The Atacama Cosmology Telescope

A measurement of the 600 < ℓ < 8000 cosmic microwave background power spectrum at 148 GHz

J. W. Fowler, V. Acquaviva, P. A R Ade, P. Aguirre, M. Amiri, J. W. Appel, L. F. Barrientos, E. S. Battistelli, J. R. Bond, B. Brown, B. Burger, J. Chervenak, S. Das, M. J. Devlin, S. R. Dicker, W. B. Doriese, J. Dunkley, R. Dünner, T. Essinger-Hileman, R. P. Fisher & 51 others A. Hajian, M. Halpern, M. Hasselfield, C. Hernández-Monteagudo, G. C. Hilton, M. Hilton, A. D. Hincks, R. Hlozek, K. M. Huffenberger, D. H. Hughes, J. P. Hughes, L. Infante, K. D. Irwin, R. Jimenez, J. B. Juin, M. Kaul, J. Klein, A. Kosowsky, J. M. Lau, M. Limon, Y. T. Lin, R. H. Lupton, T. A. Marriage, D. Marsden, K. Martocci, Philip Mauskopf, F. Menanteau, K. Moodley, H. Moseley, C. B. Netterfield, M. D. Niemack, M. R. Nolta, L. A. Page, L. Parker, B. Partridge, H. Quintana, B. Reid, N. Sehgal, J. Sievers, D. N. Spergel, S. T. Staggs, D. S. Swetz, E. R. Switzer, R. Thornton, H. Trac, C. Tucker, L. Verde, R. Warne, G. Wilson, E. Wollack, Y. Zhao

Research output: Contribution to journalArticle

101 Citations (Scopus)

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 < 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 ∼ 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 σ 8 = 0.8. We constrain the model's amplitude ASZ < 1.63 (95% CL). If interpreted as a measurement of σ 8, this implies σ 8 SZ < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter ACDM model plus point sources and the SZ effect is consistent with these results.

Original languageEnglish (US)
Pages (from-to)1148-1161
Number of pages14
JournalAstrophysical Journal
Volume722
Issue number2
DOIs
StatePublished - Oct 20 2010
Externally publishedYes

Fingerprint

cosmology
power spectra
telescopes
microwaves
point sources
point source
silk
damping
Southern sky
galaxies
calibration
Uranus (planet)
cosmic microwave background radiation
Uranus
declination
tapering
masking
angular resolution
leakage
strip

Keywords

  • Cosmic background radiation
  • Cosmology: observations

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Fowler, J. W., Acquaviva, V., Ade, P. A. R., Aguirre, P., Amiri, M., Appel, J. W., ... Zhao, Y. (2010). The Atacama Cosmology Telescope: A measurement of the 600 < ℓ < 8000 cosmic microwave background power spectrum at 148 GHz. Astrophysical Journal, 722(2), 1148-1161. https://doi.org/10.1088/0004-637X/722/2/1148

The Atacama Cosmology Telescope : A measurement of the 600 < ℓ < 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, E. S.; 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, Philip; 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: Astrophysical Journal, Vol. 722, No. 2, 20.10.2010, p. 1148-1161.

