Editing Big Bang (section)

=== Structure formation ===
{{Main|Structure formation}}
[[File:Heic1401a-Abell2744-20140107.jpg|thumb|right|upright=1.5|[[Abell 2744]] [[galaxy cluster]] – [[Hubble Space Telescope#Frontier Fields program|Hubble Frontier Fields view]]<ref name="NASA-20140107">{{cite web |url=https://www.jpl.nasa.gov/news/news.php?release=2014-007 |url-status=live |title=NASA's Hubble and Spitzer Team up to Probe Faraway Galaxies |last1=Clavin |first1=Whitney |last2=Jenkins |first2=Ann |last3=Villard |first3=Ray |date=7 January 2014 |website=[[Jet Propulsion Laboratory]] |publisher=[[NASA]] |location=Washington, D.C. |archive-url=https://web.archive.org/web/20190903225105/https://www.jpl.nasa.gov/news/news.php?release=2014-007 |archive-date=3 September 2019 |access-date=8 January 2014}}</ref>]]
After the recombination epoch, the slightly denser regions of the uniformly distributed matter gravitationally attracted nearby matter and thus grew even denser, forming gas clouds, stars, galaxies, and the other astronomical structures observable today.<ref name="HTUW"/> The details of this process depend on the amount and type of matter in the universe. The four possible types of matter are known as [[cold dark matter]] (CDM), [[warm dark matter]], [[hot dark matter]], and [[Baryon#Baryonic matter|baryonic matter]]. The best measurements available, from the [[Wilkinson Microwave Anisotropy Probe]] (WMAP), show that the data is well-fit by a [[Lambda-CDM model]] in which dark matter is assumed to be cold. This CDM is estimated to make up about 23% of the matter/energy of the universe, while baryonic matter makes up about 4.6%.<ref name="wmap7year">{{cite journal |last1=Jarosik |first1=Norman |author1-link=Norman Jarosik |last2=Bennett |first2=Charles L. |author2-link=Charles L. Bennett |last3=Dunkley |first3=Jo |author3-link=Jo Dunkley |last4=Gold |first4=B. |last5=Greason |first5=M. R. |last6=Halpern |first6=M. |last7=Hill |first7=R. S. |last8=Hinshaw |first8=G. |last9=Kogut |first9=A. |last10=Komatsu |first10=E. |last11=Larson |first11=D. |last12=Limon |first12=M. |last13=Meyer |first13=S. S. |last14=Nolta |first14=M. R. |last15=Odegard |first15=N. |last16=Page |first16=L. |last17=Smith |first17=K. M. |last18=Spergel |first18=D. N. |last19=Tucker |first19=G. S. |last20=Weiland |first20=J. L. |last21=Wollack |first21=E. |last22=Wright |first22=E. L. |display-authors=3 |date=February 2011 |title=Seven-Year ''Wilkinson Microwave Anisotropy Probe (WMAP)'' Observations: Sky Maps, Systematic Errors, and Basic Results |url=https://lambda.gsfc.nasa.gov/product/map/dr4/pub_papers/sevenyear/basic_results/wmap_7yr_basic_results.pdf |url-status=live |journal=[[The Astrophysical Journal|The Astrophysical Journal Supplement Series]] |volume=192 |issue=2 |page=Article 14 |bibcode=2011ApJS..192...14J |arxiv=1001.4744 |doi=10.1088/0067-0049/192/2/14 |hdl=2152/43001 |s2cid=46171526 |archive-url=https://web.archive.org/web/20190914181522/https://lambda.gsfc.nasa.gov/product/map/dr4/pub_papers/sevenyear/basic_results/wmap_7yr_basic_results.pdf |archive-date=14 September 2019 |access-date=2 December 2019}} (See Table 8.)</ref>