Diffracto-astrometry measurements: Accuracy of the measuring algorithm
Por:
Ruelas-Mayorga A., Sánchez L.J., Olivares J., Allen C., Poveda A., Costero R., Nigoche-Netro A.
Publicada:
1 ene 2014
Resumen:
We present a theoretical analysis of the Diffracto-Astrometry measuring algorithm. We generated Tiny-Tim Theoretical Point Spread Functions (PSFs) for the CCDs in the HST Wide Field Planetary Camera 2 (WFPC2). These images were then measured using only their diffraction pattern, and positions for the simulated PSFs were obtained. The measuring algorithm recovers the original positions reasonably well (±0.1 to ±0.4 pixels). However, slight deviations from the original values are observed. We adjust the differences between the real and the measured position with a quadratic function of the coordinates. Application of these transformations allows determination of the position of a stellar image within a few hundredths of a pixel.
Filiaciones:
Ruelas-Mayorga A.:
Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70-264, México, DF, 04510, Mexico
Sánchez L.J.:
Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70-264, México, DF, 04510, Mexico
Olivares J.:
Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70-264, México, DF, 04510, Mexico
Allen C.:
Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70-264, México, DF, 04510, Mexico
Poveda A.:
Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70-264, México, DF, 04510, Mexico
Costero R.:
Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70-264, México, DF, 04510, Mexico
Nigoche-Netro A.:
Instituto de Astronomía y Meteorología, Universidad de Guadalajara, Guadalajara, Jalisco, 44130, Mexico
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