The Tidal Tails of NGC 5466

Abstract

The study of substructure in the stellar halo of the Milky Way has made a lot of progress in recent years, especially with the advent of surveys like the Sloan Digital Sky Survey. Here, we study the newly discovered tidal tails of the Galactic globular cluster NGC 5466. By means of numerical simulations, we reproduce the shape, direction and surface density of the tidal tails, as well as the structural and kinematical properties of the present-day NGC 5466. Although its tails are very extended in SDSS data (> 45 degrees), NGC 5466 is only losing mass slowly at the present epoch and so can survive for probably a further Hubble time. The effects of tides at perigalacticon and disc crossing are the dominant causes of the slow dissolution of NGC 5466, accounting for about 60 % of the mass loss over the course of its evolution. The morphology of the tails provides a constraint on the proper motion -- the observationally determined proper motion has to be refined (within the stated error margins) to match the location of the tidal tails.

MNRAS, in press

References in corpus (3)

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• The Origin of the Bifurcation in the Sagittarius Stream
• Is Ursa Major II the Progenitor of the Orphan Stream?

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• STREGA: STRucture and Evolution of the GAlaxy. I. Survey Overview and First Results
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• Life and death of a hero - Lessons learned from modeling the dwarf spheroidal Hercules: an incorrect orbit?
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• Could Segue 1 be a destroyed star cluster? - a dynamical perspective
• Revisit NGC 5466 Tidal Stream with $Gaia$, SDSS/SEGUE and LAMOST
• A Search for Extra-Tidal RR Lyrae in the Globular Cluster NGC 5024 and NGC 5053
• A search for stellar structures around nine outer halo globular clusters in the Milky Way