Publications

BibTex format

@article{Kitching:2014:mnras/stu934,
author = {Kitching, TD and Heavens, AF and Alsing, J and Erben, T and Heymans, C and Hildebrandt, H and Hoekstra, H and Jaffe, A and Kiessling, A and Mellier, Y and Miller, L and van, Waerbeke L and Benjamin, J and Coupon, J and Fu, L and Hudson, MJ and Kilbinger, M and Kuijken, K and Rowe, BTP and Schrabback, T and Semboloni, E and Velander, M},
doi = {mnras/stu934},
journal = {Monthly Notices of the Royal Astronomical Society},
pages = {1326--1349},
title = {3D cosmic shear: cosmology from CFHTLenS},
url = {http://dx.doi.org/10.1093/mnras/stu934},
volume = {442},
year = {2014}
}

Download

RIS format (EndNote, RefMan)

TY  - JOUR
AB  - This paper presents the first application of 3D cosmic shear to a wide-field weak lensing survey. 3D cosmic shear is a technique that analyses weak lensing in three dimensions using a spherical harmonic approach, and does not bin data in the redshift direction. This is applied to CFHTLenS, a 154 square degree imaging survey with a median redshift of 0.7 and an effective number density of 11 galaxies per square arcminute usable for weak lensing. To account for survey masks we apply a 3D pseudo-C approach on weak lensing data, and to avoid uncertainties in the highly non-linear regime, we separately analyse radial wavenumbers k ≤ 1.5 and 5.0 h Mpc−1, and angular wavenumbers  ≈ 400–5000. We show how one can recover 2D and tomographic power spectra from the full 3D cosmic shear power spectra and present a measurement of the 2D cosmic shear power spectrum, and measurements of a set of 2-bin and 6-bin cosmic shear tomographic power spectra; in doing so we find that using the 3D power in the calculation of such 2D and tomographic power spectra from data naturally accounts for a minimum scale in the matter power spectrum. We use 3D cosmic shear to constrain cosmologies with parameters ΩM, ΩB, σ8, h , ns, w0 and wa. For a non-evolving dark energy equation of state, and assuming a flat cosmology, lensing combined with Wilkinson Microwave Anisotropy Probe 7 results in h = 0.78 ± 0.12, ΩM = 0.252 ± 0.079, σ8 = 0.88 ± 0.23 and w = −1.16 ± 0.38 using only scales k ≤ 1.5  h Mpc−1. We also present results of lensing combined with first year Planck results, where we find no tension with the results from this analysis, but we also find no significant improvement over the Planck results alone. We find evidence of a suppression of power compared to Lambda cold dark matter (LCDM) on small scales 1.5 < k ≤ 5.0 h Mpc−1 in the l
AU  - Kitching,TD
AU  - Heavens,AF
AU  - Alsing,J
AU  - Erben,T
AU  - Heymans,C
AU  - Hildebrandt,H
AU  - Hoekstra,H
AU  - Jaffe,A
AU  - Kiessling,A
AU  - Mellier,Y
AU  - Miller,L
AU  - van,Waerbeke L
AU  - Benjamin,J
AU  - Coupon,J
AU  - Fu,L
AU  - Hudson,MJ
AU  - Kilbinger,M
AU  - Kuijken,K
AU  - Rowe,BTP
AU  - Schrabback,T
AU  - Semboloni,E
AU  - Velander,M
DO  - mnras/stu934
EP  - 1349
PY  - 2014///
SN  - 0035-8711
SP  - 1326
TI  - 3D cosmic shear: cosmology from CFHTLenS
T2  - Monthly Notices of the Royal Astronomical Society
UR  - http://dx.doi.org/10.1093/mnras/stu934
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000339423100032&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - https://academic.oup.com/mnras/article/442/2/1326/985112
UR  - http://hdl.handle.net/10044/1/19689
VL  - 442
ER  -

Download

Professor Andrew H Jaffe

Contact

Assistant

Location

Summary

Citation

BibTex format

RIS format (EndNote, RefMan)