BEYONDPLANCK - XI. Bayesian CMB analysis with sample-based end-to-end error propagation

BeyondPlanck: end-to-end Bayesian analysis of Planck LFI

Open Access

Table 2.

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

		Galactic coordinates
Experiment	Amplitude [μK_CMB]	l [deg]	b [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	8.265 ± 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	This paper

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 indicate 1σ uncertainties, and include statistical uncertainties as defined by the global BEYONDPLANCK posterior framework; they thus account for instrumental noise, gain fluctuations, parametric foreground variations etc., but not for potential modeling error uncertainties.

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