Research output: Contribution to journalArticle

Fowler, JW, Acquaviva, V, Ade, PAR, Aguirre, P, Amiri, M, Appel, JW, Barrientos, LF, Battistelli, ES, Bond, JR, Brown, B, Burger, B, Chervenak, J, Das, S, Devlin, MJ, Dicker, SR, Doriese, WB, Dunkley, J, Dünner, R, Essinger-Hileman, T, Fisher, RP, Hajian, A, Halpern, M, Hasselfield, M, Hernández-Monteagudo, C, Hilton, GC, Hilton, M, Hincks, AD, Hlozek, R, Huffenberger, KM, Hughes, DH, Hughes, JP, Infante, L, Irwin, KD, Jimenez, R, Juin, JB, Kaul, M, Klein, J, Kosowsky, A, Lau, JM, Limon, M, Lin, YT, Lupton, RH, Marriage, TA, Marsden, D, Martocci, K, Mauskopf, P, Menanteau, F, Moodley, K, Moseley, H, Netterfield, CB, Niemack, MD, Nolta, MR, Page, LA, Parker, L, Partridge, B, Quintana, H, Reid, B, Sehgal, N, Sievers, J, Spergel, DN, Staggs, ST, Swetz, DS, Switzer, ER, Thornton, R, Trac, H, Tucker, C, Verde, L, Warne, R, Wilson, G, Wollack, E & Zhao, Y 2010, 'The Atacama Cosmology Telescope: A measurement of the 600 < ℓ < 8000 cosmic microwave background power spectrum at 148 GHz', Astrophysical Journal, vol. 722, no. 2, pp. 1148-1161. https://doi.org/10.1088/0004-637X/722/2/1148
Fowler, J. W. ; Acquaviva, V. ; Ade, P. A R ; Aguirre, P. ; Amiri, M. ; Appel, J. W. ; Barrientos, L. F. ; Battistelli, E. S. ; 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, Philip ; 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. / The Atacama Cosmology Telescope : A measurement of the 600 < ℓ < 8000 cosmic microwave background power spectrum at 148 GHz. In: Astrophysical Journal. 2010 ; Vol. 722, No. 2. pp. 1148-1161.
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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 < 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 ∼ 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 σ 8 = 0.8. We constrain the model's amplitude ASZ < 1.63 (95{\%} CL). If interpreted as a measurement of σ 8, this implies σ 8 SZ < 0.86 (95{\%} CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter ACDM model plus point sources and the SZ effect is consistent with these results.",
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TY - JOUR

T1 - The Atacama Cosmology Telescope

T2 - A measurement of the 600 < ℓ < 8000 cosmic microwave background power spectrum at 148 GHz

AU - Fowler, J. W.

AU - Acquaviva, V.

AU - Ade, P. A R

AU - Aguirre, P.

AU - Amiri, M.

AU - Appel, J. W.

AU - Barrientos, L. F.

AU - Battistelli, E. S.

AU - Bond, J. R.

AU - Brown, B.

AU - Burger, B.

AU - Chervenak, J.

AU - Das, S.

AU - Devlin, M. J.

AU - Dicker, S. R.

AU - Doriese, W. B.

AU - Dunkley, J.

AU - Dünner, R.

AU - Essinger-Hileman, T.

AU - Fisher, R. P.

AU - Hajian, A.

AU - Halpern, M.

AU - Hasselfield, M.

AU - Hernández-Monteagudo, C.

AU - Hilton, G. C.

AU - Hilton, M.

AU - Hincks, A. D.

AU - Hlozek, R.

AU - Huffenberger, K. M.

AU - Hughes, D. H.

AU - Hughes, J. P.

AU - Infante, L.

AU - Irwin, K. D.

AU - Jimenez, R.

AU - Juin, J. B.

AU - Kaul, M.

AU - Klein, J.

AU - Kosowsky, A.

AU - Lau, J. M.

AU - Limon, M.

AU - Lin, Y. T.

AU - Lupton, R. H.

AU - Marriage, T. A.

AU - Marsden, D.

AU - Martocci, K.

AU - Mauskopf, Philip

AU - Menanteau, F.

AU - Moodley, K.

AU - Moseley, H.

AU - Netterfield, C. B.

AU - Niemack, M. D.

AU - Nolta, M. R.

AU - Page, L. A.

AU - Parker, L.

AU - Partridge, B.

AU - Quintana, H.

AU - Reid, B.

AU - Sehgal, N.

AU - Sievers, J.

AU - Spergel, D. N.

AU - Staggs, S. T.

AU - Swetz, D. S.

AU - Switzer, E. R.

AU - Thornton, R.

AU - Trac, H.

AU - Tucker, C.

AU - Verde, L.

AU - Warne, R.

AU - Wilson, G.

AU - Wollack, E.

AU - Zhao, Y.

PY - 2010/10/20

Y1 - 2010/10/20

N2 - 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 < 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 ∼ 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 σ 8 = 0.8. We constrain the model's amplitude ASZ < 1.63 (95% CL). If interpreted as a measurement of σ 8, this implies σ 8 SZ < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter ACDM model plus point sources and the SZ effect is consistent with these results.

AB - 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 < 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 ∼ 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 σ 8 = 0.8. We constrain the model's amplitude ASZ < 1.63 (95% CL). If interpreted as a measurement of σ 8, this implies σ 8 SZ < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter ACDM model plus point sources and the SZ effect is consistent with these results.

KW - Cosmic background radiation

KW - Cosmology: observations

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U2 - 10.1088/0004-637X/722/2/1148

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EP - 1161

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JF - Astrophysical Journal

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