All of space observable from the Earth at the present
Observable universe
Visualization of the observable universe. The scale is such that the fine grains represent collections of large numbers of superclusters. TheVirgo Supercluster—home of theMilky Way—is marked at the center, but is too small to be seen.
The wordobservable in this sense does not refer to the capability of modern technology to detect light or other information from an object, or whether there is anything to be detected. It refers to the physical limit created by thespeed of light itself. No signal can travel faster than light and the universe has only existed for about 14 billion years. Objects which emit light but which exist too far away for that light to have reached Earth are beyond theparticle horizon, outside the observable universe. Every location in the universe has its own observable universe, which may or may not overlap with the one centered on Earth.
According to calculations, the currentcomoving distance to particles from which thecosmic microwave background radiation (CMBR) was emitted, which represents the radius of the visible universe, is about 14.0 billionparsecs (about 45.7 billion light-years). The comoving distance to the edge of the observable universe is about 14.3 billion parsecs (about 46.6 billion light-years),[7] about 2% larger. Theradius of the observable universe is therefore estimated to be about 46.5 billion light-years.[8][9] Using thecritical density and the diameter of the observable universe, the total mass of ordinary matter in the universe can be calculated to be about1.5×1053 kg.[10] In November 2018, astronomers reported thatextragalactic background light (EBL) amounted to4×1084 photons.[11][12]
As the universe's expansion is accelerating, all currently observable objects, outside the localsupercluster, will eventually appear to freeze in time, while emitting progressively redder and fainter light. For instance, objects with the currentredshiftz from 5 to 10 will only be observable up to an age of 4–6 billion years. In addition, light emitted by objects currently situated beyond a certain comoving distance (currently about 19 gigaparsecs (62 Gly)) will never reach Earth.[13]
Observable Universe as a function of time and distance, in context of theexpanding Universe
The universe's size is unknown, and it may be infinite in extent.[14] Some parts of the universe are too far away for the light emitted since theBig Bang to have had enough time to reach Earth or space-based instruments, and therefore lie outside the observable universe. In the future, light from distant galaxies will have had more time to travel, so one might expect that additional regions will become observable. Regions distant from observers (such as us) are expanding away faster than the speed of light, at rates estimated byHubble's law.[note 1] Theexpansion rate appears to be accelerating, whichdark energy was proposed to explain.
Assuming dark energy remains constant (an unchangingcosmological constant) so that the expansion rate of the universe continues to accelerate, there is a "future visibility limit" beyond which objects will never enter the observable universe at any time in the future because light emitted by objects outside that limit could never reach the Earth. Note that, because theHubble parameter is decreasing with time, there can be cases where a galaxy that is receding from Earth only slightly faster than light emits a signal that eventually reaches Earth.[9][15] This future visibility limit is calculated at acomoving distance of 19 billion parsecs (62 billion light-years), assuming the universe will keep expanding forever, which implies the number of galaxies that can ever be theoretically observed in the infinite future is only larger than the number currently observable by a factor of 2.36 (ignoring redshift effects).[note 2]
In principle, more galaxies will become observable in the future; in practice, an increasing number of galaxies will become extremelyredshifted due to ongoing expansion, so much so that they will seem to disappear from view and become invisible.[16][17][18] A galaxy at a given comoving distance is defined to lie within the "observable universe" if we can receive signals emitted by the galaxy at any age in its history, say, a signal sent from the galaxy only 500 million years after the Big Bang. Because of the universe's expansion, there may be some later age at which a signal sent from the same galaxy can never reach the Earth at any point in the infinite future, so, for example, we might never see what the galaxy looked like 10 billion years after the Big Bang,[13] even though it remains at the same comoving distance less than that of the observable universe.
This can be used to define a type of cosmicevent horizon whose distance from the Earth changes over time. For example, the current distance to this horizon is about 16 billion light-years, meaning that a signal from an event happening at present can eventually reach the Earth if the event is less than 16 billion light-years away, but the signal will never reach the Earth if the event is further away.[9]
The space before this cosmic event horizon can be called "reachable universe", that is all galaxies closer than that could be reached if we left for them today, at the speed of light; all galaxies beyond that are unreachable.[19][20] Simple observation will show the future visibility limit (62 billion light-years) is exactly equal to the reachable limit (16 billion light-years) added to the current visibility limit (46 billion light-years).[21][7]
The reachable Universe as a function of time and distance, in context of the expanding Universe.
