<?xml version="1.0" encoding="UTF-8"?><!DOCTYPE article PUBLIC "-//NLM//DTD Journal Publishing DTD v3.0 20080202//EN" "http://dtd.nlm.nih.gov/publishing/3.0/journalpublishing3.dtd">
<article xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink" dtd-version="3.0" xml:lang="en" article-type="research article">
 <front>
  <journal-meta>
   <journal-id journal-id-type="publisher-id">
    jamp
   </journal-id>
   <journal-title-group>
    <journal-title>
     Journal of Applied Mathematics and Physics
    </journal-title>
   </journal-title-group>
   <issn pub-type="epub">
    2327-4352
   </issn>
   <issn publication-format="print">
    2327-4379
   </issn>
   <publisher>
    <publisher-name>
     Scientific Research Publishing
    </publisher-name>
   </publisher>
  </journal-meta>
  <article-meta>
   <article-id pub-id-type="doi">
    10.4236/jamp.2024.1210207
   </article-id>
   <article-id pub-id-type="publisher-id">
    jamp-136952
   </article-id>
   <article-categories>
    <subj-group subj-group-type="heading">
     <subject>
      Articles
     </subject>
    </subj-group>
    <subj-group subj-group-type="Discipline-v2">
     <subject>
      Physics 
     </subject>
     <subject>
       Mathematics
     </subject>
    </subj-group>
   </article-categories>
   <title-group>
    The CMB Luminosity Distance and Cosmological Redshifts
   </title-group>
   <contrib-group>
    <contrib contrib-type="author" xlink:type="simple">
     <name name-style="western">
      <surname>
       Espen Gaarder
      </surname>
      <given-names>
       Haug
      </given-names>
     </name>
    </contrib>
   </contrib-group> 
   <aff id="affnull">
    <addr-line>
     aTempus Gravitational Laboratory, Ås, Norway
    </addr-line> 
   </aff> 
   <pub-date pub-type="epub">
    <day>
     08
    </day> 
    <month>
     10
    </month>
    <year>
     2024
    </year>
   </pub-date> 
   <volume>
    12
   </volume> 
   <issue>
    10
   </issue>
   <fpage>
    3496
   </fpage>
   <lpage>
    3501
   </lpage>
   <history>
    <date date-type="received">
     <day>
      29,
     </day>
     <month>
      September
     </month>
     <year>
      2024
     </year>
    </date>
    <date date-type="published">
     <day>
      26,
     </day>
     <month>
      September
     </month>
     <year>
      2024
     </year> 
    </date> 
    <date date-type="accepted">
     <day>
      26,
     </day>
     <month>
      October
     </month>
     <year>
      2024
     </year> 
    </date>
   </history>
   <permissions>
    <copyright-statement>
     © Copyright 2014 by authors and Scientific Research Publishing Inc. 
    </copyright-statement>
    <copyright-year>
     2014
    </copyright-year>
    <license>
     <license-p>
      This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/
     </license-p>
    </license>
   </permissions>
   <abstract>
    We will outline the relationship between luminosity distance and cosmological redshifts, demonstrating that it is consistent with a new cosmological model recently proposed by Haug and Tatum [1], which appears to resolve the Hubble tension within the 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
        R
       </mi> 
       <mi>
        h
       </mi> 
      </msub> 
      <mo>
       =
      </mo>
      <mi>
       c
      </mi>
      <mi>
       t
      </mi>
     </mrow> 
    </math> cosmology.
   </abstract>
   <kwd-group> 
    <kwd>
     Luminosity Distance
    </kwd> 
    <kwd>
      Angular Distance
    </kwd> 
    <kwd>
      Co-Moving Distance
    </kwd>
   </kwd-group>
  </article-meta>
 </front>
 <body>
  <sec id="s1">
   <title>1. Luminosity Distance Consistent with the Haug and Tatum Cosmological Model</title>
   <p>According to the Stefan-Boltzmann law <xref ref-type="bibr" rid="scirp.136952-2">
     [2]
    </xref> <xref ref-type="bibr" rid="scirp.136952-3">
     [3]
    </xref>, the luminosity of a spherical black body is given by:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        L 
      </mi> 
      <mo>
        = 
      </mo> 
      <mn>
        4 
      </mn> 
      <mi>
        π 
      </mi> 
      <msup> 
       <mi>
         R 
       </mi> 
       <mn>
         2 
       </mn> 
      </msup> 
      <mi>
        σ 
      </mi> 
      <msup> 
       <mi>
         T 
       </mi> 
       <mn>
         4 
       </mn> 
      </msup> 
     </mrow> 
    </math> (1)</p>
   <p>where 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mi>
       T 
     </mi> 
    </math> is the black body temperature and 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        σ 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <msup> 
         <mi>
           π 
         </mi> 
         <mn>
           5 
         </mn> 
        </msup> 
        <msubsup> 
         <mi>
           k 
