THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE 600 &lt; ℓ &lt; 8000 COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 GHz

Fowler, Joseph W.; Acquaviva, Viviana; Aguirre, Paula; Amiri, M.; Appel, John W.; Barrientos, L. Felipe; Battistelli, E. S.; Bond, J. R.; Brown, Ben; Burger, B.; Chervenak, James A.; Das, Sudeep; Devlin, Mark J.; Dicker, Simon; Doriese, W. B.; Dunkley, Joanna; Dünner, Rolando; Essinger‐Hileman, T.; Fisher, R. P.; Hajian, Amir; Halpern, M.; Hasselfield, Matthew; Hernández-Monteagudo, C.; Hilton, G. C.; Hilton, Matt; Hincks, Adam D.; Hložek, Renée; Huffenberger, K. M.; Hughes, D. H.; Hughes, John P.; Infante, L.; Irwin, K. D.; Jiménez, Raúl; Juin, J. B.; Kaul, Madhuri; Klein, J.; Kosowsky, Arthur; Lau, Judy M.; Limon, M.; Lin, Yen Ting; Lupton, Robert H.; Marriage, Tobias A.; Marsden, Danica; Martocci, Krista; Mauskopf, Philip Daniel; Menanteau, F.; Moodley, Kavilan; Moseley, H.; Netterfield, C. B.; Niemack, Michael D.; Nolta, Michael R.; Page, Lyman A.; Parker, Lucas; Partridge, B.; Quintana, H.; Reid, Beth; Sehgal, Neelima; Sievers, Jonathan; Spergel, David N.; Staggs, Suzanne T.; Swetz, Daniel S.; Switzer, Eric R.; Thornton, Robert J.; Trac, Hy; Tucker, C.; Verde, Licia; Warne, Ryan; Wilson, Grant; Wollack, Edward J.; Zhao, Yue

doi:10.1088/0004-637x/722/2/1148

Cited by 112 publications

(110 citation statements)

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“…Multiple peaks in the spectrum have been measured most recently by Brown et al (2009), Friedman et al (2009), Reichardt et al (2009a, 2009b, Sayers et al (2009), Lueker et al (2010, Sharp et al (2010), Fowler et al (2010, Das et al (2011), andNolta et al (2009). Secondary anisotropies include CMB lensing, which acts to smooth out the peaks and add excess power to the damping tail; and the SZ effect, which distorts the primordial CMB signal.…”

Section: Cmbmentioning

confidence: 99%

“…The tropical location of ACT permits observations of both the northern and southern celestial hemispheres. Further details on the instrument are presented in Swetz et al (2010), Fowler et al (2010), and references therein. 26 The ACT maps used in this paper are made from data taken during the 2008 observing season (at 148 GHz and218 GHz, or 2030 and1380 μm, respectively) and are identical to the maps used in Hajian et al (2010) and Das et al (2011).…”

Section: Actmentioning

confidence: 99%

“…Anisotropic, large-scale noise is evident at the center of the two-dimensional power spectrum, as shown in Figure 4. Noise weighting downweights the noisy vertical stripe that passes through the origin, which is predominantly due to large-scale unconstrained modes in the map (see also Fowler et al 2010). To further ensure that our results are not contaminated by this stripe, we mask a vertical band spanning | x | < 500 before averaging the two-dimensional power spectra in annuli.…”

Section: Weights and Masksmentioning

confidence: 99%

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Correlations in the (Sub)millimeter Background From Act × Blast

Hajian

Viero

Addison

et al. 2011

ApJ

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We present measurements of the auto-and cross-frequency correlation power spectra of the cosmic (sub)millimeter background at 250, 350, and 500 μm (1200, 860, and 600 GHz) from observations made with the Balloonborne Large Aperture Submillimeter Telescope (BLAST); and at 1380 and 2030 μm (218 and 148 GHz) from observations made with the Atacama Cosmology Telescope (ACT). The overlapping observations cover 8.6 deg 2 in an area relatively free of Galactic dust near the south ecliptic pole. The ACT bands are sensitive to radiation from the cosmic microwave background, to the Sunyaev-Zel'dovich effect from galaxy clusters, and to emission by radio and dusty star-forming galaxies (DSFGs), while the dominant contribution to the BLAST bands is from DSFGs. We confirm and extend the BLAST analysis of clustering with an independent pipeline and also detect correlations between the ACT and BLAST maps at over 25σ significance, which we interpret as a detection of the DSFGs in the ACT maps. In addition to a Poisson component in the cross-frequency power spectra, we detect a clustered signal at 4σ , and using a model for the DSFG evolution and number counts, we successfully fit all of our spectra with a linear clustering model and a bias that depends only on redshift and not on scale. Finally, the data are compared to, and generally agree with, phenomenological models for the DSFG population. This study demonstrates the constraining power of the cross-frequency correlation technique to constrain models for the DSFGs. Similar analyses with more data will impose tight constraints on future models.

