1704:
570:
47:
582:
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Luminous Red Galaxy catalog. Their ISW detection traces the localised ISW effect produced by supervoids and superclusters have on the CMB. However, the amplitude of this localised detection is controversial, as it is significantly larger than the expectations and depends on several assumptions of
760:
to travel through them. A photon gets a kick of energy going into a potential well (a supercluster), and it keeps some of that energy after it exits, after the well has been stretched out and shallowed. Similarly, a photon has to expend energy entering a supervoid, but will not get all of it back
701:
around to affect the
Universe's expansion. Although it is physically the same as the late-time ISW, for observational purposes it is usually lumped in with the primordial CMB, since the matter fluctuations that cause it are in practice undetectable.
768:
between the galaxy density (the number of galaxies per square degree) and the temperature of the CMB, because superclusters gently heat photons, while supervoids gently cool them. This correlation has been detected at moderate to high significance.
696:
There are two contributions to the ISW effect. The "early-time" ISW occurs immediately after the (non-integrated) Sachs–Wolfe effect produces the primordial CMB, as photons course through density fluctuations while there is still enough
1612:
718:, starts to govern the Universe's expansion. Unfortunately, the nomenclature is a bit confusing. Often, "late-time ISW" implicitly refers to the late-time ISW effect to
171:
947:
Fosalba, P.; et al. (2003). "Detection of the
Integrated Sachs–Wolfe and Sunyaev–Zeldovich Effects from the Cosmic Microwave Background-Galaxy Correlation".
645:, causing the CMB spectrum to appear uneven. This effect is the predominant source of fluctuations in the CMB for angular scales larger than about ten degrees.
1327:
1194:
Granett, B. R.; Neyrinck, M. C.; Szapudi, I. (2008). "An
Imprint of Superstructures on the Microwave Background due to the Integrated Sachs–Wolfe Effect".
1347:
542:
1352:
1139:
772:
In May 2008, Granett, Neyrinck & Szapudi showed that the late-time ISW can be pinned to discrete supervoids and superclusters identified in the
791:
1418:
1019:
Ho, S.; et al. (2008). "Correlation of CMB with large-scale structure. I. Integrated Sachs–Wolfe tomography and cosmological implications".
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665:
The integrated Sachs–Wolfe (ISW) effect is also caused by gravitational redshift, but it occurs between the surface of last scattering and the
1532:
612:
1320:
730:(linear + higher-order) late-time ISW effect, especially in the case of individual voids and clusters, is sometimes known as the
1587:
1567:
810:
Sachs, R. K.; Wolfe, A. M. (1967). "Perturbations of a
Cosmological Model and Angular Variations of the Microwave Background".
17:
1074:
Giannantonio, T.; et al. (2008). "Combined analysis of the integrated Sachs–Wolfe effect and cosmological implications".
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1408:
677:
is dominated in its energy density by something other than matter. If the
Universe is dominated by matter, then large-scale
638:
657:. The effect is not constant across the sky due to differences in the matter/energy density at the time of last scattering.
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1313:
346:
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1253:
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with only matter, but dominates over the higher-order part of the effect in a universe with dark energy. The full
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574:
121:
892:
Crittenden, R. G.; Turok, N. (1996). "Looking for a
Cosmological Constant with the Rees–Sciama Effect".
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The non-integrated Sachs–Wolfe effect is caused by gravitational redshift occurring at the
521:
493:
315:
847:
Rees, M. J.; Sciama, D. W. (1968). "Large-scale
Density Inhomogeneities in the Universe".
8:
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1131:"A reassessment of the evidence of the Integrated Sachs–Wolfe effect through the
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in density perturbations. This linear part of the effect entirely vanishes in a
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154:
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wells and hills do not evolve significantly. If the
Universe is dominated by
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1300:"Dark Energy and the Imprint of Super-Structures on the Microwave Background"
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The "late-time" ISW effect arises quite recently in cosmic history, as
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428:
689:, though, those potentials do evolve, subtly changing the energy of
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due to dark energy causes even strong large-scale potential wells (
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A signature of the late-time ISW is a non-zero cross-
648:
761:upon exiting the slightly reduced potential hill.
