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<h2 id="prototype-gliese-229b">Prototype Gliese 229B</h2> <p class="note">Main article: <a href="/facts/Gliese_229/AT2BsGbJ">Gliese 229</a></p> <p>The first T-dwarf discovered was Gliese 229B, which was discovered in 1995.<a class="footnote-ref" id="fnref:7" href="#fn:7"><sup>7</sup></a> This object had a temperature below 1000 <a href="/facts/Kelvin/E3trzC4C">K</a> and showed <a href="/facts/Methane/kBHneYnh">methane</a> (CH4), <a href="/facts/Water_vapor/DX5IUFG0">water vapor</a> (H2O) and <a href="/facts/Carbon_monoxide/CKuLtEMJ">carbon monoxide</a> (CO) in its spectrum. In the upper atmosphere CO is converted into CH4 and H2O, while the opposite is true for the hotter lower atmosphere.<a class="footnote-ref" id="fnref:8" href="#fn:8"><sup>8</sup></a><a class="footnote-ref" id="fnref:9" href="#fn:9"><sup>9</sup></a><a class="footnote-ref" id="fnref:10" href="#fn:10"><sup>10</sup></a> It also showed absorption due to <a href="/facts/Caesium/dXKN1S5k">caesium</a> (Cs), but absorption features commonly found in <a href="/facts/Red_dwarf/56CMQcF0">M-dwarfs</a> (<a href="/facts/Calcium_monohydride/nNTdvFTA">CaH</a>, <a href="/facts/Iron(I)_hydride/MmRrJG8S">FeH</a>, <a href="/facts/Titanium(II)_oxide/5ek4Vasd">TiO</a>, and <a href="/facts/Vanadium(II)_oxide/5b9whSBm">VO</a>) were missing.<a class="footnote-ref" id="fnref:11" href="#fn:11"><sup>11</sup></a> <a href="/facts/Ammonia/MtLtJFtz">Ammonia</a> (NH3) was included in the analysis of the spectrum.<a class="footnote-ref" id="fnref:12" href="#fn:12"><sup>12</sup></a> <a href="/facts/Sodium/eYuSPu2V">Sodium</a> (Na) and <a href="/facts/Potassium/5lcumVgo">potassium</a> (K) are also detected in this T-dwarf.<a class="footnote-ref" id="fnref:13" href="#fn:13"><sup>13</sup></a> Later work found a dynamical mass of 70 ± 5 <a href="/facts/Jupiter_mass/EtLUmeEN">MJ</a> for Gliese 229B, which is much higher than the cooling models would suggest.<a class="footnote-ref" id="fnref:14" href="#fn:14"><sup>14</sup></a> The spectral type is somewhat ambiguous. This is because it shows strong CH4 absorption at 1.3 and 1.6 μm, indicative of a T7 type, but weaker CH4 and H2O features at 1.1, 1.4, 1.9, and 2.2 μm, indicative of a T5-T6 type.<a class="footnote-ref" id="fnref:15" href="#fn:15"><sup>15</sup></a> It is also suspected that Gliese 229B is a binary, which could explain its high mass and its unusual spectrum.<a class="footnote-ref" id="fnref:16" href="#fn:16"><sup>16</sup></a> The binarity was confirmed in 2024 with instruments on the <a href="/facts/Very_Large_Telescope/xUQCLysQ">Very Large Telescope</a>, which resolved the pair and constrained their orbit to be a tight <a href="/facts/Semi-major_axis/l7JES2wo">semi-major axis</a> of about 16 Earth-Moon distances and an orbital period of about 12.1 days. Gliese 229Ba has a mass of about 38 MJ and Gliese 229Bb has a mass of about 34 MJ.<a class="footnote-ref" id="fnref:17" href="#fn:17"><sup>17</sup></a> </p> <h2 id="spectral-type-t">Spectral type T</h2> <p>The spectral type "T" was first proposed in 1999 with Gliese 229B as its only representative at the time.