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Constraints on Inflationary Gravitational Waves with Two Years of SPT-3G Data

Fuente: arXiv

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Main Authors:	Zebrowski, J. A., Reichardt, C. L., Anderson, A. J., Ansarinejad, B., Archipley, M., Balkenhol, L., Barry, P., Benabed, K., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Bouchet, F. R., Bryant, L., Camphuis, E., Carlstrom, J. E., Chang, C. L., Chaubal, P., Chichura, P. M., Chokshi, A., Chou, T. -L., Coerver, A., Crawford, T. M., Daley, C., de Haan, T., Dibert, K. R., Dobbs, M. A., Doohan, M., Doussot, A., Dutcher, D., Everett, W., Feng, C., Ferguson, K. R., Fichman, K., Foster, A., Galli, S., Gambrel, A. E., Gardner, R. W., Ge, F., Goeckner-Wald, N., Gualtieri, R., Guidi, F., Guns, S., Halverson, N. W., Hivon, E., Holder, G. P., Holzapfel, W. L., Hood, J. C., Hryciuk, A., Huang, N., Kéruzoré, F., Khalife, A. R., Knox, L., Korman, M., Kornoelje, K., Kuo, C. -L., Levy, K., Li, Y., Lowitz, A. E., Lu, C., Lynch, G. P., Maniyar, A., Martsen, E. S., Menanteau, F., Millea, M., Montgomery, J., Nakato, Y., Natoli, T., Noble, G. I., Omori, Y., Ouellette, A., Pan, Z., Paschos, P., Phadke, K. A., Pollak, A. W., Prabhu, K., Quan, W., Raghunathan, S., Rahimi, M., Rahlin, A., Rouble, M., Ruhl, J. E., Simpson, A., Schiappucci, E., Sobrin, J. A., Stark, A. A., Stephen, J., Tandoi, C., Thorne, B., Trendafilova, C., Umilta, C., Vieira, J. D., Vieregg, A. G., Vitrier, A., Wan, Y., Whitehorn, N., Wu, W. L. K., Young, M. R.
Format:	Preprint
Published:	2025
Subjects:	Cosmology and Nongalactic Astrophysics
Online Access:	Acceder al recurso
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author	Zebrowski, J. A. Reichardt, C. L. Anderson, A. J. Ansarinejad, B. Archipley, M. Balkenhol, L. Barry, P. Benabed, K. Bender, A. N. Benson, B. A. Bianchini, F. Bleem, L. E. Bouchet, F. R. Bryant, L. Camphuis, E. Carlstrom, J. E. Chang, C. L. Chaubal, P. Chichura, P. M. Chokshi, A. Chou, T. -L. Coerver, A. Crawford, T. M. Daley, C. de Haan, T. Dibert, K. R. Dobbs, M. A. Doohan, M. Doussot, A. Dutcher, D. Everett, W. Feng, C. Ferguson, K. R. Fichman, K. Foster, A. Galli, S. Gambrel, A. E. Gardner, R. W. Ge, F. Goeckner-Wald, N. Gualtieri, R. Guidi, F. Guns, S. Halverson, N. W. Hivon, E. Holder, G. P. Holzapfel, W. L. Hood, J. C. Hryciuk, A. Huang, N. Kéruzoré, F. Khalife, A. R. Knox, L. Korman, M. Kornoelje, K. Kuo, C. -L. Levy, K. Li, Y. Lowitz, A. E. Lu, C. Lynch, G. P. Maniyar, A. Martsen, E. S. Menanteau, F. Millea, M. Montgomery, J. Nakato, Y. Natoli, T. Noble, G. I. Omori, Y. Ouellette, A. Pan, Z. Paschos, P. Phadke, K. A. Pollak, A. W. Prabhu, K. Quan, W. Raghunathan, S. Rahimi, M. Rahlin, A. Rouble, M. Ruhl, J. E. Simpson, A. Schiappucci, E. Sobrin, J. A. Stark, A. A. Stephen, J. Tandoi, C. Thorne, B. Trendafilova, C. Umilta, C. Vieira, J. D. Vieregg, A. G. Vitrier, A. Wan, Y. Whitehorn, N. Wu, W. L. K. Young, M. R.
author_facet	Zebrowski, J. A. Reichardt, C. L. Anderson, A. J. Ansarinejad, B. Archipley, M. Balkenhol, L. Barry, P. Benabed, K. Bender, A. N. Benson, B. A. Bianchini, F. Bleem, L. E. Bouchet, F. R. Bryant, L. Camphuis, E. Carlstrom, J. E. Chang, C. L. Chaubal, P. Chichura, P. M. Chokshi, A. Chou, T. -L. Coerver, A. Crawford, T. M. Daley, C. de Haan, T. Dibert, K. R. Dobbs, M. A. Doohan, M. Doussot, A. Dutcher, D. Everett, W. Feng, C. Ferguson, K. R. Fichman, K. Foster, A. Galli, S. Gambrel, A. E. Gardner, R. W. Ge, F. Goeckner-Wald, N. Gualtieri, R. Guidi, F. Guns, S. Halverson, N. W. Hivon, E. Holder, G. P. Holzapfel, W. L. Hood, J. C. Hryciuk, A. Huang, N. Kéruzoré, F. Khalife, A. R. Knox, L. Korman, M. Kornoelje, K. Kuo, C. -L. Levy, K. Li, Y. Lowitz, A. E. Lu, C. Lynch, G. P. Maniyar, A. Martsen, E. S. Menanteau, F. Millea, M. Montgomery, J. Nakato, Y. Natoli, T. Noble, G. I. Omori, Y. Ouellette, A. Pan, Z. Paschos, P. Phadke, K. A. Pollak, A. W. Prabhu, K. Quan, W. Raghunathan, S. Rahimi, M. Rahlin, A. Rouble, M. Ruhl, J. E. Simpson, A. Schiappucci, E. Sobrin, J. A. Stark, A. A. Stephen, J. Tandoi, C. Thorne, B. Trendafilova, C. Umilta, C. Vieira, J. D. Vieregg, A. G. Vitrier, A. Wan, Y. Whitehorn, N. Wu, W. L. K. Young, M. R.
