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Table 6.

Comparison of Solar dipole measurements from COBE, WMAP, and Planck.

Galactic coordinates
Amplitude l b
Experiment [μKCMB] [deg] [deg] Reference
COBE (a)(b) 3358 ± 23 264.31 ± 0.16 48.05 ± 0.09 Lineweaver et al. (1996)
WMAP (c) 3355 ± 8 263.99 ± 0.14 48.26 ± 0.03 Hinshaw et al. (2009)
LFI 2015 (b) 3365.5 ± 3.0 264.01 ± 0.05 48.26 ± 0.02 Planck Collaboration II (2016)
HFI 2015 (d) 3364.29 ± 1.1 263.914 ± 0.013 48.265 ± 0.002 Planck Collaboration VIII (2016)
LFI 2018 (b) 3364.4 ± 3.1 263.998 ± 0.051 48.265 ± 0.015 Planck Collaboration II (2020)
HFI 2018 (d) 3362.08 ± 0.99 264.021 ± 0.011 48.253 ± 0.005 Planck Collaboration III (2020)
Bware 3361.90 ± 0.40 263.959 ± 0.019 48.260 ± 0.008 Delouis et al. (2021)
Planck PR4 (a)(c) 3366.6 ± 2.6 263.986 ± 0.035 48.247 ± 0.023 Planck Collaboration Int. LVII (2020)
BEYONDPLANCK(e) 3362.7 ± 1.4 264.11 ± 0.07 48.279 ± 0.026 Colombo et al. (2023)
COSMOGLOBE(e) 3366.2 ± 1.4 264.08 ± 0.07 48.273 ± 0.024 This work

Notes.

(a)

Statistical and systematic uncertainty estimates are added in quadrature.

(b)

Computed with a naive dipole estimator that does not account for higher-order CMB fluctuations.

(c)

Computed with a Wiener-filter estimator that estimates, and marginalizes over, higher-order CMB fluctuations jointly with the dipole.

(d)

Higher-order fluctuations as estimated by subtracting a dipole-adjusted CMB-fluctuation map from frequency maps prior to dipole evaluation.

(e)

Estimated with a sky fraction of 68%. Error bars include only statistical uncertainties, as defined by the global COSMOGLOBE posterior framework, and they thus account for instrumental noise, gain fluctuations, parametric foreground variations, etc.

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