%0 Generic %1 chang2022joint %A Chang, C. %A Omori, Y. %A Baxter, E. J. %A Doux, C. %A Choi, A. %A Pandey, S. %A Alarcon, A. %A Alves, O. %A Amon, A. %A Andrade-Oliveira, F. %A Bechtol, K. %A Becker, M. R. %A Bernstein, G. M. %A Bianchini, F. %A Blazek, J. %A Bleem, L. E. %A Camacho, H. %A Campos, A. %A Rosell, A. Carnero %A Kind, M. Carrasco %A Cawthon, R. %A Chen, R. %A Cordero, J. %A Crawford, T. M. %A Crocce, M. %A Davis, C. %A DeRose, J. %A Dodelson, S. %A Drlica-Wagner, A. %A Eckert, K. %A Eifler, T. F. %A Elsner, F. %A Elvin-Poole, J. %A Everett, S. %A Fang, X. %A Ferté, A. %A Fosalba, P. %A Friedrich, O. %A Gatti, M. %A Giannini, G. %A Gruen, D. %A Gruendl, R. A. %A Harrison, I. %A Herner, K. %A Huang, H. %A Huff, E. M. %A Huterer, D. %A Jarvis, M. %A Kovacs, A. %A Krause, E. %A Kuropatkin, N. %A Leget, P. F. %A Lemos, P. %A Liddle, A. R. %A MacCrann, N. %A McCullough, J. %A Muir, J. %A Myles, J. %A Navarro-Alsina, A. %A Park, Y. %A Porredon, A. %A Prat, J. %A Raveri, M. %A Rollins, R. P. %A Roodman, A. %A Rosenfeld, R. %A Ross, A. J. %A Rykoff, E. S. %A Sánchez, C. %A Sanchez, J. %A Secco, L. F. %A Sevilla-Noarbe, I. %A Sheldon, E. %A Shin, T. %A Troxel, M. A. %A Tutusaus, I. %A Varga, T. N. %A Weaverdyck, N. %A Wechsler, R. H. %A Wu, W. L. K. %A Yanny, B. %A Yin, B. %A Zhang, Y. %A Zuntz, J. %A Abbott, T. M. C. %A Aguena, M. %A Allam, S. %A Annis, J. %A Bacon, D. %A Benson, B. A. %A Bertin, E. %A Bocquet, S. %A Brooks, D. %A Burke, D. L. %A Carlstrom, J. E. %A Carretero, J. %A Chang, C. L. %A Chown, R. %A Costanzi, M. %A da Costa, L. N. %A Crites, A. T. %A Pereira, M. E. S. %A de Haan, T. %A De Vicente, J. %A Desai, S. %A Diehl, H. T. %A Dobbs, M. A. %A Doel, P. %A Everett, W. %A Ferrero, I. %A Flaugher, B. %A Friedel, D. %A Frieman, J. %A García-Bellido, J. %A Gaztanaga, E. %A George, E. M. %A Giannantonio, T. %A Halverson, N. W. %A Hinton, S. R. %A Holder, G. P. %A Hollowood, D. L. %A Holzapfel, W. L. %A Honscheid, K. %A Hrubes, J. D. %A James, D. J. %A Knox, L. %A Kuehn, K. %A Lahav, O. %A Lee, A. T. %A Lima, M. %A Luong-Van, D. %A March, M. %A McMahon, J. J. %A Melchior, P. %A Menanteau, F. %A Meyer, S. S. %A Miquel, R. %A Mocanu, L. %A Mohr, J. J. %A Morgan, R. %A Natoli, T. %A Padin, S. %A Palmese, A. %A Paz-Chinchón, F. %A Pieres, A. %A Malagón, A. A. Plazas %A Pryke, C. %A Reichardt, C. L. %A Rodríguez-Monroy, M. %A Romer, A. K. %A Ruhl, J. E. %A Sanchez, E. %A Schaffer, K. K. %A Schubnell, M. %A Serrano, S. %A Shirokoff, E. %A Smith, M. %A Staniszewski, Z. %A Stark, A. A. %A Suchyta, E. %A Tarle, G. %A Thomas, D. %A To, C. %A Vieira, J. D. %A Weller, J. %A Williamson, R. %D 2022 %K library %T Joint analysis of DES Year 3 data and CMB lensing from SPT and Planck II: Cross-correlation measurements and cosmological constraints %U http://arxiv.org/abs/2203.12440 %X Cross-correlations of galaxy positions and galaxy shears with maps of gravitational lensing of the cosmic microwave background (CMB) are sensitive to the distribution of large-scale structure in the Universe. Such cross-correlations are also expected to be immune to some of the systematic effects that complicate correlation measurements internal to galaxy surveys. We present measurements and modeling of the cross-correlations between galaxy positions and galaxy lensing measured in the first three years