<?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>S0185-11012024000200227</article-id>
<article-id pub-id-type="doi">10.22201/ia.01851101p.2024.60.02.03</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[New catalog of distances to planetary nebulae based on Gaia parallaxes and statistical distances]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Hernández-Juárez]]></surname>
<given-names><![CDATA[Diego]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Rodríguez]]></surname>
<given-names><![CDATA[Mónica]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Peña]]></surname>
<given-names><![CDATA[Miriam]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Universidad Nacional Autónoma de México Instituto de Astronomía ]]></institution>
<addr-line><![CDATA[Ciudad de México ]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Instituto Nacional de Astrofísica, Optica y Electrónica  ]]></institution>
<addr-line><![CDATA[Puebla ]]></addr-line>
<country>México</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>227</fpage>
<lpage>239</lpage>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012024000200227&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012024000200227&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012024000200227&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract We have developed a method to determine the most reliable distances for a large group of planetary nebulae. For this purpose, we analyze the distances obtained from Gaia parallaxes and three determinations of statistical distances. The most reliable distance is derived for 2211 objects, and uncertainties for these distances are calculated in a homogeneous way. Using our most reliable distances, we compare the distributions of Galactic heights of hydrogen-poor and hydrogen-rich central stars of planetary nebulae. We find that [WR] central stars are closer to the Galactic plane than hydrogen-rich central stars and than other hydrogen-poor central stars. The latter have a similar distribution to hydrogen-rich central stars, which is significantly di&#64256;erent from the one of [WR] central stars. This result disagrees with the proposed evolutionary sequence for hydrogen-poor central stars.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[Resumen Desarrollamos un método que determina las distancias más fiables de un grupo amplio de nebulosas planetarias a partir de las distancias obtenidas con paralajes de Gaia y tres determinaciones de distancias estadísticas. Calculamos las distancias más fiables para 2211 objetos y les asignamos incertidumbres. Con estas distancias, comparamos las distribuciones de alturas sobre el plano galáctico de objetos con estrellas ricas y pobres en hidrógeno. Encontramos que las nebulosas planetarias con estrellas [WR] están más cerca del plano galáctico que aquellas con estrellas ricas en hidrógeno y con otras estrellas pobres en hidrógeno. Estas últimas se distribuyen de manera similar a los objetos con estrellas ricas en hidrógeno, y de forma significativamente distinta que los objetos con estrellas [WR]. Esto está en desacuerdo con la secuencia evolutiva propuesta para estrellas centrales pobres en hidrógeno.]]></p></abstract>
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<kwd lng="en"><![CDATA[parallaxes]]></kwd>
<kwd lng="en"><![CDATA[planetary nebulae: general]]></kwd>
<kwd lng="en"><![CDATA[stars: distances]]></kwd>
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