius}}. The estimated [[Semi-major and semi-minor axes|semi-major axis]] of this binary is {{Val|0.0098|0.002|0.006}} [[Astronomical unit|astronomical units]] or {{Val|20|4|12}} {{Jupiter radius}}. Sonora Bobcat however predicts a lower age (1.4 Gyrs) and mass (9.982 {{Jupiter mass}}) when using the temperature and gravity from Sonora Elf Owl atmospheric model grid. Future observations could look for [[Doppler spectroscopy|radial velocity variations]] to confirm the binary.<ref name=":1" />


=== Comparison ===
=== Comparison ===


[[File:BrownDwarfs Comparison 01.png|thumb|left|400px|[[Brown dwarf]]s {{nowrap|[[Teide 1]]}}, [[Gliese 229B]], and ''WISE 1828+2650'' compared to red dwarf [[Gliese 229A]], Jupiter and our Sun]]
[[File:BrownDwarfs Comparison 01.png|thumb|left|400px|[[Brown dwarf]]s {{nowrap|[[Teide 1]]}}, [[Gliese 229B]], and ''WISE 1828+2650'' compared to red dwarf [[Gliese 229A]], Jupiter and the Sun]]
{{clear}}
{{clear}}


Line 116: Line 148:
*[[WISE 1738+2732]] (Y0)
*[[WISE 1738+2732]] (Y0)
*[[WISE 2056+1459]] (Y0)
*[[WISE 2056+1459]] (Y0)
Lists:
*[[List of star systems within 30–35 light-years]]
*[[List of Y-dwarfs]]


== Notes ==
== Notes ==


{{Reflist|colwidth=30em|group=~}}
{{Reflist|group=~}}


== References ==
== References ==


{{reflist|colwidth=30em|refs=
{{reflist|colwidth=30em|refs=

<ref name="Cushing2011">{{cite journal |last=Cushing |first=Michael C. |title=The Discovery of Y Dwarfs using Data from the Wide-field Infrared Survey Explorer (WISE) |year=2011 |doi=10.1088/0004-637X/743/1/50 |bibcode=2011ApJ...743...50C|journal=The Astrophysical Journal |volume= 743 |pages=50 |number =1 |last2=Kirkpatrick |first2=J. Davy |last3=Gelino |first3=Christopher R. |last4=Griffith |first4=Roger L. |last5=Skrutskie |first5=Michael F. |last6=Mainzer |first6=A. |last7=Marsh |first7=Kenneth A. |last8=Beichman |first8=Charles A. |last9=Burgasser |first9=Adam J. |last10=Prato |first10=Lisa A. |last11=Simcoe |first11=Robert A. |last12=Marley |first12=Mark S. |last13=Saumon |first13=D. |last14=Freedman |first14=Richard S. |last15=Eisenhardt |first15=Peter R. |last16=Wright |first16=Edward L. }}</ref>
<ref name="Cushing2011">{{cite journal |last1=Cushing |first1=Michael C. |title=The Discovery of Y Dwarfs using Data from the Wide-field Infrared Survey Explorer (WISE) |year=2011 |doi=10.1088/0004-637X/743/1/50 |bibcode=2011ApJ...743...50C |journal=The Astrophysical Journal |volume=743 |pages=50 |number=1 |last2=Kirkpatrick |first2=J. Davy |last3=Gelino |first3=Christopher R. |last4=Griffith |first4=Roger L. |last5=Skrutskie |first5=Michael F. |last6=Mainzer |first6=Amy K. |last7=Marsh |first7=Kenneth A. |last8=Beichman |first8=Charles A. |last9=Burgasser |first9=Adam J. |last10=Prato |first10=Lisa A. |last11=Simcoe |first11=Robert A. |last12=Marley |first12=Mark S. |last13=Saumon |first13=Didier |last14=Freedman |first14=Richard S. |last15=Eisenhardt |first15=Peter R. |last16=Wright |first16=Edward L. |arxiv=1108.4678 |s2cid=286881 }}</ref>
⚫
<ref name="Kirkpatrick2011">{{cite journal | authorlink=J. Davy Kirkpatrick | last=Kirkpatrick |first=J. Davy |author2=Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, A.; Eisenhardt, Peter R.; McLean, Ian S.; Thompson, Maggie A.; Bauer, James M.; Benford, Dominic J.; Bridge, Carrie R.; Lake, Sean E.; Petty, Sara M.; Stanford, S. A.; Tsai, Chao-Wei; Bailey, Vanessa; Beichman, Charles A.; Bloom, Joshua S.; Bochanski, John J.; Burgasser, Adam J.; Capak, Peter L.; Cruz, Kelle L.; Hinz, Philip M.; Kartaltepe, Jeyhan S.; Knox, Russell P.; Manohar, Swarnima; Masters, Daniel; Morales-Calderon, Maria; Prato, Lisa A.; Rodigas, Timothy J.; Salvato, Mara; Schurr, Steven D.; Scoville, Nicholas Z.; Simcoe, Robert A.; Stapelfeldt, Karl R.; Stern, Daniel; Stock, Nathan D.; Vacca, William D. | title=The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE) | date=2011 | journal=[[The Astrophysical Journal Supplement]] | volume=197 | issue=2 | pages=19 | arxiv=1108.4677v1 | doi=10.1088/0067-0049/197/2/19 | bibcode=2011ApJS..197...19K}}</ref>