of data from the Dark Energy Survey with CMB lensing maps derived from a combination of data from the 2500 deg$^2$ SPT-SZ survey conducted with the South Pole Telescope and full-sky data from the Planck satellite. The CMB lensing maps used in this analysis have been constructed in a way that minimizes biases from the thermal Sunyaev Zel'dovich effect, making them well suited for cross-correlation studies. The total signal-to-noise of the cross-correlation measurements is 23.9 (25.7) when using a choice of angular scales optimized for a linear (nonlinear) galaxy bias model. We use the cross-correlation measurements to obtain constraints on cosmological parameters. For our fiducial galaxy sample, which consist of four bins of magnitude-selected galaxies, we find constraints of $Ømega_m = 0.27^+0.03_-0.05$ and $S_8 \sigma_8 Ømega_m/0.3= 0.74^+0.03_-0.04$ ($Ømega_m = 0.25^+0.03_-0.04$ and $S_8 = 0.73^+0.04_-0.03$) when assuming linear (nonlinear) galaxy bias in our modeling. Considering only the cross-correlation of galaxy shear with CMB lensing, we find $Ømega_m= 0.27^+0.04_-0.06$ and $S_8= 0.74^+0.03_-0.04$. Our constraints on $S_8$ are consistent with recent cosmic shear measurements, but lower than the values preferred by primary CMB measurements from Planck.

@misc{chang2022joint, abstract = {Cross-correlations of galaxy positions and galaxy shears with maps of gravitational lensing of the cosmic microwave background (CMB) are sensitive to the distribution of large-scale structure in the Universe. Such cross-correlations are also expected to be immune to some of the systematic effects that complicate correlation measurements internal to galaxy surveys. We present measurements and modeling of the cross-correlations between galaxy positions and galaxy lensing measured in the first three years of data from the Dark Energy Survey with CMB lensing maps derived from a combination of data from the 2500 deg$^2$ SPT-SZ survey conducted with the South Pole Telescope and full-sky data from the Planck satellite. The CMB lensing maps used in this analysis have been constructed in a way that minimizes biases from the thermal Sunyaev Zel'dovich effect, making them well suited for cross-correlation studies. The total signal-to-noise of the cross-correlation measurements is 23.9 (25.7) when using a choice of angular scales optimized for a linear (nonlinear) galaxy bias model. We use the cross-correlation measurements to obtain constraints on cosmological parameters. For our fiducial galaxy sample, which consist of four bins of magnitude-selected galaxies, we find constraints of $\Omega_{m} = 0.27^{+0.03}_{-0.05}$ and $S_{8} \equiv \sigma_8 \sqrt{\Omega_{m}/0.3}= 0.74^{+0.03}_{-0.04}$ ($\Omega_{m} = 0.25^{+0.03}_{-0.04}$ and $S_{8} = 0.73^{+0.04}_{-0.03}$) when assuming linear (nonlinear) galaxy bias in our modeling. Considering only the cross-correlation of galaxy shear with CMB lensing, we find $\Omega_{m}= 0.27^{+0.04}_{-0.06}$ and $S_{8}= 0.74^{+0.03}_{-0.04}$. Our constraints on $S_8$ are consistent with recent cosmic shear measurements, but lower than the values preferred by primary CMB measurements from Planck.