Boundary and Invariant Scans

Flux Constant Output Three-Row Scan

A flux-constant-output scan holds the source luminosity fixed and varies distance across three rows, checking that the observed flux follows f = L / (4 * pi * d^2) at each. The arithmetic is exact only for the stated luminosity, distances, and rows in the ideal point-source model. Real observations add calibration, finite cadence/bandpass, noise, stellar variability, line-identification uncertainty, detector response, and measurement uncertainty.

Three exact rows keep luminosity over distance square fixed. Exact arithmetic here means exact results for the stated model inputs; measured inputs still carry uncertainty and significant-figure limits.

highlighted = computed this step

Matched luminosity and distance keep flux fixed

The pinned luminosity and distance change together. The rendered distance square is recomputed, and the output flux stays fixed.

F=422=1F={4\over2^{2}}=1
Flux row oneThe rendered distance square recomputes the flux.source to observerluminosity=4 Wdistance=2 mdistanceSquared=4 m^2flux=1 W/m^2

Matched luminosity and distance keep flux fixed

The pinned luminosity and distance change together. The rendered distance square is recomputed, and the output flux stays fixed.

F=932=1F={9\over3^{2}}=1
Flux row twoThe rendered distance square recomputes the flux.source to observerluminosity=9 Wdistance=3 mdistanceSquared=9 m^2flux=1 W/m^2

Matched luminosity and distance keep flux fixed

The pinned luminosity and distance change together. The rendered distance square is recomputed, and the output flux stays fixed.

F=3662=1F={36\over6^{2}}=1
Flux row threeThe rendered distance square recomputes the flux.source to observerluminosity=36 Wdistance=6 mdistanceSquared=36 m^2flux=1 W/m^2