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Go from raw multi-megabyte CSV files to interactive, hardware-accelerated scientific plots with zero code and instant delimiter detection.
Read ArticleScientific Insights & Methodologies
Peer-ready methodologies, spectroscopic & XRD application notes, and computational GPU rendering deep-dives.
Publication-Ready Research Plots
Meet Nature and IEEE journal standards with crisp vector PDF/SVG exports, LaTeX mathematical labels, error bars, and colorblind-safe palettes.
Read ArticleCurve Fitting Without Coding
Fit linear, exponential, and Gaussian peak models to your experimental data in 3 clicks with instant R² and uncertainty calculations.
Read ArticleSavitzky-Golay Parameter Selection
Learn how to select the optimal window size and polynomial order to smooth spectral noise without eroding peak heights or broadening FWHM.
Read ArticleScherrer Equation & XRD FWHM
Extract exact Full Width at Half Maximum (FWHM) from X-ray Diffraction peaks and calculate average crystallite domain size.
Read ArticleLaser & ASE Analysis
Characterize a laser diode's spectral output, separate laser emission from Amplified Spontaneous Emission (ASE), calculate SMSR, and analyze pulses.
Read Article100M Points at 60 FPS
Discover the GPU-accelerated rendering pipeline, level-of-detail downsampling, and zero-copy data flow that powers AltaiPlot.
Read ArticleFitting Gaussian Peaks
A deep dive into Gaussian profiles, non-linear least squares solver parameters, robust heuristics, and SciPy implementation.
Read ArticleXRD Peak Fitting
Learn Bragg's Law, instrumentation peak broadening, Pseudo-Voigt fits, and calculating crystallite size via the Scherrer formula.
Read ArticleBaseline Correction
Compare baseline subtraction methods, Whittaker smoothers, statistics-sensitive peak clipping, and Asymmetric Least Squares (AsLS).
Read ArticleSavitzky-Golay Filter
How local linear polynomial regression smoothing filters high-frequency noise while preserving peak amplitudes, positions, and widths.
Read ArticleRaman Spectrum Analysis
An analytical pipeline for Raman spectra: cosmic ray filtering, fluorescence subtraction, signal smoothing, and multi-peak fits.
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