<?xml version="1.0" encoding="ISO-8859-1"?><article xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance">
<front>
<journal-meta>
<journal-id>1692-3324</journal-id>
<journal-title><![CDATA[Revista Ingenierías Universidad de Medellín]]></journal-title>
<abbrev-journal-title><![CDATA[Rev. ing. univ. Medellín]]></abbrev-journal-title>
<issn>1692-3324</issn>
<publisher>
<publisher-name><![CDATA[Universidad de Medellín]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S1692-33242025000100004</article-id>
<article-id pub-id-type="doi">10.22395/rium.v24n46a4</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[FROM IRAF TO PYTHON: NEW SOFTWARE ARCHITECTURE FOR ECHELLE SPECTROSCOPY AT UNIVERSIDAD TECNOLOGICA DE PEREIRA OBSERVATORY]]></article-title>
<article-title xml:lang="es"><![CDATA[DE IRAF A PYTHON: NUEVA ARQUITECTURA DE SOFTWARE PARA ESPECTROSCOPÍA ECHELLE EN EL OBSERVATORIO DE LA UNIVERSIDAD TECNOLÓGICA DE PEREIRA]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Rentería]]></surname>
<given-names><![CDATA[Carlos Lino Rengifo]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Ruso]]></surname>
<given-names><![CDATA[Astrid Daniela Henao]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Pardo]]></surname>
<given-names><![CDATA[Manuel Alejandro Pastrana]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Antonio José Camacho University Faculty of Engineering ]]></institution>
<addr-line><![CDATA[Cali ]]></addr-line>
<country>Colombia</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Technological University of Pereira Faculty of Engineering ]]></institution>
<addr-line><![CDATA[Pereira ]]></addr-line>
<country>Colombia</country>
</aff>
<aff id="Af3">
<institution><![CDATA[,Antonio José Camacho University Faculty of Engineering ]]></institution>
<addr-line><![CDATA[Cali ]]></addr-line>
<country>Colombia</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>06</month>
<year>2025</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>06</month>
<year>2025</year>
</pub-date>
<volume>24</volume>
<numero>46</numero>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.co/scielo.php?script=sci_arttext&amp;pid=S1692-33242025000100004&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.co/scielo.php?script=sci_abstract&amp;pid=S1692-33242025000100004&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.co/scielo.php?script=sci_pdf&amp;pid=S1692-33242025000100004&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[ABSTRACT With the evolution of technologies and the discontinuation of IRAF support for, Universidad Tecnológica de Pereira Observatory (OAUTP) identified the need to migrate to a new tool that would not only replace Image Reduction and Analysis Facility (IRAF) but also significantly enhance the Echelle spectra reduction process. To address this need, we created and implemented a new software architecture in Python, utilizing Astropy and PyReduce libraries to improve the processing of Echelle spectra at the UTP Observatory. Our methodology was structured into five steps: (1) requirements analysis, (2) solution design, (3) software development, (4) quality testing, and (5) system deployment. We analyzed data from stars HD108, HD12560, and HD194649 using a ThAr lamp to detect and create 2D spectra. The findings indicate that the new architecture effectively identifies orders and generates 2D spectra, establishing a formal foundation for software development at the UTP Observatory. This represents a significant advancement in astronomical spectroscopy, offering an improved alternative for processing Echelle spectra in astronomical telescopes.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[RESUMEN Con la evolución de las tecnologías y la interrupción del soporte de IRAF para [Aquí falta información sobre el Observatorio de la Universidad Tecnológica de Pereira (OAUTP)], se identificó la necesidad de migrar a una nueva herramienta que no solo reemplazara a la Instalación de Reducción y Análisis de Imágenes (IRAF), sino que también mejorara significativamente el proceso de reducción de espectros Echelle. Para abordar esta necesidad, se creó e implementó una nueva arquitectura de software en Python, utilizando las bibliotecas Astropy y PyReduce para mejorar el procesamiento de los espectros Echelle en el Observatorio UTP. Nuestra metodología se estructuró en cinco pasos: (1) análisis de requisitos, (2) diseño de la solución, (3) desarrollo de software, (4) pruebas de calidad y (5) implementación del sistema. Se analizaron datos de las estrellas HD108, HD12560 y HD194649 utilizando una lámpara ThAr para detectar y generar espectros 2D. Los hallazgos indican que la nueva arquitectura identifica eficazmente los órdenes y genera espectros 2D, sentando las bases para el desarrollo de software en el Observatorio UTP. Esto representa un avance significativo en la espectroscopía astronómica, ofreciendo una alternativa mejorada para el procesamiento de espectros Echelle en telescopios astronómicos.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[Echelle spectrum processing]]></kwd>
<kwd lng="en"><![CDATA[PyReduce]]></kwd>
<kwd lng="en"><![CDATA[process optimization]]></kwd>
<kwd lng="en"><![CDATA[software architecture]]></kwd>
<kwd lng="es"><![CDATA[Procesamiento de espectros a escala]]></kwd>
<kwd lng="es"><![CDATA[PyReduce]]></kwd>
<kwd lng="es"><![CDATA[optimización de procesos]]></kwd>
<kwd lng="es"><![CDATA[arquitectura de software]]></kwd>
</kwd-group>
</article-meta>
</front><back>
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