OTS 44 is a free-floating planetary-mass object or brown dwarf located at 530 ly in the constellation Chamaeleon near the reflection nebula IC 2631. It is among the lowest-mass free-floating substellar objects, with approximately 11.5 times the mass of Jupiter, or approximately 1.1% that of the Sun. Its radius is estimated to be 3.2 or 3.6 times that of Jupiter. OTS 44 was discovered in 1998 by Oasa, Tamura, and Sugitani as a member of the star-forming region Chamaeleon I. Based upon infrared observations with the Spitzer Space Telescope and the Herschel Space Observatory, 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 (gas+dust) has a SED-fitted mass of at about 30 Earth masses. Observations with the SINFONI spectrograph at the Very Large Telescope show that the disk is accreting matter at the rate of approximately 10−11 of the mass of the Sun per year. It could eventually develop into a planetary system. Observations with ALMA detected the disk in millimeter wavelengths. The observations constrained the dust mass of the disk between 0.07 and 0.63, but these mass estimates are limited by assumptions on poorly constrained parameters. Another work estimates the dust mass to 0.064 (5.2 ) for dust particles of 1 mm in size and 0.295 (24 ) for dust particles of 1 μm in size.