Echo mapping of active galactic nuclei broad-line regions: Fundamental algorithms

Details Echo mapping of active galactic nuclei broad-line regions: Fundamental algorithms Echo mapping of active galactic nuclei broad-line regions: Fundamental algorithms

Oct 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasp..106.1091v&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 106, no. 704, p. 1091-1103

Astronomy and Astrophysics

Astronomy

12

Active Galactic Nuclei, Algorithms, Astronomical Models, Continuous Spectra, Echoes, Emission Spectra, Line Spectra, Mapping, Data Sampling, Kernel Functions, Light Curve, Mathematical Models, Maximum Entropy Method

Scientific paper

We formulate and test a series of algorithms for echo mapping the emission-line regions near active galactic nuclei from measurements of correlated variability in their line and continuum light curves. The linear regularization method (LRM) employs a direct inversion of evenly spaced light-curve data, with a regularization parameter that can be used to control the trade-off between noise and resolution. Matrix formulas express the formal solution as well as its variance and covariance in terms of uncertainties in the measurements. Unlike the maximum-entropy method (MEM), LRM applies to kernels with both positive and negative values, but the results are somewhat limited by ringing effects. A positivity constraint proves effective in controlling the ringing. MEM combines regularization and positivity in a natural way, but similar results are also found using positivity constraints with nonentropic regularization functions. Direct inversions of unevenly sampled light curves require interpolating the noisy data. In this case better results are found by solving for both the continuum light curve and kernel function in a simultaneous fit to the data. Our conclusion is that while echo mapping currently gives ambiguous results, the algorithms are not the limiting factor. Progress depends on efforts to increase the accuracy and completeness of sampling of the observed light curves.

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