SR 12 (also known as V2247 Oph) is a weak-line T-Tauri binary that has a planetary-mass companion with a detected accretion disk.

[3] The binary does not have any detection of circumbinary dust from Spitzer and ALMA observations.

[2] SR 12c was first detected in 2002 using the Infrared Survey Facility (IRSF), which was constructed and operated by Nagoya University and NAOJ and is located at the South African Astronomical Observatory.

[2] The near-infrared spectrum suggested a spectral type of M9.0 ± 0.5 of the planetary-mass companion (PMC) and a mass of 14+7−8 MJ.

[12] An additional higher-resolution near-infrared spectrum was taken in 2014, which showed signs of very low surface gravity, which is an indicator of youth.

[15] A later work found that SR 12c is less massive with 11 ±3 MJ and SED-fitting yielded a spectral type of L0 ±1.

Observations with the VLT X-SHOOTER showed hydrogen emission lines, especially Hydrogen-alpha.