<?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>S0185-11012018000200355</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[&#120517; mus revisited: Rectifying a 82 yr-old mistake]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Pourbaix]]></surname>
<given-names><![CDATA[Dimitri]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
<xref ref-type="aff" rid="Aaf"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Boffin]]></surname>
<given-names><![CDATA[Henri M. J.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Université Libre de Bruxelles Institut d&#8217;Astronomie et d&#8217;Astrophysique ]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>Belgium</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Natinal Fund for Scientific Research F.R.S. ]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>Belgium</country>
</aff>
<aff id="Af3">
<institution><![CDATA[,European Southern Observatory  ]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>Germany</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2018</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2018</year>
</pub-date>
<volume>54</volume>
<numero>2</numero>
<fpage>355</fpage>
<lpage>361</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012018000200355&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012018000200355&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012018000200355&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract The red giant &#948; Muscae is known since 1919 to be a spectroscopic binary, and the first and only orbit was determined in 1936, claiming the period to be 847 days. This was discrepant with the Hipparcos determined astrometric orbit. Using the latest data available for this object - leading to a 100 yr timespan - we show here that the correct period is 423 d, and are able for the first time to combine the spectroscopic orbit with the Hipparcos orbit. Using all the available information, we find that the &#8776; 1.2 M&#8857; red giant must have a &#8776; 0.3 &#8722; 0.4 M&#8857; M dwarf companion, and that the system will soon evolve towards a He WD binary system. Given its relatively short period, &#948; Muscae may be an ideal benchmark for testing astrometric orbits obtained by Gaia for very bright stars.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen Desde 1919 se sabe que la gigante roja &#948; Muscae es una binaria espectroscópica. La primera (y única)órbita fue determinada en 1936 y se reportó un período de 847 días. Este período discrepa del de la órbita astrométrica obtenida con el Hipparcos. Con los últimos datos disponibles para este objeto, que permiten ya abarcar un intervalo de 100 años, mostramos que el período correcto es de 423 años. Por primera vez se combina la órbita espectroscópica con la de Hipparcos. Con toda la información disponible encontramos que la gigante roja, con una masa de &#8776; 1.2 M&#8857; debe tener una compañera enana M de &#8776; 0.3&#8722;0.4 M&#8857;, y que el sistema pronto evolucionar &#769;a hacia una binaria enana blanca de He. Dado su período relativamente corto, &#948; Muscae podría ser ideal para confirmar las órbitas astrométricas obtenidas por Gaia para estrellas muy brillantes.]]></p></abstract>
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<kwd lng="en"><![CDATA[astrometry]]></kwd>
<kwd lng="en"><![CDATA[binaries: spectroscopic]]></kwd>
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