Both popular and professional research articles in cosmology often use the term "universe" to mean "observable universe".[citation needed] This can be justified on the grounds that we can never know anything by direct observation about any part of the universe that iscausally disconnected from the Earth, although many credible theories require a total universe much larger than the observable universe.[citation needed] No evidence exists to suggest that the boundary of the observable universe constitutes a boundary on the universe as a whole, nor do any of the mainstream cosmological models propose that the universe has any physical boundary in the first place. However, some models propose it could be finite but unbounded,[note 3] like a higher-dimensional analogue of the 2D surface of a sphere that is finite in area but has no edge.
It is plausible that thegalaxies within the observable universe represent only a minuscule fraction of the galaxies in the universe. According to the theory ofcosmic inflation initially introduced byAlan Guth andD. Kazanas,[22] if it is assumed that inflation began about 10−37 seconds after the Big Bang and that the pre-inflation size of the universe was approximately equal to the speed of light times its age, that would suggest that at present the entire universe's size is at least1.5×1034 light-years — this is at least3×1023 times the radius of the observable universe.[23]
If the universe is finite but unbounded, it is also possible that the universe issmaller than the observable universe. In this case, what we take to be very distant galaxies may actually be duplicate images of nearby galaxies, formed by light that has circumnavigated the universe. It is difficult to test this hypothesis experimentally because different images of a galaxy would show different eras in its history, and consequently might appear quite different. Bielewicz et al.[24] claim to establish a lower bound of 27.9 gigaparsecs (91 billion light-years) on the diameter of the last scattering surface. This value is based on matching-circle analysis of theWMAP 7-year data. This approach has been disputed.[25]
Hubble Ultra-Deep Field image of a region of the observable universe (equivalent sky area size shown in bottom left corner), near theconstellation Fornax. Each spot is agalaxy, consisting of billions of stars. The light from the smallest, mostredshifted galaxies originated around 12.6 billion years ago,[26] close to theage of the universe.
Thecomoving distance from Earth to the edge of the observable universe is about 14.26 gigaparsecs (46.5 billionlight-years or 4.40×1026 m) in any direction.[27]: 2 The observable universe is thus a sphere with a diameter of about 28.5 gigaparsecs[28] (93 billion light-years or 8.8×1026 m).[29] Assuming that space is roughlyflat (in the sense of being aEuclidean space), this size corresponds to a comoving volume of about1.22×104 Gpc3 (4.22×105 Gly3 or3.57×1080 m3).[30]
These are distances now (incosmological time), not distances at the time the light was emitted. For example, the cosmic microwave background radiation that we see right now was emitted at thetime of photon decoupling, estimated to have occurred about380,000 years after the Big Bang,[31][32] which occurred around 13.8 billion years ago. This radiation was emitted by matter that has, in the intervening time, mostly condensed into galaxies, and those galaxies are now calculated to be about 46 billion light-years from Earth.[7][9] To estimate the distance to that matter at the time the light was emitted, we may first note that according to theFriedmann–Lemaître–Robertson–Walker metric, which is used to model the expanding universe, if we receive light with aredshift ofz, then thescale factor at the time the light was originally emitted is given by[33][34]
.
WMAP nine-year results combined with other measurements give the redshift of photon decoupling asz = 1091.64±0.47,[35] which implies that the scale factor at the time of photondecoupling would be1⁄1092.64. So if the matter that originally emitted the oldest CMBRphotons has a present distance of 46 billion light-years, then the distance would have been only about 42 million light-years at the time of decoupling.
