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T dwarf

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An object with the spectral type T (also called T dwarf or methane brown dwarf)[1] is either a brown dwarf[2] or young free-floating planetary-mass object.[3] An directly imaged exoplanet with a young age can also be a T-dwarf.[4] T dwarfs are colder than L dwarfs,[1] but warmer than Y dwarfs.[5]

Prototype Gliese 229B

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Main article: Gliese 229
 
Hubble image of Gliese 229B

The first T-dwarf discovered was Gliese 229B, which was discovered in 1995.[6] This object had a temperature below 1000 K and showed methane (CH4), water vapor (H2O) and carbon monoxide (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.[7][8][9] It also showed absorption due to caesium (Cs), but absorption features commonly found in M-dwarfs (CaH, FeH, TiO, and VO) were missing.[10] Ammonia (NH3) was included in the analysis of the spectrum.[11] Sodium (Na) and potassium (K) are also detected in this T-dwarf.[12] Later work found a dynamical mass of 70 ± 5 MJ for Gliese 229B, which is much higher than the cooling models would suggest.[2] 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.[13] It is also suspected that Gliese 229B is a binary, which could explain its high mass and its unusual spectrum.[14]

Spectral type T

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Spectra of mid to late T-dwarfs, showing absorption due to methane, water vapor, CIA hydrogen and potassium

The spectral type "T" was first proposed in 1999 with Gliese 229B as its only representative at the time.[1] Next came the discovery of Gliese 570D,[15] SDSS 1624+00 (first field T-dwarf)[16] and SDSS 1346-00 (second field T-dwarf).[17] 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 Sloan Digital Sky Survey in 2000. These objects show weaker CH4 absorption than previously discovered T-dwarfs.[18] CH4 appears first in the K-band in L8 dwarfs and L- and T-dwarfs are distinguished by the appearance of CH4 in the H-band 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.[19] One of the coldest T-dwarfs was discovered with UKIDSS, called UGPS 0722-05.[20][21] Researchers used WISE 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 WISE 1738+2732 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.[5][22] Another important T-dwarf is Luhman 16B, 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.[23][24] Observations of T-dwarfs in the near- and mid-infrared with JWST clearly show additional absorption features due to NH3, CH4, H2O, CO and carbon dioxide (CO2).[25]

Subdwarfs

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Main article: Subdwarf

Subdwarfs with a T spectral type are known, with 2MASSI J0937347+293142 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 collision induced absorption (CIA) of hydrogen (H2).[26][27] Subdwarfs have a low metallicity and at first only a small sample with moderate low metallicity was known. In 2020 the backyard worlds citizen science project discovered the first extreme subdwarfs of spectral type T, called WISEA 0414−5854 and WISEA 1810−1010. These objects have unusual blue colors, indicative of a lower absorption from CH4.[28] 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".[29]

Brown dwarfs

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Main article: Brown dwarf

Most T-dwarfs are brown dwarfs. Brown dwarfs have a mass lower than the hydrogen burning minimum mass (0.075 M☉ or 78.5 MJ).[30] There are currently 920 objects in the UltracoolSheet with an infrared spectral type of T.[31] The table of ultracool fundamental parameters lists objects with an infrared spectral type of T that have masses between 2 and 58 MJ.[32][33] Additional T-type brown dwarfs that orbit stars or white dwarfs are known and the age of the primary can help to determine the mass of the T-dwarfs.[34][35][36] One of the oldest known T-dwarfs is Wolf 1130C, which is around 10 billion years old.[37]

Planetary-mass objects and exoplanets

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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 AB Doradus moving group.[38] Another significant discovery is one of the closest planetary-mass objects, called SIMP J013656.5+093347 (T2.5, 12.7 ±1.0 MJ), which is part of the 200 Myr old Carina-Near moving group.[3] This object is also variable with a period of 2.4 hours, likely due to clouds.[39] It also shows radio emission due to aurorae.[40] Additional young T-dwarf candidates are known from other young stellar associations and these objects show red colors compared to field T-dwarfs.[41] Young directly imaged exoplanets and planetary-mass companions sometimes show a T spectral type, such as 51 Eridani b (T4.5-T6).[4]

Clouds and variability

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Cloud models in early (SIMP J0136+09, 2MASS J2139+02) and a late-type T-dwarf (2MASS J0050–3322)

Two of the most variable brown dwarfs are the T-dwarfs Luhman 16B, showing a variation up to 20%[42] and 2MASS J2139+02, which varies with an amplitude as high as 26%.[43] 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.[44] These early T-dwarfs are thought to have an iron cloud deck and a patchy silicate 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.[45] 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.[24] Late T-dwarfs should also have cloud layers made of chromium, potassium chloride and different sulfides. These cloud layers are thin and exist above the silicate clouds.[45] One late T-dwarf that is variable is WISE 0458+6434 (T8.5), which varied with 13% in one epoch.[46]

Binaries

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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 astronomical units (AU).[47] One well-known T dwarf binary is Epsilon Indi B.[48] This binary consists of a T1 and a T6 dwarf that orbit each other with a separation of 2.65 AU.[49]

See also

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References

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