<?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>0185-1101</journal-id>
<journal-title><![CDATA[Revista mexicana de astronomía y astrofísica]]></journal-title>
<abbrev-journal-title><![CDATA[Rev. mex. astron. astrofis]]></abbrev-journal-title>
<issn>0185-1101</issn>
<publisher>
<publisher-name><![CDATA[Universidad Nacional Autónoma de México, Instituto de Astronomía]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S0185-11012025000100155</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2025.61.01.11</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Characterization of a Double Wollaston Module for Polarimetry in Astrophysics]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[García-Pérez]]></surname>
<given-names><![CDATA[A.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Luna]]></surname>
<given-names><![CDATA[A.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Castro-Ramos]]></surname>
<given-names><![CDATA[J.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Serrano-Bernal]]></surname>
<given-names><![CDATA[E. O.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Medina]]></surname>
<given-names><![CDATA[S.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Instituto Nacional de Astrofísica, Óptica y Electrónica  ]]></institution>
<addr-line><![CDATA[San Andrés Cholula Puebla]]></addr-line>
<country>México</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Tyndall National Institute  ]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>Ireland</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2025</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2025</year>
</pub-date>
<volume>61</volume>
<numero>1</numero>
<fpage>155</fpage>
<lpage>171</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012025000100155&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012025000100155&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012025000100155&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract The Wedge Double Wollaston (WeDoWo) or &#8220;double Wollaston" module is a device capable of displaying four images of a single field of view (FOV); each image corresponds to a different polarization angle (0°, 45°, 90°, and 135°), providing enough information for the Stokes I, Q, and U parameters calculation and the linear polarization angle and fraction values retrieved from the source observed, in this case, an astronomical source, in a single exposure (single-shot). In this paper, we present the design of a SiO2 (Crystalline Silica) WeDoWo module, describe the characterization process carried out in the laboratory and the subsequent calibration. Likewise, we show the application of this module for imaging astronomical polarimetry using the 1.0-meter telescope of the National Astronomical Observatory from Tonantzintla, Puebla (OAN-TNT), and illustrate the advantages and limitations of this technique and the optimal performance of this module.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen El módulo Wedge Double Wollaston (WeDoWo) o &#8220;doble Wollaston" es un dispositivo capaz de desplegar 4 imágenes de diferente ángulo de polarización (0°, 45°, 90°, 135°), permitiendo calcular los parámetros de Stokes I, Q y U, así como el grado y ángulo de polarización lineal de la fuente observada en una sola exposición. En este artículo presentamos el diseño de un módulo WeDoWo en SiO2 (Sílice Cristalina) y describimos la caracterización realizada en laboratorio a distintas longitudes de onda y su posterior calibración. De igual manera mostramos la aplicación de este módulo para polarimetría astronómica utilizando el telescopio de 1 metro del Observatorio Astronómico Nacional de Tonantzintla, Puebla (OAN-TNT); exponemos las ventajas y limitaciones que presenta esta técnica y el rendimiento óptimo que se puede lograr.]]></p></abstract>
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<kwd lng="en"><![CDATA[instrumentation: polarimeters]]></kwd>
<kwd lng="en"><![CDATA[methods: observational]]></kwd>
<kwd lng="en"><![CDATA[polarization]]></kwd>
<kwd lng="en"><![CDATA[techniques: polarimetric]]></kwd>
</kwd-group>
</article-meta>
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