Mass-to-light ratios for globular clusters. 3: M107 (NGC 6171; GC1629-129)

Details Mass-to-light ratios for globular clusters. 3: M107 (NGC 6171; GC1629-129) Mass-to-light ratios for globular clusters. 3: M107 (NGC 6171; GC1629-129)

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aj....107.1397p&link_type=abstract

The Astronomical Journal, vol. 107, no. 4, p. 1397-1407

Astronomy and Astrophysics

Astronomy

12

Black Holes (Astronomy), Brown Dwarf Stars, Data Reduction, Galactic Clusters, Globular Clusters, Mass To Light Ratios, Metallicity, Neutron Stars, White Dwarf Stars, Dispersions, Luminosity, Radial Velocity, Reflecting Telescopes

Scientific paper

We have measured radial velocities accurate to about 1 km s-1 for 76 stars located within 7 arcmin of the center of the globular cluster M107 (NGC 6171; GC1629-129). Nine of these stars are probably nonmembers and are excluded from the subsequent analysis. We find no signature of rotation greater than our 2 km s-1 detection threshold. The velocity dispersion decreases with radius, but this change is only about 1.3 times its uncertainty. We have fitted single- and multicomponent King models to our velocity data and to existing surface-brightness profiles. The multicomponent models have a power law or the galactic disk mass function. The single-component models imply that M107 has a mass-to-light ratio, M/Lv, of 1.8 +/- 0.4, in solar units. The best-fitting multicomponent King models have an isotropic or anisotropic (ra = 10) velocity dispersion tensor and x = 0.67. These models yield a projected central mass-to-light ratio, (M/Lv)(0), of 2.0 +/- 0.4 and a global M/Lv of 1.8 +/- 0.4. The isotropic model with x = 1.35 is also an acceptable, though poorer, fit and yields (M/Lv) (0) of 1.6 +/- 0.3 and M/Lv of 2.7 +/- 0.5. We have rejected models with the galactic disk initial mass function because their dynamical and population M/L's disagree. This suggests that the galactic disk and M107 initial mass functions were different.

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