Is HR 5171 a Spectroscopic Binary or a Symbiotic?
I found arXiv:1401.2628 which says

Modeling the light curve with the NIGHTFALL program provides clear evidence that the system is a contact or possibly over-contact eclipsing binary. A total current system mass of $39^{+40}_{-22}$ solar mass and a high mass ratio $ q&gt;10$ is inferred for the system. The low-mass companion of ${\rm HR5171 A}$ is very close to the primary star that is embedded within its dense wind. Tight constraints on the inclination and vsini of the primary are lacking, which prevents us from determining its influence precisely on the mass-loss phenomenon, but the system is probably experiencing a wind Roche-Lobe overflow.

Does the need for simulation indicate that it is a spectroscopic binary?