<a class="footnote-ref" id="fnref:18" href="#fn:18"><sup>18</sup></a> Next came the discovery of <a href="/facts/Gliese_570/rgCtfNTE">Gliese 570D</a>,<a class="footnote-ref" id="fnref:19" href="#fn:19"><sup>19</sup></a> <a href="/facts/SDSS_1624%252B00/G9SckvXl">SDSS 1624+00</a> (first field T-dwarf)<a class="footnote-ref" id="fnref:20" href="#fn:20"><sup>20</sup></a> and SDSS 1346-00 (second field T-dwarf).<a class="footnote-ref" id="fnref:21" href="#fn:21"><sup>21</sup></a> These were however mid- to late T-dwarfs and the first early T-dwarfs (SDSS 0837, SDSS 1254, and SDSS 1021) were discovered in data of the <a href="/facts/Sloan_Digital_Sky_Survey/MSHAk1RU">Sloan Digital Sky Survey</a> in 2000. These objects show weaker CH4 absorption than previously discovered T-dwarfs.<a class="footnote-ref" id="fnref:22" href="#fn:22"><sup>22</sup></a> CH4 appears first in the <a href="/facts/K_band_(infrared)/1MPj6hJ3">K-band</a> in L8 dwarfs and L- and T-dwarfs are distinguished by the appearance of CH4 in the <a href="/facts/H_band_(infrared)/Lb66NcRd">H-band</a> for T-dwarfs. T-dwarfs show an increasing absorption of H2O and CH4 from T0 to T8. Neutral Na and K features broaden in L- and T-dwarfs and the Na feature increases in depth for L/T-dwarfs with increasing spectral type.<a class="footnote-ref" id="fnref:23" href="#fn:23"><sup>23</sup></a> One of the coldest T-dwarfs was discovered with <a href="/facts/UKIRT_Infrared_Deep_Sky_Survey/f7CpySs2">UKIDSS</a>, called <a href="/facts/UGPS_J072227.51%25E2%2588%2592054031.2/5dYC6x1M">UGPS 0722-05</a>.<a class="footnote-ref" id="fnref:24" href="#fn:24"><sup>24</sup></a><a class="footnote-ref" id="fnref:25" href="#fn:25"><sup>25</sup></a> Researchers used <a href="/facts/Wide-field_Infrared_Survey_Explorer/7st7krr6">WISE</a> to discover additional late T-dwarfs and the objects of the newly discovered Y-dwarfs. The transition between T- and Y-dwarfs is defined with the help of UGPS 0722-05 as the T9 standard and <a href="/facts/WISEPA_J173835.53%252B273258.9/eLyVMIjL">WISE 1738+2732</a> as the Y0 standard. Late T and early Y-dwarfs show deep H2O and CH4 absorption features and the transition between T- and Y-dwarfs occurs near 500 K.<a class="footnote-ref" id="fnref:26" href="#fn:26"><sup>26</sup></a><a class="footnote-ref" id="fnref:27" href="#fn:27"><sup>27</sup></a> Another important T-dwarf is <a href="/facts/Luhman_16/AELwz9n5">Luhman 16</a>B, which is the closest T-dwarf. It has a spectral type of T0.5, near the L/T transition. It shows a hint of FeH in the spectrum, which weakens in late L dwarfs, but strengthens in early to mid T-dwarfs due to cloud disruption.<a class="footnote-ref" id="fnref:28" href="#fn:28"><sup>28</sup></a><a class="footnote-ref" id="fnref:29" href="#fn:29"><sup>29</sup></a> Observations of T-dwarfs in the near- and mid-infrared with <a href="/facts/James_Webb_Space_Telescope/w4GAWnWX">JWST</a> clearly show additional absorption features due to NH3, CH4, H2O, CO and <a href="/facts/Carbon_dioxide/xGzpppEp">carbon dioxide</a> (CO2).<a class="footnote-ref" id="fnref:30" href="#fn:30"><sup>30</sup></a> Observations with <a href="/facts/Gemini_Observatory/Yz6vJvms">Gemini</a> showed the first detection of <a href="/facts/Hydrogen_sulfide/UbCqjMMk">hydrogen sulfide</a> (H2S) and molecular <a href="/facts/Hydrogen/BoYHjl0J">hydrogen</a> (H2) in the T6 dwarf <a href="/facts/DENIS_J081730.0%25E2%2588%2592615520/Xpy5yfLS">DENIS J081730.0−615520</a>.