Bibcode
Asensio Ramos, A.; Collados, M.
Referencia bibliográfica
Applied Optics IP, vol. 47, Issue 14, pp.2541-2549
Fecha de publicación:
5
2008
Número de citas
6
Número de citas referidas
5
Descripción
The polarization analysis of light is typically carried out using
modulation schemes. The light of an unknown polarization state is passed
through a set of known modulation optics, and a detector is used to
measure the total intensity passing the system. The modulation optics is
modified several times, and, with the aid of several such measurements,
the unknown polarization state of the light can be inferred. How to find
the optimal demodulation process has been investigated in the past.
However, since the modulation matrix has to be measured for a given
instrument and the optical elements can present problems of
repeatability, some uncertainty is present in the elements of the
modulation matrix or covariances between these elements. We analyze in
detail this issue, presenting analytical formulas for calculating the
covariance matrix produced by the propagation of such uncertainties on
the demodulation matrix, on the inferred Stokes parameters, and on the
efficiency of the modulation process. We demonstrate that even if the
covariance matrix of the modulation matrix is diagonal, the covariance
matrix of the demodulation matrix is in general nondiagonal because
matrix inversion is a nonlinear operation. This propagates through the
demodulation process and induces correlations on the inferred Stokes
parameters.
Proyectos relacionados
Magnestismo Solar y Estelar
Los campos magnéticos son uno de los ingredientes fundamentales en la formación de estrellas y su evolución. En el nacimiento de una estrella, los campos magnéticos llegan a frenar su rotación durante el colapso de la nube molecular, y en el fin de la vida de una estrella, el magnetismo puede ser clave en la forma en la que se pierden las capas
Tobías
Felipe García
Magnetismo, Polarización y Transferencia Radiativa en Astrofísica
Los campos magnéticos están presentes en todos los plasmas astrofísicos y controlan la mayor parte de la variabilidad que se observa en el Universo a escalas temporales intermedias. Se encuentran en estrellas, a lo largo de todo el diagrama de Hertzsprung-Russell, en galaxias, e incluso quizás en el medio intergaláctico. La polarización de la luz
Tanausú del
Pino Alemán