An automated method for least cost distribution planning

Hasselfield, C.W.; Wilson, P.; Penner, L.; Lau, Meng Cheng; Gole, A.M.

doi:10.1109/wescan.1991.160543

Cited by 2 publications

(7 citation statements)

References 8 publications

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“…After subtracting the maximum likelihood signal of surrounding structures fitted simultaneously, the resulting mass estimate for the central halo is slightly lower at M200m = (6.6 +3.1 −2.6 ) × h −1 70 10 14 M ⊙ (M500c = (3.8 +1.7 −1.5 ) × h −1 70 10 14 M ⊙ ). Both our mass estimates are in agreement with the SZ masses of Vanderlinde et al (2010) and Hasselfield et al (2013), the X-ray masses of Andersson et al (2011), the combined SZ+X-ray mass of Reichardt et al (2013) and the dynamical mass of Andersson et al (2011).…”

Section: Weak Lensing Analysissupporting

confidence: 87%

“…A problem with signal extraction or calibration of the Planck SZ would likely lead to differences with other SZ observa-tions of the same clusters, and if the hypothesis of a redshift dependence should hold these differences should in turn be a function of redshift. Hasselfield et al (2013) compare SZ mass estimates of 11 clusters detected and published by both ACT and SPT with good agreement (cf. their fig.…”

Section: Comparison With Other Sz Surveysmentioning

confidence: 55%

“…The independent discovery of the cluster by ACT is listed as ACT-CL J0509-5341 (Marriage et al 2011). The SZ mass is given by Hasselfield et al (2013) 2009) perform a WL analysis of the system as one of the first SZ detected clusters. They calculate KSB shapes on i band and photometric redshifts on g-, r-, i-, and z-band public imaging data from the Blanco Cosmology Survey.…”

Section: Previous Workmentioning

confidence: 99%

“…Following the recent releases of Planck (The Planck Collaboration et al 2013a), ACT (Hasselfield et al 2013) and SPT (Williamson et al 2011;Reichardt et al 2013) catalogues, we match objects detected both in Planck and either of the other catalogues. Rejecting systems with redshift differences ∆z > 0.03 between the two respective catalogues and ones not successfully extracted with the Planck MMF3 algorithm, we find 13 matches with Hasselfield et al (2013), 11 with Reichardt et al (2013) and 19 with Williamson et al (2011) (3 of which are also in Reichardt et al 2013). Fig.…”

Section: Comparison With Other Sz Surveysmentioning

confidence: 99%

“…Deviations between model and data could be explained, for instance, by incorrect treatment of the abundance of clus- Figure 29. Comparison of Planck self-consistent mass estimates with ACT and SPT measurements (Williamson et al 2011;Hasselfield et al 2013;Reichardt et al 2013). The dotted line indicates a 20% excess, the black error bars indicate log-mean values in redshift bins.…”

Section: Centring and Shearmentioning

confidence: 99%

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Weak lensing analysis of SZ-selected clusters of galaxies from the SPT and Planck surveys

Seitz

Brimioulle

Kosyra

et al. 2014

Monthly Notices of the Royal Astronomical Society

123

161

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We present the weak lensing analysis of the Wide-Field Imager SZ Cluster of galaxy (WISCy) sample, a set of 12 clusters of galaxies selected for their Sunyaev-Zel'dovich (SZ) effect. After developing new and improved methods for background selection and determination of geometric lensing scaling factors from absolute multi-band photometry in cluster fields, we compare the weak lensing mass estimate with public X-ray and SZ data. We find consistency with hydrostatic X-ray masses with no significant bias, no mass dependent bias and less than 20% intrinsic scatter and constrain f gas,500c = 0.128 +0.029 −0.023 . We independently calibrate the South Pole Telescope significance-mass relation and find consistency with previous results. The comparison of weak lensing mass and Planck Compton parameters, whether extracted selfconsistently with a mass-observable relation (MOR) or using X-ray prior information on cluster size, shows significant discrepancies. The deviations from the MOR strongly correlate with cluster mass and redshift. This could be explained either by a significantly shallower than expected slope of Compton decrement versus mass and a corresponding problem in the previous X-ray based mass calibration, or a size or redshift dependent bias in SZ signal extraction.