<a class="footnote-ref" id="fnref:31" href="#fn:31"><sup>31</sup></a> The molecules <a href="/facts/Hydrogen_cyanide/vNtA0Mxe">hydrogen cyanide</a> (HCN) and <a href="/facts/Acetylene/yaDh6cmJ">acetylene</a> (C2H2) were found in the T-dwarf binary <a href="/facts/WISE_0458%252B6434/06oHjpG0">WISE 0458+6434</a> in 2025 with JWST.<a class="footnote-ref" id="fnref:32" href="#fn:32"><sup>32</sup></a> </p> <h3>Subdwarfs</h3> <p class="note">Main article: <a href="/facts/Subdwarf/5h8hyTHM">Subdwarf</a></p> <p>Subdwarfs with a T spectral type are known, with <a href="/facts/2MASS_J09373487%252B2931409/aVfNYFrJ">2MASSI J0937347+293142</a> being the first T-type subdwarf. It shows blue near-infrared colors due to suppression of the 2.1 μm peak, likely caused by enhanced <a href="/facts/Collision-induced_absorption_and_emission/KffUHM90">collision induced absorption</a> (CIA) of <a href="/facts/Hydrogen/BoYHjl0J">hydrogen</a> (H2).<a class="footnote-ref" id="fnref:33" href="#fn:33"><sup>33</sup></a><a class="footnote-ref" id="fnref:34" href="#fn:34"><sup>34</sup></a> Subdwarfs have a low metallicity and at first only a small sample with moderate low metallicity was known. In 2020 the <a href="/facts/Backyard_Worlds/KVuUjjcy">backyard worlds</a> citizen science project discovered the first extreme subdwarfs of spectral type T, called WISEA 0414−5854 and <a href="/facts/WISEA_1810%25E2%2588%25921010/1hh38pDR">WISEA 1810−1010</a>. These objects have unusual blue colors, indicative of a lower absorption from CH4.<a class="footnote-ref" id="fnref:35" href="#fn:35"><sup>35</sup></a> Follow-up observations of WISEA 1810−1010 show that it only shows absorption due to H2O and H2 in the optical and infrared spectra. CH4 is missing completely, which stays in contrast to the definition of T-dwarfs as "methane dwarfs" and WISEA 1810−1010 was instead called a "water vapor dwarf".<a class="footnote-ref" id="fnref:36" href="#fn:36"><sup>36</sup></a> In 2024 Burgasser et al. introduced a classification system for T subdwarfs, which allows the classification into mild subdwarfs (d/sdT), subdwarfs (sdT) and extreme subdwarfs (esdT). The signature of a low metallicity are a strong <a href="/facts/Collision-induced_absorption_and_emission/KffUHM90">collision induce absorption</a> (CIA) of hydrogen molecules, obscured methane and water features, and weak potassium K I absorption. This work also identified three brown dwarfs that are candidate members of <a href="/facts/Stellar_stream/6q1SRvDa">stellar streams</a>. Future works with <a href="/facts/James_Webb_Space_Telescope/w4GAWnWX">JWST</a>, <a href="/facts/Euclid_(spacecraft)/DfSUqzJu">Euclid</a>, <a href="/facts/Vera_C._Rubin_Observatory/n7t9ANEu">Rubin</a> and <a href="/facts/Nancy_Grace_Roman_Space_Telescope/LXBWIsMx">Roman</a> will increase the sample of T subdwarfs to thousands.<a class="footnote-ref" id="fnref:37" href="#fn:37"><sup>37</sup></a> JWST has already discovered the first distant T subdwarfs such as <a href="/facts/UNCOVER-BD-1/0aYcLclA">UNCOVER-BD-1</a>.<a class="footnote-ref" id="fnref:38" href="#fn:38"><sup>38</sup></a> </p> <h2 id="brown-dwarfs">Brown dwarfs</h2> <p class="note">Main article: <a href="/facts/Brown_dwarf/fa7kr9lH">Brown dwarf</a></p> <p>Most T-dwarfs are brown dwarfs. Brown dwarfs have a mass lower than the hydrogen burning minimum mass (0.075 <a href="/facts/Solar_mass/j6Auhku8">M☉</a> or 78.5 <a href="/facts/Jupiter_mass/EtLUmeEN">MJ</a>).