Thelight-travel distance to the edge of the observable universe is theage of the universe times thespeed of light, 13.8 billion light years. This is the distance that a photon emitted shortly after the Big Bang, such as one from thecosmic microwave background, has traveled to reach observers on Earth. Becausespacetime is curved, corresponding to theexpansion of space, this distance does not correspond to the true distance at any moment in time.[36]
The observable universe contains as many as an estimated 2 trillion galaxies[37][38][39] and, overall, as many as an estimated 1024 stars[40][41] – more stars (and, potentially, Earth-like planets) than all thegrains of beach sand on planet Earth.[42][43][44] Other estimates are in the hundreds of billions rather than trillions.[45][46][47] If the model ofcosmic inflation is correct and the universe expanded by >60 e-folds, then the universe could contain over 10100 stars.[48]
Assuming the mass of ordinary matter is about1.45×1053 kg as discussed above, and assuming all atoms arehydrogen atoms (which are about 74% of all atoms in the Milky Way by mass), the estimated total number of atoms in the observable universe is obtained by dividing the mass of ordinary matter by the mass of a hydrogen atom. The result is approximately 1080 hydrogen atoms, also known as theEddington number.[49]
The mass of the observable universe is often quoted as 1053 kg.[50] In this context, mass refers to ordinary (baryonic) matter and includes theinterstellar medium (ISM) and theintergalactic medium (IGM). However, it excludesdark matter anddark energy. This quoted value for the mass of ordinary matter in the universe can be estimated based on critical density. The calculations are for the observable universe only as the volume of the whole is unknown and may be infinite.
Critical density is the energy density for which the universe is flat.[51] If there is no dark energy, it is also thedensity for which the expansion of the universe is poised between continued expansion and collapse.[52] From theFriedmann equations, the value for critical density, is:[53]
whereG is thegravitational constant andH =H0 is the present value of theHubble constant. The value forH0, as given by the European Space Agency's Planck Telescope, isH0 = 67.15 kilometres per second per megaparsec. This gives a critical density of0.85×10−26 kg/m3, or about 5 hydrogen atoms per cubic metre. This density includes four significant types of energy/mass: ordinary matter (4.8%), neutrinos (0.1%),cold dark matter (26.8%), anddark energy (68.3%).[54]
Although neutrinos areStandard Model particles, they are listed separately because they areultra-relativistic and hencebehave like radiation rather than like matter. The density of ordinary matter, as measured by Planck, is 4.8% of the total critical density or4.08×10−28 kg/m3. To convert this density to mass we must multiply by volume, a value based on the radius of the "observable universe". Since the universe has been expanding for 13.8 billion years, thecomoving distance (radius) is now about 46.6 billion light-years. Thus, volume (4/3πr3) equals3.58×1080 m3 and the mass of ordinary matter equals density (4.08×10−28 kg/m3) times volume (3.58×1080 m3) or1.46×1053 kg.
Computer simulated image of an area of space more than 50 million light-years across, presenting a possible large-scale distribution of light sources in the universe—precise relative contributions of galaxies andquasars are unclear.
Thelarge-scale structure of the universe is the term incosmology for the character of matter distribution at the scale of the entireobservable universe.Sky surveys and mappings of the variouswavelength bands ofelectromagnetic radiation (in particular21-cm emission) have yielded much information on the content and character of theuniverse's structure. The organization of structure appears to follow ahierarchical model with organization up to thescale ofsuperclusters andfilaments. Larger than this (at scales between 30 and 200 megaparsecs),[55] there seems to be no continued structure, a phenomenon that has been referred to as theEnd of Greatness.[56] The shape of the large scale structure can be summarized by thematter power spectrum.
The most distantastronomical object identified is a galaxy classified asMoM-z14,[57] at a redshift of 14.44. In 2009, agamma ray burst,GRB 090423, was found to have aredshift of 8.2, which indicates that the collapsing star that caused it exploded when the universe was only 630 million years old.[58] The burst happened approximately 13 billion years ago,[59] so a distance of about 13 billion light-years was widely quoted in the media, or sometimes a more precise figure of 13.035 billion light-years.[58]
This would be the "light travel distance" (seeDistance measures (cosmology)) rather than the "proper distance" used in bothHubble's law and in defining the size of the observable universe. CosmologistNed Wright argues against using this measure.[60] The proper distance for a redshift of 8.2 would be about 9.2Gpc,[61] or about 30 billion light-years.
The limit of observability in the universe is set by cosmological horizons which limit—based on various physical constraints—the extent to which information can be obtained about various events in the universe. The most famous horizon is theparticle horizon which sets a limit on the precise distance that can be seen due to the finiteage of the universe. Additional horizons are associated with the possible future extent of observations, larger than the particle horizon owing to theexpansion of space, an "optical horizon" at thesurface of last scattering, and associated horizons with the surface of last scattering forneutrinos andgravitational waves.
^Special relativity prevents nearby objects in the same local region from moving faster than the speed of light with respect to each other, but there is no such constraint for distant objects when the space between them is expanding; seeuses of the proper distance for a discussion.
