<?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>S0185-11012024000200355</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2024.60.02.12</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[The radio continuum source projected near HR 8799]]></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[Zapata]]></surname>
<given-names><![CDATA[L. A.]]></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>
<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>355</fpage>
<lpage>359</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012024000200355&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012024000200355&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012024000200355&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract HR 8799 is an A5/F0 V star where exoplanets were first directly imaged. Four exoplanets were found within &#8771;    2  .  "0 from the star. Here we report the VLA detection of a faint (19.1±2.7 µJy) radio continuum (3.0 GHz) source projected at &#8771;    2  .  "2 from the star. The a priori probability of finding a background source with this flux density within a radius of    2  .  "2 is only 0.0046. However, the astrometry made with the VLA and ALMA images, separated by 5.5 years, indicates no significant proper motions and rules out the association of the radio source with the HR 8799 system and suggests it is a background millimeter galaxy with dust emission in the millimeter and partially thick synchrotron emission in the centimeter.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen HR 8799 es una estrella A5/F0 V en la cual se detectaron por primera vez exoplanetas con la técnica de imágenes directas. Se encontraron cuatro exoplanetas dentro de &#8771;    2  .  "0 de la estrella. Aquí reportamos la detección con el VLA de una fuente débil de radio continuo (19.1±2.7 µJy) a una frecuencia de 3.0 GHz proyectada a &#8771;    2  .  "2 de la estrella. La probabilidad a priori de encontrar una fuente de fondo con esta densidad de flujo dentro de un radio de    2  .  "2 es sólo 0.0046. Sin embargo, la astrometría realizada con las imágenes del VLA y ALMA, separadas por 5.5 años, indica que no hay movimientos propios significativos, descarta la asociación de la fuente de radio con el sistema HR 8799 y sugiere que se trata de una galaxia milimétrica de fondo con emisión de polvo en el milimétrico y emisión sincrotrón parcialmente ópticamente gruesa en el centimétrico.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[astrometry]]></kwd>
<kwd lng="en"><![CDATA[proper motions]]></kwd>
<kwd lng="en"><![CDATA[radio continuum: general]]></kwd>
<kwd lng="en"><![CDATA[stars: individual: HR 8799]]></kwd>
</kwd-group>
</article-meta>
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