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Section: Weak Lensing Analysissupporting

confidence: 87%

Section: Comparison With Other Sz Surveysmentioning

confidence: 55%

Section: Previous Workmentioning

confidence: 99%

Section: Comparison With Other Sz Surveysmentioning

confidence: 99%

Section: Centring and Shearmentioning

confidence: 99%

See 3 more Smart Citations

Weak lensing analysis of SZ-selected clusters of galaxies from the SPT and Planck surveys

Seitz

Brimioulle

Kosyra

et al. 2014

Monthly Notices of the Royal Astronomical Society

123

161

View full text Add to dashboard Cite

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A MEASUREMENT OF THE SECONDARY-CMB AND MILLIMETER-WAVE-FOREGROUND BISPECTRUM USING 800 deg²OF SOUTH POLE TELESCOPE DATA

Crawford

Schaffer

Bhattacharya

et al. 2014

ApJ

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We present a measurement of the angular bispectrum of the millimeter-wave sky in observing bands centered at roughly 95, 150, and 220 GHz, on angular scales of 1 ′ θ 10 ′ (multipole number 1000 l 10,000). At these frequencies and angular scales, the main contributions to the bispectrum are expected to be the thermal Sunyaev-Zel'dovich (tSZ) effect and emission from extragalactic sources, predominantly dusty, star-forming galaxies (DSFGs) and active galactic nuclei. We measure the bispectrum in 800 deg 2 of three-band South Pole Telescope data, and we use a multi-frequency fitting procedure to separate the bispectrum of the tSZ effect from the extragalactic source contribution. We simultaneously detect the bispectrum of the tSZ effect at >10σ, the unclustered component of the extragalactic source bispectrum at >5σ in each frequency band, and the bispectrum due to the clustering of DSFGs-i.e., the clustered cosmic infrared background (CIB) bispectrum-at >5σ. This is the first reported detection of the clustered CIB bispectrum. We use the measured tSZ bispectrum amplitude, compared to model predictions, to constrain the normalization of the matter power spectrum to be σ 8 = 0.787 ± 0.031 and to predict the amplitude of the tSZ power spectrum at l = 3000. This prediction improves our ability to separate the thermal and kinematic contributions to the total SZ power spectrum. The addition of bispectrum data improves our constraint on the tSZ power spectrum amplitude by a factor of two compared to power spectrum measurements alone and demonstrates a preference for a nonzero kinematic SZ (kSZ) power spectrum, with a derived constraint on the kSZ amplitude at l = 3000 of A kSZ = 2.9 ± 1.6 µK 2 , or A kSZ = 2.6 ± 1.8 µK 2 if the default A kSZ > 0 prior is removed.

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An automated method for least cost distribution planning

Cited by 2 publications

References 8 publications

Weak lensing analysis of SZ-selected clusters of galaxies from the SPT and Planck surveys

Weak lensing analysis of SZ-selected clusters of galaxies from the SPT and Planck surveys

A MEASUREMENT OF THE SECONDARY-CMB AND MILLIMETER-WAVE-FOREGROUND BISPECTRUM USING 800 deg²OF SOUTH POLE TELESCOPE DATA

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An automated method for least cost distribution planning

Cited by 2 publications

References 8 publications

Weak lensing analysis of SZ-selected clusters of galaxies from the SPT and Planck surveys

Weak lensing analysis of SZ-selected clusters of galaxies from the SPT and Planck surveys

A MEASUREMENT OF THE SECONDARY-CMB AND MILLIMETER-WAVE-FOREGROUND BISPECTRUM USING 800 deg2OF SOUTH POLE TELESCOPE DATA

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A MEASUREMENT OF THE SECONDARY-CMB AND MILLIMETER-WAVE-FOREGROUND BISPECTRUM USING 800 deg²OF SOUTH POLE TELESCOPE DATA