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Castillo-Morales, Á.
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article
The nature of the Cygnus extreme B supergiant 2MASS J20395358+4222505
Abstract
2MASS J20395358+4222505 is an obscured early B supergiant near the massive OB star association Cygnus OB2. Despite its bright infrared magnitude (K<SUB>s</SUB> = 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 H<SUB>α</SUB> 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 T<SUB>eff</SUB> = 24 000 K and log g<SUB>c</SUB> = 2.88 ± 0.15. The rotational velocity found is large for a B supergiant, $v$ sin i = 110 ± 25 $ 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<SUB>⊙</SUB>, log(L/L<SUB>⊙</SUB>) = 5.71 ± 0.04 and a spectroscopic mass of 46.5 ± 15.0 M<SUB>⊙</SUB>. The clumped mass-loss rate (clumping factor 10) is very high for the spectral type, ${M}$ = 2.4 × 10<SUP>-6</SUP> M<SUB>⊙</SUB> a<SUP>-1</SUP>. 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....