Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 489, Issue 3, Pages 3665-3669Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz2420
Keywords
galaxies: individual: NGC 1052; galaxies: kinematics and dynamics; dark matter
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Funding
- NSF [AST-1616598]
- National Science Foundation [AST-1616710]
- Research Corporation for Science Advancement Cottrell Scholar
- W. M. Keck Foundation
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The NGC 1052 group, and in particular the discovery of two ultra-diffuse galaxies with very low internal velocity dispersions, has been the subject of much attention recently. Here we present radial velocities for a sample of 77 globular clusters associated with NGC 1052 obtained on the Keck telescope. Their mean velocity and velocity dispersion are consistent with that of the host galaxy. Using a simple tracer mass estimator, we infer the enclosed dynamical mass and dark matter fraction of NGC 1052. Extrapolating our measurements with a Navarro-Frenk-White (NFW) mass profile we infer a total halo mass of 6.2(+/- 0.2) x 10(12) M-circle dot. This mass is fully consistent with that expected from the stellar mass-halo mass relation, suggesting that NGC 1052 has a normal dark matter halo mass (i.e. it is not deficient in dark matter in contrast to two ultra-diffuse galaxies in the group). We present a phase-space diagram showing the galaxies that lie within the projected virial radius (390 kpc) of NGC 1052. Finally, we briefly discuss the two dark matter-deficient galaxies (NGC 1052-DF2 and NGC 1052-DF4) and consider whether modified Newtonian dynamics (MOND) can account for their low observed internal velocity dispersions.
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