}, added-at = {2022-03-24T09:53:22.000+0100}, author = {Chang, C. and Omori, Y. and Baxter, E. J. and Doux, C. and Choi, A. and Pandey, S. and Alarcon, A. and Alves, O. and Amon, A. and Andrade-Oliveira, F. and Bechtol, K. and Becker, M. R. and Bernstein, G. M. and Bianchini, F. and Blazek, J. and Bleem, L. E. and Camacho, H. and Campos, A. and Rosell, A. Carnero and Kind, M. Carrasco and Cawthon, R. and Chen, R. and Cordero, J. and Crawford, T. M. and Crocce, M. and Davis, C. and DeRose, J. and Dodelson, S. and Drlica-Wagner, A. and Eckert, K. and Eifler, T. F. and Elsner, F. and Elvin-Poole, J. and Everett, S. and Fang, X. and Ferté, A. and Fosalba, P. and Friedrich, O. and Gatti, M. and Giannini, G. and Gruen, D. and Gruendl, R. A. and Harrison, I. and Herner, K. and Huang, H. and Huff, E. M. and Huterer, D. and Jarvis, M. and Kovacs, A. and Krause, E. and Kuropatkin, N. and Leget, P. F. and Lemos, P. and Liddle, A. R. and MacCrann, N. and McCullough, J. and Muir, J. and Myles, J. and Navarro-Alsina, A. and Park, Y. and Porredon, A. and Prat, J. and Raveri, M. and Rollins, R. P. and Roodman, A. and Rosenfeld, R. and Ross, A. J. and Rykoff, E. S. and Sánchez, C. and Sanchez, J. and Secco, L. F. and Sevilla-Noarbe, I. and Sheldon, E. and Shin, T. and Troxel, M. A. and Tutusaus, I. and Varga, T. N. and Weaverdyck, N. and Wechsler, R. H. and Wu, W. L. K. and Yanny, B. and Yin, B. and Zhang, Y. and Zuntz, J. and Abbott, T. M. C. and Aguena, M. and Allam, S. and Annis, J. and Bacon, D. and Benson, B. A. and Bertin, E. and Bocquet, S. and Brooks, D. and Burke, D. L. and Carlstrom, J. E. and Carretero, J. and Chang, C. L. and Chown, R. and Costanzi, M. and da Costa, L. N. and Crites, A. T. and Pereira, M. E. S. and de Haan, T. and De Vicente, J. and Desai, S. and Diehl, H. T. and Dobbs, M. A. and Doel, P. and Everett, W. and Ferrero, I. and Flaugher, B. and Friedel, D. and Frieman, J. and García-Bellido, J. and Gaztanaga, E. and George, E. M. and Giannantonio, T. and Halverson, N. W. and Hinton, S. R. and Holder, G. P. and Hollowood, D. L. and Holzapfel, W. L. and Honscheid, K. and Hrubes, J. D. and James, D. J. and Knox, L. and Kuehn, K. and Lahav, O. and Lee, A. T. and Lima, M. and Luong-Van, D. and March, M. and McMahon, J. J. and Melchior, P. and Menanteau, F. and Meyer, S. S. and Miquel, R. and Mocanu, L. and Mohr, J. J. and Morgan, R. and Natoli, T. and Padin, S. and Palmese, A. and Paz-Chinchón, F. and Pieres, A. and Malagón, A. A. Plazas and Pryke, C. and Reichardt, C. L. and Rodríguez-Monroy, M. and Romer, A. K. and Ruhl, J. E. and Sanchez, E. and Schaffer, K. K. and Schubnell, M. and Serrano, S. and Shirokoff, E. and Smith, M. and Staniszewski, Z. and Stark, A. A. and Suchyta, E. and Tarle, G. and Thomas, D. and To, C. and Vieira, J. D. and Weller, J. and Williamson, R.}, biburl = {https://www.bibsonomy.org/bibtex/27169540b5ee90401a9c943fcc079acbf/gpkulkarni}, description = {Joint analysis of DES Year 3 data and CMB lensing from SPT and Planck II: Cross-correlation measurements and cosmological constraints}, interhash = {8e23a5b304cf964c863f547fba0f4efb}, intrahash = {7169540b5ee90401a9c943fcc079acbf}, keywords = {library}, note = {cite arxiv:2203.12440Comment: 25 pages, 19 figures, to be submitted to PRD}, timestamp = {2022-03-24T09:53:22.000+0100}, title = {Joint analysis of DES Year 3 data and CMB lensing from SPT and Planck II: Cross-correlation measurements and cosmological constraints}, url = {http://arxiv.org/abs/2203.12440}, year = 2022 }