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The mass distribution in the Galactic Centre from interferometric astrometry of multiple stellar orbits

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arxiv 2112.07478 v1 pith:RJPKRLVI submitted 2021-12-14 astro-ph.GA astro-ph.IMgr-qc

GRAVITY Collaboration: R. Abuter , N. Aimar , A. Amorim , J. Ball , M. Bauböck , J.P. Berger , H. Bonnet , G. Bourdarot
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W. Brandner V. Cardoso Y. Clénet Y. Dallilar R. Davies P.T. de Zeeuw J. Dexter A. Drescher F. Eisenhauer N.M. Förster Schreiber A. Foschi P. Garcia F. Gao E. Gendron R. Genzel S. Gillessen M. Habibi X. Haubois G. Hei{ss}el T. Henning S. Hippler M. Horrobin L. Jochum L. Jocou A. Kaufer P. Kervella S. Lacour V. Lapeyrère J.-B. Le Bouquin P. Léna D. Lutz T. Ott T. Paumard K. Perraut G. Perrin O. Pfuhl S. Rabien J. Shangguan T. Shimizu S. Scheithauer J. Stadler A.W. Stephens O. Straub C. Straubmeier E. Sturm L.J. Tacconi K.R.W. Tristram F. Vincent S. von Fellenberg F. Widmann E. Wieprecht E. Wiezorrek J. Woillez S. Yazici A. Young G. Zins
This is my paper · ORCID
classification astro-ph.GAastro-ph.IMgr-qc
keywords massstarsaroundastrometrydataorbitsapocentreblack
verification ladder T0 review T1 audit T2 compute T3 formal
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The stars orbiting the compact radio source Sgr A* in the Galactic Centre are precision probes of the gravitational field around the closest massive black hole. In addition to adaptive optics assisted astrometry (with NACO / VLT) and spectroscopy (with SINFONI / VLT, NIRC2 / Keck and GNIRS / Gemini) over three decades, since 2016/2017 we have obtained 30-100 mu-as astrometry with the four-telescope interferometric beam combiner GRAVITY / VLTI reaching a sensitivity of mK = 20 when combining data from one night. We present the simultaneous detection of several stars within the diffraction limit of a single telescope, illustrating the power of interferometry. The new data for the stars S2, S29, S38 and S55 yield significant accelerations between March and July 2021, as these stars pass the pericenters of their orbits between 2018 and 2023. This allows for a high-precision determination of the gravitational potential around Sgr A*. Our data are in excellent agreement with general relativity orbits around a single central point mass, M = 4.30 x 10^6 M_sun with a precision of about +-0.25%. We improve the significance of our detection of the Schwarzschild precession in the S2 orbit to 7 sigma. Assuming plausible density profiles, an extended mass component inside S2's apocentre (= 0.23" or 2.4 x 10^4 R_S) must be 3000 M_sun (1 sigma), or 0.1% of M. Adding the enclosed mass determinations from 13 stars orbiting Sgr A* at larger radii, the innermost radius at which the excess mass beyond Sgr A* tentatively is seen is r = 2.5" >= 10x the apocentre of S2. This is in full harmony with the stellar mass distribution (including stellar-mass black holes) obtained from the spatially resolved luminosity function.

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Cited by 7 Pith papers

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