We 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 deg2 of the southern sky, in a 4. ◦ 2 wide strip centered on declination 53◦ 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 < < 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 ∼ 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 σ8 = 0.8. We constrain the model’s amplitude ASZ < 1.63 (95% CL). If interpreted as a measurement of σ8, this implies σSZ 8 < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter ΛCDM model plus point sources and the SZ effect is consistent with these results.
The Atacama Cosmology Telescope: A Measurement of the 600 gt ell gt 8000 Cosmic Microwave Background Power Spectrum at 148 GHz / FOWLER J., W; Acquaviva, V; ADE P., A; R, ; Aguirre, P; Amiri, M; APPEL J., W; BARRIENTOS L., F; Battistelli, Elia Stefano; BOND J., R; Brown, B; Burger, B; Chervenak, J; Das, S; DEVLIN M., J; DICKER S., R; DORIESE W., B; Dunkley, J; Dünner, R; ESSINGER HILEMAN, T; FISHER R., P; Hajian, A; Halpern, M; Hasselfield, M; HERNÁNDEZ MONTEAGUDO, C; HILTON G., C; Hilton, M; HINCKS A., D; Hlozek, R; HUFFENBERGER K., M; HUGHES D., H; HUGHES J., P; Infante, L; IRWIN K., D; Jimenez, R; JUIN J., B; Kaul, M; Klein, J; Kosowsky, A; LAU J., M; Limon, M; LIN Y., T; LUPTON R., H; MARRIAGE T., A; Marsden, D; Martocci, K; Mauskopf, P; Menanteau, F; Moodley, K; Moseley, H; NETTERFIELD C., B; NIEMACK M., D; NOLTA M., R; PAGE L., A; Parker, L; Partridge, B; Quintana, H; Reid, B; Sehgal, N; Sievers, J; SPERGEL D., N; STAGGS S., T; SWETZ D., S; SWITZER E., R; Thornton, R; Trac, H; Tucker, C; Verde, L; Warne, R; Wilson, G; Wollack, E; Zhao, Y.. - In: THE ASTROPHYSICAL JOURNAL. - ISSN 0004-637X. - 722:(2010), pp. 1148-1161. [10.1088/0004-637X/722/2/1148]
The Atacama Cosmology Telescope: A Measurement of the 600 gt ell gt 8000 Cosmic Microwave Background Power Spectrum at 148 GHz
BATTISTELLI, Elia Stefano;
2010
Abstract
We 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 deg2 of the southern sky, in a 4. ◦ 2 wide strip centered on declination 53◦ 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 < < 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 ∼ 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 σ8 = 0.8. We constrain the model’s amplitude ASZ < 1.63 (95% CL). If interpreted as a measurement of σ8, this implies σSZ 8 < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter ΛCDM model plus point sources and the SZ effect is consistent with these results.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
