Large-scale imprint of relativistic effects in the cosmic magnification

Duniya, Didam G. A.

doi:10.1103/physrevd.93.103538

Cited by 6 publications

(10 citation statements)

References 105 publications

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“…As we have not assumed any approximation to derive this expression, it is valid on all scales at the linear order. Our result is mostly consistent with the result of [13] 4 , although we additionally considered the terms evaluated at the observer position. Indeed, observer terms do not contribute to any multipoles apart from the monopole l = 0 (potential terms) and the dipole l = 1 (line-of-sight velocity).…”

Section: A Fully Relativistic Angular Power Spectrum Of the Magnificationsupporting

confidence: 89%

“…Therefore, a precise modeling of weak lensing observables over the whole celestial sphere is necessary, which has been studied in various literature (see e.g. [9,13,[32][33][34]). In particular, [9] and [13] have considered general relativistic effects, including potential terms, in their full-sky calculation of the magnification angular power spectrum.…”

Section: Analytical Expressions For the Fully Relativistic Angular Power Spectramentioning

confidence: 99%

“…[9,13,[32][33][34]). In particular, [9] and [13] have considered general relativistic effects, including potential terms, in their full-sky calculation of the magnification angular power spectrum. Here, we revise the theoretical formalism based on (spinweighted) spherical harmonics, and state the results for the magnification angular power spectrum (Sec.…”

Section: Analytical Expressions For the Fully Relativistic Angular Power Spectramentioning

confidence: 99%

“…Indeed, the impact of peculiar line-of-sight velocities on the observed radial coordinate and redshift, referred to as the Doppler magnification or Doppler lensing, is well known in literature. It was first derived in [10], and further work studied the implications for cosmological observables [11][12][13][14][15][16][17]. As concluded in [15], the Doppler magnification dominates over the standard convergence for small redshifts z 0.3 and hence can be measured directly through the magnification of sizes (see [18][19][20]).…”

Section: Introductionmentioning

confidence: 95%

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General relativistic effects in weak lensing angular power spectra

Grimm

Yoo

2021

Phys. Rev. D

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Advances in upcoming weak lensing surveys pose new challenges for an accurate modeling of the lensing observables. The wide sky coverage of Euclid makes angular scales down to lmin=10 accessible. At such large angular scales, general relativistic effects manifest themselves, and the lensing magnification cannot be correctly described by the standard lensing convergence only. The impact of lineof-sight velocities on the magnification angular power spectrum, referred to as the Doppler magnification, is already well recognized in literature. In particular, it was suggested that the Doppler magnification could be extracted by measurements of both cosmic shear and magnification. In this work, we point out two previously neglected aspects with respect to this method. First, the impact of the Doppler magnification is reduced through nonvanishing cross terms with the standard lensing convergence. This is particularly relevant when the sources are averaged over a bin of width Δz0.1, such as in Euclid's tomographic weak lensing survey. Second, general relativistic potential terms slightly enhance the signal. We present numerical calculations of all relativistic effects in the weak lensing angular power spectra on large scales.

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Section: A Fully Relativistic Angular Power Spectrum Of the Magnificationsupporting

confidence: 89%

Section: Analytical Expressions For the Fully Relativistic Angular Power Spectramentioning

confidence: 99%

Section: Analytical Expressions For the Fully Relativistic Angular Power Spectramentioning

confidence: 99%

Section: Introductionmentioning

confidence: 95%

See 2 more Smart Citations

General relativistic effects in weak lensing angular power spectra

Grimm

Yoo

2021

Phys. Rev. D

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“…And these differences between two scales decrease with increasing redshifts because of the same reason that the scale dependence comes only through the dark energy perturbation which plays an extra role only on large scales. Next, we introduce a quantity f = − k 2 vm H∆m which is related to the velocity perturbation and gives rise to the redshift space distortion [90]. The reason to introduce this quantity is that it plays an important role to the observed galaxy power spectrum which is discussed in the next section.…”

Section: A Initial Conditionsmentioning

confidence: 99%

Observed galaxy power spectrum in cubic Galileon model

Dinda

Hossain

Sen

2018

J. Cosmol. Astropart. Phys.

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In this paper, we study the effects of general relativistic corrections on the observed galaxy power spectrum in thawing class of cubic Galileon model with linear potential that preserves the shift symmetry. In this scenario, the observed galaxy power spectrum differs from the standard matter power spectrum mainly due to redshift space distortion (RSD) factor and relativistic effects. The RSD term enhances the matter power spectrum both at larger and smaller scales whereas the relativistic terms further enhance the matter power spectrum only at larger scales. In comparison with ΛCDM, the observed galaxy power spectrum is always suppressed at large scales in this scenario although this suppression is always small compared to the canonical quintessence scenario.

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Probing beyond-Horndeski gravity on ultra-large scales

Moloi

Clarkson

Larena

et al. 2020

J. Cosmol. Astropart. Phys.

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The beyond-Horndeski gravity has recently been reformulated in the dark energy paradigm—which has been dubbed, Unified Dark Energy (UDE). The evolution equations for the given UDE appear to correspond to a non-conservative dark energy scenario, in which the total energy-momentum tensor is not conserved. We investigate both the background cosmology and, the large-scale imprint of the UDE by probing the angular power spectrum of galaxy number counts, on ultra-large scales; taking care to include the full relativistic corrections in the observed overdensity. The background evolution shows that only an effective mass smaller than the Planck mass is needed in the early universe in order for predictions in the given theory to match current observational constraints. We found that the effective mass-evolution-rate parameter, which drives the evolution of the UDE, acts to enhance the observed power spectrum and, hence, relativistic effects (on ultra-large scales) by enlarging the UDE sound horizon. Conversely, both the (beyond) Horndeski parameter and the kineticity act to diminish the observed power spectrum, by decreasing the UDE sound horizon. Our results show that, in a universe with UDE, a multi-tracer analysis will be needed to detect the relativistic effects in the large-scale structure. In the light of a multi-tracer analysis, the various relativistic effects hold the potential to distinguish different gravity models. Moreover, while the Doppler effect will remain significant at all epochs and, thus can not be ignored, the integrated Sachs-Wolfe, the time-delay and the potential (difference) effects, respectively, will only become significant at epochs near z = 3 and beyond, and may be neglected at late epochs. In the same vein, the Doppler effect alone can serve as an effective cosmological probe for the large-scale structure or gravity models, in the angular power spectrum—at all z.

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Large-scale imprint of relativistic effects in the cosmic magnification

Cited by 6 publications

References 105 publications

General relativistic effects in weak lensing angular power spectra

General relativistic effects in weak lensing angular power spectra

Observed galaxy power spectrum in cubic Galileon model

Probing beyond-Horndeski gravity on ultra-large scales

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