1118:
963:. The detection of fluctuations is easier than the direct CIB measurements, since one does not need to determine the absolute photometric zero point ā fluctuations can be derived from differential measurements. On the other hand, fluctuations do not provide an immediate information on the CIB brightness. The measured fluctuation amplitudes either has to be confronted with a CIB model that has a prediction for the fluctuation / absolute level ratio, or it has to be compared with integrated differential light levels of
665:, early galaxies must have been significantly more powerful than they are today. In the early CIB models the absorption of starlight was neglected, therefore in these models the CIB peaked between 1ā10Ī¼m wavelengths. These early models have already shown correctly that the CIB was most probably fainter than its foregrounds, and so it was very difficult to observe. Later the discovery and observations of high luminosity infrared galaxies in the vicinity of the
559:
36:
1052:, and Ī± is the spectral index. Ī± was found to be Ī±ā-3, which is much steeper than the power spectrum of the CIB at low spatial frequencies. The cirrus component can be identified in the power spectrum at low spatial frequencies and then removed from the whole spatial frequency range. The remaining power spectrum ā after a careful correction for instrument effects ā should be that of the CIB.
571:
1132:
951:
Since the CIB is an accumulated light of individual sources there is always a somewhat different number of sources in different directions in the field of view of the observer. This cause a variation (fluctuation) in the total amount of observed incoming flux among the different line of sights. These
641:
dates back to the first half of the 19th century. Despite its importance, the first attempts were made only in the 1950-60s to derive the value of the visual background due to galaxies, at that time based on the integrated starlight of these stellar systems. In the 1960s the absorption of starlight
936:
densities, since they originate from the same, low-density structure. After the removal of the HI-correlated part, the remaining surface brightness was identified as the cosmic infrared background at 60, 100, 140, and 240Ī¼m. At shorter wavelengths the CIB level could not be correctly determined.
911:
component. The measurement has to be repeated in many directions to determine the contribution of the foregrounds. After the removal of all other components the remaining power ā if it is the same constant value in any direction ā is the CIB at that specific wavelength. In practice, one needs an
898:
The detection of the CIB is both observationally and astrophysically very challenging. It has a very few characteristics which can be used to separate it from the foregrounds. One major point is, that the CIB must be isotropic, i.e. one has to measure the same CIB value all over the sky. It also
1105:
Source count results support the "fast evolution" galaxy models. In these models galaxies nowadays look significantly different than they were at z=1...2, when they were coming through an intense star-formation phase. The source count results exclude the "steady state" scenarios, where z=1...2
935:
contribution (which was based on the measured annual variation) the remaining power at longer infrared wavelength contained basically two components: the CIB and the
Galactic cirrus emission. The infrared surface brightness of the Galactic cirrus must correlate with the neutral hydrogen column
1078:
one tries to detect as many point/compact sources in a certain field of view as possible: this is usually done at multiple wavelengths and is often complemented by other data, e.g. photometry at visual or sub-millimeter wavelengths. In this way, one has information on the broad band spectral
765:
period: they are just in a collision or in a merge with another galaxy. In the optical this is hidden by the huge amount of dust, and the galaxy is bright in the infrared due to the same reason. Galaxy collisions and mergers were more frequent in the cosmic past: the global
1079:
characteristics of the detected sources, too. The detected point sources have to be distinguished from other contaminating sources, e.g. minor bodies in the Solar System, Galactic stars and cirrus knots (local density enhancements in the
Galactic cirrus emission).
1098:). While ISO was able to resolve about 3ā10% of the total CIB light into individual sources (depending on the wavelength), Spitzer measurements have already detected ~30% of the CIB as sources, and this ratio is expected to be ~90% at some wavelengths with the
744:
of the galaxies found in our cosmic neighborhood. However, these simple models could not reproduce the observed features of the CIB. In the baryonic material of the
Universe there are two sources of large amounts of energy: nuclear fusion and gravitation.
752:. However, a significant amount of this starlight is not observed directly. Dust in the host galaxies can absorb it and re-emit it in the infrared, contributing to the CIB. Although most of today's galaxies contain little dust (e.g.
970:
The power spectrum of the CIB is usually presented in a spatial frequency vs. fluctuation power diagram. It is contaminated by the presence of the power spectrum of foreground components, so that the total power spectrum is:
1013:
In the far-infrared the CIB power spectrum can be effectively used to separate it from its strongest foreground, the
Galactic cirrus emission. The cirrus emission has a characteristic power spectrum of a power-law (that of a
815:. If intergalactic stars were to account for all of the background anisotropy, it would require a very large population, but this is not excluded by observations and could in fact also explain a fair part of the
756:
are practically dustless), there are some special stellar systems even in our vicinity which are extremely bright in the infrared and at the same time faint (often almost invisible) in the optical. These
804:. This absorbed light is again re-emitted in the infrared, and in total gives about 20ā30% of the full power of the CIB; however at some specific wavelengths this is the dominant source of CIB energy.
