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{{short description|A Y dwarf is a brown dwarf or planetary-mass object that is colder than 500 Kelvin}}
An object with a '''spectral type Y''' (also called '''Y dwarf''') is either a [[brown dwarf]] or a [[rogue planet|free-floating planetary-mass object]]. They have temperatures below around 500 [[Kelvin]] (227°C; 440°F) and are colder than [[T dwarf|T-dwarfs]].<ref name="Kirkpatrick11" /><ref name="Cushing11" /> Y-dwarfs have a similar spectrum when compared to the giant planet [[Jupiter]].<ref name="Coulter22"/>
== Early theories and discovery ==
[[File:WISE 0855-0714 NIRCam Movement.jpg|thumb|[[James Webb Space Telescope]] images, showing the movement of WISE 0855-0714, the coldest Y-dwarf]]
When the spectral classes of [[L dwarf|L dwarfs]] and [[T dwarf|T dwarfs]] were defined it was mentioned that the letter Y was available for an additional spectral class.<ref name="Kirkpatrick1999"/> In the early 2000s it was already theorized that objects "beyond the T dwarfs" should exist and that these objects would bridge the gap between T dwarfs and the [[giant planet|giant planets]] of the [[Solar System]]. Observations and discoveries with [[Wide-field Infrared Survey Explorer|WISE]], [[Spitzer Space Telescope|Spitzer]] and [[James Webb Space Telescope]] were anticipated. Modelling of such cold objects predicted the disappearance of the [[sodium]] (Na D) and [[potassium]] (K I) features at around 500 K and the appearance of [[Cloud|water clouds]] at around 400–500 K. [[Ammonia]] clouds were predicted to exist below around 160 K.<ref name="Burrows2003"/> The formation of these clouds were theorized earlier in the [[Sudarsky's gas giant classification]].<ref name="Sudarsky2003"/>
After some candidates were proposed in 2010 and 2011,<ref name="Eisenhardt2010" /><ref name="Rodriguez2011" /><ref name="Liu2011" /> a larger sample of Y-dwarfs were discovered with WISE and the Y-dwarf spectral type was established, using [[UGPS J072227.51−054031.2|UGPS 0722-05]] as the T9 standard and [[WISEPA J173835.53+273258.9|WISE 1738+2732]] as the Y0 standard.<ref name="Kirkpatrick11" /><ref name="Cushing11" /> A significant discovery was the discovery of [[WISE 0855−0714|WISE J0855−0714]], which remains the coldest and closest Y-dwarf discovered.<ref name="NASA20140425" /> It has a temperature of 285 K (12 °C; 53 °F) and has the latest spectral type of Y4.<ref name="Luhman2024" />
== The Y-class ==
[[File:The first full spectral energy distribution of a Y-dwarf.jpg|thumb|Spectrum of [[WISE 0359−5401]] with JWST, showing different molecular absorption bands.]]
A Y-dwarf is characterized by its deep [[methane]] (CH<sub>4</sub>) and [[water vapor]] (H<sub>2</sub>O) bands, as well as a narrower [[J band (infrared)|J-band]] peak than the T9 standard. The J-band peak will get narrower with a spectral type later than T8. Early observations also showed evidence of [[ammonia]] (NH<sub>3</sub>) in the near-infrared spectrum.<ref name="Kirkpatrick11" /><ref name="Cushing11" /> Modern observations with JWST detect CH<sub>4</sub>, H<sub>2</sub>O, NH<sub>3</sub>, [[carbon monoxide]] (CO) and [[carbon dioxide]] (CO<sub>2</sub>) in the atmosphere of Y-dwarfs. [[Phosphine]] (PH<sub>3</sub>) is missing from the atmosphere, despite being predicted to be present.<ref name="Beiler2023" /><ref name="Beiler2024" /> JWST observations showed that models under-predict the abundance of CO<sub>2</sub> and over-predict PH<sub>3</sub> for late T and Y dwarfs. Proposed explanations for the missing PH<sub>3</sub> are that it condenses into clouds of [[ammonium dihydrogen phosphate]] (NH<sub>4</sub>H<sub>2</sub>PO<sub>4</sub>), an incomplete understanding of [[phosphorus]] chemistry or a different mixing of the atmosphere. The overabundance of CO<sub>2</sub> is explained with a better understanding of the CO<sub>2</sub> chemistry in respect to CO chemistry.<ref name="Beiler2024b"/> CH<sub>4</sub>, H<sub>2</sub>O and NH<sub>3</sub> absorption features get deeper with lower temperature. The 5 μm peak does not show such a correlation and instead shows a large diversity. This region is influenced by multiple molecules, including CO and CO<sub>2</sub>, which vary a lot between sources. The reason for this variation could be due to a different [[surface gravity]] or due to differences in [[metallicity]].<ref name="Beiler2024" /><ref name="Tu2024" /> CO<sub>2</sub> was noted to slightly decrease from T dwarfs to Y dwarfs, but not CO.<ref name="Tu2024" /> [[Hydrogen sulfide]] (H<sub>2</sub>S) is used to improve the spectral fits of T- and Y-dwarfs. Currently the only Y-dwarfs with detected H<sub>2</sub>S are [[WISE 1828+2650|WISE 1828+26]] and [[WISE 0359−5401]].<ref name="Kothari2024"/>