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Section: Cmbmentioning

confidence: 99%

Section: Actmentioning

confidence: 99%

Section: Weights and Masksmentioning

confidence: 99%

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Correlations in the (Sub)millimeter Background From Act × Blast

Hajian

Viero

Addison

et al. 2011

ApJ

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“…It has been measured over the whole sky by COBE and WMAP, and over smaller regions by ground-based and sub-orbital experiments (e.g., Tristram et al 2005;Jones et al 2006;Reichardt et al 2009;Fowler et al 2010;Das et al 2011;Keisler et al 2011;Story et al 2013;Das et al 2014). By mapping the whole sky to scales of a few arc minutes, Planck now measures the power spectrum over an unprecedented range of scales from a single experiment.…”

Section: Introductionmentioning

confidence: 99%

Planck2013 results. XV. CMB power spectra and likelihood

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

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392

263

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This paper presents the Planck 2013 likelihood, a complete statistical description of the two-point correlation function of the CMB temperature fluctuations that accounts for all known relevant uncertainties, both instrumental and astrophysical in nature. We use this likelihood to derive our best estimate of the CMB angular power spectrum from Planck over three decades in multipole moment, , covering 2 ≤ ≤ 2500. The main source of uncertainty at < ∼ 1500 is cosmic variance. Uncertainties in small-scale foreground modelling and instrumental noise dominate the error budget at higher s. For < 50, our likelihood exploits all Planck frequency channels from 30 to 353 GHz, separating the cosmological CMB signal from diffuse Galactic foregrounds through a physically motivated Bayesian component separation technique. At ≥ 50, we employ a correlated Gaussian likelihood approximation based on a fine-grained set of angular cross-spectra derived from multiple detector combinations between the 100, 143, and 217 GHz frequency channels, marginalising over power spectrum foreground templates. We validate our likelihood through an extensive suite of consistency tests, and assess the impact of residual foreground and instrumental uncertainties on the final cosmological parameters. We find good internal agreement among the high-cross-spectra with residuals below a few µK 2 at < ∼ 1000, in agreement with estimated calibration uncertainties. We compare our results with foreground-cleaned CMB maps derived from all Planck frequencies, as well as with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters. We further show that the best-fit ΛCDM cosmology is in excellent agreement with preliminary Planck EE and T E polarisation spectra. We find that the standard ΛCDM cosmology is well constrained by Planck from the measurements at < ∼ 1500. One specific example is the spectral index of scalar perturbations, for which we report a 5.4σ deviation from scale invariance, n s = 1. Increasing the multipole range beyond 1500 does not increase our accuracy for the ΛCDM parameters, but instead allows us to study extensions beyond the standard model. We find no indication of significant departures from the ΛCDM framework. Finally, we report a tension between the Planck best-fit ΛCDM model and the low-spectrum in the form of a power deficit of 5-10% at < ∼ 40, with a statistical significance of 2.5-3σ. Without a theoretically motivated model for this power deficit, we do not elaborate further on its cosmological implications, but note that this is our most puzzling finding in an otherwise remarkably consistent data set.

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“…In recent years, high-quality observations of the CMB have been provided by the WMAP satellite [47], ACBAR [5], the South Pole Telescope (SPT) [50] and the Atacama Cosmology Telescope (ACT) [6], while the Sloan Digital Sky Survey (SDSS) [7] has probed the density perturbations at low redshifts. Further, data from the Planck satellite [8] will soon be available to the cosmological community, and several major LSS surveys are now underway or are being planned.…”

Section: Introductionmentioning

confidence: 99%

Bayesian analysis of inflation. III. Slow roll reconstruction using model selection

et al. 2012

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We implement Slow Roll Reconstruction -an optimal solution to the inverse problem for inflationary cosmology -within ModeCode, a publicly available solver for the inflationary dynamics. We obtain up-to-date constraints on the reconstructed inflationary potential, derived from the WMAP 7-year dataset and South Pole Telescope observations, combined with large scale structure data derived from SDSS Data Release 7. Using ModeCode in conjunction with the MultiNest sampler, we compute Bayesian evidence for the reconstructed potential at each order in the truncated slow roll hierarchy. We find that the data are well-described by the first two slow roll parameters, ǫ and η, and that there is no need to include a nontrivial ξ parameter.

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THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE 600 < ℓ < 8000 COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 GHz

Cited by 112 publications

References 60 publications

Correlations in the (Sub)millimeter Background From Act × Blast

Correlations in the (Sub)millimeter Background From Act × Blast

Planck2013 results. XV. CMB power spectra and likelihood

Bayesian analysis of inflation. III. Slow roll reconstruction using model selection

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