Editing Big Bang (section)

===Other lines of evidence===
The age of the universe as estimated from the Hubble expansion and the CMB is now in agreement with other estimates using the ages of the oldest stars, both as measured by applying the theory of [[stellar evolution]] to globular clusters and through [[radiometric dating]] of individual [[Stellar population#Population II stars|Population II]] stars.<ref>{{cite web |last=Perley |first=Daniel |date=21 February 2005 |title=Determination of the Universe's Age, t<sub>o</sub> |url=https://astro.berkeley.edu/~dperley/univage/univage.html |url-status=dead |archive-url=https://web.archive.org/web/20060911000604/https://astro.berkeley.edu/~dperley/univage/univage.html |archive-date=11 September 2006 |access-date=11 December 2019 |publisher=Department of Astronomy, [[University of California, Berkeley]] |language=en-us |location=Berkeley, California}}</ref> It is also in agreement with age estimates based on measurements of the expansion using [[Type Ia supernova]]e and measurements of temperature fluctuations in the cosmic microwave background.<ref name="Planck 2015">{{cite journal |author=Planck Collaboration |date=October 2016 |title=''Planck'' 2015 results. XIII. Cosmological parameters |journal=[[Astronomy & Astrophysics]] |volume=594 |page=Article A13 |arxiv=1502.01589 |bibcode=2016A&A...594A..13P |doi=10.1051/0004-6361/201525830 |s2cid=119262962 }} (See Table 4, Age/Gyr, last column.)</ref> The agreement of independent measurements of this age supports the [[Lambda-CDM model|Lambda-CDM]] (ΛCDM) model, since the model is used to relate some of the measurements to an age estimate, and all estimates turn agree. Still, some observations of objects from the relatively early universe (in particular quasar [[APM 08279+5255]]) raise concern as to whether these objects had enough time to form so early in the ΛCDM model.<ref>{{cite journal | last1=Yang | first1=R. J. | last2=Zhang | first2=S. N. | year=2010| title=The age problem in the ΛCDM model | journal=Monthly Notices of the Royal Astronomical Society | volume=407 | issue=3 | pages=1835–1841 | doi=10.1111/j.1365-2966.2010.17020.x | doi-access=free | arxiv=0905.2683 | bibcode=2010MNRAS.407.1835Y }}</ref><ref>{{cite journal | last1=Yu | first1=H. | last2=Wang | first2=F. Y. | year=2014 | title=Reconciling the cosmic age problem in the ''R''<sub>h</sub> = ''ct'' universe | journal=The European Physical Journal C | volume=74 | issue=10 | at=id. 3090 | doi=10.1140/epjc/s10052-014-3090-1 | arxiv=1402.6433 | bibcode=2014EPJC...74.3090Y }}</ref>

The prediction that the CMB temperature was higher in the past has been experimentally supported by observations of very low temperature absorption lines in gas clouds at high redshift.<ref>{{cite journal |last1=Srianand |first1=Raghunathan |author1-link=Raghunathan Srianand |last2=Noterdaeme |first2=Pasquier |last3=Ledoux |first3=Cédric |last4=Petitjean |first4=Patrick |display-authors=3 |date=May 2008 |title=First detection of CO in a high-redshift damped Lyman-α system |journal=[[Astronomy & Astrophysics]] |volume=482 |issue=3 |pages=L39–L42 |bibcode=2008A&A...482L..39S |doi=10.1051/0004-6361:200809727|arxiv=0804.0116 |doi-access=free }}</ref> This prediction also implies that the amplitude of the [[Sunyaev–Zeldovich effect|Sunyaev–Zel'dovich effect]] in clusters of galaxies does not depend directly on redshift. Observations have found this to be roughly true, but this effect depends on cluster properties that do change with cosmic time, making precise measurements difficult.<ref>{{cite journal |last1=Avgoustidis |first1=Anastasios |last2=Luzzi |first2=Gemma |last3=Martins |first3=Carlos J.A.P. |last4=Monteiro |first4=Ana M.R.V.L. |display-authors=3 |date=14 February 2012 |title=Constraints on the CMB temperature-redshift dependence from SZ and distance measurements |arxiv=1112.1862|doi=10.1088/1475-7516/2012/02/013 |volume=2012 |issue=2 |page=Article 013 |journal=[[Journal of Cosmology and Astroparticle Physics]] |bibcode=2012JCAP...02..013A |citeseerx=10.1.1.758.6956 |s2cid=119261969}}</ref><ref>{{harvnb|Belusevic|2008|p=[https://media.wiley.com/product_data/excerpt/42/35274076/3527407642.pdf 16]}}</ref>