         </mi> 
         <mi>
           b 
         </mi> 
         <mn>
           4 
         </mn> 
        </msubsup> 
       </mrow> 
       <mrow> 
        <mn>
          15 
        </mn> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <msup> 
         <mi>
           h 
         </mi> 
         <mn>
           3 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> is the Stefan-Boltzmann constant (where 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         k 
       </mi> 
       <mi>
         b 
       </mi> 
      </msub> 
     </mrow> 
    </math> is the Boltzmann constant), 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mi>
       R 
     </mi> 
    </math> is the radius and 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mi>
       L 
     </mi> 
    </math> is the luminosity.</p>
   <p>Let us assume this also holds true for a Schwarzschild <xref ref-type="bibr" rid="scirp.136952-4">
     [4]
    </xref> black hole (see<xref ref-type="bibr" rid="scirp.136952-5">
     [5]
    </xref>), where 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        R 
      </mi> 
      <mo>
        = 
      </mo> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         s 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <mi>
          G 
        </mi> 
        <mi>
          M 
        </mi> 
       </mrow> 
       <mrow> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math>, meaning the radius is equal to the Schwarzschild radius. Solving for the radius, one gets:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         D 
       </mi> 
       <mi>
         L 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        R 
      </mi> 
      <mo>
        = 
      </mo> 
      <msqrt> 
       <mrow> 
        <mfrac> 
         <mi>
           L 
         </mi> 
         <mrow> 
          <mn>
            4 
          </mn> 
          <mi>
            π 
          </mi> 
          <mi>
            σ 
          </mi> 
          <msup> 
           <mi>
             T 
           </mi> 
           <mn>
             4 
           </mn> 
          </msup> 
         </mrow> 
        </mfrac> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> (2)</p>
   <p>Furthermore, the flux density is given by:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        F 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mi>
         L 
       </mi> 
       <mrow> 
        <mn>
          4 
        </mn> 
        <mi>
          π 
        </mi> 
        <msup> 
         <mi>
           R 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (3)</p>
   <p>This means we also have:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         D 
       </mi> 
       <mi>
         L 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        R 
      </mi> 
      <mo>
        = 
      </mo> 
      <msqrt> 
       <mrow> 
        <mfrac> 
         <mi>
           L 
         </mi> 
         <mrow> 
          <mn>
            4 
          </mn> 
          <mi>
            π 
          </mi> 
          <mi>
            F 
          </mi> 
         </mrow> 
        </mfrac> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> (4)</p>
   <p>This is also called the luminosity distance. Moreover, we must have:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mfrac> 
       <mrow> 
        <msub> 
         <mi>
           F 
         </mi> 
         <mi>
           t 
         </mi> 
        </msub> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           F 
         </mi> 
         <mi>
           H 
         </mi> 
        </msub> 
       </mrow> 
      </mfrac> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <msubsup> 
         <mi>
           R 
         </mi> 
         <mi>
           t 
         </mi> 
         <mn>
           2 
         </mn> 
        </msubsup> 
       </mrow> 
       <mrow> 
        <msubsup> 
         <mi>
           R 
         </mi> 
         <mi>
           H 
         </mi> 
         <mn>
           2 
         </mn> 
        </msubsup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (5)</p>
   <p>where 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         F 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
     </mrow> 
    </math> is the flux density in a growing black hole in the 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> cosmological model at time 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mi>
       t 
     </mi> 
    </math> and at radius 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
     </mrow> 
    </math>, and 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         F 
       </mi> 
       <mi>
         H 
       </mi> 
      </msub> 
     </mrow> 
    </math> is the flux density.</p>
   <p>Haug and Tatum have demonstrated that if 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mn>