<a class="footnote-ref" id="fnref:39" href="#fn:39"><sup>39</sup></a> There are currently 920 objects in the UltracoolSheet with an infrared spectral type of T.<a class="footnote-ref" id="fnref:40" href="#fn:40"><sup>40</sup></a> The table of ultracool fundamental parameters lists objects with an infrared spectral type of T that have masses between 2 and 58 MJ.<a class="footnote-ref" id="fnref:41" href="#fn:41"><sup>41</sup></a><a class="footnote-ref" id="fnref:42" href="#fn:42"><sup>42</sup></a> Additional T-type brown dwarfs that orbit <a href="/facts/Star/euBFuo07">stars</a> or <a href="/facts/White_dwarf/gIYlTtrC">white dwarfs</a> are known and the age of the primary can help to determine the mass of the T-dwarfs.<a class="footnote-ref" id="fnref:43" href="#fn:43"><sup>43</sup></a><a class="footnote-ref" id="fnref:44" href="#fn:44"><sup>44</sup></a><a class="footnote-ref" id="fnref:45" href="#fn:45"><sup>45</sup></a> One of the oldest known T-dwarfs is <a href="/facts/Wolf_1130/9zVep4Jg">Wolf 1130</a>C, which is around 10 <a href="/facts/Bya/5E7foypY">billion years</a> old.<a class="footnote-ref" id="fnref:46" href="#fn:46"><sup>46</sup></a> </p> <h2 id="planetary-mass-objects-and-exoplanets">Planetary-mass objects and exoplanets</h2> <p>One of the first objects that was conclusively determined to be a young isolated planetary-mass object with spectral type T was SDSS J1110+0116 (T5.5), which is a member of the 120 Myr old <a href="/facts/AB_Doradus_moving_group/aHVVaQHU">AB Doradus moving group</a>.<a class="footnote-ref" id="fnref:47" href="#fn:47"><sup>47</sup></a> Another significant discovery is one of the closest planetary-mass objects, called <a href="/facts/SIMP_J013656.5%252B093347/MQ3XgFSA">SIMP J013656.5+093347</a> (T2.5, 12.7 ±1.0 MJ), which is part of the 200 Myr old Carina-Near moving group.<a class="footnote-ref" id="fnref:48" href="#fn:48"><sup>48</sup></a> This object is also variable with a period of 2.4 hours, likely due to clouds.<a class="footnote-ref" id="fnref:49" href="#fn:49"><sup>49</sup></a> It also shows <a href="/facts/Radio_astronomy/TdjF4LgL">radio emission</a> due to <a href="/facts/Aurora/6agpj9Qs">aurorae</a>.<a class="footnote-ref" id="fnref:50" href="#fn:50"><sup>50</sup></a> Additional young T-dwarf candidates are known from other <a href="/facts/Stellar_association/urBqjfYg">young stellar associations</a> and these objects show red colors compared to field T-dwarfs.<a class="footnote-ref" id="fnref:51" href="#fn:51"><sup>51</sup></a> Young directly imaged exoplanets and planetary-mass companions sometimes show a T spectral type, such as <a href="/facts/51_Eridani_b/6ruB86V3">51 Eridani b</a> (T4.5-T6).<a class="footnote-ref" id="fnref:52" href="#fn:52"><sup>52</sup></a> </p> <h2 id="clouds-and-variability">Clouds and variability</h2> <p>Two of the most variable brown dwarfs are the T-dwarfs Luhman 16B, showing a variation up to 20%<a class="footnote-ref" id="fnref:53" href="#fn:53"><sup>53</sup></a> and <a href="/facts/2MASS_J21392676%252B0220226/wBzUkDJ2">2MASS J2139+02</a>, which varies with an amplitude as high as 26%.<a class="footnote-ref" id="fnref:54" href="#fn:54"><sup>54</sup></a> T-dwarfs, especially young early-type T-dwarfs are often variable. The variability has been connected to the presence of clouds, but other explanations were proposed, such as hot spots and aurorae.