Radio pulsar population synthesis with consistent flux measurements using simulation-based inference

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Volume 696 (April 2025)

A&A, 696 (2025) A114

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Table 2

Comparison between best parameters for the log-normal initial magnetic-field, initial period distributions, and the magnetic field decay at late times in the literature.

References	µ_{log B}	σ_{log B}	µ_{log P}	σ_{log P}	a_late	$μ_{\log L_{0}}$ ${\mu _{\log {L_0}}}$	α
Faucher-Giguère & Kaspi (2006)	12.65	0.55	…	…	…	…	…
Gullón et al. (2015)	12.99	0.56	…	…	…	…	…
Cieślar et al. (2020)	${12.67}_{- 0.02}^{+ 0.01}$ $12.67_{ - 0.02}^{ + 0.01}$	${0.34}_{- 0.01}^{+ 0.02}$ $0.34_{ - 0.01}^{ + 0.02}$	…	…	…
Igoshev et al. (2022)	12.44	0.44	$- {1.04}_{- 0.20}^{+ 0.15}$ $- 1.04_{ - 0.20}^{ + 0.15}$	${0.53}_{- 0.08}^{+ 0.12}$ $0.53_{ - 0.08}^{ + 0.12}$	…	…	…
Sautron et al. (2024)	12.44	0.5	−0.88	0.45	…	…	…
Shi & Ng (2024)	${12.32}_{- 0.07}^{+ 0.05}$ $12.32_{ - 0.07}^{ + 0.05}$	${0.35}_{- 0.03}^{+ 0.03}$ $0.35_{ - 0.03}^{ + 0.03}$	$- {1.40}_{- 1.30}^{+ 0.48}$ $- 1.40_{ - 1.30}^{ + 0.48}$	${0.35}_{- 0.35}^{+ 0.84}$ $0.35_{ - 0.35}^{ + 0.84}$	…	…	…
Paper I	${13.10}_{- 0.05}^{+ 0.04}$ $13.10_{ - 0.05}^{ + 0.04}$	${0.45}_{- 0.02}^{+ 0.03}$ $0.45_{ - 0.02}^{ + 0.03}$	$- {1.00}_{- 0.10}^{+ 0.11}$ $- 1.00_{ - 0.10}^{ + 0.11}$	${0.38}_{- 0.10}^{+ 0.16}$ $0.38_{ - 0.10}^{ + 0.16}$	$- {1.80}_{- 0.61}^{+ 0.65}$ $- 1.80_{ - 0.61}^{ + 0.65}$	…	…
This work	${13.09}_{- 0.08}^{+ 0.10}$ $13.09_{ - 0.08}^{ + 0.10}$	${0.50}_{- 0.02}^{+ 0.02}$ $0.50_{ - 0.02}^{ + 0.02}$	$- {0.67}_{- 0.27}^{+ 0.20}$ $- 0.67_{ - 0.27}^{ + 0.20}$	${0.55}_{- 0.12}^{+ 0.10}$ $0.55_{ - 0.12}^{ + 0.10}$	$- {0.88}_{- 0.08}^{+ 0.08}$ $- 0.88_{ - 0.08}^{ + 0.08}$	${26.17}_{- 0.08}^{+ 0.09}$ $26.17_{ - 0.08}^{ + 0.09}$	${0.68}_{- 0.04}^{+ 0.05}$ $0.68_{ - 0.04}^{ + 0.05}$

Notes. We provide references and the seven relevant parameters. We note that the first three studies use a different prescription for the initial period, which prevents a direct comparison with our study. Additionally, the a_late parameter was first introduced in Paper I, so the comparison can only be made with that work. Regarding the parameters related to the luminosity, the prescription used in this work differs from that in previous studies, making direct comparisons not possible. For Gullón et al. (2015), Cieślar et al. (2020) and Shi & Ng (2024), we compare with “model D” for the radio-pulsar population, the “rotational model” and the exponential decay model for the magnetic field, respectively. Where available, we quote CIs at the 68% level (including for this work), but we note that these are difficult to compare due to the difference in inference methods and underlying models and data.

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