⚫
<ref name="Kirkpatrick2012">{{cite journal | authorlink=J. Davy Kirkpatrick | last1=Kirkpatrick | last2=Gelino |first1=J. D. | first2=C. R. | last3=Cushing | first3=M. C. | last4=Mace | first4=G. N. | last5=Griffith | first5=R. L. | last6=Skrutskie | first6=M. F. | last7=Marsh | first7=K. A. | last8=Wright | first8=E. L. | last9=Eisenhardt | first9=P. R. | last10=McLean | first10=I. S. | last11=Mainzer | first11=A. K. | last12=Burgasser | first12=A. J. | last13=Tinney | first13=C. G. | last14=Parker | first14=S. | last15=Salter | first15=G. | title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function | year=2012 | journal=[[The Astrophysical Journal]] | volume=753 | issue=2 | pages=156 | arxiv=1205.2122 | doi=10.1088/0004-637X/753/2/156 | bibcode=2012ApJ...753..156K}}</ref>
⚫
<ref name="Kirkpatrick2011">{{cite journal |doi=10.1088/0067-0049/197/2/19 |authorlink=J. Davy Kirkpatrick |last1=Kirkpatrick |first1=J. Davy |last2=Cushing |first2=Michael C. |last3=Gelino |first3=Christopher R. |last4=Griffith |first4=Roger L. |last5=Skrutskie |first5=Michael F. |last6=Marsh |first6=Kenneth A. |last7=Wright |first7=Edward L. |last8=Mainzer |first8=Amy K. |last9=Eisenhardt |first9=Peter R. |last10=McLean |first10=Ian S. |last11=Thompson |first11=Maggie A. |last12=Bauer |first12=James M. |last13=Benford |first13=Dominic J. |last14=Bridge |first14=Carrie R. |last15=Lake |first15=Sean E. |last16=Petty |first16=Sara M. |last17=Stanford |first17=Spencer Adam |last18=Tsai |first18=Chao-Wei |last19=Bailey |first19=Vanessa |last20=Beichman |first20=Charles A. |last21=Bloom |first21=Joshua S. |last22=Bochanski |first22=John J. |last23=Burgasser |first23=Adam J. |last24=Capak |first24=Peter L. |last25=Cruz |first25=Kelle L. |last26=Hinz |first26=Philip M. |last27=Kartaltepe |first27=Jeyhan S. |last28=Knox |first28=Russell P. |last29=Manohar |first29=Swarnima |last30=Masters |first30=Daniel |last31=Morales-Calderon |first31=Maria |last32=Prato |first32=Lisa A. |last33=Rodigas |first33=Timothy J. |last34=Salvato |first34=Mara |last35=Schurr |first35=Steven D. |last36=Scoville |first36=Nicholas Z. |last37=Simcoe |first37=Robert A. |last38=Stapelfeldt |first38=Karl R. |last39=Stern |first39=Daniel |last40=Stock |first40=Nathan D. |last41=Vacca |first41=William D. |title=The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE) |date=2011 |journal=[[The Astrophysical Journal Supplement]] |volume=197 |issue=2 |pages=19 |arxiv=1108.4677v1 |bibcode=2011ApJS..197...19K |s2cid=16850733 }}</ref>
⚫
<ref name="Beichman2013">{{cite journal | last=Beichman |first=C. |author2=Gelino, Christopher R. |author3=Kirkpatrick, J. Davy |author4=Barman, Travis S. |author5=Marsh, Kenneth A. |author6=Cushing, Michael C. |author7=Wright, E. L. | title=The Coldest Brown Dwarf (or Free-floating Planet)?: The Y Dwarf WISE 1828+2650 | date=2013 | journal=[[The Astrophysical Journal]] | volume=764 | issue=1 | pages=101 | arxiv=1301.1669 | doi=10.1088/0004-637X/764/1/101 | bibcode=2013ApJ...764..101B}}</ref>

