%0 Journal Article
%T MASSIVE BINARIES IN THE VICINITY OF Sgr A*
%+ Max Planck Institute for Extraterrestrial Physics (MPE)
%+ Weizmann Institute of Science [Rehovot, Israël]
%+ Laboratoire Univers et Particules de Montpellier (LUPM)
%+ Department of Astronomy [Boston]
%A Pfuhl, O.
%A Alexander, T.
%A Gillessen, S.
%A Martins, F.
%A Genzel, R.
%A Eisenhauer, F.
%A Fritz, T.
%A Ott, T.
%< avec comité de lecture
%@ 0004-637X
%J The Astrophysical Journal
%I American Astronomical Society
%V 782
%N 2
%P 101
%8 2014
%D 2014
%Z 1307.7996
%R 10.1088/0004-637x/782/2/101
%K Galaxy: center
%K binaries: eclipsing
%K infrared: stars
%K stars: early-type
%K stars: massive
%K stars: Wolf–Raye
%Z Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]Journal articles
%X A long-term spectroscopic and photometric survey of the most luminous and massive stars in the vicinity of the supermassive black hole Sgr A* revealed two new binaries: a long-period Ofpe/WN9 binary, IRS 16NE, with a modest eccentricity of 0.3 and a period of 224 days, and an eclipsing Wolf-Rayet binary with a period of 2.3 days. Together with the already identified binary IRS 16SW, there are now three confirmed OB/WR binaries in the inner 0.2 pc of the Galactic center. Using radial velocity change upper limits, we were able to constrain the spectroscopic binary fraction in the Galactic center to F SB = 0.30 +0.34 −0.21 at a confidence level of 95%, a massive binary fraction close to that observed in dense clusters. The fraction of eclipsing binaries with photometric amplitudes Δm > 0.4 is F GC EB = 3% ± 2%, which is consistent with local OB star clusters (F EB = 1%). Overall, the Galactic center binary fraction seems to be similar to the binary fraction in comparable young clusters.
%G English
%2 https://hal.science/hal-01992904/document
%2 https://hal.science/hal-01992904/file/Pfuhl_2014_ApJ_782_101.pdf
%L hal-01992904
%U https://hal.science/hal-01992904
%~ IN2P3
%~ CNRS
%~ UNIV-MONTP2
%~ LUPM
%~ MIPS
%~ UNIV-MONTPELLIER
%~ LUPM_AS
%~ UM1-UM2