MONITORING STELLAR ORBITS AROUND THE MASSIVE BLACK HOLE IN THE GALACTIC CENTER

被引:1268
作者
Gillessen, S. [1 ]
Eisenhauer, F. [1 ]
Trippe, S. [1 ]
Alexander, T. [3 ]
Genzel, R. [1 ,2 ]
Martins, F. [4 ]
Ott, T. [1 ]
机构
[1] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany
[2] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[3] Weizmann Inst Sci, Fac Phys, IL-76100 Rehovot, Israel
[4] Univ Montpellier 2, CNRS, GRAAL, F-34095 Montpellier, France
关键词
black hole physics; astrometry; Galaxy: center; infrared: stars; SAGITTARIUS-A-ASTERISK; GLOBULAR-CLUSTER; ADAPTIVE OPTICS; INFRARED FLARES; PROPER MOTIONS; CENTRAL PARSEC; STAR; KINEMATICS; RESOLUTION; DYNAMICS;
D O I
10.1088/0004-637X/692/2/1075
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present the results of 16 years of monitoring stellar orbits around the massive black hole in the center of the Milky Way, using high-resolution near-infrared techniques. This work refines our previous analysis mainly by greatly improving the definition of the coordinate system, which reaches a long-term astrometric accuracy of approximate to 300 mu as, and by investigating in detail the individual systematic error contributions. The combination of a long-time baseline and the excellent astrometric accuracy of adaptive optics data allows us to determine orbits of 28 stars, including the star S2, which has completed a full revolution since our monitoring began. Our main results are: all stellar orbits are fit extremely well by a single-point-mass potential to within the astrometric uncertainties, which are now approximate to 6x better than in previous studies. The central object mass is (4.31 +/- 0.06 vertical bar(stat) +/- 0.36 vertical bar(R0)) x 10(6)M(circle dot), where the fractional statistical error of 1.5% is nearly independent from R-0, and the main uncertainty is due to the uncertainty in R-0. Our current best estimate for the distance to the Galactic center is R-0 = 8.33 +/- 0.35 kpc. The dominant errors in this value are systematic. The mass scales with distance as (3.95 +/- 0.06) x 10(6)(R-0/8 kpc)M-2.19(circle dot). The orientations of orbital angular momenta for stars in the central arcsecond are random. We identify six of the stars with orbital solutions as late-type stars, and six early-type stars as members of the clockwise-rotating disk system, as was previously proposed. We constrain the extended dark mass enclosed between the pericenter and apocenter of S2 at less than 0.066, at the 99% confidence level, of the mass of Sgr A*. This is two orders of magnitudes larger than what one would expect from other theoretical and observational estimates.
引用
收藏
页码:1075 / 1109
页数:35
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