Home / Science / Physics / Optics and photonics / Sellmeier fitterTool #935

Sellmeier and Cauchy equation fitter: fit refractive index against wavelength, Abbe number and dispersion

Paste or open measured refractive index against wavelength and fit a Sellmeier (1 to 3 terms) or Cauchy equation: coefficients with standard errors, residuals, the index at any wavelength, Abbe number, group index and group-velocity dispersion, with every model compared.

Keep it one tap away for everyday use.

Bookmark Sellmeier fitter?

Press Ctrl + D now. Your browser opens its own bookmark box, where you choose the name and folder.

  1. Data
  2. Fit
  3. Coefficients
  4. Download
Nothing is uploadedWorks offline once open

Measured index

Sellmeier: n² = 1 + Σ Bᵢλ²/(λ² − Cᵢ), λ in µm, each term a resonance at √Cᵢ µm; it extrapolates well. Cauchy: n = A + B/λ² + C/λ⁴, a simpler fit for visible light. The first two numbers on each line are used. The example glass is made up.

Fit

All models compared

Least-squares fit to the refractive index (Levenberg-Marquardt, started from a separable linear solve). ± is one standard error from the fit, assuming independent errors of equal size. Outside the measured wavelengths every model is an extrapolation. For study and planning; for lens design use measured, certified glass data.

Download

What it does

The refractive index of glass, crystals and liquids changes with wavelength: that is dispersion, the reason a prism splits white light. To use a material in a design you need a smooth formula for n(λ) that passes through your measurements. This tool fits the two standard ones:

  • Sellmeier: n² = 1 + Σ Bᵢ λ² / (λ² − Cᵢ). Each term is a resonance (an absorption) at a wavelength √Cᵢ, usually two in the ultraviolet and one in the infrared. It is physically based and extrapolates well.
  • Cauchy: n = A + B/λ² + C/λ⁴. Simple and fine across visible light, but it goes wrong further out.

From the fitted curve it gives the index at any wavelength, the Abbe number, the group index, the group-velocity dispersion β₂ and the fibre-optics dispersion parameter D.

How to use it

  1. Paste two columns, wavelength and refractive index, from a spreadsheet or text file, or press Open a file (CSV, TSV, TXT or Excel). A header row is fine.
  2. Choose the wavelength unit, or let it guess (values above 50 are taken as nm).
  3. Pick a model. You need more data points than coefficients: 7 or more for a 3-term Sellmeier.
  4. Set the wavelength to evaluate at. The table at the bottom compares every model on your data.

What the results mean

  • Residuals (measured minus fitted) should look like random scatter around zero at about the size of your measurement error. A wave-like pattern means the model is too simple.
  • Standard errors come from the fit. With visible-only data, the infrared Sellmeier term’s B and C are strongly correlated and get large errors, even though the curve itself is well fixed.
  • Abbe number V_d = (n_d − 1)/(n_F − n_C): high (above about 50) for low-dispersion crown-like glasses, low for flint-like ones.
  • Group index n − λ dn/dλ sets the speed of a light pulse; β₂ tells you whether short pulses spread with red ahead (positive, normal dispersion) or blue ahead (negative, anomalous).

Worked example

The example is a made-up glass: 14 points from 380 to 1,600 nm, generated from invented Sellmeier coefficients with small made-up noise and rounded to five decimals. The 3-term Sellmeier fit leaves an RMS residual of 1.1 × 10⁻⁵ (largest 1.6 × 10⁻⁵), at the level of the added noise, with resonances at 0.0863, 0.188 and 15.2 µm. It gives n_d = 1.52968 and an Abbe number of 49.64. At 1,550 nm the index is 1.51038, the group index 1.53103 and β₂ = −15.80 fs²/mm (anomalous, D = 12.39 ps/(nm·km)). The comparison table shows the 2-term Sellmeier nine times worse (RMS 9.8 × 10⁻⁵) and the 3-term Cauchy about a hundred times worse (1.0 × 10⁻³): Cauchy cannot follow the index into the infrared.

FAQ

Which model should I use? The simplest one whose residuals look like noise. Sellmeier with 2 or 3 terms for data spanning visible to infrared; Cauchy for a narrow visible range.

Can I trust it outside my data? Sellmeier extrapolates sensibly a little way; Cauchy does not. The page marks extrapolated values.

Is this a glass catalogue? No: no catalogue data is included. Use your own measurements, or your supplier’s certified data for real designs. For study and planning.

Where the numbers come from

  • Sellmeier and Cauchy dispersion equations, Abbe number with the d, F and C Fraunhofer lines (587.5618, 486.1327 and 656.2725 nm, general spectroscopic constants), group index and group-velocity dispersion: standard textbook results, for example Born and Wolf, Principles of Optics, and Agrawal, Nonlinear Fiber Optics, chapter 1.
  • Fitting: separable (variable projection) linear least squares for the B coefficients, Nelder-Mead for the resonances, then Levenberg-Marquardt on the index residuals.
  • Checked against SciPy least_squares (Sellmeier) and NumPy lstsq (Cauchy) on the same data, and derivatives against SymPy. The example 'glass' is generated from made-up coefficients with made-up noise; no glass catalogue data is copied.

Standard scientific values, such as constants, atomic weights and melting points, are facts found in every textbook; we name where ours were checked. If you are an author or publisher and want a value, a credit or a table changed or removed, tell us and we will act quickly.

Last updated 2026-11-09.

Related tools

Thin-film coating simulator #931 Stack thin layers on glass and see how much light they reflect and transmit at every wavelength and angle, for s, p or unpolarised light, by the transfer-matrix method: anti-reflection coatings, Bragg mirrors, soap films and thin absorbing layers. Lens ray tracer #932 Type a lens system as a list of spherical surfaces and trace exact rays through it: focal length, f-number, image position, a spot diagram against the Airy disc, spherical aberration, ray fans, best focus, distortion and Petzval field curvature, drawn as a lens layout. Fibre optic calculator #934 From a fibre's core and cladding indices, core size and wavelength, get the numerical aperture, acceptance angle, V-number, single-mode cut-off, the guided LP modes, effective index and mode-field diameter, then pulse spreading, bandwidth and a full link power budget. Spectrometer calibration #937 Open a photo from a phone or webcam spectrometer, take a brightness profile across the spectrum, find the bright lines, match them to well-known mercury, neon, hydrogen or sodium lines, and fit a pixel-to-wavelength polynomial to get a calibrated spectrum. Publication plot maker #27 Paste columns or open a CSV or Excel file and get a clean scientific figure with error bars, sized for a journal column. Download vector SVG or PDF, or PNG at 300 or 600 dpi. Your data stays in your browser. Gaussian beam calculator #930 Put lenses and curved mirrors on an optical rail and follow a laser beam through them with the complex beam parameter q and ABCD matrices: the size and position of every new waist, Rayleigh range, divergence, beam radius and wavefront curvature anywhere, with M² for real lasers.