Editing Cosmic Background Explorer (section)

=== Cosmological implications ===
In addition to the science results detailed in the last section, there are numerous cosmological questions left unanswered by COBE's results. A direct measurement of the [[extragalactic background light]] (EBL) can also provide important constraints on the integrated cosmological history of star formation, metal and dust production, and the conversion of starlight into infrared emissions by dust.<ref name=dwek>{{cite journal |author=Dwek, E. |author2=R. G. Arendt |author3=M. G. Hauser |author4=D. Fixsen |author5=T. Kelsall |author6=D. Leisawitz |author7=Y. C. Pei |author8=E. L. Wright |author9=J. C. Mather |author10=S. H. Moseley |author11=N. Odegard |author12=R. Shafer |author13=R. F. Silverberg |author14=J. L. Weiland |name-list-style=amp |date=1998 |title=The COBE Diffuse Infrared Background Experiment search for the cosmic infrared background: IV. Cosmological Implications |bibcode=1998ApJ...508..106D |journal=Astrophysical Journal |volume=508 |issue=1 |pages=106–122 |doi=10.1086/306382 |arxiv=astro-ph/9806129 |s2cid=14706133}}</ref>

By looking at the results from DIRBE and FIRAS in the 140 to 5000 μm we can detect that the integrated EBL intensity is ≈16 [[Watt|nW]]/(m<sup>2</sup>·sr). This is consistent with the energy released during [[nucleosynthesis]] and constitutes about 20–50% of the total energy released in the formation of [[helium]] and metals throughout the history of the universe. Attributed only to nuclear sources, this intensity implies that more than 5–15% of the baryonic mass density implied by Big Bang nucleosynthesis analysis has been processed in stars to helium and heavier elements.<ref name=dwek/>

There were also significant implications into [[star formation]]. COBE observations provide important constraints on the cosmic star formation rate and help us calculate the EBL spectrum for various star formation histories. Observation made by COBE require that star formation rate at redshifts of ''z'' ≈ 1.5 to be larger than that inferred from UV-optical observations by a factor of 2. This excess stellar energy must be mainly generated by massive stars in yet - undetected dust enshrouded galaxies or extremely dusty star-forming regions in observed galaxies.<ref name=dwek/> The exact star formation history cannot unambiguously be resolved by COBE and further observations must be made in the future.

On 30 June 2001, NASA launched a follow-up mission to COBE led by DMR Deputy Principal Investigator [[Charles L. Bennett]]. The [[Wilkinson Microwave Anisotropy Probe]] has clarified and expanded upon COBE's accomplishments. Following WMAP, the European Space Agency's probe, [[Planck (spacecraft)|Planck]] has continued to increase the resolution at which the background has been mapped.<ref>{{cite web |last=Thomas |first=Christopher |title=Planck's Probe Map - A picture of the Universe |date=3 April 2013 |url=http://dawn.com/2013/04/03/plank-probes-map-a-picture-of-our-universe/ |publisher=Spider Magazine |access-date=28 May 2013}}</ref><ref>{{cite web |title=Planck's HFI Completes Its Survey of the Early Universe |url=http://www.esa.int/Our_Activities/Space_Science/Planck/Planck_s_HFI_completes_its_survey_of_early_Universe |publisher=ESA |access-date=28 May 2013}}</ref>