contents	We present a measurement of the $B$-mode polarization power spectrum of the cosmic microwave background anisotropies at 32 $\le$ $\ell$ $<$ 502 for three bands centered at 95, 150, and 220 GHz using data from the SPT-3G receiver on the South Pole Telescope. This work uses SPT-3G observations from the 2019 and 2020 winter observing seasons of a $\sim$1500 deg$^2$ patch of sky that directly overlaps with fields observed with the BICEP/Keck family of telescopes, and covers part of the proposed Simons Observatory and CMB-S4 deep fields. Employing new techniques for mitigating polarized atmospheric noise, the SPT-3G data demonstrates a white noise level of 9.3 (6.7) $μ$K-arcmin at $\ell \sim 500$ for the 95 GHz (150 GHz) data, with a $1/\ell$ noise knee at $\ell$=128 (182). We fit the observed six auto- and cross-frequency $B$-mode power spectra to a model including lensed $Λ$CDM $B$-modes and a combination of Galactic and extragalactic foregrounds. This work characterizes foregrounds in the vicinity of the BICEP/Keck survey area, finding foreground power consistent with that reported by the BICEP/Keck collaboration within the same region, and a factor of $\sim$ 3 higher power over the full SPT-3G survey area. Using SPT-3G data over the BICEP/Keck survey area, we place a 95% upper limit on the tensor-to-scalar ratio of $r < 0.25$ and find the statistical uncertainty on $r$ to be $σ(r) = 0.067$.
format	Preprint
id	arxiv_https___arxiv_org_abs_2505_02827
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	Constraints on Inflationary Gravitational Waves with Two Years of SPT-3G Data Zebrowski, J. A. Reichardt, C. L. Anderson, A. J. Ansarinejad, B. Archipley, M. Balkenhol, L. Barry, P. Benabed, K. Bender, A. N. Benson, B. A. Bianchini, F. Bleem, L. E. Bouchet, F. R. Bryant, L. Camphuis, E. Carlstrom, J. E. Chang, C. L. Chaubal, P. Chichura, P. M. Chokshi, A. Chou, T. -L. Coerver, A. Crawford, T. M. Daley, C. de Haan, T. Dibert, K. R. Dobbs, M. A. Doohan, M. Doussot, A. Dutcher, D. Everett, W. Feng, C. Ferguson, K. R. Fichman, K. Foster, A. Galli, S. Gambrel, A. E. Gardner, R. W. Ge, F. Goeckner-Wald, N. Gualtieri, R. Guidi, F. Guns, S. Halverson, N. W. Hivon, E. Holder, G. P. Holzapfel, W. L. Hood, J. C. Hryciuk, A. Huang, N. Kéruzoré, F. Khalife, A. R. Knox, L. Korman, M. Kornoelje, K. Kuo, C. -L. Levy, K. Li, Y. Lowitz, A. E. Lu, C. Lynch, G. P. Maniyar, A. Martsen, E. S. Menanteau, F. Millea, M. Montgomery, J. Nakato, Y. Natoli, T. Noble, G. I. Omori, Y. Ouellette, A. Pan, Z. Paschos, P. Phadke, K. A. Pollak, A. W. Prabhu, K. Quan, W. Raghunathan, S. Rahimi, M. Rahlin, A. Rouble, M. Ruhl, J. E. Simpson, A. Schiappucci, E. Sobrin, J. A. Stark, A. A. Stephen, J. Tandoi, C. Thorne, B. Trendafilova, C. Umilta, C. Vieira, J. D. Vieregg, A. G. Vitrier, A. Wan, Y. Whitehorn, N. Wu, W. L. K. Young, M. R. Cosmology and Nongalactic Astrophysics We present a measurement of the $B$-mode polarization power spectrum of the cosmic microwave background anisotropies at 32 $\le$ $\ell$ $<$ 502 for three bands centered at 95, 150, and 220 GHz using data from the SPT-3G receiver on the South Pole Telescope. This work uses SPT-3G observations from the 2019 and 2020 winter observing seasons of a $\sim$1500 deg$^2$ patch of sky that directly overlaps with fields observed with the BICEP/Keck family of telescopes, and covers part of the proposed Simons Observatory and CMB-S4 deep fields. Employing new techniques for mitigating polarized atmospheric noise, the SPT-3G data demonstrates a white noise level of 9.3 (6.7) $μ$K-arcmin at $\ell \sim 500$ for the 95 GHz (150 GHz) data, with a $1/\ell$ noise knee at $\ell$=128 (182). We fit the observed six auto- and cross-frequency $B$-mode power spectra to a model including lensed $Λ$CDM $B$-modes and a combination of Galactic and extragalactic foregrounds. This work characterizes foregrounds in the vicinity of the BICEP/Keck survey area, finding foreground power consistent with that reported by the BICEP/Keck collaboration within the same region, and a factor of $\sim$ 3 higher power over the full SPT-3G survey area. Using SPT-3G data over the BICEP/Keck survey area, we place a 95% upper limit on the tensor-to-scalar ratio of $r < 0.25$ and find the statistical uncertainty on $r$ to be $σ(r) = 0.067$.
title	Constraints on Inflationary Gravitational Waves with Two Years of SPT-3G Data
topic	Cosmology and Nongalactic Astrophysics
url	https://arxiv.org/abs/2505.02827