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%astro-ph/0608215
\documentclass{emulateapj}
\begin{document}
\title{GCIRS16SW: a massive eclipsing binary in the Galactic Center
\footnote{Based on observations collected at the ESO Very Large
Telescope (programs 075.B-0547 and 076
.B-0259)}}
\author{F. Martins \altaffilmark{1}, S. Trippe \altaffilmark{1}, T.
Paumard \altaffilmark{1}, T. Ott \altaffilmark{1}, R. Genzel
\altaffilmark{1,2}, G. Rauw \altaffilmark
{3}, F. Eisenhauer \altaffilmark{1}, S. Gillessen \altaffilmark{1}, H.
Maness \altaffilmark{4}, R. Abuter \altaffilmark{5}}
\altaffiltext{1}{MPE, Postfach 1312, D-85741, Garching, Germany}
\altaffiltext{2}{Department of Physics, University of California, CA
94720, Berkeley, USA}
\altaffiltext{3}{Institut d'Astrophysique et de G\'eophysique,
Universit\'e de Li\`ege, All\'ee du 6 Ao\^ut 17, B\^at. B5c, 4000
Li\`ege, Belgium}
\altaffiltext{2}{Department of Astronomy, University of California, CA
94720, Berkeley, USA}
\altaffiltext{5}{ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany}
\begin{abstract}
We report on the spectroscopic monitoring of GCIRS16SW, an Ofpe/WN9
star and LBV candidate in the central parsec of the Galaxy. SINFONI
observations show strong daily spectroscopic changes in the K
band. Radial velocities are derived from the He~{\sc i} $2.112 \mu m$
line complex and vary regularly with a period of 19.45 days,
indicating that the star is most likely an eclipsing binary. Under
various assumptions, we are able to derive a mass of $\sim$ 50 \msun\
for each component.
\end{abstract}
\keywords{Stars: binaries:eclipsing --- Stars: early-type --- Galaxy:
center}
--------------090602000305010604090606
Content-Type: text/html; charset=us-ascii
Content-Transfer-Encoding: 7bit
\documentclass{emulateapj}
\begin{document}
\title{GCIRS16SW: a massive eclipsing binary in the Galactic Center
\footnote{Based on observations collected at the ESO Very Large
Telescope (programs 075.B-0547 and 076
.B-0259)}}
\author{F. Martins \altaffilmark{1}, S. Trippe \altaffilmark{1}, T.
Paumard \altaffilmark{1}, T. Ott \altaffilmark{1}, R. Genzel
\altaffilmark{1,2}, G. Rauw \altaffilmark
{3}, F. Eisenhauer \altaffilmark{1}, S. Gillessen \altaffilmark{1}, H.
Maness \altaffilmark{4}, R. Abuter \altaffilmark{5}}
\email{martins@mpe.mpg.de}
\altaffiltext{1}{MPE, Postfach 1312, D-85741, Garching, Germany}
\altaffiltext{2}{Department of Physics, University of California, CA
94720, Berkeley, USA}
\altaffiltext{3}{Institut d'Astrophysique et de G\'eophysique,
Universit\'e de Li\`ege, All\'ee du 6 Ao\^ut 17, B\^at. B5c, 4000
Li\`ege, Belgium}
\altaffiltext{2}{Department of Astronomy, University of California, CA
94720, Berkeley, USA}
\altaffiltext{5}{ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching,
Germany}
\begin{abstract}
We report on the spectroscopic monitoring of GCIRS16SW, an Ofpe/WN9
star and LBV candidate in the central parsec of the Galaxy. SINFONI
observations show strong daily spectroscopic changes in the K
band. Radial velocities are derived from the He~{\sc i} $2.112 \mu m$
line complex and vary regularly with a period of 19.45 days,
indicating that the star is most likely an eclipsing binary. Under
various assumptions, we are able to derive a mass of $\sim$ 50 \msun\
for each component.
\end{abstract}
\keywords{Stars: binaries:eclipsing --- Stars: early-type --- Galaxy:
center}
--------------090602000305010604090606--