The nature of the Cygnus extreme B supergiant 2MASS J20395358+4222505
Lennon, D. J.; Herrero, A.; Comerón, F.; Simón-Díaz, S.; Puls, J.; Urbaneja, M. A.; Najarro, F.; Garcia, M.; Ramírez Alegría, S.; Gallego, J.; Cardiel, N.; Gil de Paz, A.; Gómez-Alvarez, P.; Berlanas, S. R.; Carrasco, E.; Iglesias, J.; Cedazo, R.; García Vargas, M. L.; Castillo-Morales, Á.; Pascual, S.; Pérez-Calpena, A.; Martínez-Delgado, I.
Spain, Germany, Chile, Austria, Mexico
Abstract
2MASS J20395358+4222505 is an obscured early B supergiant near the massive OB star association Cygnus OB2. Despite its bright infrared magnitude (Ks = 5.82) it has remained largely ignored because of its dim optical magnitude (B = 16.63, V = 13.68). In a previous paper, we classified it as a highly reddened, potentially extremely luminous, early B-type supergiant. We obtained its spectrum in the U, B and R spectral bands during commissioning observations with the instrument MEGARA at the Gran Telescopio CANARIAS. It displays a particularly strong Hα emission for its spectral type, B1 Ia. The star seems to be in an intermediate phase between supergiant and hypergiant, a group that it will probably join in the near (astronomical) future. We observe a radial velocity difference between individual observations and determine the stellar parameters, obtaining Teff = 24 000 K and log gc = 2.88 ± 0.15. The rotational velocity found is large for a B supergiant, $v$ sin i = 110 ± 25 $\rm km\, s^{-1}$. The abundance pattern is consistent with solar, with a mild C underabundance (based on a single line). Assuming that J20395358+4222505 is at the distance of Cyg OB2, we derive the radius from infrared photometry, finding R = 41.2 ± 4.0 R⊙, log(L/L⊙) = 5.71 ± 0.04 and a spectroscopic mass of 46.5 ± 15.0 M⊙. The clumped mass-loss rate (clumping factor 10) is very high for the spectral type, $\dot{M}$ = 2.4 × 10-6 M⊙ a-1. The high rotational velocity and mass-loss rate place the star at the hot side of the bi-stability jump. Together with the nearly solar CNO abundance pattern, they may also point to evolution in a binary system, J20395358+4222505 being the initial secondary.