         0 
       </mn> 
      </msub> 
      <mrow> 
       <mo>
         ( 
       </mo> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          + 
        </mo> 
        <mi>
          z 
        </mi> 
       </mrow> 
       <mo>
         ) 
       </mo> 
      </mrow> 
     </mrow> 
    </math> (which seems to be supported by observations, see <xref ref-type="bibr" rid="scirp.136952-6">
     [6]
    </xref>-<xref ref-type="bibr" rid="scirp.136952-8">
     [8]
    </xref>), then in their type of 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> cosmology, one must have:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math> (6)</p>
   <p>Solved for 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
     </mrow> 
    </math>, this gives:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            + 
          </mo> 
          <mi>
            z 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mn>
         2 
       </mn> 
      </msup> 
     </mrow> 
    </math> (7)</p>
   <p>where 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
     </mrow> 
    </math> is the co-moving transverse luminosity distance. This also means the luminosity distance must follow accordingly. We can rearrange this to:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           h 
         </mi> 
        </msub> 
       </mrow> 
       <mrow> 
        <msup> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mn>
              1 
            </mn> 
            <mo>
              + 
            </mo> 
            <mi>
              z 
            </mi> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math></p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        − 
      </mo> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        − 
      </mo> 
      <mfrac> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           h 
         </mi> 
        </msub> 
       </mrow> 
       <mrow> 
        <msup> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mn>
              1 
            </mn> 
            <mo>
              + 
            </mo> 
            <mi>
              z 
            </mi> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math></p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        − 
      </mo> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mi>
         c 
       </mi> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
       </mrow> 
      </mfrac> 
      <mrow> 
       <mo>
         ( 
       </mo> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          − 
        </mo> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mrow> 
          <msup> 
           <mrow> 
            <mrow> 
             <mo>
               ( 
             </mo> 
             <mrow> 
              <mn>
                1 
              </mn> 
              <mo>
                + 
              </mo> 
              <mi>
                z 
              </mi> 
             </mrow> 
             <mo>
               ) 
             </mo> 
            </mrow> 
           </mrow> 
           <mn>
             2 
           </mn> 
          </msup> 
         </mrow> 
        </mfrac> 
       </mrow> 
       <mo>
         ) 
       </mo> 
      </mrow> 
     </mrow> 
    </math></p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        − 
      </mo> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <mi>
          c 
        </mi> 
        <mi>
          z 
        </mi> 
        <mo>
          + 
        </mo> 
        <mi>
          c 
        </mi> 
        <msup> 
         <mi>
           z 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
        <msup> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mn>
              1 
            </mn> 
            <mo>
              + 
            </mo> 
            <mi>
              z 
            </mi> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (8)</p>
   <p>We define 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        − 
      </mo> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        D 
      </mi> 
     </mrow> 
    </math>, which is the distance to the object emitting photons toward us, so we have:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        D 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <mi>
          c 
        </mi> 
        <mi>
          z 
        </mi> 
        <mo>
          + 
        </mo> 
        <mi>
          c 
        </mi> 
        <msup> 
         <mi>
           z 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
        <msup> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mn>
              1 
            </mn> 
            <mo>
              + 
            </mo> 
            <mi>
              z 