⚫
<ref name="Dupuy2013">{{rr/2013arXiv1309.1422D}}</ref>
⚫
<ref name="Kirkpatrick2012">{{cite journal |author-link=J. Davy Kirkpatrick |last1=Kirkpatrick |first1=J. Davy |last2=Gelino |first2=Christopher R. |last3=Cushing |first3=Michael C. |last4=Mace | first4=Gregory N. |last5=Griffith |first5=Roger L. |last6=Skrutskie |first6=Michael F. |last7=Marsh |first7=Kenneth A. |last8=Wright |first8=Edward L. |last9=Eisenhardt |first9=Peter R. |last10=McLean |first10=Ian S. |last11=Mainzer | first11=Amy K. |last12=Burgasser |first12=Adam J. |last13=Tinney |first13=Chris G. |last14=Parker |first14=Stephen |last15=Salter |first15=Graeme |title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function |year=2012 |journal=[[The Astrophysical Journal]] |volume=753 |issue=2 |pages=156 |arxiv=1205.2122 |doi=10.1088/0004-637X/753/2/156 |bibcode=2012ApJ...753..156K |s2cid=119279752 }}</ref>

⚫
<ref name="Beichman2013">{{cite journal |last=Beichman |first=Charles A. |author2=Gelino, Christopher R. |author3=Kirkpatrick, J. Davy |author4=Barman, Travis S. |author5=Marsh, Kenneth A. |author6=Cushing, Michael C. |author7=Wright, Edward L. |title=The Coldest Brown Dwarf (or Free-floating Planet)?: The Y Dwarf WISE 1828+2650 |date=2013 |journal=[[The Astrophysical Journal]] |volume=764 |issue=1 |pages=101 |arxiv=1301.1669 |doi=10.1088/0004-637X/764/1/101 |bibcode=2013ApJ...764..101B |s2cid=118575478 }}</ref>

⚫
<ref name="Dupuy2013">{{Cite journal
| doi = 10.1126/science.1241917
| title = Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects
| journal = Science
| volume = 341
| issue = 6153
| pages = 1492–5
| year = 2013
| last1 = Dupuy | first1 = Trent J.
| last2 = Kraus | first2 = Adam L.
|arxiv = 1309.1422 |bibcode = 2013Sci...341.1492D | pmid=24009359| s2cid = 30379513
}}</ref>

