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The Local Group Mass in the Light of Gaia

Published version
Peer-reviewed

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Authors

Evans, NW 
Davis, AC 
Hartl, OV 

Abstract

High accuracy proper motions (PMs) of M31 and other Local Group satellites have now been provided by the {\it Gaia} satellite. We revisit the Timing Argument to compute the total mass M of the Local Group from the orbit of the Milky Way and M31, allowing for the Cosmological Constant. We rectify for a systematic effect caused by the presence of the Large Magellanic Cloud (LMC). The interaction of the LMC with the Milky Way induces a motion towards the LMC. This contribution to the measured velocity of approach of the Milky Way and M31 must be removed. We allow for cosmic bias and scatter by extracting correction factors tailored to the accretion history of the Local Group. The distribution of correction factors is centered around 0.63 with a scatter ±0.2, indicating that the Timing Argument significantly overestimates the true mass. Adjusting for all these effects, the estimated mass of the Local Group is $ M = 3.4^{+1.4}{-1.1} \times 10^{12} M{\odot}$ (68 % CL) when using the M31 tangential velocity $ 82^{+38}{-35}$ km/s. Lower tangential velocity models with 59−38+42 km/s (derived from the same PM data with a flat prior on the tangential velocity) lead to an estimated mass of $ M = 3.1^{+1.3}{-1.0} \times 10^{12} M_{\odot}$ (68 % CL). By making an inventory of the total mass associated with the 4 most substantial LG members (the Milky Way, M31, M33 and the LMC), we estimate the known mass is in the range 3.7−0.5+0.5×1012M.

Description

Keywords

astro-ph.GA, astro-ph.GA, astro-ph.CO, astro-ph.HE, gr-qc

Journal Title

Astrophysical Journal Letters

Conference Name

Journal ISSN

2041-8205
2041-8213

Volume Title

928

Publisher

American Astronomical Society