Constraints on $Λ$CDM Extensions from the SPT-3G 2018 $EE$ and $TE$ Power Spectra

Balkenhol, L.; Dutcher, D.; Ade, P. A. R.; Ahmed, Z.; Anderes, E.; Anderson, A. J.; Archipley, M.; Avva, J. S.; Aylor, K.; Barry, P. S.; Thakur, R. Basu; Benabed, K.; Bender, A. N.; Benson, B. A.; Bianchini, F.; Bleem, L. E.; Bouchet, F. R.; Bryant, L.; Byrum, K.; Carlstrom, J. E.; Carter, F. W.; Cecil, T. W.; Chang, C. L.; Chaubal, P.; Chen, G.; Cho, H. -M.; Chou, T. -L.; Cliche, J. -F.; Crawford, T. M.; Cukierman, A.; Daley, C.; de Haan, T.; Denison, E. V.; Dibert, K.; Ding, J.; Dobbs, M. A.; Everett, W.; Feng, C.; Ferguson, K. R.; Foster, A.; Fu, J.; Galli, S.; Gambrel, A. E.; Gardner, R. W.; Goeckner-Wald, N.; Gualtieri, R.; Guns, S.; Gupta, N.; Guyser, R.; Halverson, N. W.; Harke-Hosemann, A. H.; Harrington, N. L.; Henning, J. W.; Hilton, G. C.; Hivon, E.; Holder, G. P.; Holzapfel, W. L.; Hood, J. C.; Howe, D.; Huang, N.; Irwin, K. D.; Jeong, O. B.; Jonas, M.; Jones, A.; Khaire, T. S.; Knox, L.; Kofman, A. M.; Korman, M.; Kubik, D. L.; Kuhlmann, S.; Kuo, C. -L.; Lee, A. T.; Leitch, E. M.; Lowitz, A. E.; Lu, C.; Meyer, S. S.; Michalik, D.; Millea, M.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nguyen, H.; Noble, G. I.; Novosad, V.; Omori, Y.; Padin, S.; Pan, Z.; Paschos, P.; Pearson, J.; Posada, C. M.; Prabhu, K.; Quan, W.; Rahlin, A.; Reichardt, C. L.; Riebel, D.; Riedel, B.; Rouble, M.; Ruhl, J. E.; Sayre, J. T.; Schiappucci, E.; Shirokoff, E.; Smecher, G.; Sobrin, J. A.; Stark, A. A.; Stephen, J.; Story, K. T.; Suzuki, A.; Thompson, K. L.; Thorne, B.; Tucker, C.; Umilta, C.; Vale, L. R.; Vanderlinde, K.; Vieira, J. D.; Wang, G.; Whitehorn, N.; Wu, W. L. K.; Yefremenko, V.; Yoon, K. W.; Young, M. R.

doi:10.48550/arxiv.2103.13618

Cited by 25 publications

(35 citation statements)

References 25 publications

(55 reference statements)

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“…This data set combination is confirmed in Ref. [45], which showed H 0 = 67.49 ± 0.53 km/s/Mpc for ΛCDM model. As mentioned, it might be better to discard the small scale part of Planck's TT, so when combine Planck measurement with ACT and SPT data, we cut the Planck's high-TT power spectrum to TT,max = 1000.…”

Section: Model Data and Methodologysupporting

confidence: 80%

Towards early dark energy and $n_s$=1 with Planck, ACT and SPT

Jiang,

Piao

2022

Preprint

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We investigate the constraints on early dark energy (EDE) by combining the most recent CMB observations available, ACT DR4, SPT-3G, and Planck2018 ( TT,max = 1000) data. This combined CMB dataset favors non-zero EDE fractions and large Hubble constants, i.e. H 0 = 72.3(73.4) +2.2 −1.7 and 73.32(72.98) +0.68 −0.95 km/s/Mpc for axion-like EDE and AdS-EDE, respectively. The inclusion of BAO+Pantheon data has little efffect on the results. The axion-like EDE can fit the data significantly better (∆χ 2 −10) than ΛCDM, which is mainly driven by the ACT data. It is found again that if the current H 0 measured locally is correct, complete resolution of the Hubble tension seems to be pointing towards a scale invariant Harrison-Zeldovich spectrum of primordial scalar perturbation, i.e. n s = 1 for H 0 ∼ 73 km/s/Mpc.

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Section: Model Data and Methodologysupporting

confidence: 80%

Towards early dark energy and $n_s$=1 with Planck, ACT and SPT

Jiang,

Piao

2022

Preprint

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“…Already, measurements of the EE and T E power spectra using four months of SPT-3G data in 2018 (half of a typical observing season) have improved upon previous results from SPTpol at multipoles 1500 (Bender et al 2020), and provided stronger constraints on extensions to the ΛCDM cosmological model (Balkenhol et al 2021).…”

Section: Discussionmentioning

confidence: 95%

The Design and Integrated Performance of SPT-3G

Sobrin,

Anderson,

Bender

et al. 2021

Preprint

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SPT-3G is the third survey receiver operating on the South Pole Telescope dedicated to highresolution observations of the cosmic microwave background (CMB). Sensitive measurements of the temperature and polarization anisotropies of the CMB provide a powerful dataset for constraining cosmology. Additionally, CMB surveys with arcminute-scale resolution are capable of detecting galaxy clusters, millimeter-wave bright galaxies, and a variety of transient phenomena. The SPT-3G instrument provides a significant improvement in mapping speed over its predecessors, SPT-SZ and SPTpol. The broadband optics design of the instrument achieves a 430 mm diameter image plane across observing bands of 95 GHz, 150 GHz, and 220 GHz, with 1.2 arcmin FWHM beam response at 150 GHz. In the receiver, this image plane is populated with 2690 dual-polarization, tri-chroic pixels (∼16000 detectors) read out using a 68× digital frequency-domain multiplexing readout system. In 2018, SPT-3G began a multiyear survey of 1500 deg 2 of the southern sky. We summarize the unique optical, cryogenic, detector, and readout technologies employed in SPT-3G, and we report on the integrated performance of the instrument.

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“…In particular, the precision expected from upcoming data releases from SPT and ACT (as mentioned in the conclusions of Refs. [34,38,78,79]) with combined temperature, polarization, and lensing likelihoods will be capable of constraining the parameter space of the EDE model even more tightly 17 as well as of clarifying how the small-scale CMB TT measurements impact the EDE constraints. This will not only provide a valuable crosscheck on the Planck measurements, but also an opportunity to obtain tight and robust constraints through joint analyses, which can be of primary importance to test physics scenarios beyond ΛCDM with CMB data (as in the case of e.g.…”

Section: Discussionmentioning

confidence: 99%