<a class="footnote-ref" id="fnref:55" href="#fn:55"><sup>55</sup></a> These early T-dwarfs are thought to have an <a href="/facts/Iron/DkICCKIC">iron</a> cloud deck and a patchy <a href="/facts/Silicate/7NdthSRM">silicate</a> cloud layer on top of it. The silicate clouds are thought to dissipate near the L/T transition, resulting into the patchy silicate cloud layer and high amplitude variability for late L and early T dwarfs.<a class="footnote-ref" id="fnref:56" href="#fn:56"><sup>56</sup></a> The disruption of clouds make deeper layers accessible for observations. These deeper layers are warmer and contain FeH. This explains the reappearance and strengthening of FeH and the blue near-infrared color for early to mid T-dwarfs.<a class="footnote-ref" id="fnref:57" href="#fn:57"><sup>57</sup></a> Late T-dwarfs should also have cloud layers made of <a href="/facts/Chromium/6sVk6Uu7">chromium</a>, <a href="/facts/Potassium_chloride/RgT2MdPa">potassium chloride</a> and different <a href="/facts/Sulfide/d8YMjLeu">sulfides</a>. These cloud layers are thin and exist above the silicate clouds.<a class="footnote-ref" id="fnref:58" href="#fn:58"><sup>58</sup></a> A few late T-dwarfs are known to be variable, such as <a href="/facts/Ross_458/FoFJBsNB">Ross 458C</a> (T8),<a class="footnote-ref" id="fnref:59" href="#fn:59"><sup>59</sup></a> <a href="/facts/WISE_0458%252B6434/06oHjpG0">WISE 0458+6434</a> (T8.5),<a class="footnote-ref" id="fnref:60" href="#fn:60"><sup>60</sup></a> and <a href="/facts/2MASS_J09393548%25E2%2588%25922448279/5PvICkkR">2MASS J09393548-2448279</a> (T8).<a class="footnote-ref" id="fnref:61" href="#fn:61"><sup>61</sup></a> </p> <h2 id="magnetic-field-and-aurorae">Magnetic field and aurorae</h2> <p>The first T-dwarf detected in <a href="/facts/Radio_astronomy/TdjF4LgL">radio emission</a> was <a href="/facts/2MASS_J10475385%252B2124234/rNW7NWpW">2MASS J1047+21</a> (T6.5), which was discovered with the <a href="/facts/Arecibo_Telescope/gkK6QE9G">Arecibo radio telescope</a>.<a class="footnote-ref" id="fnref:62" href="#fn:62"><sup>62</sup></a> Since then several other T-dwarfs with radio emission were discovered, including the planetary-mass object SIMP J013656.5+093347 (T2.5)<a class="footnote-ref" id="fnref:63" href="#fn:63"><sup>63</sup></a> and the discovery of the T-dwarf BDR J1750+3809 with the help of radio emission.<a class="footnote-ref" id="fnref:64" href="#fn:64"><sup>64</sup></a> The coldest T-dwarf with a radio emission is <a href="/facts/WISEPA_J062309.94-045624.6/4Xsb6qBM">WISEPA J062309.94-045624.6</a> (T8).<a class="footnote-ref" id="fnref:65" href="#fn:65"><sup>65</sup></a> Radio emission in T-dwarfs is thought to be generated by an <a href="/facts/Aurora/6agpj9Qs">aurora</a>, similar to late L-dwarfs. Additionally <a href="/facts/Hydrogen-alpha/Akk50rbI">H-alpha</a> emission is often connected to radio emission in L4-T8 dwarfs and is thought to come from aurorae.<a class="footnote-ref" id="fnref:66" href="#fn:66"><sup>66</sup></a> <a href="/facts/2MASS_1237%252B6526/u2segSla">2MASS 1237+6526</a> (T6.5) is an unusual strong H-alpha emitting T-dwarf that was discovered in 2000.<a class="footnote-ref" id="fnref:67" href="#fn:67"><sup>67</sup></a> It was theorized that the H-alpha emission, <a href="/facts/Ultraviolet/kncBUqn5">UV</a> emission and radio emission come either from a cold companion (1-2.8 <a href="/facts/Earth_radius/PVsf0g2I">R🜨</a>; <500 K) or from an aurora.