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<ref name=apj620_1_L51>{{citation | display-authors=1 | last1=Luhman | first1=K. L. | last2=D'Alessio | first2=Paola | last3=Calvet | first3=Nuria | last4=Allen | first4=Lori E. | last5=Hartmann | first5=Lee | last6=Megeath | first6=S. T. | last7=Myers | first7=P. C. | last8=Fazio | first8=G. G. | title=Spitzer Identification of the Least Massive Known Brown Dwarf with a Circumstellar Disk | journal=The Astrophysical Journal | volume=620 | issue=1 | pages=L51-L54 | |
<ref name=apj620_1_L51>{{citation | display-authors=1 | last1=Luhman | first1=K. L. | last2=D'Alessio | first2=Paola | last3=Calvet | first3=Nuria | last4=Allen | first4=Lori E. | last5=Hartmann | first5=Lee | last6=Megeath | first6=S. T. | last7=Myers | first7=P. C. | last8=Fazio | first8=G. G. | title=Spitzer Identification of the Least Massive Known Brown Dwarf with a Circumstellar Disk | journal=The Astrophysical Journal | volume=620 | issue=1 | pages=L51-L54 |date=February 2005 | doi=10.1086/428613 | bibcode=2005ApJ...620L..51L |arxiv = astro-ph/0502100 }}</ref> |
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Chamaeleon |
| Right ascension | 11h10m 11.5s |
| Declination | –76° 32′ 13″ |
| Characteristics | |
| Spectral type | M9.5[1] |
| Astrometry | |
| Distance | 554 ly (170 pc) |
| Details | |
| Mass | 0.015[1] M☉ |
| Radius | 0.23[1] R☉ |
| Luminosity | 0.0013[1] L☉ |
| Temperature | 2,300 K |
OTS 44 is a brown dwarf located about 550 light-years (170 pc) away in constellation Chamaeleon. It is among the smallest known brown dwarfs, with about 15 times the mass of Jupiter, or about 1.5% that of the Sun. Its radius is about 23% of the Sun's.[1]
This brown dwarf is located in the star-forming region Chamaeleon I. Based upon infrared observations with the Spitzer Space Telescope, OTS 44 emits an excess of infrared radiation for an object of its type, suggesting it has a circumstellar disk of dust and particles of rock and ice. This disk has an inner radius roughly three times the radius of OTS 44 and is accreting matter at the rate of about 10−10 the mass of the Sun per year. It could eventually develop into a planetary system.[1]
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