Cross-correlation of gravitational lensing from DES Science Verification data with SPT and Planck lensing

被引：51

作者：

Kirk, D. ^{[1
]}

Omori, Y. ^{[2
]}

Benoit-Levy, A. ^{[1
,3
,4
,5
,6
]}

Cawthon, R. ^{[6
,7
]}

Chang, C. ^{[8
]}

Larsen, P. ^{[9
,10
]}

Amara, A. ^{[8
]}

Bacon, D. ^{[11
]}

Crawford, T. M. ^{[6
,7
]}

Dodelson, S. ^{[5
,6
,12
]}

Fosalba, P. ^{[13
]}

Giannantonio, T. ^{[9
,10
,14
]}

Holder, G. ^{[2
]}

Jain, B. ^{[15
]}

Kacprzak, T. ^{[8
]}

Lahav, O. ^{[1
]}

MacCrann, N. ^{[16
]}

Nicola, A. ^{[8
]}

Refregier, A. ^{[8
]}

Sheldon, E. ^{[17
]}

Story, K. T. ^{[6
,12
]}

Troxel, M. A. ^{[16
]}

Vieira, J. D. ^{[18
,19
]}

Vikram, V. ^{[20
]}

Zuntz, J. ^{[16
]}

Abbott, T. M. C. ^{[21
]}

Abdalla, F. B. ^{[1
,22
]}

Becker, M. R. ^{[17
,23
]}

Benson, B. A. ^{[5
,6
,7
,28
]}

Bernstein, G. M. ^{[15
]}

Bernstein, R. A. ^{[24
]}

Bleem, L. E. ^{[6
,20
]}

Bonnett, C. ^{[25
]}

Bridle, S. L. ^{[16
]}

Brooks, D. ^{[1
]}

Buckley-Geer, E. ^{[5
]}

Burke, D. L. ^{[23
,26
]}

Capozzi, D. ^{[11
]}

Carlstrom, J. E. ^{[6
,7
,12
]}

Carnero Rosell, A. ^{[27
,28
]}

Kind, M. Carrasco ^{[18
,19
,29
]}

Carretero, J. ^{[13
,25
]}

Crocce, M. ^{[13
]}

Cunha, C. E. ^{[23
]}

D'Andrea, C. B. ^{[11
,30
,32
]}

da Costa, L. N. ^{[27
,28
]}

Desai, S. ^{[31
,32
]}

Diehl, H. T. ^{[5
]}

Dietrich, J. P. ^{[31
,32
]}

Doel, P. ^{[1
]}

机构：

[1] UCL, Dept Phys & Astron, Astrophys Grp, 132 Hampstead Rd, London NW1 2PS, England

[2] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada

[3] Univ Paris 06, Sorbonne Univ, 98 Bis Bd Arago, F-75014 Paris, France

[4] CNRS, UMR 7095, Inst Astrophys Paris, 98 Bis Bd Arago, F-75014 Paris, France

[5] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[6] Univ Chicago, Kavli Inst Cosmol Phys, 933 East 56th St, Chicago, IL 60637 USA

[7] Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA

[8] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland

[9] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

[10] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[11] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[12] Univ Chicago, Dept Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA

[13] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[14] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England

[15] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[16] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England

[17] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA

[18] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[19] Univ Illinois, Dept Phys, 1002 W Green St, Urbana, IL 61801 USA

[20] Argonne Natl Lab, Div High Energy Phys, 9700 S Cass Ave, Argonne, IL 60439 USA

[21] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile

[22] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa

[23] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA

[24] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA

[25] Barcelona Inst Sci & Technol, Inst Fis Altes Energies, Campus UAB, Bellaterra 08193, Barcelona, Spain

[26] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[27] Lab Interinst & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[28] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[29] Natl Ctr Supercomputing Applicat, 1205 West Clark St, Urbana, IL 61801 USA

[30] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[31] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany

[32] Univ Munich, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany

[33] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[34] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[35] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[36] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA

[37] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA

[38] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany

[39] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA

[40] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA

[41] Australian Astron Observ, N Ryde, NSW 2113, Australia

[42] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil

[43] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA

[44] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

[45] Inst Catalana Rec & Estudis Avancats, E-08010 Barcelona, Spain

[46] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia

[47] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA

[48] CIEMAT, E-28040 Madrid, Spain

[49] Univ Estadual Paulista, Inst Fis Teor, Rua Dr Bento T Ferraz 271, BR-01140070 Sao Paulo, SP, Brazil

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2016年 / 459卷 / 01期

基金：

美国国家科学基金会; 欧洲研究理事会; 英国科学技术设施理事会;

关键词：

gravitational lensing: weak; methods: data analysis; cosmic background radiation; DARK ENERGY SURVEY; INTRINSIC ALIGNMENTS; COSMIC SHEAR; STATISTICAL-ANALYSIS; GALAXY ALIGNMENTS; POWER SPECTRUM; WEAK; CONSTRAINTS; INFORMATION; COSMOLOGY;

D O I：

10.1093/mnras/stw570

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We measure the cross-correlation between weak lensing of galaxy images and of the cosmic microwave background (CMB). The effects of gravitational lensing on different sources will be correlated if the lensing is caused by the same mass fluctuations. We use galaxy shape measurements from 139 deg(2) of the Dark Energy Survey (DES) Science Verification data and overlapping CMB lensing from the South Pole Telescope (SPT) and Planck. The DES source galaxies have a median redshift of z(med) similar to 0.7, while the CMB lensing kernel is broad and peaks at z similar to 2. The resulting cross-correlation is maximally sensitive to mass fluctuations at z similar to 0.44. Assuming the Planck 2015 best-fitting cosmology, the amplitude of the DESxSPT cross-power is found to be A(SPT) = 0.88 +/- 0.30 and that from DESxPlanck to be A(Planck) = 0.86 +/- 0.39, where A = 1 corresponds to the theoretical prediction. These are consistent with the expected signal and correspond to significances of 2.9 sigma and 2.2 sigma, respectively. We demonstrate that our results are robust to a number of important systematic effects including the shear measurement method, estimator choice, photo-z uncertainty and CMB lensing systematics. We calculate a value of A = 1.08 +/- 0.36 for DESxSPT when we correct the observations with a simple intrinsic alignment model. With three measurements of this cross-correlation now existing in the literature, there is not yet reliable evidence for any deviation from the expected LCDM level of cross-correlation. We provide forecasts for the expected signal-to-noise ratio of the combination of the five-year DES survey and SPT-3G.

引用

页码：21 / 34

页数：14

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