1140:Monthly Notices of the Royal Astronomical Society
1728:
792:Cosmic microwave background spectral distortions
660:
1302:, a webpage by Granett, Neyrinck & Szapudi.
891:
1321:
1263:Sachs–Wolfe effect in some anisotropic models
998:(2003). "Physical Evidence for Dark Energy".
606:
1073:
1337:Cosmic microwave background radiation (CMB)
742:elucidated the following physical picture.
1328:
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1128:
846:
809:
613:
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45:
1209:
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1089:
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641:(CMB), in which photons from the CMB are
1273:
946:
706:Late-time integrated Sachs–Wolfe effect
14:
1729:
669:, so it is not part of the primordial
1309:
639:cosmic microwave background radiation
1260:Aguiar, Paulo, and Paulo Crawford,
1129:Raccanelli, A.; et al. (2008).
756:) to decay over the time it takes a
27:Phenomenon of redshift in cosmology
24:
1018:
341:2dF Galaxy Redshift Survey ("2dF")
25:
1748:
1274:White, Martin; Hu, Wayne (1997).
1254:The Integrated Sachs–Wolfe Effect
1245:
649:Non-integrated Sachs–Wolfe effect
556:Timeline of cosmological theories
321:Cosmic Background Explorer (COBE)
1714:
1702:
1172:10.1111/j.1365-2966.2008.13189.x
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336:Sloan Digital Sky Survey (SDSS)
189:Future of an expanding universe
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1012:
987:
940:
885:
840:
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679:gravitational potential energy
551:History of the Big Bang theory
347:Wilkinson Microwave Anisotropy
13:
1:
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661:Integrated Sachs–Wolfe effect
543:Discovery of cosmic microwave
194:Ultimate fate of the universe
1543:Arcminute Microkelvin Imager
1257:. University of Chicago, IL.
7:
1618:Mobile Anisotropy Telescope
1578:Cosmic Anisotropy Telescope
1538:Atacama Cosmology Telescope
996:et al. (SDSS collaboration)
780:
311:Black Hole Initiative (BHI)
10:
1753:
1348:Discovery of CMB radiation
1283:Astronomy and Astrophysics
1108:10.1103/PhysRevD.77.123520
1053:10.1103/PhysRevD.78.043519
926:10.1103/PhysRevLett.76.575
655:surface of last scattering
643:gravitationally redshifted
74:Chronology of the universe
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1464:
1426:
1417:
1400:
1361:
1353:Timeline of CMB astronomy
1343:
167:Expansion of the universe
1583:Cosmic Background Imager
1389:Sunyaev–Zeldovich effect
1276:"The Sachs–Wolfe effect"
787:Sunyaev–Zeldovich effect
331:Planck space observatory
117:Gravitational wave (GWB)
895:Physical Review Letters
637:, is a property of the
184:Inhomogeneous cosmology
693:passing through them.
673:. It occurs when the
1197:Astrophysical Journal
950:Astrophysical Journal
813:Astrophysical Journal
746:Accelerated expansion
716:cosmological constant
275:Large-scale structure
253:Shape of the universe
1663:South Pole Telescope
1407:image (2018) of the
766:correlation function
587:Astronomy portal
545:background radiation
522:List of cosmologists
1563:BICEP (1,2,3,Array)
1220:2008ApJ...683L..99G
1163:2008MNRAS.386.2161R
1100:2008PhRvD..77l3520G
1045:2008PhRvD..78d3519H
973:2003ApJ...597L..89F
918:1996PhRvL..76..575C
863:1968Natur.217..511R
826:1967ApJ...147...73S
287:Structure formation
179:Friedmann equations
69:Age of the universe
33:Part of a series on
1737:Physical cosmology
1658:Simons Observatory
1394:Thomson scattering
1384:Sachs–Wolfe effect
1294:Sachs–Wolfe effect
1135:–NVSS correlation"
732:Rees–Sciama effect
720:linear/first order
627:Sachs–Wolfe effect
326:Dark Energy Survey
270:Large quasar group
39:Physical cosmology
18:Rees–Sciama effect
1690:
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1374:Diffusion damping
1077:Physical Review D
1022:Physical Review D
857:(5128): 511–516.
