Superelative Brown Dwarfs
- WD 0137-349 B: first confirmed brown dwarf to have survived the primary's red giant phase.
- In 1984 it was postulated by some astronomers that the Sun may be orbited by an undetected brown dwarf (sometimes referred to as Nemesis) which could interact with the Oort cloud just as passing stars can. But this dated theory has fallen out of favor.
| Brown Dwarfs | |||||
|---|---|---|---|---|---|
| Title | Brown Dwarf Name | Spectral Type | RA/Dec | Constellation | Notes |
| First discovered | Teide 1 (Pleiades Open Star Cluster) | M8 | 3h47m18.0s +24°22'31" | Taurus | Imaged in 1989 and 1994 |
| First imaged with coronography | Gliese 229 B | T6.5 | 06h10m34.62s −21°51'52.1" | Lepus | Discovered 1994 |
| First with planemo | 2MASSW J1207334-393254 | M8 | 12h07m33.47s −39°32'54.0" | Centaurus | |
| First with a planetary mass in orbit about it | 2M1207 | ||||
| First with a dust disk | |||||
| First with bipolar outflow | |||||
| First field type (solitary) | Teide 1 | M8 | 3h47m18.0s +24°22'31" | Taurus | 1995 |
| First as a companion to a normal star | Gliese 229 B | T6.5 | 06h10m34.62s −21°51'52.1" | Lepus | 1995 |
| First spectroscopic binary brown dwarf | PPL 15 A, B | M6.5 | Taurus | Basri and Martin 1999 | |
| First binary brown dwarf of T Type | Epsilon Indi Ba, Bb | T1 + T6 | Indus | Distance: 3.626pc | |
| First trinary brown dwarf | DENIS-P J020529.0-115925 A/B/C | L5, L8 and T0 | 02h05m29.40s −11°59'29.7" | Cetus | Delfosse et al. 1997, mentions |
| First halo brown dwarf | 2MASS J05325346+8246465 | sdL7 | 05h32m53.46s +82°46'46.5" | Gemini | Adam J. Burgasser, et al. 2003 |
| First Late-M spectra | Teide 1 | M8 | 3h47m18.0s +24°22'31" | Taurus | 1995 |
| First L spectra | |||||
| First T spectra | Gliese 229 B | T6.5 | 06h10m34.62s −21°51'52.1" | Lepus | 1995 |
| Latest T spectrum | ULAS J0034-00 | T9 | Cetus | 2007 | |
| First Y spectrum | CFBDS0059 – pending. This is also classified as a T9 dwarf, due to its close resemblance to other T dwarfs | ~Y0 | 2008 | ||
| First X-ray-emitting | Cha Halpha 1 | M8 | Chamaeleon | 1998 | |
| First X-ray flare | LP 944-20 | M9V | 03h39m35.22s −35°25'44.1" | Fornax | 1999 |
| First radio emission (in flare and quiescence) | LP 944-20 | M9V | 03h39m35.22s −35°25'44.1" | Fornax | 2000 |
| Brown Dwarfs | |||||
|---|---|---|---|---|---|
| Title | Brown Dwarf Name | Spectral Type | RA/Dec | Constellation | Notes |
| Oldest | |||||
| Youngest | |||||
| Heaviest | |||||
| Metal-rich | |||||
| Metal-poor | 2MASS J05325346+8246465 | sdL7 | 05h32m53.46s +82°46'46.5" | Gemini | distance is ~10–30pc, metallicity is 0.1–0.01ZSol |
| Lightest | |||||
| Largest | |||||
| Smallest | |||||
| Furthest | WISP 0307-7243 | T4.5 | 03h07m45.12s −72°43'57.5" | Distance: 400pc | |
| Nearest | WISE 1541-2250 | Y | Distance: 9 ly | ||
| Nearest binary | Epsilon Indi Ba, Bb | T1 + T6 | Indus | Distance: 12 ly | |
| Brightest | |||||
| Dimmest | 2MASS J09393548-2448279 | ||||
| Hottest | |||||
| Coolest | WISE 1828+2650 | Y | Temperature 300 K | ||
| Most dense | COROT-3b | Transiting brown dwarf COROT-3b has 22 MJ with a diameter 1.01±0.07 times that of Jupiter. This makes it twice as dense as the metal platinum. | |||
| Least dense | |||||
- This list is incomplete; you can help by expanding it.
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