<?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>0035-001X</journal-id>
<journal-title><![CDATA[Revista mexicana de física]]></journal-title>
<abbrev-journal-title><![CDATA[Rev. mex. fis.]]></abbrev-journal-title>
<issn>0035-001X</issn>
<publisher>
<publisher-name><![CDATA[Sociedad Mexicana de Física]]></publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id>S0035-001X2022000200505</article-id>
<article-id pub-id-type="doi">10.31349/revmexfis.68.020705</article-id>
<title-group>
<article-title xml:lang="en"><![CDATA[The cosmic microwave background and mass power spectrum profiles for a novel and efficient model of dark energy]]></article-title>
</title-group>
<contrib-group>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Matos]]></surname>
<given-names><![CDATA[T.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
<contrib contrib-type="author">
<name>
<surname><![CDATA[Tellez-Tovar]]></surname>
<given-names><![CDATA[L. O.]]></given-names>
</name>
<xref ref-type="aff" rid="Aff"/>
</contrib>
</contrib-group>
<aff id="Af1">
<institution><![CDATA[,Instituto Politécnico Nacional Centro de Investigacion y de Estudios Avanzados Departamento de Física]]></institution>
<addr-line><![CDATA[CDMX ]]></addr-line>
<country>Mexico</country>
</aff>
<aff id="Af2">
<institution><![CDATA[,Instituto Politécnico Nacional Centro de Investigación y de Estudios Avanzados Departamento de Física]]></institution>
<addr-line><![CDATA[CDMX ]]></addr-line>
<country>Mexico</country>
</aff>
<pub-date pub-type="pub">
<day>00</day>
<month>04</month>
<year>2022</year>
</pub-date>
<pub-date pub-type="epub">
<day>00</day>
<month>04</month>
<year>2022</year>
</pub-date>
<volume>68</volume>
<numero>2</numero>
<copyright-statement/>
<copyright-year/>
<self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_arttext&amp;pid=S0035-001X2022000200505&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_abstract&amp;pid=S0035-001X2022000200505&amp;lng=en&amp;nrm=iso"></self-uri><self-uri xlink:href="http://www.scielo.org.mx/scielo.php?script=sci_pdf&amp;pid=S0035-001X2022000200505&amp;lng=en&amp;nrm=iso"></self-uri><abstract abstract-type="short" xml:lang="en"><p><![CDATA[Abstract In a previous work [1] it was shown that by considering the quantum nature of the gravitational field mediator, it is possible to introduce the momentum energy of the graviton into the Einstein equations as an effective cosmological constant. The Compton Mass Dark Energy model proposes that this momentum can be interpreted as dark energy, with a Compton wavelength given by the size of the observable universe R  H , implying that the dark energy varies depending on this size. The main result of this previous work is the existence of an effective cosmological constant &#923; = 2&#960; 2 /&#955; 2 that varies very slowly, being &#955; = (c/H 0)R  H the graviton Compton wavelength. In the present work we use that the dark energy density parameter is given by    &#937;  &#923; = 2   &#960;  2 / 3 /   R  H  2, it only has the curvature &#8486; k as a free constant and depends exclusively on the radiation density parameter &#8486; r . Using &#8486; 0r = 9.54×10&#8722;5, the theoretical prediction for a flat universe of the dark energy density parameter is &#8486;0&#923; = 0.6922. We perform a general study for a non-flat universe, using the Planck data and a modified version of the CLASS code we find an excellent concordance with the Cosmic Microwave Background and Mass Power Spectrum profiles, provided that the Hubble parameter today is H 0 = 72.6 km/s/Mpc for an universe with curvature &#8486; 0k = &#8722;0.003. We conclude that the Compton Mass Dark Energy model provides a natural explanation for the accelerated expansion and the coincidence problem of the universe.]]></p></abstract>
<kwd-group>
<kwd lng="en"><![CDATA[Cosmological constant]]></kwd>
<kwd lng="en"><![CDATA[Hubble parameter]]></kwd>
<kwd lng="en"><![CDATA[Compton mass]]></kwd>
</kwd-group>
</article-meta>
</front><back>
<ref-list>
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<article-title xml:lang=""><![CDATA[The Cosmic Linear Anisotropy Solving System (CLASS). Part II: Approximation schemes]]></article-title>
<source><![CDATA[J. Cosmol. Astropart. Phys.]]></source>
<year>2011</year>
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<given-names><![CDATA[A. G.]]></given-names>
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<article-title xml:lang=""><![CDATA[2.4% determination of the local value of the Hubble constant]]></article-title>
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<year>2016</year>
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<source><![CDATA[Gravitation and Cosmology]]></source>
<year>1972</year>
<edition>1</edition>
<publisher-loc><![CDATA[New York ]]></publisher-loc>
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</ref-list>
</back>
</article>
