研究目的
To develop a new pure-Python pipeline (ASTROPOP) for reducing photometric and polarimetric data, designed to work fully automated with the IAGPOL polarimeter of Pico dos Dias Observatory (OPD; Brazil) and other instruments, and to compare its results with those obtained from PCCDPACK.
研究成果
ASTROPOP can produce reliable polarimetric measurements comparable to those obtained by PCCDPACK and the literature. It is suitable for performing data reduction with science quality and precision, even for large amounts of data. The pipeline is being tested with the ROBO40 telescope and has the potential to be used in situ to automatically reduce the data produced each night.
研究不足
The code currently requires additional modification to handle single-beam polarimetry, where the analyzer is a polaroid sheet that filters the light and allows just one polarized beam to reach the detector. This mode is used for extended sources and is also available on IAGPOL. A proper handling for this polarimeters is planned for future versions.
1：Experimental Design and Method Selection:
The ASTROPOP pipeline was developed in Python 3, designed to perform standard reduction processes for polarimetry or photometry. It includes modules for image preprocessing, source detection and photometry, polarimetry reduction, and astrometric and photometric calibration.
2：Sample Selection and Data Sources:
Observations were conducted using the 0.6 m Boller & Chivens telescope at OPD, equipped with the IAGPOL polarimeter. Data sets included standard-polarized stars observed between 2016 and
3：6 m Boller & Chivens telescope at OPD, equipped with the IAGPOL polarimeter. Data sets included standard-polarized stars observed between 2016 and List of Experimental Equipment and Materials:
2017.
3. List of Experimental Equipment and Materials: The IAGPOL polarimeter consists of a retarder plate, a Sarvat prism, a filter wheel, and an Andor IkonL CCD detector. Synthetic data sets were also generated for testing.
4：Experimental Procedures and Operational Workflow:
The pipeline processes include cosmic ray extraction, bias and flat-field correction, image alignment, source detection, photometry, and polarimetry reduction. The polarimetry reduction involves measuring the flux of ordinary and extraordinary beams and computing the relative difference between these fluxes.
5：Data Analysis Methods:
The pipeline uses least-squares minimization and the Levenberg–Marquardt optimization for polarimetry reduction. Photometric calibration is performed using standard online photometric catalogs.
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