Using globular clusters to test gravity in the weak acceleration regime: NGC 7099

Scarpa, R.; Marconi, G.; Gilmozzi, R.; Carraro, G.
Bibliographical reference

Astronomy and Astrophysics, Volume 462, Issue 1, January IV 2007, pp.L9-L12

Advertised on:
1
2007
Number of authors
4
IAC number of authors
0
Citations
39
Refereed citations
34
Description
Aims:A test of Newton's law of gravity in the low acceleration regime using globular clusters is presented and new results for the core collapsed globular cluster NGC 7099 given. Methods: The run of the gravitational potential as a function of distance is probed by studying the velocity dispersion profile of the cluster, as derived from a set of 125 radial velocities with accuracy better than 1 km s-1. The velocity dispersion profile is traced up to ~18 pc from the cluster center. Results: The dispersion is found to be maximal at the center, then decrease until 10 ± 2 pc from the center, well inside the cluster tidal radius of 42 pc. After that the dispersion remains basically constant with an average value of 2.2 ± 0.3 km s-1. Assuming a total V mag of M(V)=-7.43 mag for NGC 7099, the acceleration at 10± 2 pc from the center is 1.1+0.4-0.3τ × 10-8 cm s-2, where τ is the mass-to-light ratio. Thus, for τ ⪉ 2 typical of globular clusters, the flattening of the velocity dispersion profile occurs for a value of the internal acceleration of gravity that is fully consistent with a_0=1.2× 10-8 cm s-2 observed in galaxies. Conclusions: .This new result for NGC 7099 brings to 4 the clusters with velocity dispersion profile probing acceleration below a_0. All four have been found to have a flat dispersion profile at large radii where the acceleration is below a_0, thereby mimicking elliptical galaxies qualitatively and quantitatively. Whether this indicates a failure of Newtonian dynamics in the low acceleration limit or some more conventional dynamical effect (e.g., tidal heating) is still unclear. However, the similarities emerging between very different globular clusters, as well as between globular clusters and elliptical galaxies, seem to favor the first of these two possibilities. Based on observations collected at the European Southern Observatory, Chile (ESO Nos. 71.D-0311 and 075.D-0043). The radial velocities used in this work are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/462/L9