Imperial College London
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ProfessorAlanHeavens

Faculty of Natural Sciences, Department of Physics

Chair in Astrostatistics
 
 
 
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Contact

 

+44 (0)20 7594 2930a.heavens Website

 
 
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Location

 

1018EBlackett LaboratorySouth Kensington Campus

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Summary

 

Publications

Citation

BibTex format

@article{Munshi:2023:10.1103/PhysRevD.107.043516,
author = {Munshi, D and Jung, G and Kitching, TD and McEwen, J and Liguori, M and Namikawa, T and Heavens, A},
doi = {10.1103/PhysRevD.107.043516},
journal = {Physical Review D: Particles, Fields, Gravitation and Cosmology},
title = {Position-dependent correlation function of weak-lensing convergence},
url = {http://dx.doi.org/10.1103/PhysRevD.107.043516},
volume = {107},
year = {2023}
}
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RIS format (EndNote, RefMan)

TY  - JOUR
AB  - We provide a systematic study of the position-dependent correlation function in weak-lensingconvergence maps and its relation to the squeezed limit of the three-point correlation function (3PCF)using state-of-the-art numerical simulations. We relate the position-dependent correlation function toits harmonic counterpart, i.e., the position-dependent power spectrum or equivalently the integratedbispectrum (IB). We use a recently proposed improved fitting function, BiHalofit, for the bispectrum tocompute the theoretical predictions as a function of source redshifts. In addition to low redshift results(zs ¼ 1.0–2.0) we also provide results for maps inferred from lensing of the cosmic microwave background(CMB), i.e., zs ¼ 1100. We include a Euclid-type realistic survey mask and noise. In agreement with therecent studies on the position-dependent power spectrum, we find that the results from simulations areconsistent with the theoretical expectations when appropriate corrections are included. Performing a roughestimate, we find that the signal-to-noise (S/N) for the detection of position-dependent correlation functionfrom Euclid-type mask with fsky ¼ 0.35, can range between 6–12 depending on the value of the intrinsicellipticity distribution parameter σ ¼ 0.3–1.0. For reconstructed κ maps using an ideal CMB survey theS=N ≈ 1.8. We also found that a 10% deviation in σ8 can be detected using IB for the optimistic case ofσ ¼ 0.3 with a S=N ≈ 5. The S/N for such detection in case of ΩM is lower.
AU  - Munshi,D
AU  - Jung,G
AU  - Kitching,TD
AU  - McEwen,J
AU  - Liguori,M
AU  - Namikawa,T
AU  - Heavens,A
DO  - 10.1103/PhysRevD.107.043516
PY  - 2023///
SN  - 1550-2368
TI  - Position-dependent correlation function of weak-lensing convergence
T2  - Physical Review D: Particles, Fields, Gravitation and Cosmology
UR  - http://dx.doi.org/10.1103/PhysRevD.107.043516
UR  - https://www.webofscience.com/api/gateway?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000964332800014&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=a2bf6146997ec60c407a63945d4e92bb
UR  - https://journals.aps.org/prd/abstract/10.1103/PhysRevD.107.043516
UR  - http://hdl.handle.net/10044/1/108897
VL  - 107
ER  -
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