Formation of Difluorobenzyl Radicals from 2,3,4-Trifluorotoluene in Corona Excitation

Yoon, Young Wook; Lee, Gi Woo; Lee, Sang Kuk

doi:10.5012/bkcs.2011.32.6.1993

Cited by 5 publications

(1 citation statement)

References 26 publications

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“…Another interesting fact about NGC 6388 is that it appears to contain multiple stellar populations (e.g. Yoon et al 2000;Piotto 2008). This fact makes the scenario of merging clusters plausible, leading to potentially complicated dynamics in the center.…”

Section: Introductionmentioning

confidence: 99%

Kinematic signature of an intermediate-mass black hole in the globular cluster NGC 6388

Lützgendorf

Kissler-Patig

Noyola

et al. 2011

A&A

101

144

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Context. Intermediate-mass black holes (IMBHs) are of interest in a wide range of astrophysical fields. In particular, the possibility of finding them at the centers of globular clusters has recently drawn attention. IMBHs became detectable since the quality of observational data sets, particularly those obtained with HST and with high resolution ground based spectrographs, advanced to the point where it is possible to measure velocity dispersions at a spatial resolution comparable to the size of the gravitational sphere of influence for plausible IMBH masses. Aims. We present results from ground based VLT/FLAMES spectroscopy in combination with HST data for the globular cluster NGC 6388. The aim of this work is to probe whether this massive cluster hosts an intermediate-mass black hole at its center and to compare the results with the expected value predicted by the M • − σ scaling relation. Methods. The spectroscopic data, containing integral field unit measurements, provide kinematic signatures in the center of the cluster while the photometric data give information of the stellar density. Together, these data sets are compared to dynamical models and present evidence of an additional compact dark mass at the center: a black hole. Results. Using analytical Jeans models in combination with various Monte Carlo simulations to estimate the errors, we derive (with 68% confidence limits) a best fit black-hole mass of (17 ± 9) × 10 3 M and a global mass-to-light ratio of M/L V = (1.6 ± 0.3) M /L .

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Section: Introductionmentioning

confidence: 99%