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We conclude that the residual signature is due either to a diffuse extragalactic background of emission from discrete radio sources with properties somewhat different than the faint end of the distribution of known sources or to unmodeled residual emission from our own Galaxy. Although we believe the
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In 2011, the ARCADE 2 researchers reported, "Correcting for instrumental systematic errors in measurements such as ARCADE 2 is always a primary concern. We emphasize that we detect residual emission at 3 GHz with the ARCADE 2 data, but the result is also independently detected by a combination of
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instrument package intended to measure the heating of the universe by the first stars and galaxies after the big bang and search for the signal of relic decay or annihilation. In July 2006 a strong residual radio source was found using the radiometer, approximately six times what is predicted by
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pumps in order to drench the radiometers in liquid helium. The design also utilized heaters in order to create a cloud of helium gas, in place of using a (relatively warm) window, which also simplified processing of the observational data.
221:, with the intent to measure temperature differences as small as 1/1000 of a degree against a background which is only 3 K (−270.15 °C; −454.27 °F). The optics in the instrument package were placed near the top of the
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has been used to indicate the hypothesis that the ARCADE 2 results indicate that the actual faint end of the emission distribution of known sources is significantly different from the expected value predicted by the
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Kogut, A.; Fixsen, D; Fixsen, S; Levin, S; Limon, M; Lowe, L; Mirel, P; Seiffert, M; Singal, J; Lubin, P; Wollack, E (December 2006). "ARCADE: Absolute radiometer for cosmology, astrophysics, and diffuse emission".
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which cooled them in order to prevent the instruments from seeing the walls of the container, thereby simplifying the processing of the observational data. This design choice necessitated the use of
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Seiffert, M.; Fixsen, D. J.; Kogut, A.; Levin, S. M.; Limon, M.; Lubin, P. M.; Mirel, P.; Singal, J.; Villela, T.; Wollack, E.; Wuensche, C. A. (10 June 2011).
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ARCADE viewed about 7% of the sky. The observed region is colored on this all-sky radio map. The plane of our galaxy, the Milky Way, runs across the center.
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The ARCADE 2 science team came to the following conclusion concerning the unexpected residual emission at 3 GHz:
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The instrument is designed to detect radiation at centimeter wavelengths. The craft contained seven
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Astronomy and
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which were cooled to 2.7 K (−270.45 °C; −454.81 °F) using
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Absolute
Radiometer for Cosmology, Astrophysics, and Diffuse Emission
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Absolute
Radiometer for Cosmology, Astrophysics, and Diffuse Emission
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former to be more likely, we cannot exclude the latter explanation.
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theory. This phenomenon is known as "space roar" and remains an
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have frequencies from 30 Hz to 300 GHz. The term
323:"NASA Balloon Mission Tunes in to a Cosmic Radio Mystery"
302:"NASA Balloon Mission Tunes in to a Cosmic Radio Mystery"
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277:List of cosmic microwave background experiments
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519:Cosmic microwave background radiation (CMB)
186:. The program is composed of a team led by
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905:Cosmic microwave background experiments
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202:, conducted under the auspices of the
282:Cosmic microwave background radiation
267:given the known sources of emission.
178:ARCADE has been funded by the NASA's
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196:Columbia Scientific Balloon Facility
321:Reddy, Francis (January 7, 2009).
194:. ARCADE was launched from NASA's
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417:Goddard Space Flight Center, NASA
399:Goddard Space Flight Center, NASA
165:unsolved problem in astrophysics
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158:) is a program which utilizes
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725:Arcminute Microkelvin Imager
900:Goddard Space Flight Center
800:Mobile Anisotropy Telescope
760:Cosmic Anisotropy Telescope
720:Atacama Cosmology Telescope
395:"ARCADE Instrument Summary"
373:10.1016/j.newar.2006.09.023
192:Goddard Space Flight Center
180:Science Mission Directorate
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530:Discovery of CMB radiation
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535:Timeline of CMB astronomy
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465:10.1088/0004-637x/734/1/6
442:The Astrophysical Journal
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910:Balloon-borne telescopes
890:Astronomical instruments
765:Cosmic Background Imager
571:Sunyaev–Zeldovich effect
133:Related media on Commons
239:low-frequency data and
208:Wallops Flight Facility
32:Arcade (disambiguation)
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204:Balloon Program Office
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52:Alternative names
413:"Stupid Dewar Tricks"
343:New Astronomy Reviews
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160:high-altitude balloon
845:South Pole Telescope
589:image (2018) of the
30:For other uses, see
745:BICEP (1,2,3,Array)
455:2011ApJ...734....6S
365:2006NewAR..50..925K
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885:2006 introductions
840:Simons Observatory
576:Thomson scattering
566:Sachs–Wolfe effect
349:(11–12): 925–931.
310:. January 7, 2009.
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27:NASA space program
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601:Experiments
256:Radio waves
223:dewar flask
215:radiometers
879:Categories
795:LSPE/STRIP
790:Keck Array
785:GroundBIRD
775:COSMOSOMAS
669:LSPE/SWIPE
288:References
260:space roar
227:superfluid
190:of NASA's
188:Alan Kogut
182:under the
85:2006
70:2001
18:Space roar
835:Saskatoon
810:POLARBEAR
664:BOOMERanG
855:Tenerife
654:Archeops
633:RELIKT-1
621:LiteBIRD
448:(1): 6.
381:18757986
271:See also
110:/archive
830:QUIJOTE
647:Balloon
585:4-year
544:Effects
450:Bibcode
361:Bibcode
112:/arcade
97:Website
755:CAPMAP
703:Ground
694:TopHat
689:Spider
679:MAXIMA
659:ARCADE
627:Planck
587:Planck
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156:ARCADE
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38:ARCADE
825:QUIET
820:QUBIC
770:CLASS
730:AMiBA
715:ACBAR
609:Space
438:(PDF)
377:S2CID
351:arXiv
241:FIRAS
140:[
106:.nasa
104:.gsfc
815:QUaD
805:OVRO
780:DASI
750:BIMA
740:ATCA
735:APEX
684:QMAP
674:EBEX
638:WMAP
616:COBE
327:NASA
307:NASA
108:.gov
850:SZA
710:ABS
591:CMB
460:doi
446:734
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243:."
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