There is no sign of variability in its radial velocity, which would otherwise indicate the presence of an unseen companion.
The star also shows evidence of a long-term radial velocity trend, which may indicate the presence of an additional outer companion.
This is a single-lined spectroscopic binary, with the presence of a companion being revealed by Doppler shifts in the spectrum.
Circumstellar belt suggests the presence of a second planetary companion of the star.
Burgasser et al. (2003) have inferred the presence of a low-mass companion orbiting the brown dwarf 2M 1237+6526.
Timing analysis have revealed the possible presence of a third low-mass stellar companion in wide orbit.
The presence of a perturbing companion has not been confirmed or discarded so far.
This is a spectroscopic binary system, which means that the presence of an orbiting companion is indicated by shifts in the spectrum.
Based upon observed radial velocity changes in the star, in 2007 the presence of a planetary companion was announced.
Radial velocity measurements have likewise failed to reveal the presence of a companion orbiting this star.