<ref name="Beichman2014">{{cite journal |first1=Charles A. |last1=Beichman |first2=Christopher R. |last2=Gelino |first3=J. Davy |last3=Kirkpatrick |first4=Michael C. |last4=Cushing |first5=Sally |last5=Dodson-Robinson |first6=Mark S. |last6=Marley |first7=Caroline V. |last7=Morley |first8=Edward L. |last8=Wright |year=2014 |title=WISE Y Dwarfs As Probes of the Brown Dwarf-Exoplanet Connection |journal=[[The Astrophysical Journal]] |volume=783 |issue=2 |page=68 |arxiv=1401.1194v2 |bibcode=2014ApJ...783...68B |doi=10.1088/0004-637X/783/2/68 |s2cid=119302072 }}</ref>

<ref name="Kirkpatrick2021">{{cite journal |last1=Kirkpatrick |first1=J. Davy |last2=Gelino |first2=Christopher R. |display-authors=etal |date=March 2021 |title=The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs |journal=[[The Astrophysical Journal Supplement Series]] |volume=253 |issue=1 |pages=7 |doi=10.3847/1538-4365/abd107 |arxiv=2011.11616 |bibcode=2021ApJS..253....7K|s2cid=227126954 |doi-access=free }}</ref>

<ref name="Barrado2023">{{cite journal |last1=Barrado |first1=David |last2=Mollière |first2=Paul |display-authors=etal |date=November 2023 |title=15NH3 in the atmosphere of a cool brown dwarf |journal=[[Nature (journal)|Nature]] |volume= 624|issue= 7991|pages= 263–266|doi=10.1038/s41586-023-06813-y |arxiv=2311.08054}}</ref>

}}
}}


== External links ==
== External links ==


*{{cite news|last=Choi|first=Charles Q.|title=Y dwarf star? Because they're cool, that's Y!|publisher=[[Space.com]]|date=August 26, 2011|url=http://www.space.com/12714-coldest-failed-stars-brown-dwarfs-wise.html|accessdate=August 31, 2011}}
*{{cite news|last=Choi|first=Charles Q.|title=Y dwarf star? Because they're cool, that's Y!|publisher=[[Space.com]]|date=August 26, 2011|url=http://www.space.com/12714-coldest-failed-stars-brown-dwarfs-wise.html|access-date=August 31, 2011}}
*[http://www.nasa.gov/mission_pages/WISE/news/wise20110823.html NASA news release]
*[http://www.nasa.gov/mission_pages/WISE/news/wise20110823.html NASA news release]
*[http://science.nasa.gov/science-news/science-at-nasa/2011/23aug_coldeststars/ Science news]
*[https://science.nasa.gov/science-news/science-at-nasa/2011/23aug_coldeststars/ Science news]
*[http://apod.nasa.gov/apod/ap110830.html Infrared image of WISE 1828+2650 at Astronomy Picture of the Day, 2011 August 30]
*{{APOD |date=30 August 2011 |title=Infrared image of WISE 1828+2650}}
*[http://solstation.com/stars/new-obj.htm Solstation.com (New Objects within 20 light-years)]
*[http://solstation.com/stars/new-obj.htm Solstation.com (New Objects within 20 light-years)]


{{Nearest star systems|10}}
{{Stars of Lyra}}
{{Stars of Lyra}}


[[Category:Brown dwarfs]]
[[Category:Rogue planets]]
[[Category:Rogue planets]]
[[Category:Y-type stars]]
[[Category:Y-type brown dwarfs]]
[[Category:Lyra (constellation)]]
[[Category:Lyra]]
[[Category:Astronomical objects discovered in 2011|20110901]]
[[Category:Astronomical objects discovered in 2011|20110901]]
[[Category:WISE objects]]
[[Category:WISE objects]]

