Editing Lambda-CDM model (section)

== Successes ==
Among all cosmological models, the ΛCDM model has been the most successful; it describes a wide range of astronomical observations with remarkable accuracy.<ref name="Snowmass21"/>{{rp|58|q=...the standard ΛCDM cosmological model provides a remarkable description of a wide range of astrophysical and cosmological probes}} The notable successes include:
* Accurate modeling the high-precision CMB angular distribution measure by the [[Planck (satellite)|Planck mission]]<ref name="Planck-2018-legacy">{{Cite journal |last1=Aghanim |first1=N. |last2=Akrami |first2=Y. |last3=Arroja |first3=F. |last4=Ashdown |first4=M. |last5=Aumont |first5=J. |last6=Baccigalupi |first6=C. |last7=Ballardini |first7=M. |last8=Banday |first8=A. J. |last9=Barreiro |first9=R. B. |last10=Bartolo |first10=N. |last11=Basak |first11=S. |last12=Battye |first12=R. |last13=Benabed |first13=K. |last14=Bernard |first14=J.-P. |last15=Bersanelli |first15=M. |date=2020-09-01 |title=Planck 2018 results - I. Overview and the cosmological legacy of Planck |url=https://www.aanda.org/articles/aa/full_html/2020/09/aa33880-18/aa33880-18.html |journal=Astronomy & Astrophysics |language=en |volume=641 |pages=A1 |doi=10.1051/0004-6361/201833880 |arxiv=1807.06205 |bibcode=2020A&A...641A...1P |issn=0004-6361}}</ref> and [[Atacama Cosmology Telescope]].<ref name="Aiola-ACT-2020">{{Cite journal |last1=Aiola |first1=Simone |last2=Calabrese |first2=Erminia |last3=Maurin |first3=Loïc |last4=Naess |first4=Sigurd |last5=Schmitt |first5=Benjamin L. |last6=Abitbol |first6=Maximilian H. |last7=Addison |first7=Graeme E. |last8=Ade |first8=Peter A. R. |last9=Alonso |first9=David |last10=Amiri |first10=Mandana |last11=Amodeo |first11=Stefania |last12=Angile |first12=Elio |last13=Austermann |first13=Jason E. |last14=Baildon |first14=Taylor |last15=Battaglia |first15=Nick |date=2020-12-01 |title=The Atacama Cosmology Telescope: DR4 maps and cosmological parameters |journal=Journal of Cosmology and Astroparticle Physics |volume=2020 |issue=12 |pages=047 |doi=10.1088/1475-7516/2020/12/047 |arxiv=2007.07288 |bibcode=2020JCAP...12..047A |issn=1475-7516}}</ref><ref name="Snowmass21"/>
* Accurate description of the linear [[Polarization (cosmology)|E-mode polarization]] of the CMB radiation due to fluctuations on the surface of last scattering events.<ref name="Dutcher-EMode-2021">{{Cite journal |last1=Dutcher |first1=D. |last2=Balkenhol |first2=L. |last3=Ade |first3=P. A. R. |last4=Ahmed |first4=Z. |last5=Anderes |first5=E. |last6=Anderson |first6=A. J. |last7=Archipley |first7=M. |last8=Avva |first8=J. S. |last9=Aylor |first9=K. |last10=Barry |first10=P. S. |last11=Basu Thakur |first11=R. |last12=Benabed |first12=K. |last13=Bender |first13=A. N. |last14=Benson |first14=B. A. |last15=Bianchini |first15=F. |date=2021-07-13 |title=Measurements of the E -mode polarization and temperature- E -mode correlation of the CMB from SPT-3G 2018 data |url=https://journals.aps.org/prd/abstract/10.1103/PhysRevD.104.022003 |journal=Physical Review D |language=en |volume=104 |issue=2 |page=022003 |doi=10.1103/PhysRevD.104.022003 |arxiv=2101.01684 |bibcode=2021PhRvD.104b2003D |issn=2470-0010}}</ref><ref name="Snowmass21"/>
