The Atacama Cosmology Telescope: A Measurement of the 600 < ell < 8000 Cosmic Microwave Background Power Spectrum at 148 GHz

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dc.contributor.authorFowler, J. W.
dc.contributor.authorAcquaviva, V.
dc.contributor.authorAde, P. A. R.
dc.contributor.authorAguirre, P.
dc.contributor.authorAmiri, M.
dc.contributor.authorAppel, J. W.
dc.contributor.authorBarrientos, L. F.
dc.contributor.authorBattistelli, E. S.
dc.contributor.authorBond, J. R.
dc.contributor.authorBrown, B.
dc.contributor.authorBurger, B.
dc.contributor.authorChervenak, J.
dc.contributor.authorDas, S.
dc.contributor.authorDevlin, M. J.
dc.contributor.authorDicker, S. R.
dc.contributor.authorDoriese, W. B.
dc.contributor.authorDunkley, J.
dc.contributor.authorDünner, R.
dc.contributor.authorEssinger-Hileman, T.
dc.contributor.authorFisher, R. P.
dc.contributor.authorHajian, A.
dc.contributor.authorHalpern, M.
dc.contributor.authorHasselfield, M.
dc.contributor.authorHernández-Monteagudo, C.
dc.contributor.authorHilton, G. C.
dc.contributor.authorHilton, M.
dc.contributor.authorHincks, A. D.
dc.contributor.authorHlozek, R.
dc.contributor.authorHuffenberger, K. M.
dc.contributor.authorHughes, D. H.
dc.contributor.authorHughes, J. P.
dc.contributor.authorInfante, L.
dc.contributor.authorIrwin, K. D.
dc.contributor.authorJimenez, R.
dc.contributor.authorJuin, J. B.
dc.contributor.authorKaul, M.
dc.contributor.authorKlein, J.
dc.contributor.authorKosowsky, A.
dc.contributor.authorLau, J. M.
dc.contributor.authorLimon, M.
dc.contributor.authorLin, Y. -T.
dc.contributor.authorLupton, R. H.
dc.contributor.authorMarriage, T. A.
dc.contributor.authorMarsden, D.
dc.contributor.authorMartocci, K.
dc.contributor.authorMauskopf, P.
dc.contributor.authorMenanteau, F.
dc.contributor.authorMoodley, K.
dc.contributor.authorMoseley, H.
dc.contributor.authorNetterfield, C. B.
dc.contributor.authorNiemack, M. D.
dc.contributor.authorNolta, M. R.
dc.contributor.authorPage, L. A.
dc.contributor.authorParker, L.
dc.contributor.authorPartridge, B.
dc.contributor.authorQuintana, H.
dc.contributor.authorReid, B.
dc.contributor.authorSehgal, N.
dc.contributor.authorSievers, J.
dc.contributor.authorSpergel, D. N.
dc.contributor.authorStaggs, S. T.
dc.contributor.authorSwetz, D. S.
dc.contributor.authorSwitzer, E. R.
dc.contributor.authorThornton, R.
dc.contributor.authorTrac, H.
dc.contributor.authorTucker, C.
dc.contributor.authorVerde, L.
dc.contributor.authorWarne, R.
dc.contributor.authorWilson, G.
dc.contributor.authorWollack, E.
dc.contributor.authorZhao, Y.
dc.date.accessioned2023-05-19T20:25:09Z
dc.date.available2023-05-19T20:25:09Z
dc.date.issued2010
dc.description.abstractWe present a measurement of the angular power spectrum of the cosmic microwave background (CMB) radiation observed at 148 GHz. The measurement uses maps with 1'.4 angular resolution made with data from the Atacama Cosmology Telescope (ACT). The observations cover 228 deg(2) of the southern sky, in a 4 degrees.2 wide strip centered on declination 53 degrees south. The CMB at arcminute angular scales is particularly sensitive to the Silk damping scale, to the Sunyaev-Zel'dovich (SZ) effect from galaxy clusters, and to emission by radio sources and dusty galaxies. After masking the 108 brightest point sources in our maps, we estimate the power spectrum between 600 < l < 8000 using the adaptive multi-taper method to minimize spectral leakage and maximize use of the full data set. Our absolute calibration is based on observations of Uranus. To verify the calibration and test the fidelity of our map at large angular scales, we cross-correlate the ACT map to the WMAP map and recover the WMAP power spectrum from 250 < l < 1150. The power beyond the Silk damping tail of the CMB (l similar to 5000) is consistent with models of the emission from point sources. We quantify the contribution of SZ clusters to the power spectrum by fitting to a model normalized to sigma(8) = 0.8. We constrain the model's amplitude A(SZ) < 1.63 (95% CL). If interpreted as a measurement of sigma(8), this implies sigma(SZ)(8) < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter Lambda CDM model plus point sources and the SZ effect is consistent with these results.
dc.fuente.origenORCID-mayo23
dc.identifier.doi10.1088/0004-637X/722/2/1148
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/67296
dc.language.isoen
dc.rightsacceso restringido
dc.titleThe Atacama Cosmology Telescope: A Measurement of the 600 &lt; ell &lt; 8000 Cosmic Microwave Background Power Spectrum at 148 GHzes_ES
dc.typeartículo
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