Latest revision as of 04:51, 22 September 2024

WISEPA J182831.08+265037.8

WISE 1828+2650 is circled in the centre
(Infrared image from the WISE space telescope).
Observation data
Epoch MJD 55467.61[1]      Equinox J2000[1]
Constellation Lyra
Right ascension 18h 28m 31.10s[1]
Declination 26° 50′ 37.79″[1]
Characteristics
Spectral type >Y2V[2]
Apparent magnitude (J (MKO filter system)) 23.57 ± 0.35[1]
Apparent magnitude (H (MKO filter system)) 22.45 ± 0.08[2]
Astrometry
Proper motion (μ) RA: 1,016.5±0.8 mas/yr[3]
Dec.: 169.3±0.8 mas/yr[3]
Parallax (π)100.3 ± 2.0 mas[3]
Distance32.5 ± 0.6 ly
(10.0 ± 0.2 pc)
Details
Mass3–6 or 0.5–20[2] MJup
Temperature406±88[3] K
Age2–4 or 0.1–10[2] Gyr
Other designations
WISEPA J182831.08+265037.8[1]
WISEP J182831.08+265037.8[2]
WISEP J1828+2650[4]
WISE J1828+2650[1]
WISE 1828+2650[1]
Database references
SIMBADdata

WISE 1828+2650 (full designation WISEPA J182831.08+265037.8) is a possibly binary[5] brown dwarf or rogue planet[2] of spectral class >Y2,[2] located in the constellation Lyra at approximately 32.5 light-years from Earth.[3] It is the "archetypal member" of the Y spectral class.[4]

History of observations

[edit]

Discovery

[edit]

WISE 1828+2650 was discovered in 2011 from data collected by NASA's 40 cm (16 in) Wide-field Infrared Survey Explorer (WISE) space telescope at infrared wavelength. WISE 1828+2650 has two discovery papers: Kirkpatrick et al. (2011) and Cushing et al. (2011), however, basically with the same authors and published nearly simultaneously.[1][4]

  • Kirkpatrick et al. presented discovery of 98 new found by WISE brown dwarf systems with components of spectral types M, L, T and Y, among which also was WISE 1828+2650 – coolest of them.[1][~ 1]
  • Cushing et al. presented discovery of seven brown dwarfs – one of T9.5 type, and six of Y-type – first members of the Y spectral class, ever discovered and spectroscopically confirmed, including "archetypal member" of the Y spectral class – WISE 1828+2650.[4] These seven objects are also the faintest seven of 98 brown dwarfs, presented in Kirkpatrick et al. (2011).[1]

Distance

[edit]

Currently the most accurate distance estimate of WISE 1828+2650 is a trigonometric parallax, published in 2021 by Kirkpatrick et al.: 100.3±2.0 mas, corresponding to a distance of 10.0±0.2 pc, or 32.5±0.6 ly.[3]

WISE 1828+2650 distance estimates
Source Parallax
(mas)		 Distance
(pc)		 Distance
(ly)		 Ref
Kirkpatrick et al. (2011)
 (Table 6)		 – <9.4 <30.7 [1]
Beichman et al. (2013)
 (according to Kirkpatrick et al. (2012))		 122 ± 13 8.2+1.0
−0.8		 26.7+3.2
−2.6		 [6]
Beichman et al. (2013) 90 ± 9.5[~ 2] 11.2+1.3
−1.0		 36.5+4.2
−3.3		 [2]
Dupuy & Kraus (2013) 70 ± 14[~ 3] 14.3+3.6
−2.4		 46.6+11.6
−7.8		 [7]
Beichman et al. (2014) 106 ± 7 9.4+0.7
−0.6		 30.8+2.2
−1.9		 [8]
Kirkpatrick et al. (2021) 100.3±2.0 10.0±0.2 32.5±0.6 [3]
Non-trigonometric distance estimates are marked in italic. The most precise estimate is marked in bold.

Proper motion

[edit]

WISE 1828+2650 has a proper motion of 1,030.5±1.1 milliarcseconds per year.[3]

WISE 1828+2650 proper motion estimates
Source μ
mas/yr		 P. A.
°		 μRA
mas/yr		 μDEC
mas/yr		 Ref
Kirkpatrick et al. (2011) 1084 84 1078 ± 327 118 ± 409 [1]
Beichman et al. (2013) 966 81 954 ± 11 153 ± 12.5 [2]
Dupuy & Kraus (2013) 1034 ± 15 80.4 ± 0.9 1020 ± 15 173 ± 16 [7]
Beichman et al. (2014) 1039 80.4 1024 ± 7 174 ± 6 [8]
The best estimate is marked in bold.

