☆ 4.7 Article

Dark Energy Survey Year 1 results: constraints on intrinsic alignments and their colour dependence from galaxy clustering and weak lensing

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY (2019)

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Journal

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 489, Issue 4, Pages 5453-5482

Publisher

OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz2197

Keywords

gravitational lensing: weak; galaxies: statistics; cosmological parameters; cosmology: observations

Categories

Astronomy & Astrophysics

Funding

  1. NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF5-160138]
  2. NASA [NAS8-03060]
  3. SNSF Ambizione Fellowship
  4. U.S. Department of Energy
  5. U.S. National Science Foundation
  6. Ministry of Science and Education of Spain
  7. Science and Technology Facilities Council of the United Kingdom
  8. Higher Education Funding Council for England
  9. National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
  10. Kavli Institute of Cosmological Physics at the University of Chicago
  11. Center for Cosmology and Astro-Particle Physics at the Ohio State University
  12. Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University
  13. Financiadora de Estudos e Projetos
  14. Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro
  15. Conselho Nacional de Desenvolvimento Cientifico e Tecnologico
  16. Ministerio da Ciencia, Tecnologia e Inovacao
  17. Deutsche Forschungsgemeinschaft
  18. National Science Foundation [AST-1138766, AST-1536171]
  19. MINECO [AYA2015-71825, ESP2015-88861, FPA2015-68048, SEV-2012-0234, SEV-2016-0597, MDM-2015-0509]
  20. ERDF funds from the European Union
  21. CERCA program of the Generalitat de Catalunya
  22. European Research Council under the European Union [240672, 291329, 306478]
  23. Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO) [CE110001020]
  24. U.S. Department of Energy, Office of Science, Office of High Energy Physics [AC02-07CH11359]
  25. Argonne National Laboratory
  26. University of California at Santa Cruz
  27. University of Cambridge
  28. University of Chicago
  29. DES-Brazil Consortium
  30. University of Edinburgh
  31. Eidgenossische Technische Hochschule (ETH) Zurich
  32. University of Illinois at Urbana-Champaign
  33. Institut de Ciencies de l'Espai (IEEC/CSIC)
  34. Institut de F'isica d'Altes Energies
  35. Ludwig-Maximilians Universitat Munchen
  36. associated Excellence Cluster Universe
  37. University of Michigan
  38. National Optical Astronomy Observatory
  39. University of Nottingham
  40. Ohio State University
  41. University of Pennsylvania
  42. University of Portsmouth
  43. SLAC National Accelerator Laboratory, Stanford University
  44. University of Sussex
  45. Texas AM University
  46. OzDES Membership Consortium
  47. Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid
  48. University College London
  49. Fermi National Accelerator Laboratory
  50. Lawrence Berkeley National Laboratory
  51. STFC [ST/P000649/1, ST/S000550/1] Funding Source: UKRI

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We perform a joint analysis of intrinsic alignments and cosmology using tomographic weak lensing, galaxy clustering, and galaxy-galaxy lensing measurements from Year 1 (Y1) of the Dark Energy Survey. We define early- and late-type subsamples, which are found to pass a series of systematics tests, including for spurious photometric redshift error and point spread function correlations. We analyse these split data alongside the fiducial mixed Y1 sample using a range of intrinsic alignment models. In a fiducial non-linear alignment model analysis, assuming a flat Lambda cold dark matter cosmology, we find a significant difference in intrinsic alignment amplitude, with early-type galaxies favouring A(IA) = 2.38(-0.31)(+0.32) and latetype galaxies consistent with no intrinsic alignments at 0.05(-0.09)(+0.10). The analysis is repeated using a number of extended model spaces, including a physically motivated model that includes both tidal torquing and tidal alignment mechanisms. In multiprobe likelihood chains in which cosmology, intrinsic alignments in both galaxy samples and all other relevant systematics are varied simultaneously, we find the tidal alignment and tidal torquing parts of the intrinsic alignment signal have amplitudes A(1) = 2.66(-0.66)(+0.67), A(2) = -2.94(-1.83)(+1.94), respectively, for earlytype galaxies and A(1) = 0.62(-0.41)(+0.41), A(2) = -2.26(-1.16)(+1.30) for late-type galaxies. In the full (mixed) Y1 sample the best constraints are A(1) = 0.70(-0.38)(+0.41), A(2) = -1.36(-1.41)(+1.08). For all galaxy splits and IA models considered, we report cosmological parameter constraints consistent with the results of the main DES Y1 cosmic shear and multiprobe cosmology papers.

