3D cosmic shear: cosmology from CFHTLenS
3D cosmic shear: cosmology from CFHTLenS
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DOI：
10.1093/mnras/stu934
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发表时间：
2014-01
影响因子：
4.8
通讯作者：
T. Kitching;A. Heavens;Justin Alsing;T. Erben;C. Heymans;H. Hildebrandt;H. Hildebrandt;H. Hoekstra;A. Jaffe;A. Kiessling;Y. Mellier;L. Miller;L. Waerbeke;J. Benjamin;J. Coupon;L. Fu;M. Hudson;M. Hudson;M. Kilbinger;K. Kuijken;B. Rowe;T. Schrabback;T. Schrabback;T. Schrabback;E. Semboloni;M. Velander;M. Velander
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文献类型：
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作者：
T. Kitching;A. Heavens;Justin Alsing;T. Erben;C. Heymans;H. Hildebrandt;H. Hildebrandt;H. Hoekstra;A. Jaffe;A. Kiessling;Y. Mellier;L. Miller;L. Waerbeke;J. Benjamin;J. Coupon;L. Fu;M. Hudson;M. Hudson;M. Kilbinger;K. Kuijken;B. Rowe;T. Schrabback;T. Schrabback;T. Schrabback;E. Semboloni;M. Velander;M. Velander
本文首次将三维宇宙剪切应用于宽场弱透镜巡天。3D宇宙剪切是一种使用球谐方法分析三维弱透镜效应的技术，并且不会在红移方向上对数据进行分组。这是适用于CFHTLenS，一个154平方度的成像调查，平均红移为0.7和有效的数密度为11星系每平方角分钟可用于弱透镜。为了解释调查掩模，我们在弱透镜数据上应用3D伪Cl方法，并且为了避免高度非线性区域中的不确定性，我们分别分析径向波数k<=1.5h/Mpc和k<=5.0h/Mpc，以及角波数l~400-5000。我们展示了如何从完整的3D宇宙剪切功率谱中恢复2D和层析功率谱，并给出了2D宇宙剪切功率谱的测量结果，以及一组2-bin和6-bin宇宙剪切层析功率谱的测量结果;在这样做时，我们发现，在根据数据计算这种2D和断层摄影功率谱时使用3D功率自然地占到了功率谱中的最小尺度。物质功率谱我们使用三维宇宙剪切来约束宇宙学参数OmegaM，OmegaB，sigma 8，h，ns，w 0，wa。对于一个非演化的暗能量状态方程，并假设一个平坦的宇宙学，透镜结合WMAP 7的结果是h=0.78+/-0.12，OmegaM=0.252+/-0.079，sigma 8 =0.88+/-0.23和w=-1.16+/-0.38，只使用尺度k<=1.5h/Mpc。我们还提出了与第一年普朗克结果相结合的透镜效应结果，我们没有发现与这种分析结果的紧张关系，但我们也没有发现单独的普朗克结果的显着改善。我们发现在1.5 < k < 5.0 h/Mpc的小尺度下，与LCDM相比，在透镜数据中发现了功率抑制的证据，这与重子反馈对物质功率谱的影响的预测一致。
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-Cl approach on weak lensing data, and to avoid uncertainties in the highly non-linear regime, we separately analyse radial wave numbers k<=1.5h/Mpc and k<=5.0h/Mpc, and angular wavenumbers l~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 OmegaM, OmegaB, sigma8, h, ns, w0, wa. For a non-evolving dark energy equation of state, and assuming a flat cosmology, lensing combined with WMAP7 results in h=0.78+/-0.12, OmegaM=0.252+/-0.079, sigma8=0.88+/-0.23 and w=-1.16+/-0.38 using only scales k<=1.5h/Mpc. 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 LCDM on small scales 1.5 < k < 5.0 h/Mpc in the lensing data, which is consistent with predictions of the effect of baryonic feedback on the matter power spectrum.