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

Hajian, Amir; Viero, Marco P.; Addison, Graeme E.; Aguirre, Paula; Appel, John W.; Battaglia, Nick; Bock, J. J.; Bond, J. R.; Das, Sudeep; Devlin, Mark J.; Dicker, Simon; Dunkley, Joanna; Dünner, Rolando; Essinger-Hileman, Thomas; Hughes, John P.; Fowler, Joseph W.; Halpern, M.; Hasselfield, Matthew; Hilton, Matthew; Hincks, Adam D.; Hložek, Renée; Irwin, K. D.; Klein, Jeff; Kosowsky, Arthur; Lin, Yen Ting; Marriage, Tobias A.; Marsden, Danica; Marsden, G.; Menanteau, F.; Moodley, Kavilan; Netterfield, C. B.; Niemack, Michael D.; Nolta, Michael R.; Page, Lyman A.; Parker, Lucas; Patanchon, G.; Scott, D.; Sehgal, Neelima; Sievers, Jonathan; Spergel, David N.; Staggs, Suzanne T.; Swetz, Daniel S.; Switzer, Eric R.; Thornton, Robert J.; Wollack, Edward J.

doi:10.1088/0004-637x/744/1/40

Cited by 29 publications

(45 citation statements)

References 67 publications

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“…Figure 29 shows the power spectrum of cosmic infrared background anisotropies as computed on a simulated sky, and as measured by Planck (Planck Collaboration 2011k), and ACT . The agreement between the model and the measured power spectra is reasonable, but not perfect, and discrepancies will be addressed with improved modelling in future releases, in the light of recent advances on number counts and on correlations from observations with the BLAST balloon-borne experiment (Patanchon et al 2009;Viero et al 2009), SPT (Hall et al 2010), Herschel Cooray et al 2010), and from a combined analysis of ACT and BLAST (Hajian et al 2012). Also, the correlation between the CIB maps across the frequency range is almost unity in the current model, a feature that will have to be improved in the future using a more detailed model constrained by upcoming additional Planck observations.…”

Section: Cosmic Infrared Background Anisotropiesmentioning

confidence: 92%

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

Delabrouille

Betoule

Melin

et al. 2013

A&A

201

229

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We present the Planck Sky Model (PSM), a parametric model for generating all-sky, few arcminute resolution maps of sky emission at submillimetre to centimetre wavelengths, in both intensity and polarisation. Several options are implemented to model the cosmic microwave background, Galactic diffuse emission (synchrotron, free-free, thermal and spinning dust, CO lines), Galactic H ii regions, extragalactic radio sources, dusty galaxies, and thermal and kinetic Sunyaev-Zeldovich signals from clusters of galaxies. Each component is simulated by means of educated interpolations/extrapolations of data sets available at the time of the launch of the Planck mission, complemented by state-of-the-art models of the emission. Distinctive features of the simulations are spatially varying spectral properties of synchrotron and dust; different spectral parameters for each point source; modelling of the clustering properties of extragalactic sources and of the power spectrum of fluctuations in the cosmic infrared background. The PSM enables the production of random realisations of the sky emission, constrained to match observational data within their uncertainties. It is implemented in a software package that is regularly updated with incoming information from observations. The model is expected to serve as a useful tool for optimising planned microwave and sub-millimetre surveys and testing data processing and analysis pipelines. It is, in particular, used to develop and validate data analysis pipelines within the Planck collaboration. A version of the software that can be used for simulating the observations for a variety of experiments is made available on a dedicated website.

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Section: Cosmic Infrared Background Anisotropiesmentioning

confidence: 92%

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

Delabrouille

Betoule

Melin

et al. 2013

A&A

201

229

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“…Further theoretical investigation (Scott & White 1999;Haiman & Knox 2000) was stimulated by the detection of the infrared background in the COBE data (Puget et al 1996;Fixsen et al 1998), and the detection of bright "sub-millimetre" galaxies in SCUBA data (Hughes et al 1998). Subsequently, the clustering has been detected at 160 microns , at 250, 350 and 500 microns by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST, Viero et al 2009;Hajian et al 2012) and at 217 GHz by SPT and ACT (Hall et al 2010;Dunkley et al 2011). Recent Planck measurements of the CIB (Planck Collaboration XVIII 2011) have extended the measurements at 217 GHz, 353 GHz, and 545 GHz to larger scales, and recent Herschel measurements (Viero et al 2013) have improved on the BLAST measurements and extended them to smaller angular scales.…”

Section: Clustered Power From Unresolved Point Sourcesmentioning

confidence: 99%

Planck2013 results. XV. CMB power spectra and likelihood

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

389

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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“…Thus, the theoretical systematic uncertainty in modeling the tSZ skewness is correspondingly lower as well. In addition, at 148 GHz, dusty star-forming galaxies are less prevalent in massive, low-redshift clusters (which contribute more to the skewness) than in high-redshift groups and clusters (which contribute more to the tSZ power spectrum) [20]. Thus, we expect the correlation between tSZ signal and dusty galaxy emission, which can complicate analyses of the tSZ effect, to be smaller for a measurement of the skewness.…”

Section: Introductionmentioning

confidence: 98%

Atacama Cosmology Telescope: A measurement of the thermal Sunyaev-Zel’dovich effect using the skewness of the CMB temperature distribution

Wilson¹,

Sherwin²,

Hill³

et al. 2012

Phys. Rev. D

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We present a detection of the unnormalized skewness T 3 (n) induced by the thermal SunyaevZel'dovich (tSZ) effect in filtered Atacama Cosmology Telescope (ACT) 148 GHz cosmic microwave background temperature maps. Contamination due to infrared and radio sources is minimized by template subtraction of resolved sources and by constructing a mask using outlying values in the 218 GHz (tSZ-null) ACT maps. We measure T 3 (n) = −31 ± 6 µK 3 (Gaussian statistics assumed) or ±14 µK 3 (including non-Gaussian corrections) in the filtered ACT data, a 5σ detection. We show that the skewness is a sensitive probe of σ8, and use analytic calculations and tSZ simulations to obtain cosmological constraints from this measurement. From this signal alone we infer a value of σ8 = 0.79). Our results demonstrate that measurements of nonGaussianity can be a useful method for characterizing the tSZ effect and extracting the underlying cosmological information.

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

Cited by 29 publications

References 67 publications

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

Planck2013 results. XV. CMB power spectra and likelihood

Atacama Cosmology Telescope: A measurement of the thermal Sunyaev-Zel’dovich effect using the skewness of the CMB temperature distribution

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