Physical properties

[edit]

Until the discovery of WISE 0855−0714 in 2014, WISE 1828+2650 was considered as the coldest currently known brown dwarf or the first example of free-floating planet (it is not currently known if it is a brown dwarf or a free-floating planet).[2] It has a temperature in the range 250–400 K (−23–127 °C; −10–260 °F)[2] and was initially estimated below 300 K,[4] or about 27 °C (81 °F). It has been assigned the latest known spectral class (>Y2,[2] initially estimated as >Y0[4]).

The mass of WISE 1828+2650 is in the range 0.5–20 MJup for ages of 0.1–10 Gyr.[2] The high tangential velocity of WISE 1828+2650, characteristic of an old disk population, indicates a possible age of WISE 1828+2650 in the range 2–4 Gyr, leading to a mass estimate of about 3–6 MJup.[2] This suggests that WISE 1828+2650 may be a free-floating planet rather than a brown dwarf, since it is below the lower mass limit for deuterium fusion (~13 MJup).

WISE 1828+2650 is similar in appearance to the other Y-type object WD 0806-661 B. WD 0806-661 B could have formed as a planet close to its primary, WD 0806-661 A, and later, when the primary became a white dwarf and lost most of its mass, have migrated into a larger orbit of 2500 AU, and similarity between WD 0806-661 B and WISE 1828+2650 may indicate that WISE 1828+2650 had formed in the same way.[2]

JWST observation with MIRI detected water vapor (H2O), methane (CH4) and ammonia (NH3) in the atmosphere of WISE 1828+2650. The work detected a low amount of ammonia containing the 15N isotope when compared to ammonia containing the 14N isotope. The 14NH3-to-15NH3 ratio was measured as 670. This amount of 15NH3 is lower than in any Solar System body and it is an indication that WISE 1828+2650 has formed like a star and not like a planet. Thus, this provides evidence that the object is a (sub-)brown dwarf and not a free-floating planet.[9][10] Another team used the NIRSpec instrument on JWST and detected water vapor, methane, ammonia, carbon monoxide (12CO), carbon dioxide (CO2) and hydrogen sulfide (H2S). These molecules are the major carbon, nitrogen, oxygen, and sulfur bearing species in the atmosphere of WISE 1828+2650. The carbon-to-oxygen ratio (C/O ratio) is with 0.45±0.01 close to the solar ratio. The abundance of carbon, oxygen and sulfur is higher than the sun, but the abundance of nitrogen is likely similar to the sun.[11]

Elemental Abundances of WISE 1828+2650[11]
Normalized element abundance Abundance

([M/H]=0 is solar)

[C/H] +0.24+0.01
−0.02
[O/H] ≥ +0.34+0.01
−0.02
[N/H] > −0.31±0.02, might be +0.04
[S/H] +0.14±0.03

Possible binarity

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Comparison between WISE 1828+2650 and WD 0806-661 B may suggest that WISE 1828+2650 is a system of two equal-mass objects. Observations with Hubble Space Telescope (HST) and Keck-II LGS-AO system had not revealed binarity, suggesting that if any such companion exists, it would have an orbit less than 0.5 AU, and no direct evidence for binarity yet exists.[2] However, the spectrum of the system best fits a pair of brown dwarfs, each with an effective temperature of about 325 K and a mass of about 5 MJ.[5]

JWST NIRCam imaging observations did not find a companion at a separation larger than 0.5 astronomical units.[12] NIRSpec low resolution prism observations cannot be explained with existing Sonora Bobcat models of planetary objects, neither single nor multiple.[13] The binary model fails to provide an improved fit for the existing photometric data.[12] A newer analysis of the NIRSpec data compared radius determined with atmospheric retrieval framework CHIMERA and evolutionary model Sonora Bobcat. The CHIMERA radius for a single object (1.23±0.01 RJ) compared with predicted radius from Sonora Bobcat (10 Gyrs, 33 MJ,0.87 RJ) is too large for its age, which might be an indication that WISE 1828+2650 is an equal mass binary with both objects having a radius of 0.87 RJ. The estimated semi-major axis of this binary is 0.0098+0.002
−0.006 astronomical units or 20+4
−12 RJ. Sonora Bobcat however predicts a lower age (1.4 Gyrs) and mass (9.982 MJ) when using the temperature and gravity from Sonora Elf Owl atmospheric model grid. Future observations could look for radial velocity variations to confirm the binary.[11]

