<?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>S0185-11012024000200397</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2024.60.02.17</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Radio proper motions and a search for the origin of PSR B1849+00]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Rodríguez]]></surname>
<given-names><![CDATA[L. F.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
<xref ref-type="aff" rid="Aaf"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Dzib]]></surname>
<given-names><![CDATA[S. A.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Zapata]]></surname>
<given-names><![CDATA[L. A.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Loinard]]></surname>
<given-names><![CDATA[L.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Universidad Nacional Autónoma de México Instituto de Radioastronomía y Astrofísica ]]></institution>
<addr-line><![CDATA[Morelia Michoacán]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Universidad Autónoma de Chiapas Mesoamerican Center for Theoretical Physics ]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af3">
<institution><![CDATA[,Max-Planck-Institut für Radioastronomie  ]]></institution>
<addr-line><![CDATA[Bonn ]]></addr-line>
<country>Germany</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2024</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2024</year>
</pub-date>
<volume>60</volume>
<numero>2</numero>
<fpage>397</fpage>
<lpage>402</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012024000200397&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012024000200397&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012024000200397&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract Until now it has not been possible to obtain the proper motion of PSR B1849+00 with timing techniques or VLBI imaging, given the enhanced interstellar scattering along its line of sight. We present an analysis of archive Very Large Array observations at epochs from 2012 to 2022 that indicates a total proper motion of 23.9±5.5 mas yr&#8722;1 toward the southwest. After correction for the proper motions produced by galactic rotation, we find a peculiar transverse velocity of &#8771;740 km s&#8722;1. We searched unsuccessfully along the past trajectory of the pulsar for an associated supernova remnant. In particular, W44 is in this trajectory but its distance is di&#64256;erent from that of PSR B1849+00.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen Hasta ahora no ha sido posible obtener el movimiento propio de PSR B1849+00 con técnicas de sincronización o imágenes de VLBI debido a la fuerte dispersión en su línea de visión. Presentamos un análisis de datos del archivo del Very Large Array en épocas de 2012 a 2022 que indican un movimiento propio total de 23.9±5.5 mas año&#8722;1 hacia el suroeste. Después de corregir por el movimiento propio producido por la rotación galáctica encontramos una velocidad transversal peculiar de &#8771;740 km s&#8722;1. Buscamos infructuosamente en la trayectoria pasada del pulsar una remanente de supernova asociada. En particular, W44 está en esta trayectoria pero su distancia es diferente a la de PSR B1849+00.]]></p></abstract>
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<kwd lng="en"><![CDATA[pulsars: general]]></kwd>
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