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16:(Redirected from
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1147:(4): 2161–2166.
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1016:
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1005:astro-ph/0307335
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964:astro-ph/0307249
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1369:Cosmic variance
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1204:(2): L99–L102.
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631:Rainer K. Sachs
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994:Scranton, R.;
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981:10.1086/379848
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834:10.1086/148982
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349:Probe (WMAP)
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280:Reionization
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155:Hubble's law
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125:
97:
60:
1419:Experiments
736:Martin Rees
712:dark energy
687:dark energy
304:Experiments
237:Dark matter
230:Dark energy
172:FLRW metric
109:Backgrounds
1613:LSPE/STRIP
1608:Keck Array
1603:GroundBIRD
1593:COSMOSOMAS
1487:LSPE/SWIPE
957:(2): L89.
798:References
384:Copernicus
362:Scientists
217:Components
1653:Saskatoon
1628:POLARBEAR
1482:BOOMERanG
1211:0805.3695
1154:0802.0084
1091:0801.4380
1036:0801.0642
728:nonlinear
714:, or the
699:radiation
683:radiation
514:Zeldovich
414:Friedmann
389:de Sitter
316:BOOMERanG
245:Structure
210:Structure
94:Inflation
1731:Category
1673:Tenerife
1472:Archeops
1451:RELIKT-1
1439:LiteBIRD
1296:Level 5.
1236:15976818
1181:15054396
1116:21763795
1061:38383124
934:10061494
781:See also
734:, since
685:, or by
675:Universe
575:Category
494:Suntzeff
454:Lemaître
404:Einstein
369:Aaronson
162:Redshift
64:Universe
57:Big Bang
1709:Physics
1695:Portals
1648:QUIJOTE
1465:Balloon
1403:4-year
1362:Effects
1270:format)
1216:Bibcode
1159:Bibcode
1096:Bibcode
1041:Bibcode
969:Bibcode
914:Bibcode
879:4168044
859:Bibcode
822:Bibcode
691:photons
499:Sunyaev
484:Schmidt
474:Penzias
469:Penrose
444:Huygens
434:Hawking
419:Galileo
1573:CAPMAP
1521:Ground
1512:TopHat
1507:Spider
1497:MAXIMA
1477:ARCADE
1445:Planck
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820:: 73.
758:photon
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459:Mather
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439:Hubble
399:Ehlers
379:Alpher
374:Alfvén
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149:Future
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1721:Space
1643:QUIET
1638:QUBIC
1588:CLASS
1548:AMiBA
1533:ACBAR
1427:Space
1289:: 89.
1279:(PDF)
1232:S2CID
1206:arXiv
1177:S2CID
1149:arXiv
1112:S2CID
1086:arXiv
1057:S2CID
1031:arXiv
1000:arXiv
959:arXiv
904:arXiv
875:S2CID
754:voids
667:Earth
489:Smoot
479:Rubin
424:Gamow
409:Ellis
394:Dicke
1633:QUaD
1623:OVRO
1598:DASI
1568:BIMA
1558:ATCA
1553:APEX
1502:QMAP
1492:EBEX
1456:WMAP
1434:COBE
1133:WMAP
930:PMID
774:SDSS
738:and
633:and
625:The
429:Guth
1668:SZA
1528:ABS
1409:CMB
1287:321
1268:PDF
1266:. (
1224:doi
1202:683
1167:doi
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