            </mi> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (9)</p>
   <p>This is the same formula that Haug and Tatum have presented, namely:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        D 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mi>
         c 
       </mi> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
       </mrow> 
      </mfrac> 
      <mrow> 
       <mo>
         ( 
       </mo> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          − 
        </mo> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mrow> 
          <msup> 
           <mrow> 
            <mrow> 
             <mo>
               ( 
             </mo> 
             <mrow> 
              <mn>
                1 
              </mn> 
              <mo>
                + 
              </mo> 
              <mi>
                z 
              </mi> 
             </mrow> 
             <mo>
               ) 
             </mo> 
            </mrow> 
           </mrow> 
           <mn>
             2 
           </mn> 
          </msup> 
         </mrow> 
        </mfrac> 
       </mrow> 
       <mo>
         ) 
       </mo> 
      </mrow> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <mi>
          c 
        </mi> 
        <mi>
          z 
        </mi> 
        <mo>
          + 
        </mo> 
        <mi>
          c 
        </mi> 
        <msup> 
         <mi>
           z 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
        <msup> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mn>
              1 
            </mn> 
            <mo>
              + 
            </mo> 
            <mi>
              z 
            </mi> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (10)</p>
   <p>when 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        ≪ 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math> this can be approximated as:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        D 
      </mi> 
      <mo>
        ≈ 
      </mo> 
      <mfrac> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <mi>
          c 
        </mi> 
        <mi>
          z 
        </mi> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (11)</p>
   <p>The well-known Etherington <xref ref-type="bibr" rid="scirp.136952-9">
     [9]
    </xref> equation gives the relationship between the luminosity distance of standard candles and the angular diameter distance, which is given by:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         D 
       </mi> 
       <mi>
         L 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            + 
          </mo> 
          <mi>
            z 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mn>
         2 
       </mn> 
      </msup> 
      <msub> 
       <mi>
         D 
       </mi> 
       <mi>
         A 
       </mi> 
      </msub> 
     </mrow> 
    </math> (12)</p>
   <p>Here, 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         D 
       </mi> 
       <mi>
         A 
       </mi> 
      </msub> 
     </mrow> 
    </math> represents the angular-diameter distance. We can see that this closely resembles our Equation (7). We have already proven that the luminosity distance in our 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> cosmology is identical to 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
     </mrow> 
    </math> (at present) and that before the present time, it corresponds to 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
     </mrow> 
    </math>. This implies that we have essentially demonstrated that the angular-diameter distance is identical to the luminosity distance in the Haug and Tatum cosmology model, which assumes 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>. However, this should naturally be studied carefully over time; for example, one should carefully study whether the Etherington formula is also valid under 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> cosmology. We suspect it is, as our theory is consistent with the critical Friedmann equation <xref ref-type="bibr" rid="scirp.136952-10">
     [10]
    </xref>. It is also worth mentioning that there is a different variation of the Haug and Tatum cosmology, where they propose 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           h 
         </mi> 
        </msub> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           t 
         </mi> 
        </msub> 
       </mrow> 
      </mfrac> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>, which would yield different results that could also be studied further. However, as we will point out in the next section, the scaling 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math> seems preferable.</p>
  </sec><sec id="s2">
   <title>
    <xref ref-type="bibr" rid="scirp.136952-"></xref>2. 

