Mass models of NGC 6624 without an intermediate-mass black hole

Abstract

An intermediate-mass black hole (IMBH) was recently reported to reside in the centre of the Galactic globular cluster (GC) NGC 6624, based on timing observations of a millisecond pulsar (MSP) located near the cluster centre in projection. We present dynamical models with multiple mass components of NGC 6624 - without an IMBH - which successfully describe the surface brightness profile and proper motion kinematics from the Hubble Space Telescope (HST) and the stellar mass function at different distances from the cluster centre. The maximum line-of-sight acceleration at the position of the MSP accommodates the inferred acceleration of the MSP, as derived from its first period derivative. With discrete realizations of the models we show that the higher-order period derivatives - which were previously used to derive the IMBH mass - are due to passing stars and stellar remnants, as previously shown analytically in literature. We conclude that there is no need for an IMBH to explain the timing observations of this MSP.

8 pages, 7 figures, MNRAS. Updated to match final journal style

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Cited by in corpus (5)

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• Spherical models of star clusters with potential escapers
• Spectral properties and detectability of supermassive stars in protoglobular clusters at high redshift
• A consistency-test for determining whether ultra-compact dwarf galaxies could be the remnant nuclei of threshed galaxies
• Mergers of globular clusters in the Galactic disc: intermediate mass black hole coalescence and implications for gravitational waves detection