Multiprobe cosmology from the abundance of SPT clusters and des galaxy clustering and weak lensing

Bocquet, S.; Grandis, S.; Krause, E.; To, C.; Bleem, L. E.; Klein, M.; Mohr, J. J.; Schrabback, T.; Alarcon, A.; Alves, O.; Amon, A.; Andrade-Oliveira, F.; Baxter, E. J.; Bechtol, K.; Becker, M. R.; Bernstein, G. M.; Blazek, J.; Camacho, H.; Campos, A.; Carnero Rosell, A.; Carrasco Kind, M.; Cawthon, R.; Chang, C.; Chen, R.; Choi, A.; Cordero, J.; Crocce, M.; Davis, C.; Derose, J.; Diehl, H. T.; Dodelson, S.; Doux, C.; Drlica-Wagner, A.; Eckert, K.; Eifler, T. F.; Elsner, F.; Elvin-Poole, J.; Everett, S.; Fang, X.; Ferte, A.; Fosalba, P.; Friedrich, O.; Frieman, J.; Gatti, M.; Giannini, G.; Gruen, D.; Gruendl, R. A.; Harrison, I.; Hartley, W. G.; Herner, K.; Huang, H.; Huff, E. M.; Huterer, D.; Jarvis, M.; Kuropatkin, N.; Leget, P. -F.; Lemos, P.; Liddle, A. R.; Maccrann, N.; Mccullough, J.; Muir, J.; Myles, J.; Navarro-Alsina, A.; Pandey, S.; Park, Y.; Porredon, A.; Prat, J.; Raveri, M.; Rollins, R. P.; Roodman, A.; Rosenfeld, R.; Rykoff, E. S.; Sanchez, C.; Sanchez, J.; Secco, L. F.; Sevilla-Noarbe, I.; Sheldon, E.; Shin, T.; Troxel, M. A.; Tutusaus, I.; Varga, T. N.; Weaverdyck, N.; Wechsler, R. H.; H. -Y., Wu; Yanny, B.; Yin, B.; Zhang, Y.; Zuntz, J.; Abbott, T. M. C.; Ade, P. A. R.; Aguena, M.; Allam, S.; Allen, S. W.; Anderson, A. J.; Ansarinejad, B.; Austermann, J. E.; Bayliss, M.; Beall, J. A.; Bender, A. N.; Benson, B. A.; Bianchini, F.; Brodwin, M.; Brooks, D.; Bryant, L.; Burke, D. L.; Canning, R. E. A.; Carlstrom, J. E.; Carretero, J.; Castander, F. J.; Chang, C. L.; Chaubal, P.; Chiang, H. C.; Chou, T. -L.; Citron, R.; Corbett Moran, C.; Costanzi, M.; Crawford, T. M.; Crites, A. T.; Da Costa, L. N.; Pereira, M. E. S.; Davis, T. M.; De Haan, T.; Dobbs, M. A.; Doel, P.; Everett, W.; Farahi, A.; Flaugher, B.; Flores, A. M.; Floyd, B.; Gallicchio, J.; Gaztanaga, E.; George, E. M.; Gladders, M. D.; Gupta, N.; Gutierrez, G.; Halverson, N. W.; Hinton, S. R.; Hlavacek-Larrondo, J.; Holder, G. P.; Hollowood, D. L.; Holzapfel, W. L.; Hrubes, J. D.; Huang, N.; Hubmayr, J.; Irwin, K. D.; James, D. J.; Keruzore, F.; Khullar, G.; Kim, K.; Knox, L.; Kraft, R.; Kuehn, K.; Lahav, O.; Lee, A. T.; Lee, S.; Li, D.; Lidman, C.; Lima, M.; Lowitz, A.; Mahler, G.; Mantz, A.; Marshall, J. L.; Mcdonald, M.; Mcmahon, J. J.; Mena-Fernandez, J.; Meyer, S. S.; Miquel, R.; Montgomery, J.; Natoli, T.; Nibarger, J. P.; Noble, G. I.; Novosad, V.; Ogando, R. L. C.; Padin, S.; Paschos, P.; Patil, S.; Plazas Malagon, A. A.; Pryke, C.; Reichardt, C. L.; Roberson, J.; Romer, A. K.; Romero, C.; Ruhl, J. E.; Saliwanchik, B. R.; Salvati, L.; Samuroff, S.; Sanchez, E.; Santiago, B.; Sarkar, A.; Saro, A.; Schaffer, K. K.; Sharon, K.; Sievers, C.; Smecher, G.; Smith, M.; Somboonpanyakul, T.; Sommer, M.; Stalder, B.; Stark, A. A.; Stephen, J.; Strazzullo, V.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, D.; Tucker, C.; Tucker, D. L.; Veach, T.; Vieira, J. D.; Von Der Linden, A.; Wang, G.; Whitehorn, N.; W. L. K., Wu; Yefremenko, V.; Young, M.; Zebrowski, J. A.; Zohren, H.

doi:10.1103/PhysRevD.111.063533

Cosmic shear, galaxy clustering, and the abundance of massive halos each probe the large-scale structure of the Universe in complementary ways. We present cosmological constraints from the joint analysis of the three probes, building on the latest analyses of the lensing-informed abundance of clusters identified by the South Pole Telescope (SPT) and of the auto- and cross-correlation of galaxy position and weak lensing measurements (3×2pt) in the Dark Energy Survey (DES). We consider the cosmological correlation between the different tracers and we account for the systematic uncertainties that are shared between the large-scale lensing correlation functions and the small-scale lensing-based cluster mass calibration. Marginalized over the remaining Λ cold dark matter (ΛCDM) parameters (including the sum of neutrino masses) and 52 astrophysical modeling parameters, we measure ωm=0.300±0.017 and σ8=0.797±0.026. Compared to constraints from Planck primary cosmic microwave background (CMB) anisotropies, our constraints are only 15% wider with a probability to exceed of 0.22 (1.2σ) for the two-parameter difference. We further obtain S8σ8(ωm/0.3)0.5=0.796±0.013 which is lower than the Planck measurement at the 1.6σ level. The combined SPT cluster, DES 3×2pt, and Planck datasets mildly prefer a nonzero positive neutrino mass, with a 95% upper limit mν<0.25 eV on the sum of neutrino masses. Assuming a wCDM model, we constrain the dark energy equation of state parameter w=-1.15-0.17+0.23 and when combining with Planck primary CMB anisotropies, we recover w=-1.20-0.09+0.15, a 1.7σ difference with a cosmological constant. The precision of our results highlights the benefits of multiwavelength multiprobe cosmology and our analysis paves the way for upcoming joint analyses of next-generation datasets.