Abstract: pPXF extracts the stellar kinematics or stellar population from absorption-line spectra of galaxies using the Penalized Pixel-Fitting method (pPXF) developed by Cappellari & Emsellem (2004, PASP, 116, 138). Additional features implemented in the pPXF routine include:
<ul><li>Optimal template: Fitted together with the kinematics to minimize template-mismatch errors. Also useful to extract gas kinematics or derive emission-corrected line-strengths indexes. One can use synthetic templates to study the stellar population of galaxies via "Full Spectral Fitting" instead of using traditional line-strengths.</li><li>Regularization of templates weights: To reduce the noise in the recovery of the stellar population parameters and attach a physical meaning to the output weights assigned to the templates in term of the star formation history (SFH) or metallicity distribution of an individual galaxy.</li><li>Iterative sigma clipping: To clean the spectra from residual bad pixels or cosmic rays.</li><li>Additive/multiplicative polynomials: To correct low frequency continuum variations. Also useful for calibration purposes.</li></ul>
The code is available in IDL and in Python versions.
Credit: Cappellari, Michele
Preferred citation method: https://ui.adsabs.harvard.edu/abs/2017MNRAS.466..798C; also cite https://ui.adsabs.harvard.edu/abs/2010MNRAS.404.1639V if using MILES, or https://ui.adsabs.harvard.edu/abs/2006MNRAS.366.1151S if using GANDALF with pPXF