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A Statistical Inference Method for Interpreting the CLASP Observations

  • Authors: J. Štěpán, J. Trujillo Bueno, L. Belluzzi, A. Asensio Ramos, R. Manso Sainz, T. del Pino Alemán, R. Casini, R. Kano, A. Winebarger, F. Auchère, R. Ishikawa, N. Narukage, K. Kobayashi, T. Bando, Y. Katsukawa, M. Kubo, S. Ishikawa, G. Giono, H. Hara, Y. Suematsu, T. Shimizu, T. Sakao, S. Tsuneta, K. Ichimoto, J. Cirtain, P. Champey, B. De Pontieu, and M. Carlsson

2018 The Astrophysical Journal 865 48.

  • Provider: AAS Journals

Caption: Figure 4.

Multiple random realizations of the line-center Q/I (left panels) and U/I (right panels) signals of the Lyα line sampled from the CTR model with parameters ﹩{{\boldsymbol{\theta }}}_{0}=\{{a}_{0},{\bar{B}}_{0}\}=\{5,50\,{\rm{G}}\}﹩. For an increasing number of data points, N (i.e., the number of pixels along the imaginary spectrograph slit extending from μ = 0.1 to 0.9), the fractional polarization signals are distributed around the average CLV curves (shown with the red lines) according to the PDF ﹩{P}_{0}^{{\mu }_{i}}({q}_{i},{u}_{i}| {{\boldsymbol{\theta }}}_{0})﹩, where i = 1, …, N. We have added Gaussian noise with a standard deviation σ = 0.05% to the data (the 1σ bars are only shown in the top panels).

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