* Prediction of the observed [[Polarization (cosmology)|B-mode polarization]] of the CMB light due to primordial gravitational waves.<ref name="Ade-BModes-2021">{{Cite journal |last1=Ade |first1=P. A. R. |last2=Ahmed |first2=Z. |last3=Amiri |first3=M. |last4=Barkats |first4=D. |last5=Thakur |first5=R. Basu |last6=Bischoff |first6=C. A. |last7=Beck |first7=D. |last8=Bock |first8=J. J. |last9=Boenish |first9=H. |last10=Bullock |first10=E. |last11=Buza |first11=V. |last12=Cheshire |first12=J. R. |last13=Connors |first13=J. |last14=Cornelison |first14=J. |last15=Crumrine |first15=M. |date=2021-10-04 |title=Improved Constraints on Primordial Gravitational Waves using Planck , WMAP, and BICEP/ Keck Observations through the 2018 Observing Season |url=https://journals.aps.org/prl/abstract/10.1103/PhysRevLett.127.151301 |journal=Physical Review Letters |language=en |volume=127 |issue=15 |page=151301 |doi=10.1103/PhysRevLett.127.151301 |pmid=34678017 |arxiv=2110.00483 |bibcode=2021PhRvL.127o1301A |issn=0031-9007}}</ref><ref name="Snowmass21"/> 
* Observations of H<sub>2</sub>O emission spectra from a galaxy 12.8 billion light years away consistent with molecules excited by cosmic background radiation much more energetic – 16-20K – than the CMB we observe now, 3K.<ref name="Riechers-2022">{{Cite journal |last1=Riechers |first1=Dominik A. |last2=Weiss |first2=Axel |last3=Walter |first3=Fabian |last4=Carilli |first4=Christopher L. |last5=Cox |first5=Pierre |last6=Decarli |first6=Roberto |last7=Neri |first7=Roberto |date=February 2022 |title=Microwave background temperature at a redshift of 6.34 from H2O absorption |journal=Nature |language=en |volume=602 |issue=7895 |pages=58–62 |doi=10.1038/s41586-021-04294-5 |issn=1476-4687 |pmc=8810383 |pmid=35110755}}</ref><ref name="Snowmass21"/>	
* Predictions of the primordial abundance of [[deuterium]] as a result of [[Big Bang nucleosynthesis]].<ref name="Cooke-2014">{{Cite journal |last=Cooke |first=Ryan J. |last2=Pettini |first2=Max |last3=Jorgenson |first3=Regina A. |last4=Murphy |first4=Michael T. |last5=Steidel |first5=Charles C. |date=2014-01-03 |title=PRECISION MEASURES OF THE PRIMORDIAL ABUNDANCE OF DEUTERIUM |journal=The Astrophysical Journal |volume=781 |issue=1 |pages=31 |doi=10.1088/0004-637x/781/1/31 |issn=0004-637X}}</ref> The observed abundance matches the one derived from the nucleosynthesis model with the value for baryon density derived from CMB measurements.<ref name="Turner"/>{{rp|4.1.2}}
In addition to explaining many pre-2000 observations, the model has made a number of successful predictions: notably the existence of the [[baryon acoustic oscillation]] feature, discovered in 2005 in the predicted location; and the statistics of weak [[gravitational lensing]], first observed in 2000 by several teams. The [[Cosmic microwave background#Polarization|polarization]] of the CMB, discovered in 2002 by DASI,<ref>{{cite journal |last1=Kovac|first1=J. M.|last2=Leitch|first2=E. M.|last3=Pryke|first3=C.|author3-link=Clement Pryke|last4=Carlstrom|first4=J. E.|last5=Halverson|first5=N. W. |last6=Holzapfel |first6=W. L.|title=Detection of polarization in the cosmic microwave background using DASI |journal=Nature |year=2002|volume=420|issue=6917 |pages=772–787 |doi=10.1038/nature01269 |pmid=12490941 |arxiv=astro-ph/0209478|bibcode=2002Natur.420..772K|s2cid=4359884|url=https://cds.cern.ch/record/582473}}</ref> has been successfully predicted by the model: in the 2015 ''Planck'' data release,<ref>{{cite journal |title=Planck 2015 Results. XIII. Cosmological Parameters |arxiv=1502.01589 |author1=Planck Collaboration |year=2016 |doi=10.1051/0004-6361/201525830 |volume=594 |issue=13 |journal=Astronomy & Astrophysics |page=A13 |bibcode=2016A&A...594A..13P|s2cid=119262962 }}</ref> there are seven observed peaks in the temperature (TT) power spectrum, six peaks in the temperature–polarization (TE) cross spectrum, and five peaks in the polarization (EE) spectrum. The six free parameters can be well constrained by the TT spectrum alone, and then the TE and EE spectra can be predicted theoretically to few-percent precision with no further adjustments allowed.{{citation needed|date=February 2024}}