Radial Acceleration Relation in Rotationally Supported Galaxies.

@article{McGaugh2016RadialAR,
  title={Radial Acceleration Relation in Rotationally Supported Galaxies.},
  author={Stacy S. McGaugh and Federico Lelli and James M. Schombert},
  journal={Physical review letters},
  year={2016},
  volume={117 20},
  pages={
          201101
        }
}
We report a correlation between the radial acceleration traced by rotation curves and that predicted by the observed distribution of baryons. The same relation is followed by 2693 points in 153 galaxies with very different morphologies, masses, sizes, and gas fractions. The correlation persists even when dark matter dominates. Consequently, the dark matter contribution is fully specified by that of the baryons. The observed scatter is small and largely dominated by observational uncertainties… 

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References

SHOWING 1-10 OF 85 REFERENCES

A scaling relation for disc galaxies: Circular-velocity gradient versus central surface brightness

For disc galaxies, a close relation exists between the distribution of light and the shape of the rotation curve. We quantify this relation by measuring the inner circular-velocity gradient dRV(0)

Balance of dark and luminous mass in rotating galaxies.

A fine balance between dark and baryonic mass is observed in spiral galaxies, and this poses a fine-tuning problem for galaxy formation models, and may point to new physics for dark matter particles or even a modification of gravity.

The Baryonic Tully-Fisher Relation

The Tully-Fisher relation appears fundamentally to be a relation between rotation velocity and total baryonic mass of the form Md~V4c.

The Mass Discrepancy-Acceleration Relation: Disk Mass and the Dark Matter Distribution

The mass discrepancy in disk galaxies is shown to be well correlated with acceleration, increasing systematically with decreasing acceleration below a critical scale a0 ≈ 3700 km2 s-2 kpc-1 = 1.2 ×

The Core-Cusp Problem

This paper gives an overview of the attempts to determine the distribution of dark matter in low surface brightness disk and gas-rich dwarf galaxies, both through observations and computer

Mass discrepancies in galaxies: dark matter and alternatives

Neutral hydrogen line observations of the extended rotation curves of spiral galaxies imply that there exist significant discrepancies between the luminous and dynamical mass beyond the bright

THE RELATION BETWEEN STELLAR AND DYNAMICAL SURFACE DENSITIES IN THE CENTRAL REGIONS OF DISK GALAXIES

We use the Spitzer Photometry and Accurate Rotation Curves (SPARC) database to study the relation between the central surface density of stars Σ ⋆ ( 0 ) and dynamical mass Σ dyn ( 0 ) in 135 disk

Novel test of modified Newtonian dynamics with gas rich galaxies.

A test using gas rich galaxies for which both axes of the BTFR can be measured independently of the theories being tested and without the systematic uncertainty in stellar mass that affects the same test with star dominated spirals is reported.

Dark matter in spiral galaxies

  • T. S. van AlbadaR. Sancisi
  • Physics
    Philosophical Transactions of the Royal Society of London. Series A, Mathematical and Physical Sciences
  • 1986
Mass models of spiral galaxies based on the observed light distribution, assuming constant M /L for bulge and disc, are able to reproduce the observed rotation curves in the inner regions, but fail

The Ursa Major Cluster of Galaxies. V. H I Rotation Curve Shapes and the Tully-Fisher Relations

This paper investigates the statistical properties of the Tully-Fisher (TF) relations for a volume-limited complete sample of spiral galaxies in the nearby Ursa Major Cluster. The merits of B, R, I,
...