703:
In the early 1980s there were only upper limits available for the CIB. The real observations of the CIB began after the era of astronomical satellites working in the infrared, started by the
160:
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688:, which are very bright in the infrared. He also pointed out, that the CIB cause a significant attenuation for very high energy electrons, protons and gamma-rays of the
886:- although physically it is not a "foreground" - is also considered as an important contaminating source of emission at very long infrared wavelengths (Ī»>300Ī¼m)
601:
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lacks suspicious spectral features, since the final shape of its spectrum is the sum of the spectra of sources in the line of sight at various redshifts.
812:
1419:
G. Lagache; et al. (2007). "Correlated anisotropies in the cosmic far-infrared background detected by MIPS/Spitzer: Constraint on the bias".
924:
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907:
Direct measurements are simple, but very difficult. One just has to measure the total incoming power, and determine the contribution of each
1637:
1297:
Cooray; et al. (22 October 2012). "A measurement of the intrahalo light fraction with near-infrared background anisotropies". Nature.
335:
920:). Since the instrument parts, including the shutter, have non-zero temperatures and emit in the infrared, this is a very difficult task.
999:, zodiacal emission and noise (instrument noise) power spectrum components, respectively, and Ī¦ is the power spectrum of the telescope's
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A summary on the history of CIB research can be found in the review papers by M.G. Hauser and E. Dwek (2001) and A. Kashlinsky (2005).
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showed, that the peak of the CIB is most likely at longer wavelengths (around 50Ī¼m), and its full power could be ~1ā10% of that of the
544:
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Cs. Kiss; et al. (2001). "Sky confusion noise in the far-infrared: Cirrus, galaxies and the cosmic far-infrared background".
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One of the most important questions about the CIB is the source of its energy. In the early models the CIB was built up from the
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Autocorrelation and power spectrum studies resulted in the CIB fluctuation amplitudes at 1.25, 2.2, 3.5, 12ā100Ī¼m based on the
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Zemcov; et al. (5 November 2014). "On the Origin of Near-Infrared
Extragalactic Background Light Anisotropy". Nature.
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105:
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Nuclear fusion takes place inside the stars, and we can really see this light redshifted: this is the main source of the
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1063:. Recently, the clustering of the galaxies have also been identified in the power spectrum at 160Ī¼m using this method.
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P. ĆbrahĆ”m; et al. (1997). "Search for brightness fluctuations in the zodiacal light at 25 MU M with ISO".
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by dust was already taken into account, but without considering the re-emission of this absorbed energy in the
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For most of the infrared zodiacal emission fluctuation are negligible in the "cosmic windows", far from the
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1059:/DIRBE measurements, and later at 90 and 170Ī¼m, based on the observations of the ISOPHOT instrument of the
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H. Dole; et al. (2004). "Far-infrared Source Counts at 70 and 160 Microns in
Spitzer Deep Surveys".
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Later, short-wavelength DIRBE measurements at 2.2 and 3.5Ī¼ were combined with the Two Micron Sky Survey (
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emphasized, the CIB is very important in the understanding of some special astronomical objects, like
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916:, i.e. it has some mechanism to fully block incoming light for an accurate zero level determination (
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M.G. Hauser & E. Dwek (2001). "The Cosmic
Infrared Background: Measurements and Implications".
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654:-created Universe, there must have been a cosmic infrared background (CIB) ā different from the
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943:) source count data, and this led to the detection of the CIB at these two wavelengths.
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The first, and still the most extensive, direct CIB measurements were performed by the
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A. Kashlinsky (2005). "Cosmic infrared background and early galaxy evolution".
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gives the most extensive picture about the sources building up the CIB. In a
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658:ā that can account for the formation and evolution of stars and galaxies.
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Recognizing the cosmological importance of the darkness of the night sky (
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Source counts were important tasks for the recent infrared missions like
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galaxies look similar to those we see today in our cosmic neighborhood.
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have been shown to explain the CIB as well as the other elements of the
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The most important foreground components of the CIB are the following:
800:, which would escape unless they are absorbed by the dust torus of the
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1527:"Modeling infrared galaxy evolution using a phenomenological approach"
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The
Spitzer wide area surveys have detected anisotropies in the CIB.
