Its rapid rotation may enable strong auroral radio emissions via charged particle interactions in its magnetic field, as observed in other known rapidly-rotating brown dwarfs.

[2] 2MASS J0348−6022 was first catalogued as a point source in June 2003 by the Two Micron All-Sky Survey (2MASS) organized by the University of Massachusetts Amherst and the Infrared Processing and Analysis Center under the California Institute of Technology.

A previous estimate by Burgasser and collaborators from the spectrophotometric relation of spectral type and near-infrared absolute magnitude resulted in a value of 9 ± 4 parsecs (29 ± 13 ly), based on 2MASS JHK-band photometry.

[3][7] 2MASS J0348−6022 is classified as a late T-type brown dwarf with the spectral class T7, distinguished by the presence of strong methane (CH4) and water (H2O) absorption bands in its near-infrared spectrum between wavelengths 1.2 and 2.35 μm.

[7] The near-infrared spectrum of a brown dwarf can be modelled by a photosphere primarily defined by two fixed intrinsic properties: effective temperature (Teff) and surface gravity (log g).

[2] In a 2021 study, Megan Tannock and collaborators compared the near-infrared spectrum of 2MASS J0348−6022 to various published photospheric models and derived multiple best-fit solutions for its effective temperature and surface gravity.

From their adopted effective temperature and surface gravity values from photospheric modelling, Tannock and collaborators derive a mass of 0.041+0.021−0.017 M☉ (~43 MJup), a Jupiter-like equatorial radius of 0.093+0.016−0.010 R☉ (69,700 km), and an age of 3.5+11.5−2.9 billion years.

[2] The high estimated age of 2MASS J0348−6022 is due to its late T-type spectral class, which is generally expected to describe the later evolutionary stages of brown dwarfs as they cool.

[2] 2MASS J0348−6022 is expected to exhibit significant linear polarization in its optical and infrared thermal emission due to its oblate, dusty atmosphere induced by its rapid rotation and lower surface gravity.

Taking into account of magnetic dynamos generated by the brown dwarf's metallic hydrogen interior, the rotational velocity threshold may be even lower and implies that 2MASS J0348−6022 may be closer to breakup than predicted.

This in turn enables strong aurorae in the form of circularly polarized radio wave emissions via charged particle interactions in its magnetic field, which are driven by the so-called electron cyclotron maser instability that has been observed in other known rapidly-rotating and radio-emitting brown dwarfs.