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Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck. I. Construction of CMB lensing maps and modeling choices

Y. Omori, E. J. Baxter, C. Chang, O. Friedrich, A. Alarcon, O. Alves, A. Amon, F. Andrade-Oliveira, K. Bechtol, M. R. Becker, G. M. Bernstein, J. Blazek, L. E. Bleem, H. Camacho, A. Campos, A. Carnero Rosell, M. Carrasco Kind, R. Cawthon, R. Chen, A. Choi, J. Cordero, T. M. Crawford, M. Crocce, C. Davis, J. DeRose, S. Dodelson, C. Doux, A. Drlica-Wagner, K. Eckert, T. F. Eifler, F. Elsner, J. Elvin-Poole, S. Everett, X. Fang, A. Ferte, P. Fosalba, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, I. Harrison, K. Herner, H. Huang, E. M. Huff, D. Huterer, M. Jarvis, E. Krause, N. Kuropatkin, P. -F. Leget, P. Lemos, A. R. Liddle, N. MacCrann, J. McCullough, J. Muir, J. Myles, A. Navarro-Alsina, S. Pandey, Y. Park, A. Porredon, J. Prat, M. Raveri, R. P. Rollins, A. Roodman, R. Rosenfeld, A. J. Ross, E. S. Rykoff, C. Sanchez, J. Sanchez, L. F. Secco, I. Sevilla-Noarbe, E. Sheldon, T. Shin, M. A. Troxel, I. Tutusaus, T. N. Varga, N. Weaverdyck, R. H. Wechsler, W. L. K. Wu, B. Yanny, B. Yin, Y. Zhang, J. Zuntz, T. M. C. Abbott, M. Aguena, S. Allam, J. Annis, D. Bacon, B. A. Benson, E. Bertin, S. Bocquet, D. Brooks, D. L. Burke, J. E. Carlstrom, J. Carretero, C. L. Chang, R. Chown, M. Costanzi, L. N. da Costa, A. T. Crites, M. E. S. Pereira, T. de Haan, J. De Vicente, S. Desai, H. T. Diehl, M. A. Dobbs, P. Doel, W. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. Garcia-Bellido, E. Gaztanaga, E. M. George, T. Giannantonio, N. W. Halverson, S. R. Hinton, G. P. Holder, D. L. Hollowood, W. L. Holzapfel, K. Honscheid, J. D. Hrubes, D. J. James, L. Knox, K. Kuehn, O. Lahav, A. T. Lee, M. Lima, D. Luong-Van, M. March, J. J. McMahon, P. Melchior, F. Menanteau, S. S. Meyer, R. Miquel, L. Mocanu, J. J. Mohr, R. Morgan, T. Natoli, S. Padin, A. Palmese, F. Paz-Chinchon, A. Pieres, A. A. Plazas Malagon, C. Pryke, C. L. Reichardt, A. K. Romer, J. E. Ruhl, E. Sanchez, K. K. Schaffer, M. Schubnell, S. Serrano, E. Shirokoff, M. Smith, Z. Staniszewski, A. A. Stark, E. Suchyta, G. Tarle, D. Thomas, C. To, J. D. Vieira, J. Weller, R. Williamson

Summary: Joint analyses of cross-correlations between galaxy measurements and lensing of the cosmic microwave background (CMB) provide powerful constraints on the large-scale structure of the Universe. In this article, we present an improved CMB lensing map in the SPT-SZ survey footprint and the analysis methodology to extract cosmological information. We find that the joint analysis of CMB lensing cross-correlations can provide constraints on the shear calibration amplitude at the 5% to 10% level.

