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Line-of-sight mass estimator and the masses of the Milky Way and Andromeda Galaxy
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abstract
The total mass of a galaxy group, such as the Milky Way (MW) and the Andromeda Galaxy (M 31), is typically determined from the kinematics of satellites within their virial zones. Bahcall and Tremaine (1981) proposed the $v^2r$ estimator as an alternative to the virial theorem. In this work, we extend their approach by incorporating the three-dimensional spatial distribution of satellites within the system to improve the reliability and accuracy of galaxy mass estimates. Applying this method to a comprehensive dataset of Local Group satellites based on recent, high-precision distance measurements, we estimate the total mass of the MW to be $(7.9 \pm 2.3) \times 10^{11}$ $M_\odot$ and that of M~31 to be $(15.5 \pm 3.4) \times 10^{11}$ $M_\odot$. The effectiveness of the method is constrained by the precision of distance measurements, making it particularly well suited for the Local Group, but challenging to apply to more distant systems.
Forward citations
Cited by 5 Pith papers
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An X-ray Absorption-Line Survey of the Circumgalactic Medium of M31 with XMM-Newton
The first multi-sightline X-ray absorption survey toward M31 reports a 2.2-2.3 sigma excess in O VII and O VIII equivalent widths inside 300-350 kpc, consistent with a hot circumgalactic medium.
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The frozen outskirts: a cold Hubble flow and the mass of the Local Group
The Local Group's outer Hubble flow has a velocity dispersion of only 15 km/s, implying a total mass of (2.47 +/- 0.15) e12 solar masses and a Milky Way to Andromeda mass ratio of 0.74 +/- 0.10.
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Tighter Dark Matter Constraints from the Projected Mass Method: A Neural Network Enhanced Method for Galaxy Groups and Clusters
A simulation-trained neural network removes most of the systematic overestimate of the Projected Mass Estimator, yielding Milky Way, M81, and NGC 5128 halo masses in line with the literature.
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Refining primordial black hole dark matter constraints with dust heating: the role of spin and halo profile dependence
Dust-heating constraints on PBH dark matter tighten to f_PBH ≈ 10^-4 when PBH spin is included, with the strongest limits for the Isothermal halo profile and weakest for Burkert.
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Line-of-Sight Velocity Projection Impact on the Local Group Mass
After calibration with TNG50 simulations, the authors report a Local Group mass of (2.99 +/- 0.60) x 10^12 solar masses.
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