^The comoving distance of the future visibility limit is calculated on p. 8 of Gott et al.'sA Map of the Universe to be 4.50 times theHubble radius, given as 4.220 billion parsecs (13.76 billion light-years), whereas the current comoving radius of the observable universe is calculated on p. 7 to be 3.38 times the Hubble radius. The number of galaxies in a sphere of a given comoving radius is proportional to the cube of the radius, so as shown on p. 8 the ratio between the number of galaxies observable in the future visibility limit to the number of galaxies observable today would be (4.50/3.38)3 = 2.36.
^This does not mean "unbounded" in the mathematical sense; a finite universe would have an upper bound on the distance between two points. Rather, it means that there is no boundary past which there is nothing. SeeGeodesic manifold.
^Using Tiny Particles To Answer Giant Questions. Science Friday, 3 Apr 2009. According to thetranscript,Brian Greene makes the comment "And actually, in the far future, everything we now see, except for our local galaxy and a region of galaxies will have disappeared. The entire universe will disappear before our very eyes, and it's one of my arguments for actually funding cosmology. We've got to do it while we have a chance."
^Bielewicz, P.; Banday, A. J.; Gorski, K. M. (2013). Auge, E.; Dumarchez, J.; Tran Thanh Van, J. (eds.). "Constraints on the Topology of the Universe".Proceedings of the XLVIIth Rencontres de Moriond.2012 (91).arXiv:1303.4004.Bibcode:2013arXiv1303.4004B.
^Mota, B.; Reboucas, M. J.; Tavakol, R. (1 July 2010). "Observable circles-in-the-sky in flat universes".arXiv:1007.3466 [astro-ph.CO].
^Lauer, T. R.; Postman, M.; Spencer, J. R.; Weaver, H. A.; Stern, S. A.; Gladstone, G. R.; Binzel, R. P.; Britt, D. T.; Buie, M. W.; Buratti, B. J.; Cheng, A. F.; Grundy, W. M.; Horányi, M.; Kavelaars, J. J.; Linscott, I. R.; Lisse, C. M.; McKinnon, W. B.; McNutt, R. L.; Moore, J. M.; Núñez, J. I.; Olkin, C. B.; Parker, J. W.; Porter, S. B.; Reuter, D. C.; Robbins, S. J.; Schenk, P. M.; Showalter, M. R.; Singer, K. N.; Verbiscer, A. J.; Young, L. A. (2022)."Anomalous Flux in the Cosmic Optical Background Detected with New Horizons Observations".The Astrophysical Journal Letters.927 (1): L8.arXiv:2202.04273.Bibcode:2022ApJ...927L...8L.doi:10.3847/2041-8213/ac573d.
^Lauer, Tod R.; Postman, Marc; Weaver, Harold A.; Spencer, John R.; Stern, S. Alan; Buie, Marc W.; Durda, Daniel D.; Lisse, Carey M.; Poppe, A. R.; Binzel, Richard P.; Britt, Daniel T.; Buratti, Bonnie J.; Cheng, Andrew F.; Grundy, W. M.; Horányi, Mihaly; Kavelaars, J. J.; Linscott, Ivan R.; McKinnon, William B.; Moore, Jeffrey M.; Núñez, J. I.; Olkin, Catherine B.; Parker, Joel W.; Porter, Simon B.; Reuter, Dennis C.; Robbins, Stuart J.; Schenk, Paul; Showalter, Mark R.; Singer, Kelsi N.; Verbiscer, Anne J.; Young, Leslie A. (11 January 2021)."New Horizons Observations of the Cosmic Optical Background".The Astrophysical Journal.906 (2): 77.arXiv:2011.03052.Bibcode:2021ApJ...906...77L.doi:10.3847/1538-4357/abc881.hdl:1721.1/133770.S2CID226277978.
^Meszaros, Attila; et al. (2009). "Impact on cosmology of the celestial anisotropy of the short gamma-ray bursts".Baltic Astronomy.18:293–296.arXiv:1005.1558.Bibcode:2009BaltA..18..293M.
The Universe Within 14 Billion Light Years – NASA Atlas of the Universe – Note, this map only gives a rough cosmographical estimate of the expected distribution of superclusters within the observable universe; very little actual mapping has been done beyond a distance of one billion light-years.