<a class="footnote-ref" id="fnref:68" href="#fn:68"><sup>68</sup></a> </p> <h2 id="binaries">Binaries</h2> <p>Late T dwarf binaries are less common than L-type binaries. Only 8±6% systems with a T5–Y0 primary are binaries and these systems usually have a separation of a few <a href="/facts/Astronomical_unit/gjsbu5xU">astronomical units</a> (AU).<a class="footnote-ref" id="fnref:69" href="#fn:69"><sup>69</sup></a> One well-known T dwarf binary is <a href="/facts/Epsilon_Indi/4Hjwnlh0">Epsilon Indi B</a>.<a class="footnote-ref" id="fnref:70" href="#fn:70"><sup>70</sup></a> This binary consists of a T1 and a T6 dwarf that orbit each other with a separation of 2.65 AU.<a class="footnote-ref" id="fnref:71" href="#fn:71"><sup>71</sup></a> T dwarf triple systems also exist, with <a href="/facts/2MASS_J08381155%252B1511155/vYaWmCQo">2M0838+15</a> being the first fully resolved triple T dwarf that was discovered.<a class="footnote-ref" id="fnref:72" href="#fn:72"><sup>72</sup></a> </p> <h2 id="see-also">See also</h2> <ul><li><a href="/facts/List_of_brown_dwarfs/4Xsb6qBM">List of brown dwarfs</a></li></ul> <h2 id="references">References</h2> <ol> <li id="fn:1"><p>Kirkpatrick, J. Davy; Reid, I. Neill; Liebert, James; Cutri, Roc M.; Nelson, Brant; Beichman, Charles A.; Dahn, Conard C.; Monet, David G.; Gizis, John E.; Skrutskie, Michael F. (1999-07-01). "Dwarfs Cooler than M: The Definition of Spectral Type L Using Discoveries from the 2 Micron All-Sky Survey (2MASS)". The Astrophysical Journal. 519 (2): 802–833. Bibcode:1999ApJ...519..802K. doi:10.1086/307414. ISSN 0004-637X. <a href="https://ui.adsabs.harvard.edu/abs/1999ApJ...519..802K/abstract" target="_blank">https://ui.adsabs.harvard.edu/abs/1999ApJ...519..802K/abstract</a> <a href="#fnref:1" class="footnote-back-ref">↩</a></p></li> <li id="fn:2"><p>Brandt, Timothy D.; Dupuy, Trent J.; Bowler, Brendan P.; Bardalez Gagliuffi, Daniella C.; Faherty, Jacqueline; Brandt, G. Mirek; Michalik, Daniel (October 2020). "A Dynamical Mass of 70 ± 5 MJup for Gliese 229B, the First T Dwarf". The Astronomical Journal. 160 (4): 196. arXiv:1910.01652. Bibcode:2020AJ....160..196B. doi:10.3847/1538-3881/abb45e. ISSN 0004-6256. <a href="https://doi.org/10.3847%2F1538-3881%2Fabb45e" target="_blank">https://doi.org/10.3847%2F1538-3881%2Fabb45e</a> <a href="#fnref:2" class="footnote-back-ref">↩</a></p></li> <li id="fn:3"><p>Gagné, Jonathan; Faherty, Jacqueline K.; Burgasser, Adam J.; Artigau, Étienne; Bouchard, Sandie; Albert, Loïc; Lafrenière, David; Doyon, René; Bardalez Gagliuffi, Daniella C. (2017-05-01). "SIMP J013656.5+093347 Is Likely a Planetary-mass Object in the Carina-Near Moving Group". The Astrophysical Journal. 841 (1): L1. arXiv:1705.01625. Bibcode:2017ApJ...841L...1G. doi:10.3847/2041-8213/aa70e2. ISSN 0004-637X. <a href="https://doi.org/10.3847%2F2041-8213%2Faa70e2" target="_blank">https://doi.org/10.3847%2F2041-8213%2Faa70e2</a> <a href="#fnref:3" class="footnote-back-ref">↩</a></p></li> <li id="fn:4"><p>Macintosh, B.; Graham, J. R.; Barman, T.; De Rosa, R. J.; Konopacky, Q.; Marley, M. S.; Marois, C.; Nielsen, E. L.; Pueyo, L.; Rajan, A.; Rameau, J.; Saumon, D.; Wang, J. 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