=== Colder lower atmosphere ===
Usually brown dwarfs have a [[pressure]]–[[temperature]] (P–T) profile in an [[Adiabatic process|adiabatic]] form, which means that the pressure and temperature increase with depth. JWST spectroscopy and [[Photometry (astronomy)|photometry]] suggest that Y-dwarfs have P–T profiles that are not in the standard adiabatic form. This means that upper layers of the atmosphere have a warmer temperature and lower layers of the atmosphere have a colder temperature. This is explained by the rapid [[rotation]] of these isolated objects. The rapid rotation leads to dynamical, thermal, and chemical changes, which disrupt the [[Convection|convective]] transport of heat from the lower to the upper atmosphere. This different P–T profile influences the shape of the spectrum and influences the composition of carbon- and nitrogen-bearing molecules in the atmospheres of Y-dwarfs.<ref name="Leggett+Tremblin"/>
=== Clouds and variability ===
Water clouds were theorized since the early 2000s to exist in Y-dwarfs.<ref name="Sudarsky2003" /><ref name="Burrows2003" /> The Y-dwarfs do however likely also have clouds made of other condensates, such as [[Sulfide|sulfides]], [[potassium chloride]] (KCl) and possibly [[ammonium dihydrogen phosphate]] (NH<sub>4</sub>H<sub>2</sub>PO<sub>4</sub>). These clouds would exist below any water clouds for colder Y-dwarfs.<ref name="Morley2012"/> Some Y-dwarfs are likely too warm to form water clouds, but could have other observable clouds.<ref name="Leggett2016"/> The first discovered variable Y-dwarf was [[WISE 1405+5534]] (Y0) and its variability is modelled with a single bright spot.<ref name="Cushing2016"/> Another variable Y dwarf is [[WISEPA J173835.53+273258.9|WISE 1738+2732]] (Y0) and its variability is explained with the breakup of KCl and [[sodium sulfide]] (Na<sub>2</sub>S) clouds into a patchy cloud cover.<ref name="Leggett2016" /> WISE 0855−0714 (Y4) is suspected to have [[Ice|water ice]] clouds, which should produce large amplitude variations. It does show relatively small variations of 4–5%, which could mean that both hemispheres have a similar cloud cover.<ref name="Esplin2016"/>
=== Peculiar Y-dwarfs ===
[[File:Atmospheric methane of brown dwarfs W1935 and W2220 (NIRSpec) (browndwarfs-aurora).jpg|thumb|Aurora in CWISEP J1935-1546 detected by its methane emission]]
Currently only the suffix pec, standing for "peculiar" or unusual, exists for Y-dwarfs. Any spectral peculiarity is denoted this way, such as the Y-band peak and Y-J color of [[WISE 1639−6847]] (Y0pec), which is different from other Y-dwarfs.<ref name="Schneider2015"/> In some cases the peculiarity is explained with a non-solar [[metallicity]] or an unusual [[surface gravity]]. An example is [[CWISE J1055+5443]], for which researchers find that low gravity models fit the spectrum better, likely due to a young age.<ref name="Robbins232"/> JWST observations found two Y-dwarfs with unusual spectral features of the carbon-bearing molecules. [[CWISEP J1047+5457|CWISEP J1047+54]] showed abnormally strong CO and CO<sub>2</sub> and likely weaker CH4.<ref name="Beiler2024" /> Similar strong CO and CO<sub>2</sub> absorption features were found in [[WISE J1206+8401]].<ref name="Tu2024"/> [[WISE 0535−7500|WISE J0535−75]] on the other hand showed no discernable CO<sub>2</sub> and almost undetectable CO, but it also showed stronger NH<sub>3</sub> absorption when compared to Y-dwarfs with similar temperature.<ref name="Beiler2024" /> Another notable spectral discovery with JWST is the emission of methane in [[CWISEP J1935-1546]], which is interpreted with the presence of an [[aurora]].<ref name="Faherty2024"/> One of the first suspected Y-type [[Subdwarf|subdwarfs]] is [[WISE 1534–1043|WISEA J1534−1043]], which shows an unusual blue color. Spectroscopic observations are however required to confirm this hypothesis.<ref name="Kirkpatrick et al."/>
