Abstract
High resolution observations (NTT, VLT and KECK) showed that the super-massive black hole (SBH) at the Galactic Centre is located at the centre of a compact stellar cluster [2,5]. However, the observed stellar sources may represent only a fraction of the total mass implying high M/L(2μm). Stars like S2, with orbital periods as short as 15 yrs [4,7] play a key role in determining the potential in the vicinity of the SBH. We show that it is possible, by fitting the available data on S2, to estimate an upper limit on the amount of the extended dark mass and thus on the M/L(2μm) that could be present at the very centre of the Galaxy.
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Mouawad, N., Pfalzner, S., Schödel, R., Spurzem, R., Moultaka, J., Eckart, A. Non-Keplerian Potential at the Galactic Centre?. In: Merloni, A., Nayakshin, S., Sunyaev, R.A. (eds) Growing Black Holes: Accretion in a Cosmological Context. ESO Astrophysics Symposia. Springer, Berlin, Heidelberg. https://doi.org/10.1007/11403913_42
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DOI: https://doi.org/10.1007/11403913_42
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Publisher Name: Springer, Berlin, Heidelberg
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