    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
  
      <msub> 
   
       <mstyle mathvariant="bold" mathsize="normal">
    
        <mi>
         
     R
    
        </mi>
   
       </mstyle> 
   
       <mstyle mathvariant="bold" mathsize="normal">
    
        <mi>
         
     h
    
        </mi>
   
       </mstyle> 
  
      </msub> 
  
      <mo>
       
   =
  
      </mo>
  
      <mstyle mathvariant="bold" mathsize="normal">
   
       <mi>
        
    c
   
       </mi>
   
       <mi>
        
    t
   
       </mi>
  
      </mstyle>
 
     </mrow>

    </math> Model Distance and the Hubble Tension</title>
   <p>The Hubble tension remains unresolved in standard cosmology, see Valentino et al. <xref ref-type="bibr" rid="scirp.136952-11">
     [11]
    </xref>. Krishnan et al. <xref ref-type="bibr" rid="scirp.136952-12">
     [12]
    </xref> have even suggested that the Hubble tension could even indicate a breakdown in standard cosmology, that is, in FLRW, which is the cornerstone of Λ-CDM cosmology.</p>
   <p>Haug and Tatum <xref ref-type="bibr" rid="scirp.136952-1">
     [1]
    </xref> have shown, through a combination of trial-and-error methods and intelligent search algorithms, that the Hubble tension can be resolved within a specific class of 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> cosmology, where the Hubble sphere is essentially treated as a black hole. They achieve this by fitting their model to the complete distance ladder of observed Type Ia supernovae from the Union2 database, where they get a close to perfect fit without the need to rely on dark energy or any additional free parameters. This is made possible by a new exact mathematical relationship between the current (and past) CMB temperature and the Hubble constant, in conjunction with the 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> principle.</p>
   <p>
    <xref ref-type="bibr" rid="scirp.136952-"></xref>They achieved this for both a model with 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math> and a model with 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           h 
         </mi> 
        </msub> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           t 
         </mi> 
        </msub> 
       </mrow> 
      </mfrac> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>. However, they have shown that only 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math> predicts 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
     </mrow> 
    </math> 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mn>
         0 
       </mn> 
      </msub> 
      <mrow> 
       <mo>
         ( 
       </mo> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          + 
        </mo> 
        <mi>
          z 
        </mi> 
       </mrow> 
       <mo>
         ) 
       </mo> 
      </mrow> 
     </mrow> 
    </math>, which is consistent with observations. The more commonly assumed 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           h 
         </mi> 
        </msub> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           t 
         </mi> 
        </msub> 
       </mrow> 
      </mfrac> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>, is inside this framework instead consistent with 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mn>
         0 
       </mn> 
      </msub> 
      <msubsup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            + 
          </mo> 
          <mi>
            z 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow></mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msubsup> 
     </mrow> 
    </math> that do not seem supported by observational studies.</p>
   <p>Haug <xref ref-type="bibr" rid="scirp.136952-13">
     [13]
    </xref> has recently extended on the Haug-Tatum model and provided a formal mathematical proof that the Hubble tension can be resolved by a closed-form solution for the more general redshift function 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mi>
         x 
       </mi> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>, where 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mi>
       x 
     </mi> 
    </math> can take any real value. The Haug-Tatum model is a special case of this general model, with 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        x 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mn>
         1 
       </mn> 
       <mn>
         2 
       </mn> 
      </mfrac> 
     </mrow> 
    </math> and 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        x 
      </mi> 
      <mo>
        = 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>. Resolving the Hubble tension alone is not sufficient for a model to be considered a good representation of the cosmos; it must also be consistent with various other cosmological aspects. Haug demonstrates that only when 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        x 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mn>
         1 
       </mn> 
       <mn>
         2 
       </mn> 
      </mfrac> 
     </mrow> 
    </math> (the Haug-Tatum model) does it predict and remain consistent with the observed 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mn>
         0 
       </mn> 
      </msub> 
      <mrow> 
       <mo>
         ( 
       </mo> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          + 
        </mo> 
