The New Generation Planetary Population Synthesis (NGPPS) - VIII. Impact of host star metallicity on planet occurrence rates, orbital periods, eccentricities, and radius valley morphology

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Volume 701 (September 2025)

A&A, 701 (2025) A94

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Table 1

Dependence of the planetary properties as a function of stellar [Fe/H] derived from the synthetic NG76Longshot population.

	Synthetic results	Comparison with observations
Sect. 4: occurrence rate vs. [Fe/H]
Giant planets (Fig. 2)	Positively correlated as F ∝ 10^~1.3×[Fe/H]	Quantitatively consistent
Neptune-sized (Fig. 3)	Positively correlated as F ∝ 10^{~0.5–1×[Fe/H]}	Quantitatively consistent
Small planets (1–3.5 R_⊕) (Fig. 4)	First increase before [Fe/H] ≲ 0.1 dex and then decrease	Qualitatively consistent
Sub-Earths (Fig. 6)	Anti-correlated as F ∝ 10^{−1.9×[Fe/H]}	Awaiting further observational results
Sect. 5: radius valley morphology vs. [Fe/H] (Figs. 8, 9, 10)
C_Valley (Eq. (6))	Positively correlated (Eq. (11))
C_Valley (Eq. (7))	Positively correlated (Eq. (11))
$R_{Valley}^{+}$ $\[R_{\text {Valley}}^{+}\]$ (Eq. (8))	Positively correlated (Eq. (13))	All quantitatively consistent
$R_{Valley}^{-}$ $\[R_{\text {Valley}}^{-}\]$ (Eq. (9))	Not correlated (Eq. (14))
f_NP (Eq. (10))	Positively correlated (Eq. (15))
Sect. 6: orbital periods vs. [Fe/H]
All planets	Higher [Fe/H] at short period (Δ[Fe/H] = 0.05 ± 0.01, Fig. 12)
Large planets	No significant [Fe/H] variation (Δ[Fe/H] = −0.05 ± 0.04, Fig. 13)	All qualitatively consistent but quantitatively weaker
Sub-Neptunes	Higher [Fe/H] at short period (Δ[Fe/H] = 0.02 ± 0.01)
Terrestrial planets	Significantly higher [Fe/H] at short period (Δ[Fe/H] = 0.07 ± 0.01)
Sect. 7: orbital eccentricity vs. [Fe/H]
Giant planets	Positively correlated (Figs. 17, 18)	Qualitatively consistent but less significant
Small planets with OGPs	Positively correlated (Fig. 22, Eq. (23))	Quantitatively consistent
Small planets w/o OGPs	Not correlated	Inconsistent (Potential reasons in Sect. 7.2)

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