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    Summary of the Pi of the Sky photometry improving methods

    Access Status
    Fulltext not available
    Authors
    Opiela, R.
    Malek, K.
    Mankiewicz, L.
    Siudek, M.
    Sokolowski, Marcin
    Zarnecki, A.
    Date
    2014
    Type
    Conference Paper
    
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    Citation
    Opiela, R. and Malek, K. and Mankiewicz, L. and Siudek, M. and Sokolowski, M. and Zarnecki, A. 2014. Summary of the Pi of the Sky photometry improving methods.
    Source Title
    Proceedings of SPIE - The International Society for Optical Engineering
    DOI
    10.1117/12.2075211
    ISBN
    9781628413694
    School
    Curtin Institute of Radio Astronomy (Physics)
    URI
    http://hdl.handle.net/20.500.11937/53240
    Collection
    • Curtin Research Publications
    Abstract

    © 2014 SPIE.Pi of the Sky is a system of five wide field of view robotic telescopes, which search for short timescale astrophysical phenomena, especially for prompt optical GRB emissions. The system was designed for autonomous operation, monitoring a large fraction of the sky with 12m - 13m range and time resolution of the order of 1-10 seconds. Five fully automatic Pi of the Sky detectors located in Spain (INTA - INTA El Arenosillo Test Centre in Mazagón, near Huelva.) and Chile (SPDA - San Pedro de Atacama Observatory.) have been observing the sky almost every night in search of rare optical phenomena. They also collect a lot of useful observations which include e.g. observations of many kinds of variable stars. To be able to draw proper conclusions from the data received, adequate quality of the data is very important. Unfortunately Pi of the Sky data is subject to systematic errors caused by various factors, such as cloud cover, seen as significant fluctuations in the number of stars observed by the detector, problems with conducting mounting, a strong background of the Moon or the passing of a bright object, e.g. a planet, near the observed star. Some of these adverse effects can be easily detected during the cataloging of individual measurements, but the quality of our data was still not satisfactory for us. In order to improve the quality of our data, we have developed two new procedures based on two different approaches. In this article we will report on these procedures, give some examples, and show how these procedures improve the quality of our data.1 Later we will compare developed methods, give they advantages and disadvantages and show how we can obtain the best data quality, based only on the best combination of used algorithms results. At the end of this article we will describe how these corrections improve the period detection error, what is the most important result when we want to obtain the physical parameters of the analyzed stars.

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