        <mi>
          z 
        </mi> 
       </mrow> 
       <mo>
         ) 
       </mo> 
      </mrow> 
     </mrow> 
    </math> relationship. Furthermore, only when 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        x 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mn>
         1 
       </mn> 
       <mn>
         2 
       </mn> 
      </mfrac> 
     </mrow> 
    </math> do all three distances-luminosity distance, angular diameter distance, and comoving distance-become the same.</p>
   <p>All of these 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> cosmological models based on the Haug-Tatum model will predict the same Hubble constant, but only one appears consistent with 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mn>
         0 
       </mn> 
      </msub> 
      <mrow> 
       <mo>
         ( 
       </mo> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          + 
        </mo> 
        <mi>
          z 
        </mi> 
       </mrow> 
       <mo>
         ) 
       </mo> 
      </mrow> 
     </mrow> 
    </math>, which is also the model that offers maximum simplification, as the three different distances converge into one.</p>
   <p>In conclusion, we can infer that the Λ-CDM model likely predicts incorrect distances for emitting photons. Additionally, its various types of distances for a given observed 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mi>
       z 
     </mi> 
    </math> seem overly complex, even if such complexity is required when assuming accelerated expansion of space. While this is internally consistent within their model, a much simpler model seems capable of explaining the cosmos. The Haug-Tatum model strongly suggests that no accelerated expansion is necessary and that a simpler model can address phenomena such as the Hubble tension.</p>
  </sec><sec id="s3">
   <title>
    <xref ref-type="bibr" rid="scirp.136952-"></xref>3. The Mattig Formula</title>
   <p>The Mattig <xref ref-type="bibr" rid="scirp.136952-14">
     [14]
    </xref> formula (see also <xref ref-type="bibr" rid="scirp.136952-15">
     [15]
    </xref>) is used to calculate the luminosity distance in terms of redshift and is inside FLRW cosmology given by:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        R 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mi>
         c 
       </mi> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
       </mrow> 
      </mfrac> 
      <mfrac> 
       <mrow> 
        <msub> 
         <mi>
           q 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
        <mi>
          z 
        </mi> 
        <mo>
          + 
        </mo> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <msub> 
           <mi>
             q 
           </mi> 
           <mn>
             0 
           </mn> 
          </msub> 
          <mo>
            − 
          </mo> 
          <mn>
            1 
          </mn> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <msqrt> 
           <mrow> 
            <mn>
              1 
            </mn> 
            <mo>
              + 
            </mo> 
            <mn>
              2 
            </mn> 
            <msub> 
             <mi>
               q 
             </mi> 
             <mn>
               0 
             </mn> 
            </msub> 
            <mi>
              z 
            </mi> 
           </mrow> 
          </msqrt> 
          <mo>
            − 
          </mo> 
          <mn>
            1 
          </mn> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <msubsup> 
         <mi>
           q 
         </mi> 
         <mn>
           0 
         </mn> 
         <mn>
           2 
         </mn> 
        </msubsup> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            + 
          </mo> 
          <mi>
            z 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (13)</p>
   <p>If we set 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         q 
       </mi> 
       <mn>
         0 
       </mn> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>, we obtain:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        d 
      </mi> 
      <mo>
        = 
      </mo> 
      <mi>
        R 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <mi>
          c 
        </mi> 
        <mi>
          z 
        </mi> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            + 
          </mo> 
          <mi>
            z 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (14)</p>
   <p>This is the same distance as given by the Haug and Tatum model when they assume 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           h 
         </mi> 
        </msub> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           R 
         </mi> 
         <mi>
           t 
         </mi> 
        </msub> 
       </mrow> 
      </mfrac> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>. The first-term Taylor series expansion of this is the well-known distance formula often used in the Λ-CDM model:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        d 
      </mi> 
      <mo>
        ≈ 
      </mo> 
      <mfrac> 
       <mrow> 
        <mi>
          c 
        </mi> 
        <mi>
          z 
        </mi> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (15)</p>
  </sec><sec id="s4">
   <title>
    <xref ref-type="bibr" rid="scirp.136952-"></xref>4. Speculative Equivalent Mattig Formula for 

