A measurement of secondary cosmic microwave background anisotropies from the 2500 square-degree SPT-SZ survey

• Published in: The Astrophysical Journal
• Main Authors: George, E. M., Reichardt, C. L., Aird, K. A., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Cho, H-M., Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Dudley, J., Halverson, N. W., Harrington, N. L., Holder, G. P., Holzapfel, W. L., Hou, Z., Hrubes, J. D., Keisler, R., Knox, L., Lee, A. T., Leitch, E. M., Lueker, M., Luong-Van, D., McMahon, J. J., Mehl, J., Meyer, S. S., Millea, M., Mocanu, L. M., Mohr, J. J., Montroy, T. E., Padin, S., Plagge, T., Pryke, C., Ruhl, J. E., Schaffer, K. K., Shaw, L., Shirokoff, E., Spieler, H. G., Staniszewski, Z., Stark, A. A., Story, K. T., van Engelen, A., Vanderlinde, K., Vieira, J. D., Williamson, R., Zahn, O.
• Language: unknown
• Published: 2022
• Subjects: 79 ASTRONOMY AND ASTROPHYSICS; South Pole; South pole
• Online Access: http://www.osti.gov/servlets/purl/1362117; https://www.osti.gov/biblio/1362117; https://doi.org/10.1088/0004-637X/799/2/177

Here, we present measurements of secondary cosmic microwave background (CMB) anisotropies and cosmic infrared background (CIB) fluctuations using data from the South Pole Telescope (SPT) covering the complete 2540 deg2 SPT-SZ survey area. Data in the three SPT-SZ frequency bands centered at 95, 150, and 220 GHz, are used to produce six angular power spectra (three single-frequency auto-spectra and three cross-spectra) covering the multipole range 2000 < ℓ < 11, 000 (angular scales 5' gsim θ gsim 1'). These are the most precise measurements of the angular power spectra at ℓ > 2500 at these frequencies. The main contributors to the power spectra at these angular scales and frequencies are the primary CMB, CIB, thermal and kinematic Sunyaev-Zel'dovich effects (tSZ and kSZ), and radio galaxies. We include a constraint on the tSZ power from a measurement of the tSZ bispectrum from 800 deg2 of the SPT-SZ survey. We measure the tSZ power at 143 GHz to be $D^{\rm tSZ}_{3000} = 4.08^{+0.58}_{-0.67}\,\mu {\rm K}^2{}$ and the kSZ power to be $D^{\rm kSZ}_{3000} = 2.9 \pm 1.3\, \mu {\rm K}^2{}$. The data prefer positive kSZ power at 98.1% CL. We measure a correlation coefficient of $\xi = 0.113^{+0.057}_{-0.054}$ between sources of tSZ and CIB power, with ξ < 0 disfavored at a confidence level of 99.0%. The constraint on kSZ power can be interpreted as an upper limit on the duration of reionization. When the post-reionization homogeneous kSZ signal is accounted for, we find an upper limit on the duration Δz < 5.4 at 95% CL.