PHYSICAL REVIEW D (2023)

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Article Astronomy & Astrophysics

Measurement of the mean central optical depth of galaxy clusters via the pairwise kinematic Sunyaev-Zel'dovich effect with SPT-3G and DES

E. Schiappucci, F. Bianchini, M. Aguena, M. Archipley, L. Balkenhol, L. E. Bleem, P. Chaubal, T. M. Crawford, S. Grandis, Y. Omori, C. L. Reichardt, E. Rozo, E. S. Rykoff, C. To, T. M. C. Abbott, P. A. R. Ade, O. Alves, A. J. Anderson, F. Andrade-Oliveira, J. Annis, J. S. Avva, D. Bacon, K. Benabed, A. N. Bender, B. A. Benson, G. M. Bernstein, E. Bertin, S. Bocquet, F. R. Bouchet, D. Brooks, D. L. Burke, J. E. Carlstrom, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, T. W. Cecil, C. L. Chang, P. M. Chichura, T. -L. Chou, M. Costanzi, A. Cukierman, L. N. da Costa, C. Daley, T. de Haan, S. Desai, K. R. Dibert, H. T. Diehl, M. A. Dobbs, P. Doel, C. Doux, D. Dutcher, S. Everett, W. Everett, C. Feng, K. R. Ferguson, I. Ferrero, A. Ferte, B. Flaugher, A. Foster, J. Frieman, S. Galli, A. E. Gambrel, J. Garcia-Bellido, R. W. Gardner, M. Gatti, T. Giannantonio, N. Goeckner-Wald, D. Gruen, R. Gualtieri, S. Guns, G. Gutierrez, N. W. Halverson, S. R. Hinton, E. Hivon, G. P. Holder, D. L. Hollowood, W. L. Holzapfel, K. Honscheid, J. C. Hood, N. Huang, D. J. James, L. Knox, M. Korman, K. Kuehn, C. -L. Kuo, O. Lahav, A. T. Lee, C. Lidman, M. Lima, A. E. Lowitz, C. Lu, M. March, J. Mena-Fernandez, F. Menanteau, M. Millea, R. Miquel, J. J. Mohr, J. Montgomery, J. Muir, T. Natoli, G. I. Noble, V. Novosad, R. L. C. Ogando, S. Padin, Z. Pan, F. Paz-Chinchon, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagon, K. Prabhu, J. Prat, W. Quan, A. Rahlin, M. Raveri, M. Rodriguez-Monroy, A. K. Romer, M. Rouble, J. E. Ruhl, E. Sanchez, V. Scarpine, M. Schubnell, G. Smecher, M. Smith, M. Soares-Santos, J. A. Sobrin, E. Suchyta, A. Suzuki, G. Tarle, D. Thomas, K. L. Thompson, B. Thorne, C. Tucker, C. Umilta, J. D. Vieira, M. Vincenzi, G. Wang, N. Weaverdyck, J. Weller, N. Whitehorn, W. L. K. Wu, V. Yefremenko, M. R. Young

Summary: We use the pairwise kinematic Sunyaev-Zel'dovich (KSZ) effect to infer the average optical depth of a sample of optically selected galaxy clusters from the Dark Energy Survey. The pairwise KSZ signal is detected at 4.1 sigma in cosmic microwave background temperature maps from two years of observations with the SPT-3G camera. After data cuts, there are 24,580 clusters in the observed area. We calculate the mean optical depth using two techniques: the pairwise KSZ signal gives tau over bar e = (2.97 +/- 0.73) x 10-3, while the thermal SZ signal gives tau over bar e = (2.51 +/- 0.55stat +/- 0.15syst) x 10-3. The two measures agree within 0.6 sigma. We perform systematic checks to ensure the validity of our analysis.

PHYSICAL REVIEW D (2023)

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