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Another important component of the CIB is the infrared emission by
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Astronomers
Discover an Infrared Background Glow in the Universe
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fluctuations are traditionally described by the two dimensional
862:
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These components must be separated for a clear CIB detection.
670:
1045:
is the fluctuation power at the reference spatial frequency
834:: the thermal emission of microscopic dust particles in the
931:
satellite. After the removal of the precisely determined
1602:
TeV Blazars and Cosmic
Infrared Background Radiation
1034:is the fluctuation power at the spatial frequency
1532:Monthly Notices of the Royal Astronomical Society
1176:"NASA spots glow of universe's first objects."
719:. Exploration of the CIB was continued by the
1193:Annual Review of Astronomy & Astrophysics
894:Observation of the cosmic infrared background
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813:diffuse extragalactic background radiation
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750:cosmic ultraviolet- and visual background
16:Infrared radiation caused by stellar dust
733:Origin of the cosmic infrared background
1474:Astrophysical Journal Supplement Series
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792:of the matter falling into the central
700:and electron-positron pair production.
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205:
97:
26:
807:A hitherto unrecognised population of
7:
1590:Cosmic InfraRed Background Radiation
912:instrument that is able to perform
761:(ULIRGs) are just in a very active
637:) and the first speculations on an
330:2dF Galaxy Redshift Survey ("2dF")
14:
545:Timeline of cosmological theories
310:Cosmic Background Explorer (COBE)
1564:10.1046/j.1365-8711.2003.05971.x
1525:G. Lagache; et al. (2003).
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1614:, Release Number: STScI-1998-01
788:. In these systems most of the
759:ultraluminous infrared galaxies
686:ultraluminous infrared galaxies
325:Sloan Digital Sky Survey (SDSS)
178:Future of an expanding universe
1223:10.1146/annurev.astro.39.1.249
790:gravitational potential energy
770:of the Universe peaked around
639:extragalactic background light
540:History of the Big Bang theory
336:Wilkinson Microwave Anisotropy
1:
1276:10.1016/j.physrep.2004.12.005
532:Discovery of cosmic microwave
183:Ultimate fate of the universe
1368:Astronomy & Astrophysics
1341:Astronomy & Astrophysics
849:(from near- to mid-infrared)
838:(from near- to mid-infrared)
707:(IRAS), and followed by the
705:Infrared Astronomy Satellite
661:In order to produce today's
1638:Cosmic background radiation
1151:Cosmic microwave background
884:cosmic microwave background
656:cosmic microwave background
615:Cosmic infrared background
300:Black Hole Initiative (BHI)
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1398:10.1051/0004-6361:20011394
1100:Herschel Space Observatory
1096:Herschel Space Observatory
1088:Infrared Space Observatory
1061:Infrared Space Observatory
956:, or by the corresponding
841:Thermal emission of small
721:Herschel Space Observatory
713:Infrared Space Observatory
709:Cosmic Background Explorer
63:Chronology of the universe
156:Expansion of the universe
995:(f) are the total, CIB,
967:at the same wavelength.
954:autocorrelation function
853:Galactic cirrus emission
320:Planck space observatory
106:Gravitational wave (GWB)
1628:Observational astronomy
1390:2001A&A...379.1161K
1353:1997A&A...328..702A
1215:2001ARA&A..39..249H
1156:Cosmic X-ray background
1092:Spitzer Space Telescope
717:Spitzer Space Telescope
650:pointed out that, in a
173:Inhomogeneous cosmology
1421:Astrophysical Journal
1001:point spread function
872:Infrared emission of
264:Large-scale structure
242:Shape of the universe
723:, launched in 2009.
621:radiation caused by
576:Astronomy portal
534:background radiation
511:List of cosmologists
1555:2003MNRAS.338..555L
1496:2004ApJS..154...87D
1443:2007ApJ...665L..89L
1268:2005PhR...409..361K
1018:spatial structure)
947:Fluctuation studies
914:absolute photometry
809:intergalactic stars
768:star formation rate
754:elliptical galaxies
276:Structure formation
168:Friedmann equations
58:Age of the universe
22:Part of a series on
1633:Physical cosmology
927:instrument of the
796:is converted into
694:Compton scattering
315:Dark Energy Survey
259:Large quasar group
28:Physical cosmology
933:zodiacal emission
874:intracluster dust
832:Zodiacal emission
819:problem as well.
715:(ISO) and by the
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1181:, June 8, 2012.
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1622:Categories
1162:References
794:black hole
739:redshifted
373:Copernicus
351:Scientists
206:Components
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1551:Bibcode
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786:quasars
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629:History
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863:stars
478:Smoot
468:Rubin
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398:Ellis
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1057:COBE
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882:The
617:is
418:Guth
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