Fu et al. A New Sesquiterpene from the Fruits of Daucus carota L. Molecules 2009, 14, 2862-2867

Fu, Hongwei; Zhang, Lin; Tao, Yi; Tian, Jingkui

doi:10.3390/molecules14103868

Cited by 68 publications

(87 citation statements)

References 1 publication

(1 reference statement)

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“…Pierpaoli et al 2003, for a review). The dominant discrepancy between cosmic shear and X-ray clusters has recently been reduced by Jarvis et al (2006), who measured σ 8 ≈ 0.81 for m = 0.26 when using cosmic shear alone, followed by Benjamin et al (2007), who used the improved galaxy photometric redshifts of Ilbert et al (2006), and measured σ 8 = 0.84 for m = 0.24 and Fu et al (2008), who found a consistent value. To clarify these discrepancies, one needs to measure both the power-spectrum and the M-T relation normalizations σ 8 and M * , as we discuss here.…”

Section: Discussionmentioning

confidence: 99%

Combined analysis of weak lensing and X-ray blind surveys

Bergé¹,

Pacaud²,

Réfrégier³

et al. 2008

Monthly Notices RAS

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We present a joint weak lensing and X-ray analysis of 4 deg$^2$ from the CFHTLS and XMM-LSS surveys. Our weak lensing analysis is the first analysis of a real survey using shapelets, a new generation weak lensing analysis method. We create projected mass maps of the images, and extract 6 weak-lensing-detected clusters of galaxies. We show that their counts can be used to constrain the power spectrum normalisation $\sigma_8 =0.92_{-0.30}^{+0.26}$ for $\Omega_m=0.24$. We show that despite the large scatter generally observed in the M-T relation derived from lensing masses, tight constraints on both its slope and normalisation $M_*$ can be obtained with a moderate number of sources provided that the covered mass range is large enough. Adding clusters from Bardeau et al. (2007) to our sample, we measure $M_* = 2.71_{-0.61}^{+0.79} 10^{14} h^{-1} M_\odot$. Although they are dominated by shot noise and sample variance, our measurements are consistent with currently favoured values, and set the stage for future surveys. We thus investigate the dependence of those estimates on survey size, depth, and integration time, for joint weak lensing and X-ray surveys. We show that deep surveys should be dedicated to the study of the physics of clusters and groups of galaxies. For a given exposure time, wide surveys provide a larger number of detected clusters and are therefore preferred for the measurement of cosmological parameters such as $\sigma_8$ and $M_*$. We show that a wide survey of a few hundred square degrees is needed to improve upon current measurements of these parameters. More ambitious surveys covering 7000 deg$^2$ will provide the 1% accuracy in the estimation of the power spectrum and the M-T relation normalisations.Comment: MNRAS in press Matches accepted version. References update

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Section: Discussionmentioning

confidence: 99%

Combined analysis of weak lensing and X-ray blind surveys

Bergé¹,

Pacaud²,

Réfrégier³

et al. 2008

Monthly Notices RAS

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“…This is what the approach which is usually adopted such as in [7] for the CFHTLenS survey and in [8] for the DES survey. There exist however alternative approaches that give complementary information.…”

Section: Introductionmentioning

confidence: 90%

Large deviation principle at work: Computation of the statistical properties of the exact one-point aperture mass

Reimberg

Bernardeau

2018

Phys. Rev. D

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This paper presents a general formalism that allows the derivation of the cumulant generating function and one-point Probability Distribution Function (PDF) of the aperture mass (Map), a common observable for cosmic shear observations. Our formalism is based on the Large Deviation Principle (LDP) applied, in such cosmological context, to an arbitrary set of densities in concentric cells. We show here that the LDP can indeed be used for a much larger family of observables than previously envisioned, such as those built from continuous and nonlinear functionals of the density profiles. The general expression of the observable aperture mass depends on reduced shear profile making it a rather involved function of the projected density field. Because of this difficulty, an approximation that is commonly employed consists in replacing the reduced shear by the shear in such a construction neglecting therefore non-linear effects. We were precisely able to quantify how this approximation affects theMap statistical properties. In particular we derive the corrective term for the skewness of theMap and reconstruct its one-point PDF.

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“…Gravitational lensing information and the integrated Sachs-Wolfe effect of the cosmic microwave background act to constrain G light . We have seen that current data are weak in the ability to test G matter , with uncertainties of order one, while G light can be determined to roughly 10% from the Canada-France-Hawaii Telescope Legacy Survey lensing data [10] and the WMAP CMB temperature power spectrum [11]. However, note that this precision does not indicate accuracy; the deviation from GR seen in the bottom right panel, for example, arises from acknowledged observational systematics [8].…”

Section: The Differences Of Gravitymentioning

confidence: 99%

“…Constraints are shown on the 8 parameters of post-GR model independent gravity, from current and simulated future data. Dotted contours show the 68% and 95% confidence regions from current WMAP CMB [11], CFHTLS lensing [10], and Union2.1 supernova distance data [12], while solid black contours show constraints from simulated data of the next generation BigBOSS galaxy redshift survey (marginalized over galaxy bias) plus Stage III experiments. Small red contours include as well a highly optimistic galaxy weak lensing survey covering 4000 deg 2 with a galaxy number density of 55 arcmin −2 .…”

Section: The Paths Of Gravitymentioning

confidence: 99%

The direction of gravity

Linder

2014

J. Phys.: Conf. Ser.

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Abstract. Gravity directs the paths of light rays and the growth of structure. Moreover, gravity on cosmological scales does not simply point down: It accelerates the universal expansion by pulling outward, either due to a highly negative pressure dark energy or an extension of general relativity. We have examined methods to test the properties of gravity through cosmological measurements. We have then considered specific possibilities for a sound gravitational theory based on the Galilean shift symmetry. The evolution of the laws of gravity from the early universe to the present acceleration to the future fate -the paths of gravitycarries rich information on this fundamental force of physics, and on the mystery of dark energy.

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Fu et al. A New Sesquiterpene from the Fruits of Daucus carota L. Molecules 2009, 14, 2862-2867

Abstract: We realized that the affiliations of the authors were incorrectly listed in our paper published in Molecules recently [1]. [...

Cited by 68 publications

References 1 publication

Combined analysis of weak lensing and X-ray blind surveys

Combined analysis of weak lensing and X-ray blind surveys

Large deviation principle at work: Computation of the statistical properties of the exact one-point aperture mass

The direction of gravity

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