Comparison

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Brown dwarfs Teide 1, Gliese 229B, and WISE 1828+2650 compared to red dwarf Gliese 229A, Jupiter and the Sun

See also

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The other six discoveries of brown dwarfs, published by Cushing et al. in 2011:[4]

Lists:

Notes

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  1. ^ These 98 brown dwarf systems are only among first, not all brown dwarf systems, discovered from data, collected by WISE: six discoveries were published earlier (however, also listed in Kirkpatrick et al. (2011)) in Mainzer et al. (2011) and Burgasser et al. (2011), and the other discoveries were published later.
  2. ^ According to Dupuy & Kraus (2013), this measurement uncertainty is likely underestimated.
  3. ^ Relative parallax.

References

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  1. ^ a b c d e f g h i j k l m Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, Amy K.; Eisenhardt, Peter R.; McLean, Ian S.; Thompson, Maggie A.; Bauer, James M.; Benford, Dominic J.; Bridge, Carrie R.; Lake, Sean E.; Petty, Sara M.; Stanford, Spencer Adam; Tsai, Chao-Wei; Bailey, Vanessa; Beichman, Charles A.; Bloom, Joshua S.; Bochanski, John J.; Burgasser, Adam J.; Capak, Peter L.; Cruz, Kelle L.; Hinz, Philip M.; Kartaltepe, Jeyhan S.; Knox, Russell P.; Manohar, Swarnima; Masters, Daniel; Morales-Calderon, Maria; Prato, Lisa A.; Rodigas, Timothy J.; Salvato, Mara; Schurr, Steven D.; Scoville, Nicholas Z.; Simcoe, Robert A.; Stapelfeldt, Karl R.; Stern, Daniel; Stock, Nathan D.; Vacca, William D. (2011). "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal Supplement. 197 (2): 19. arXiv:1108.4677v1. Bibcode:2011ApJS..197...19K. doi:10.1088/0067-0049/197/2/19. S2CID 16850733.
  2. ^ a b c d e f g h i j k l m n o p Beichman, Charles A.; Gelino, Christopher R.; Kirkpatrick, J. Davy; Barman, Travis S.; Marsh, Kenneth A.; Cushing, Michael C.; Wright, Edward L. (2013). "The Coldest Brown Dwarf (or Free-floating Planet)?: The Y Dwarf WISE 1828+2650". The Astrophysical Journal. 764 (1): 101. arXiv:1301.1669. Bibcode:2013ApJ...764..101B. doi:10.1088/0004-637X/764/1/101. S2CID 118575478.
  3. ^ a b c d e f g Kirkpatrick, J. Davy; Gelino, Christopher R.; et al. (March 2021). "The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs". The Astrophysical Journal Supplement Series. 253 (1): 7. arXiv:2011.11616. Bibcode:2021ApJS..253....7K. doi:10.3847/1538-4365/abd107. S2CID 227126954.
  4. ^ a b c d e f g Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Mainzer, Amy K.; Marsh, Kenneth A.; Beichman, Charles A.; Burgasser, Adam J.; Prato, Lisa A.; Simcoe, Robert A.; Marley, Mark S.; Saumon, Didier; Freedman, Richard S.; Eisenhardt, Peter R.; Wright, Edward L. (2011). "The Discovery of Y Dwarfs using Data from the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal. 743 (1): 50. arXiv:1108.4678. Bibcode:2011ApJ...743...50C. doi:10.1088/0004-637X/743/1/50. S2CID 286881.
