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 eisenhauer
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Lorant,

sorry for the trouble - I was just copying from Micro$oft Word (in which 
the paper is written) and thought I disregarded all formatting. I 
converted the abstract to LaTeX, and attach it to this e-mail.

Sorry again for the inconvenience.

Thomas

GCNEWS newsletter wrote:

>Hi Thomas
>
>Your absract contained a lot of unreadable characters. I think I got
>them all converted, but it would be a good idea if you could check
>the changes I made. Maybe next time you can send in the *.tex or plain
>ASCII version of the paper/abstract. Thanks for submitting anyway
>
>Lorant
>
>
>  
>

-- 
Dr. Thomas Ott,                   | email: ott@mpe.mpg.de
MPI f. extraterrestrische Physik, | phone: +49 (89) 30000-3276
Postfach 1312,                    | fax:   +49 (89) 30000-3390
D-85741 Garching, Germany         | web:   http://www.mpe.mpg.de/~ott/


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%astro-ph/0502129

\documentstyle{article}

\def\arcsec{\hbox{$^{\prime\prime}$}}

\begin{document}

\title{SINFONI in the Galactic Center: young stars and IR flares in the 
central light month}

\author{F.Eisenhauer, R.Genzel, T.Alexander, R.Abuter, T.Paumard, T.Ott, 
A.Gilbert, S.Gillessen, M.Horrobin, S.Trippe, H.Bonnet, C.Dumas, 
N.Hubin, A.Kaufer, M.Kissler-Patig, G.Monnet, S.Str\"obele, T.Szeifert, 
A.Eckart, R.Sch\"odel & S.Zucker}


\begin{abstract}
We report 75 milli-arcsec resolution, near-IR imaging spectroscopy 
within the central 30 light days of the Galactic Center, taken with the 
new adaptive optics assisted, integral field spectrometer SINFONI on the 
ESO-VLT. To a limiting magnitude of K~16, 9 of 10 stars in the central 
0.4\arcsec, and 13 of 17 stars out to 0.7\arcsec from the central black hole have 
spectral properties of B0-B9, main sequence stars. Based on the $2.1127\mu$m 
HeI line width all brighter early type stars have normal rotation 
velocities, similar to solar neighborhood stars.

We combine the new radial velocities with SHARP/NACO astrometry to 
derive improved 3d stellar orbits for six of these 'S'-stars in the 
central 0.5\arcsec. Their orientations in space appear random. Their orbital 
planes are not co-aligned with those of the two disks of massive young 
stars 1-10\arcsec from SgrA*. We can thus exclude the hypothesis that the 
S-stars as a group inhabit the inner regions of these disks. They also 
cannot have been located/formed in these disks and then migrated inwards 
within their planes. From the combination of their normal rotation and 
random orbital orientations we conclude that the S-stars were most 
likely brought into the central light month by strong individual 
scattering events.

The updated estimate of distance to the Galactic center from the S2 
orbit fit is R$_0=7.62\pm0.32$ kpc, resulting in a central mass value of 
$3.61\pm0.32\times10^6 M_\odot$.

We happened to catch two smaller flaring events from SgrA* during our 
spectral observations. The 1.7-2.45$\mu$m spectral energy distributions of 
these flares are fit by a featureless, 'red' power law of spectral index 
$\alpha^\prime=-4\pm1(S_\nu\approx\nu^{\alpha^\prime})$ . 
The observed spectral slope is in good agreement with 
synchrotron models in which the infrared emission comes from accelerated 
non-thermal, high energy electrons in a radiative inefficient accretion 
flow in the central R~10 Rs region.

\end{abstract}
Key words: black hole physics- Galaxy: center âGalaxy: structureâ
infrared stars, techniques: spectroscopic


\end{document}

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