• DOI:10.1086/427175
• Corpus ID: 8656531

Stellar Orbits around the Galactic Center Black Hole

@article{Ghez2005StellarOA,
  title={Stellar Orbits around the Galactic Center Black Hole},
  author={Andrea M. Ghez and Samir Salim and Seth D. Hornstein and Angelle Tanner and J. R. Lu and Mark R. Morris and Eric Edward Becklin and Gaspard Duch{\^e}ne},
  journal={The Astrophysical Journal},
  year={2005},
  volume={620},
  pages={744-757}
}

• A. Ghez, S. Salim, +5 authors G. Duchêne
• Published 5 June 2003
• Physics
• The Astrophysical Journal

Wepresentnew diffraction-limitedimagesoftheGalacticcenter, obtainedwith theW.M.KeckI10mtelescope. Within0B4oftheGalaxy’scentraldarkmass,17proper-motionstars,withKmagnitudesrangingfrom 14.0to16.8, areidentified,and10ofthesearenewdetections(sixwerealsoindependentlydiscoveredbyothers).Inthissample, three newly identified (S0-16, S0-19, and S0-20) and four previously known (S0-1, S0-2, S0-4, and S0-5) sources have measured proper motions that reveal orbital solutions. Orbits are derived simultaneously so that they jointly constrain the central dark object’s properties: its mass,its position, and, for the first time using orbits, its motion on the plane of the sky. This analysis pinpoints the Galaxy’s central dark mass to within 1.3 mas (10 AU) and limits its propermotionto1:5 � 0:5masyr � 1 (orequivalently60 � 20kms � 1 )withrespecttothecentralstellarcluster.This localizationofthecentraldarkmassisconsistentwithourderivationofthepositionoftheradiosourceSgrA*inthe infrared reference frame (� 10 mas) but with an uncertainty that is a factor of 8 times smaller, which greatly facilitates searches for near-infrared counterparts to the central black hole. Consequently, one previous claim for such a counterpart can now be ascribed to a close stellar passage in 1996. Furthermore, we can place a conservative upper limit of 15.5 mag on any steady state counterpart emission. The estimated central dark mass from orbital motions is 3:7(� 0:2) ;10 6 R0= 8k pc ðÞ ½� 3 M� ; this is a more direct measure of mass than those obtained from velocitydispersion measurements,which are asmuchasafactorof2 smaller.The Galactic center’sdistance,which adds an additional 19% uncertainty in the estimated mass, is now the limiting source of uncertainty in the absolute mass. For stars in this sample, the closest approach is achieved by S0-16, which came within a mere 45 AU (=0:0002 pc ¼ 600Rs) at a velocity of 12,000 km s � 1 . This increases the inferred dark mass density by 4 orders of magnitude compared to earlier analyses based on velocity and acceleration vectors, making the Milky Way the strongest existing case for a supermassive black hole at the center of a normal-type galaxy. Well-determined orbital parameters for these seven Sgr A* cluster stars also provide new constraints on how these apparently massive, young (<10 Myr) stars formed in a region that seems to be hostile to star formation. Unlike the more distant He i emission line stars—another population of young stars in the Galactic center—that appear to have coplanar orbits, the Sgr A* cluster stars have orbital properties (eccentricities, angular momentum vectors, and apoapse directions) that are consistent with an isotropic distribution. Therefore, many of the mechanisms proposed for the formation of the He i stars, such as formation from a preexisting disk, are unlikely solutions for the Sgr A* cluster stars. Unfortunately, alternative theories for producing young stars, or old stars that look young, in close proximity to a centralsupermassiveblackholeareallalsosomewhatproblematic.Understandingtheapparentyouthofstarsinthe Sgr A* cluster, as well as the more distant Hei emission line stars, has now become one of the major outstanding issues in the study of the Galactic center. Subject headingg black hole physics — Galaxy: center — Galaxy: kinematics and dynamics — infrared: stars — techniques: high angular resolution