RT Journal Article
T1 The nature of the Cygnus extreme B supergiant 2MASS J20395358+4222505
A1 Herrero, A.
A1 Gil De Paz, Armando
A1 Berlanas, S.R.
A1 Comerón, F.
A1 Puls, J.
A1 Ramírez Alegría, S.
A1 García, M.
A1 Lennon, D.J.
A1 Najarro, F.
A1 Simón Díaz, S.
A1 Urbaneja, M.A.
A1 Gallego Maestro, Jesús
A1 Carrasco, E.
A1 Iglesias, J.
A1 Cedazo, R.
A1 García Vargas, M. L.
A1 Castillo Morales, María África
A1 Pascual Ramírez, Sergio
A1 Cardiel López, Nicolás
A1 Pérez Calpena, A.
AB 2MASS J20395358+4222505 is an obscured early B supergiant near the massive OB star association Cygnus OB2. Despite its bright infrared magnitude (K-s = 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-alpha 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-eff = 24 000 K and log g(c) = 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-circle dot, log(L/L-circle dot) = 5.71 +/- 0.04 and a spectroscopic mass of 46.5 +/- 15.0 M-circle dot. The clumped mass-loss rate (clumping factor 10) is very high for the spectral type, (M) over dot = 2.4 x10(-6) M-circle dot 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.
PB Wiley
SN 0035-8711
YR 2022
FD 2022-02-22
LK https://hdl.handle.net/20.500.14352/72017
UL https://hdl.handle.net/20.500.14352/72017
LA eng
NO © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.SS-D and AH acknowledge support from the Spanish Government Ministerio de Ciencia e Innovación through grants PGC-2018-091 3741-B-C22 and CEX2019-000920-S and from the Canarian Agency for Research, Innovation and Information Society (ACIISI), of the Canary Islands Government, and the European Regional Development Fund (ERDF), under grant with reference ProID2020010016. MG and FN acknowledge financial support through Spanish grant PID2019-105552RB-C41 (MINECO/MCIU/AEI/FEDER) and from the Spanish State Research Agency (AEI) through the Unidad de Excelencia 'María de Maeztu'-Centro de Astrobiología (CSIC-INTA) project No. MDM-2017-0737. SRB acknowledges support by the Spanish Government under grants AYA2015-68012-C2-2-P and PGC2018-093741-B-C21/C22 (MICIU/AEI/FEDER, UE). SRA acknowledges funding support from the FONDECYT Iniciacion project 11171025 and the FONDECYT Regular project 1201490. JIP acknowledges finantial support from projects Estallidos6 AYA2016-79724-C4 (Spanish Ministerio de Economía y Competitividad), Estallidos7 PID2019-107408GB-C44 (Spanish Ministerio de Ciencia e Innovación), grant P18-FR-2664 (Junta de Andalucía), and grant SEV-2017-0709 'Centro de Excelencia Severo Ochoa Program' (Spanish Science Ministry). AGP, SP, AG-M, JG and NC acknowledge support from the Spanish MCI through project RTI2018-096188-B-I00.; This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.; This publication makes use of data products from the Two-Micron All-Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.; This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.
NO Ministerio de Ciencia e Innovación (MICINN)
NO Ministerio de Economía y Competitividad (MINECO)/FEDER
NO Ministerio de Ciencia e Innovación (MICINN)/FEDER
NO Unidad de Excelencia María de Maeztu
NO Centro de Excelencia Severo Ochoa
NO Gobierno de Canarias/FEDER
NO Junta de Andalucía
NO FONDECYT Iniciación Project Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)CONICYT FONDECYT
NO FONDECYT Regular project Comision Nacional de Investigación Cientifíca y Tecnológica (CONICYT)CONICYT FONDECYT
NO National Aeronautics and Space Administration  (NASA)
NO National Science Foundation (NSF)
DS Docta Complutense
RD 5 abr 2025