CMB lensing tomography with the DES Science Verification galaxies
CMB lensing tomography with the DES Science Verification galaxies
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DOI：
10.1093/mnras/stv2678
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发表时间：
2015-07
影响因子：
4.8
通讯作者：
T. Giannantonio;P. Fosalba;R. Cawthon;Y. Omori;M. Crocce;F. Elsner;B. Leistedt;S. Dodelson;A. Benoit-Lévy;E. Gaztañaga;G. Holder;H. Peiris;W. Percival;D. Kirk;A. Bauer;B. Benson;G. Bernstein;J. Carretero;T. Crawford;R. Crittenden;D. Huterer;B. Jain;E. Krause;C. Reichardt;A. Ross;G. Simard;B. Soergel;A. Stark;K. Story;J. Vieira;J. Weller;T. Abbott;F. Abdalla;S. Allam;R. Armstrong;M. Banerji;R. Bernstein;E. Bertin;D. Brooks;E. Buckley-Geer;D. Burke;D. Capozzi;J. Carlstrom;A. Rosell;M. Kind;F. Castander;C. Chang;C. Cunha;L. Costa;C. D'Andrea;D. Depoy;S. Desai;H. Diehl;J. Dietrich;P. Doel;T. Eifler;A. Evrard;A. F. Neto;E. Fernandez;D. Finley;B. Flaugher;J. Frieman;D. Gerdes;D. Gruen;R. Gruendl;G. Gutiérrez;W. Holzapfel;K. Honscheid;D. James;K. Kuehn;N. Kuropatkin;O. Lahav;T. Li;M. Lima;M. March;J. Marshall;P. Martini;Peter Melchior;R. Miquel;J. Mohr;R. Nichol;B. Nord;R. Ogando;A. Plazas;A. Romer;A. Roodman;E. Rykoff;M. Sako;B. Saliwanchik;E. Sánchez;M. Schubnell;I. Sevilla-Noarbe;R. C. Smith;M. Soares-Santos;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;J. Thaler;D. Thomas;V. Vikram;A. Walker;R. Wechsler;J. Zuntz
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作者：
T. Giannantonio;P. Fosalba;R. Cawthon;Y. Omori;M. Crocce;F. Elsner;B. Leistedt;S. Dodelson;A. Benoit-Lévy;E. Gaztañaga;G. Holder;H. Peiris;W. Percival;D. Kirk;A. Bauer;B. Benson;G. Bernstein;J. Carretero;T. Crawford;R. Crittenden;D. Huterer;B. Jain;E. Krause;C. Reichardt;A. Ross;G. Simard;B. Soergel;A. Stark;K. Story;J. Vieira;J. Weller;T. Abbott;F. Abdalla;S. Allam;R. Armstrong;M. Banerji;R. Bernstein;E. Bertin;D. Brooks;E. Buckley-Geer;D. Burke;D. Capozzi;J. Carlstrom;A. Rosell;M. Kind;F. Castander;C. Chang;C. Cunha;L. Costa;C. D'Andrea;D. Depoy;S. Desai;H. Diehl;J. Dietrich;P. Doel;T. Eifler;A. Evrard;A. F. Neto;E. Fernandez;D. Finley;B. Flaugher;J. Frieman;D. Gerdes;D. Gruen;R. Gruendl;G. Gutiérrez;W. Holzapfel;K. Honscheid;D. James;K. Kuehn;N. Kuropatkin;O. Lahav;T. Li;M. Lima;M. March;J. Marshall;P. Martini;Peter Melchior;R. Miquel;J. Mohr;R. Nichol;B. Nord;R. Ogando;A. Plazas;A. Romer;A. Roodman;E. Rykoff;M. Sako;B. Saliwanchik;E. Sánchez;M. Schubnell;I. Sevilla-Noarbe;R. C. Smith;M. Soares-Santos;F. Sobreira;E. Suchyta;M. Swanson;G. Tarlé;J. Thaler;D. Thomas;V. Vikram;A. Walker;R. Wechsler;J. Zuntz
我们测量暗能量调查（DES）科学验证数据中的星系密度与普朗克卫星和南极望远镜（SPT）重建的宇宙微波背景（CMB）透镜之间的互相关。当使用DES主星系样本在整个红移范围0.2 2西格玛）检测在所有的箱子。与基准普朗克宇宙学相比，我们发现信号的红移演化符合预期，尽管振幅始终低于红移区间的预测。我们测试了可能影响我们结果的系统学，没有发现明显污染的证据。最后，我们展示了如何使用这些测量来约束整个宇宙时间的结构的增长。我们发现这些数据符合一个模型，其中z< 1.2宇宙的结构振幅是Lambda冷暗物质普朗克宇宙学预测的0.73 ± 0.16倍，偏差为1.7 σ。
We measure the cross-correlation between the galaxy density in the Dark Energy Survey (DES) Science Verification data and the lensing of the cosmic microwave background (CMB) as reconstructed with the Planck satellite and the South Pole Telescope (SPT). When using the DES main galaxy sample over the full redshift range 0.2 2sigma) detections in all bins. Comparing to the fiducial Planck cosmology, we find the redshift evolution of the signal matches expectations, although the amplitude is consistently lower than predicted across redshift bins. We test for possible systematics that could affect our result and find no evidence for significant contamination. Finally, we demonstrate how these measurements can be used to constrain the growth of structure across cosmic time. We find the data are fit by a model in which the amplitude of structure in the z< 1.2 universe is 0.73 ± 0.16 times as large as predicted in the Lambda cold dark matter Planck cosmology, a 1.7sigma deviation.