Planets similar in size are often dissimilar in interior

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Table 2

Intra-system dispersion D for radii (r), masses (m), densities (ρ) and period ratios (p)

Main sample D N_pps>1, $\sum \frac{(σ_{p \pm})}{p} \leq 2$ $\sum {{{\left( {{\sigma _{p \pm }}} \right)} \over p}} \le 2$
	N_pl, N_s	D	$\bar{D_{err}}$ $\overline {{D_{{\rm{err }}}}}$	$\bar{D_{sim}}$ $\overline {{D_{{\rm{sim }}}}}$

r	493, 171	0.317	0.322 ± 0.003	–
m	319, 127	0.540	0.566 ± 0.012	0.647 ± 0.031
ρ	296, 120	0.584	0.619 ± 0.047	0.706 ± 0.031

D, N_pps > 1, $\sum \frac{(σ_{r \pm})}{r} \leq 0.5$ $\sum {{{\left( {{\sigma _{r \pm }}} \right)} \over r}} \le 0.5$

r	483, 167	0.318	0.320 ± 0.003	–
m	137, 58	0.494	0.500 ± 0.008	0.647 ± 0.057
ρ	86, 36	0.500	0.505 ± 0.013	0.714 ± 0.06

D for subsample N_pps > 2

r	329, 89	0.341	0.343 ± 0.003	–
m	147, 41	0.711	0.727 ± 0.014	0.761 ± 0.051
ρ	130, 37	0.742	0.762 ± 0.020	0.862 ± 0.053
pr	374, 99	0.615	0.615 ± 0.002	–

D for subsample M_p < 100 M_⊕

r	422, 146	0.284	0.289 ± 0.003	–
m	282, 113	0.446	0.476 ± 0.013	0.615 ± 0.032
ρ	266, 107	0.550	0.588 ± 0.052	0.699 ± 0.033
pr (N_ppS > 2)	317, 84	0.559	0.558 ± 0.002	–

D for RV subsample

r	171, 66	0.337	0.340 ± 0.005	–
m	140, 55	0.502	0.521 ± 0.016	0.645 ± 0.046
ρ	132, 53	0.561	0.581 ± 0.308	0.722 ± 0.048
pr (N_pps > 2)	107, 29	0.689	0.689 ± 0.000	–

D for TTVs subsample

r	166, 71	0.230	0.238 ± 0.005	–
m	156, 65	0.517	0.547 ± 0.018	0.642 ± 0.044
ρ	146, 61	0.585	0.631 ± 0.022	0.679 ± 0.045
pr (N_pps > 2)	61, 17	0.455	0.455 ± 0.000	–

D for HCR subsample

r	250, 96	0.108	0.116 ± 0.004	–
m	172, 75	0.351	0.388 ± 0.016	0.561 ± 0.040
ρ	158, 68	0.398	0.437 ± 0.020	0.579 ± 0.041

D for radius from Gaia DR3

r_flame	419, 147	0.333	0.333 ± 0.002	–
r_gspphot	419, 147	0.333	0.335 ± 0.003	–

Notes. N_pps stand for the number of planets per system, and N_s, N_pl the same as in Table 1. $\bar{D_{err}}$ $\overline {{D_{{\rm{err }}}}}$ stands for average dispersion and σ in parameter after the error-accommodation test for uncertainty to our exoplanet sample. $\bar{D_{sim}}$ $\overline {{D_{{\rm{sim }}}}}$ stands for average dispersion and σ after 10⁵ simulation of mass and density populations from the non-parametric MRR (Ning et al. 2018) giving the observed radii.

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