    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
  
      <mstyle mathvariant="bold" mathsize="normal">
   
       <mi>
        
    z
   
       </mi>
  
      </mstyle>
  
      <mo>
       
   =
  
      </mo>
  
      <msubsup> 
   
       <mrow> 
    
        <mrow>
     
         <mo>
           ( 
         </mo> 
     
         <mrow> 
          <mrow> 
           <mrow> 
            <msub> 
             <mstyle mathvariant="bold" mathsize="normal"> 
              <mi>
                R 
              </mi> 
             </mstyle> 
             <mstyle mathvariant="bold" mathsize="normal"> 
              <mi>
                h 
              </mi> 
             </mstyle> 
            </msub> 
           </mrow> 
           <mo>
             / 
           </mo> 
           <mrow> 
            <msub> 
             <mstyle mathvariant="bold" mathsize="normal"> 
              <mi>
                R 
              </mi> 
             </mstyle> 
             <mstyle mathvariant="bold" mathsize="normal"> 
              <mi>
                t 
              </mi> 
             </mstyle> 
            </msub> 
           </mrow> 
          </mrow> 
         </mrow> 
     
         <mo>
           ) 
         </mo>
    
        </mrow>
   
       </mrow> 
   
       <mrow></mrow> 
   
       <mrow> 
    
        <mfrac> 
     
         <mn>
           1 
         </mn> 
     
         <mn>
           2 
         </mn> 
    
        </mfrac> 
   
       </mrow> 
  
      </msubsup> 
  
      <mo>
       
   −
  
      </mo>
  
      <mn>
       
   1
  
      </mn>
 
     </mrow>

    </math> Scaling</title>
   <p>We are suggesting a speculative modification to the Mattig <xref ref-type="bibr" rid="scirp.136952-14">
     [14]
    </xref> formula in an attempt to make it consistent with 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>. Equation (16) is the only equation in this paper that is not strictly based on derivation, so it should simply be regarded as an initial guess (that could be wrong). The idea is that the Mattig formula may require modification to accommodate the redshift scaling 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math> inside 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> cosmology. Based on a qualified assumption, we propose the following:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        d 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mi>
         c 
       </mi> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
       </mrow> 
      </mfrac> 
      <mfrac> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <msub> 
         <mi>
           q 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
        <mi>
          z 
        </mi> 
        <mo>
          + 
        </mo> 
        <msup> 
         <mi>
           z 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <msubsup> 
         <mi>
           q 
         </mi> 
         <mn>
           0 
         </mn> 
         <mn>
           2 
         </mn> 
        </msubsup> 
        <mo>
          + 
        </mo> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <msub> 
           <mi>
             q 
           </mi> 
           <mn>
             0 
           </mn> 
          </msub> 
          <mo>
            − 
          </mo> 
          <mn>
            1 
          </mn> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <msqrt> 
           <mrow> 
            <mn>
              1 
            </mn> 
            <mo>
              + 
            </mo> 
            <mn>
              2 
            </mn> 
            <msub> 
             <mi>
               q 
             </mi> 
             <mn>
               0 
             </mn> 
            </msub> 
            <mi>
              z 
            </mi> 
           </mrow> 
          </msqrt> 
          <mo>
            − 
          </mo> 
          <mn>
            1 
          </mn> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <msubsup> 
         <mi>
           q 
         </mi> 
         <mn>
           0 
         </mn> 
         <mn>
           2 
         </mn> 
        </msubsup> 
        <msup> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mn>
              1 
            </mn> 
            <mo>
              + 
            </mo> 
            <mi>
              z 
            </mi> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (16)</p>
   <p>When 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         q 
       </mi> 
       <mn>
         0 
       </mn> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>, we obtain:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        d 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <mi>
          c 
        </mi> 
        <mi>
          z 
        </mi> 
        <mo>
          + 
        </mo> 
        <mi>
          c 
        </mi> 
        <msup> 
         <mi>
           z 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           H 
         </mi> 
         <mn>
           0 
         </mn> 
        </msub> 
        <msup> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mn>
              1 
            </mn> 
            <mo>
              + 
            </mo> 
            <mi>
              z 
            </mi> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> (17)</p>
   <p>This is equivalent to the distance Haug and Tatum <xref ref-type="bibr" rid="scirp.136952-1">
     [1]
    </xref> presented when they assume 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>. Naturally, someone should derive an equivalent Mattig formula from scratch, as our speculative suggestion in this section could be wrong as it is not based on derivations but a speculative guess. It is simply meant to point to an additional idea that can be investigated.</p>
  </sec><sec id="s5">
   <title>
    <xref ref-type="bibr" rid="scirp.136952-"></xref>5. Conclusion</title>
   <p>The Haug-Tatum cosmological model, in which they propose the redshift scaling 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        z 
      </mi> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               h 
             </mi> 
            </msub> 
           </mrow> 
           <mrow> 
            <msub> 
             <mi>
               R 
             </mi> 
             <mi>
               t 
             </mi> 
            </msub> 
           </mrow> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mn>
           1 
         </mn> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </msup> 
      <mo>
        − 
      </mo> 
      <mn>
        1 
      </mn> 
     </mrow> 
    </math>, leads to a co-moving luminosity distance relationship of 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
     </mrow> 
    </math> 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         t 
       </mi> 
      </msub> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            + 
          </mo> 
          <mi>
            z 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mn>
         2 
       </mn> 
      </msup> 
     </mrow> 
    </math>, as was already indirectly suggested in their paper. We have pointed out that the angular diameter distance in their model appears to be identical to this. In our 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         R 
       </mi> 
       <mi>
         h 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> cosmological model, it seems that many types of cosmological distances converge to the same value. We suspect that some of the many different types of cosmological distances in the Λ-CDM model may result from an overly complex framework that does not represent the cosmos as accurately.</p>
  </sec>
 </body><back>
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