== Exoplanets and companions ==
Masses estimated for Y-dwarfs are between 3–29 {{Jupiter mass|link=true}}, but more typically below 21 {{Jupiter mass}}. This makes them similar to massive exoplanets.<ref name="Leggett17"/><ref name="Fontanive23"/><ref name="Leggett24"/>
There is only one confirmed Y-dwarf that co-moves with a [[white dwarf]], called [[WD 0806−661 B]].<ref name="Luhman2011" /> Though of planetary mass, Rodriguez et al. suggest it is unlikely to have formed in the same manner as planets.<ref name="Rodriguez2011" /> Additionally there is the T/Y companion [[Ross 19|Ross 19B]], which orbits a main-sequence star.<ref name="Schneider21" /> A small sample of (candidate) exoplanets exist with a temperature below 500 K, which could be spectroscopically confirmed as Y-dwarfs in the future. These exoplanets are [[Epsilon Indi Ab]] (275 K),<ref name="Matthews2024"/> [[WD 1202–232]]<nowiki/>b, [[WD 2105–82]]<nowiki/>b (both low temperature),<ref name="Mullally2024" /> [[GALEX J071816.4+373139]]<nowiki/>b (400 K),<ref name="Sihao2024"/> and [[WD 0310–688]]<nowiki/>b ({{Val|248|84|61}} K).<ref name="Limbach2024"/>
== Binaries ==
Binaries consisting of a late T dwarf primary and a Y dwarf secondary are known since the discovery of [[CFBDSIR J145829+101343|CFBDS J1458+10]] during the early discovery of Y-dwarfs.<ref name="Liu2011" /> Other such binaries are [[WISE 1217+1626|WISEPC J1217+1626]]<ref name="Liu12"/> and [[WISE 0146+4234|WISE J0146+4234]].<ref name="Dupuy152"/> The first Y+Y binary is [[WISE J0336−0143]], discovered in 2023 with JWST.<ref name="Calissendorff23"/>
== Individual discoveries ==
{{see also|List of Y-dwarfs}}
Timeline of Y-dwarf discoveries:
* April 2010: Two newly discovered ultracool [[sub-brown dwarf]]s ([[UGPS J072227.51−054031.2|UGPS 0722-05]] and SDWFS 1433+35) were proposed as prototypes for spectral class Y0.<ref name="Eisenhardt2010"/>
* February 2011: Luhman et al. reported the discovery of [[WD 0806−661 B]], a brown dwarf companion to a nearby white dwarf, with a temperature of c.&nbsp;{{cvt|300|K|C F}} and mass of [[Jupiter mass|{{Jupiter mass|7}}]].<ref name="Luhman2011"/>
* February 2011: Shortly after that, Liu et al. published an account of a "very cold" (c.&nbsp;{{cvt|370|K|C F}}) brown dwarf orbiting another very-low-mass brown dwarf and noted, "Given its low luminosity, atypical colors and cold temperature, [[CFBDSIR J145829+101343|CFBDS J1458+10B]] is a promising candidate for the hypothesized Y spectral class."<ref name="Liu2011"/>
* August 2011: Scientists using data from NASA's [[Wide-field Infrared Survey Explorer]] (WISE) discovered six objects that they classified as Y dwarfs with temperatures as cool as {{cvt|25|C|K F}}.<ref name="Plait2011"/><ref name="NASA2011"/> These were published in two papers.<ref name="Kirkpatrick11"/><ref name="Cushing11"/>
* July 2012: Seven new Y-dwarfs were discovered, making the total number of confirmed Y-dwarfs fourteen.<ref name="Kirkpatrick12"/><ref name="DwarfArchives" /> One of the Y dwarfs, called [[WISE 1828+2650]], was, as of August 2011, the record holder for the coldest brown dwarf—emitting no visible light at all, this type of object resembles a free-floating planet more than a star. WISE 1828+2650 was initially estimated to have an atmospheric temperature cooler than {{cvt|300|K|C F}}.<ref name="Morse2011"/> Its temperature has since been revised, and newer estimates put it in the range of {{cvt|250|to|400|K|C F}}.<ref name="Beichman2013"/>
* November 2012: [[WISE 1639−6847|WISE J1639−6847]] was discovered. As of February 2024, it was the second-closest known Y-dwarf to Earth.<ref name="Tinney12"/>
* April 2014: [[WISE 0855−0714]] was announced, with a temperature profile estimated around {{cvt|225|to(-)|260|K|C F}} and a mass of {{Jupiter mass|3 to 10|link=yes}}.<ref name="NASA20140425"/> It was also unusual in that its observed parallax meant a distance close to {{nowrap|7.2 ± 0.7}} light-years from the Solar System.