  5. ^ a b Cushing, Michael C.; Schneider, Adam C.; Kirkpatrick, J. Davy; Morley, Caroline V.; Marley, Mark S.; Gelino, Christopher R.; Mace, Gregory N.; Wright, Edward L.; Eisenhardt, Peter R.; Skrutskie, Michael F.; Marsh, Kenneth A. (2021). "An Improved Near-infrared Spectrum of the Archetype Y Dwarf WISEP J182831.08+265037.8". The Astrophysical Journal. 920 (1): 20. arXiv:2107.00506. Bibcode:2021ApJ...920...20C. doi:10.3847/1538-4357/ac12cb. S2CID 235694398.
  6. ^ Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Eisenhardt, Peter R.; McLean, Ian S.; Mainzer, Amy K.; Burgasser, Adam J.; Tinney, Chris G.; Parker, Stephen; Salter, Graeme (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal. 753 (2): 156. arXiv:1205.2122. Bibcode:2012ApJ...753..156K. doi:10.1088/0004-637X/753/2/156. S2CID 119279752.
  7. ^ a b Dupuy, Trent J.; Kraus, Adam L. (2013). "Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects". Science. 341 (6153): 1492–5. arXiv:1309.1422. Bibcode:2013Sci...341.1492D. doi:10.1126/science.1241917. PMID 24009359. S2CID 30379513.
  8. ^ a b Beichman, Charles A.; Gelino, Christopher R.; Kirkpatrick, J. Davy; Cushing, Michael C.; Dodson-Robinson, Sally; Marley, Mark S.; Morley, Caroline V.; Wright, Edward L. (2014). "WISE Y Dwarfs As Probes of the Brown Dwarf-Exoplanet Connection". The Astrophysical Journal. 783 (2): 68. arXiv:1401.1194v2. Bibcode:2014ApJ...783...68B. doi:10.1088/0004-637X/783/2/68. S2CID 119302072.
  9. ^ "An ammonia trail to exoplanets". www.phys.ethz.ch. 2023-11-07. Retrieved 2023-11-07.
  10. ^ Barrado, David; Mollière, Paul; et al. (November 2023). "15NH3 in the atmosphere of a cool brown dwarf". Nature. 624 (7991): 263–266. arXiv:2311.08054. doi:10.1038/s41586-023-06813-y.
  11. ^ a b c Lew, Ben W.P.; Roellig, Thomas; Batalha, Natasha E.; Line, Michael; Greene, Thomas; Murkherjee, Sagnick; Freedman, Richard; Meyer, Michael; Beichman, Charles; De Oliveira, Catarina Alves; De Furio, Matthew; Johnstone, Doug; Greenbaum, Alexandra Z.; Marley, Mark; J. Fortney, Jonathan (8 Feb 2024). "High-precision atmospheric characterization of a Y dwarf with JWST NIRSpec G395H spectroscopy: isotopologue, C/O ratio, metallicity, and the abundances of six molecular species". The Astronomical Journal. 167 (5): 237. arXiv:2402.05900. Bibcode:2024AJ....167..237L. doi:10.3847/1538-3881/ad3425.
  12. ^ a b 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 (2023-05-01). "JWST Observations of the Enigmatic Y-Dwarf WISE 1828+2650. I. Limits to a Binary Companion". The Astrophysical Journal. 948 (2): 92. arXiv:2302.12723. Bibcode:2023ApJ...948...92D. doi:10.3847/1538-4357/acbf1e. ISSN 0004-637X.
  13. ^ Beichman, Charles; De Furio, Matthew; Roellig, Thomas; Lew, Ben; Greene, Thomas; Leisenring, Jarron; Misselt, Karl; Stansberry, John; Boyer, Martha; Rieke, Marcia; Meyer, Michael; Albert, Loic; Kelly, Douglas; Greenbaum, Alexendra; Bryden, Geoffrey (2023-01-01). "JWST Observations of the Enigmatic Y Dwarf WISE 1828+2650". American Astronomical Society Meeting Abstracts. 55 (2): 345.05. Bibcode:2023AAS...24134505B.
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