Skip to main content
Sandbox Physics
Galaxy rotation curves and mass models

Galaxy rotation curves · L1

What a flat rotation curve measures

Sandbox Physics ·

A flat rotation curve tells us that substantial inward gravity is still needed far from a galaxy’s centre. Turning that force into a mass estimate also requires the shape of the matter and the viewing geometry.

The outer gas keeps its speed through a larger turn

Picture a path from the bright centre of a disk galaxy towards its faint outskirts. Astronomers measure shifts in gas spectral lines to estimate motion along our line of sight. With a model of the galaxy’s orientation, they infer how fast the gas travels around the centre. A rotation curve plots that circular speed against radius. Its horizontal axis is position, not time.

Many galaxies have an outer interval over which the speed changes little. This is the flat part of the curve. The outer gas still takes longer to finish a circuit: it has a larger circumference to travel at about the same speed. Equal orbital speed does not mean equal angular speed.

The Solar System encourages a different expectation. Planets farther from the Sun generally travel more slowly, because almost all the mass is concentrated in the Sun. A galaxy spreads its stars and gas across a large region. Its gravitational pull depends on that distribution, together with any additional extended mass.

Reading: Lelli, McGaugh & Schombert (2016), SPARC, AJ152,157

Speed gives the acceleration needed to bend the path

A particle moving around a circle continually changes the direction of its velocity. It needs an acceleration towards the centre even when its speed stays constant. Double the speed at the same radius and the required acceleration becomes four times larger. Keep the speed and double the radius, and it becomes half as large.

The flat part of a rotation curve follows the second comparison. Gravity remains important at large radius, and declines more slowly than the distant pull of a concentrated mass. That statement concerns the total acceleration required by the motion. We can make it before deciding which component supplies the acceleration.

gin(R)=vc2(R)Rg_{\rm in}(R)=\frac{v_c^2(R)}{R}
RR is the circular-orbit radius, vcv_c the circular speed and ging_{\rm in} the required total inward acceleration.

Reading: Independent saved-observation rotation-curve calculation

Light locates stars; stellar populations help weigh them

An infrared image maps stellar light. Converting light to stellar mass requires a mass-to-light ratio: the amount of mass associated with a unit of luminosity. Stars of different ages and types can give different ratios. A heavier stellar disk supplies more of the gravity needed by a given rotation curve.

Gas supplies gravity too, and its distribution is estimated from other observations. In a Newtonian mass model, an extended dark halo can supply the force left after the stellar and gas contributions. A halo describes a spatial mass distribution. Identifying its particles requires further evidence beyond the fitted mass distribution.

Own synthetic speeds with errors and a newly fitted NFW component decomposition
Own48-point synthetic observation. Independent Python fits the saved speeds, errors and component basis; points and curves are not a measured galaxy image. Equivalent component speeds encode forces whose signed squares add. Open the full figure

Reading: Lelli, McGaugh & Schombert (2016), SPARC, AJ152,157

Disk and halo can compensate for each other

A heavier stellar disk may be paired with a weaker halo. A lighter disk may need a stronger halo. Across a limited range of radii, different allocations can produce similar total speeds. This compensation is the disk–halo degeneracy. The total radial pull can be clearer than the division of that pull among components.

Geometry matters as well. A spherical shell has cancellations that a disk does not share. Material outside a chosen disk radius can still pull on an interior test particle. Using a spherical mass formula for a disk can therefore introduce a geometrical error into the inferred enclosed mass.

Distance and orientation move the inference coherently. At a larger distance, the same angle on the sky spans a larger physical radius. A more face-on disk needs a larger circular speed to give the same line-of-sight motion. Better geometry and independent stellar-mass estimates can narrow the room available for compensating mass models.

Reading: Independent saved-observation rotation-curve calculation · Lelli, McGaugh & Schombert (2016), SPARC, AJ152,157

A force map becomes stronger with other observations

A rotation curve gives a radial map of the required force. Stellar spectra, gas measurements and gravitational lensing can add information from different directions. The question then becomes concrete: which mass distributions explain these measurements together, and which require unusual stellar masses or viewing parameters? Comparing those conditions brings us closer to an answer than choosing a curve by appearance alone.

Reading: Smith et al., Dark Matter and MOND successes and degeneracies, arXiv:2610.33157v1

Exercises and explained answers

  1. Two gas parcels have the same circular speed. One has twice the orbital radius. What is the ratio of their required inward accelerations?

    Read the explanation

    The outer parcel needs half the inward acceleration. At fixed speed, circular acceleration decreases in inverse proportion to radius. A flat speed curve still requires a changing gravitational force.

  2. Can the same total curve be compatible with a heavier stellar disk and a weaker dark halo?

    Read the explanation

    Yes, over a finite radial interval, if their force contributions compensate and each agrees with its other observations. The quality of that compensation must be checked across the whole curve. This is what the disk–halo degeneracy asks us to calculate.

Try the prediction

Compare the stellar disk and conditional halo

  1. Identify the stellar, gas and halo contributions in the own synthetic default.
  2. Increase only the stellar mass-to-light ratio, then adjust the halo. Compare which radii can be brought back towards the saved samples.
  3. Read the matter colours as a conditional mass diagram and use the external curves to compare the resulting forces.

Sources and calculation scope

  1. Lelli, McGaugh & Schombert (2016), SPARC, AJ152,157

    Official fixed Table1 and Rotmod_LTG.zip; named NGC2403 member only. The master paper sections3.1–3.3/5.1–5.3 and original Table2 notes establish signed gas, unit stellar mass-to-light, finite thickness and error meaning. Fresh source acquisition is separate from cached replay. Original rows and measured-derived plots stay local.

  2. Smith et al., Dark Matter and MOND successes and degeneracies, arXiv:2610.33157v1

    Full fixed26-page preprint read; Figures1/5/6/10/14 and Table3 visually inspected. Watermark23October2026; abstract says MNRAS Accepted, while the PDF retains placeholder acceptance and2025 style year. Guide follows sections2–6, fixed/varying geometry, internal BIC references and stacked-lensing conditions. No147-object MCMC or privately supplied covariance is reproduced. Original PDF/figures are excluded.

  3. Independent saved-observation rotation-curve calculation

    Own MIT Python produces synthetic observations, actual six-start fits, profiles, commonD/i scenarios, positive-density/ring-potential/Jacobian references and SVGs. Optional exact named-source acquisition and73-row conversion/fits were actually run. Default is offline; ZIP contains no App Engine, original SPARC rows, paper or measured-derived graph.

FeedbackSomething broken, confusing, or missing on this page?Tell us
What kind of feedback?

Sent with this page’s address, its Lab ID, the site language and your device type. Please leave out personal details. Feedback is kept for up to 12 months.Privacy policy