* May 2014: The Y-dwarf [[WISE J2209+2711]] was published.<ref name="Cushing14"/>
* November 2014: The object [[WISEA J1141−3326]] was estimated to be a Y-dwarf<ref name="Tinney14"/> and it was later confirmed.<ref name="Tinney18"/>
* April 2015: The T+Y dwarf binary [[WISE 0146+4234|WISE J0146+4234 AB]] was discovered.<ref name="Dupuy15"/>
* May 2015: Three Y-dwarfs were discovered with Hubble, bringing the total number of confirmed Y-dwarfs to 21.<ref name="Schneider15"/>
* June 2018: [[WISEA J0302−5817]] was published as a Y-dwarf, and WISEA J1141−3326 was confirmed as a Y-dwarf.<ref name="Tinney18" />
* August 2019: A search of the CatWISE catalog revealed [[CWISEP J1935-1546]], one of the coldest brown dwarfs with an estimated temperature of {{cvt|270|to(-)|360|K|C F}}.<ref name="Marocco_etal_2019"/> In 2023 it was announced that CWISEP J1935-1546 had methane emission due to an aurora.<ref name="NASApressAurora"/>
* January 2020: In January 2020 the discovery of [[WISE J0830+2837]], initially discovered by [[Citizen science|citizen scientists]] of the [[Backyard Worlds]] project, was presented at the 235th meeting of the [[American Astronomical Society]]. This Y dwarf is 36.5 light-years distant from the Solar System and has a temperature of about {{cvt|350|K|C F}}.<ref name="Bardalez Gagliuffi2020"/>
* February 2020: The CatWISE catalog combined NASA's WISE and [[NEOWISE]] surveys.<ref name="Eisenhardt2020"/> It expanded the number of faint sources and has therefore been used to find the faintest brown dwarfs, including Y dwarfs. Seventeen candidate Y dwarfs were discovered by the CatWISE researchers. Initial color with the [[Spitzer Space Telescope]] indicated that [[CWISEP J1446−2317|CW1446]] is one of the reddest and coldest Y dwarfs.<ref name="Meisner2020"/> Additional data with Spitzer showed that CW1446 is the fifth-reddest brown dwarf, with a temperature of about {{cvt|310|to(-)|360|K|C F}} and a distance of about 10 parsecs.<ref name="Marocco2020"/>
* August 2020: Five candidate Y-dwarfs were discovered via the Backyard Worlds project.<ref name="Meisner2020b" />
* April 2021: New Y-dwarf candidates were published by the CatWISE and Backyard Worlds teams in a collaborative paper.<ref name="Kirkpatrick212"/>
* August 2021: [[Ross_19|Ross 19B]], an old object near the T/Y-boundary orbiting an M-dwarf, was discovered by the Backyard Worlds team.<ref name="Schneider21"/>
* April 2023: [[WISE J0336−0143]] was confirmed as a Y-dwarf binary with JWST.<ref name="Calissendorff2023" /> The B secondary is likely one of the coldest confirmed Y-dwarfs as of December 2023, with an estimated temperature of {{cvt|246|to(-)|404|K|C F}}.<ref name="Kirkpatrick23"/>
* November 2023: [[CWISE J1055+5443]], an object previously classified as a T-dwarf, was confirmed as a nearby Y-dwarf.<ref name="Robbins23"/>
* December 2023: Three new Y-dwarf candidates were published.<ref name="Kirkpatrick23" /> The total number of confirmed Y-dwarfs was 27, and 30 additional Y-dwarf candidates existed as of February 2024.
== References ==
{{reflist | refs=
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<ref name="DwarfArchives">
{{cite web
|first1=J. Davy |last1=Kirkpatrick |author1-link=J. Davy Kirkpatrick
|first2=Adam J. |last2=Burgasser
|date=6 November 2012
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|publisher=California Institute of Technology
|place=Pasadena, CA
|url=http://spider.ipac.caltech.edu/staff/davy/ARCHIVE/index.shtml
|access-date=2012-12-28
}} (M=536, L=918, T=355, Y=14)
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}}
[[Category:Y-type brown dwarfs]]
[[Category:Brown dwarfs]]
[[Category:Rogue planets]]