<?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>S0185-11012017000200023</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[Infrared Characteristics of the Bis Catalog Objects]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Gaudenzi]]></surname>
<given-names><![CDATA[S.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Nesci]]></surname>
<given-names><![CDATA[R.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Rossi]]></surname>
<given-names><![CDATA[C.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
<xref ref-type="aff" rid="Aaf"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Sclavi]]></surname>
<given-names><![CDATA[S.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Gigoyan]]></surname>
<given-names><![CDATA[K. S.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Mickaelian]]></surname>
<given-names><![CDATA[A. M.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,INAF IAPS ]]></institution>
<addr-line><![CDATA[Roma ]]></addr-line>
<country>Italy</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,INAF Osservatorio Astronomico di Roma ]]></institution>
<addr-line><![CDATA[RM ]]></addr-line>
<country>Italy</country>
</aff>
<aff id="Af3">
<institution><![CDATA[,Università La Sapienza Dipartimento di Fisica ]]></institution>
<addr-line><![CDATA[Roma ]]></addr-line>
<country>Italy</country>
</aff>
<aff id="Af4">
<institution><![CDATA[,Ambartsumian Byurakan Astrophysical Observatory  ]]></institution>
<addr-line><![CDATA[ ]]></addr-line>
<country>Armenia</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>00</month>
<year>2017</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>00</month>
<year>2017</year>
</pub-date>
<volume>53</volume>
<numero>2</numero>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0185-11012017000200023&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0185-11012017000200023&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0185-11012017000200023&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[ABSTRACT We studied several color-color infrared diagrams of the 276 late type stars of the BIS catalog. For 95 of these stars we derived spectral classification from our slit spectroscopy. From the 2MASS color diagram we concluded that none of the sample stars is a dwarf. The WISE 3.4-12 vs 12-22 plot is the best to discriminate the variability type (Mira, irregular and not-variable), as well as carbon stars. IRAS colors are less useful due to the poor quality of the data for most of the BIS stars. Mixed plots involving 2MASS, AKARI and WISE were also explored: the 2MASSAKARI J-[S09] vs [S09]-[L18] plot is efficient to discriminate carbon and Mira stars. From the color plots and our spectroscopy we can statistically predict that in the whole BIS catalog no other dusty carbon star is present, while a few Miras and CH or R carbon stars could be discovered. Only about 15% of the BIS stars are of early M type.]]></p></abstract>
<abstract abstract-type="short" xml:lang="es"><p><![CDATA[RESUMEN Estudiamos diagramas color-color en el infrarrojo de 276 estrellas tardías del catálogo BIS. Obtuvimos clasificaciones espectrales para 95 de ellas. Con el diagrama de color del 2MASS concluímos que ninguna de las estrellas estudiadas es enana. La gráfica 3.4-12 vs 12-22 del WISE permite diferenciar el tipo de variabilidad (Mira, irregular, no variable, o estrellas de carbón). Los colores del IRAS son menos útiles por la pobre calidad de los datos de muchas estrellas BIS. Se exploraron varias gráficas de datos del 2MASS, AKARI y WISE. La gráfica 2MASS-AKARI J-[S09] vs [S09]-[L18] es útil para diferenciar entre las estrellas de carbón y las Miras. Con las gráficas de colores y la espectroscopía que obtuvimos predecimos estadísticamente que en el catálogo BIS no existe otra estrella de carbón con polvo, pero puede haber algunas estrellas Miras y de carbón tipo CH o R aún no descubiertas. Alrededor del 15% de las estrellas BIS son de tipo M temprano.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[stars: infrared sources]]></kwd>
<kwd lng="en"><![CDATA[stars: late type]]></kwd>
<kwd lng="en"><![CDATA[stars: variables: general]]></kwd>
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