Super-Earth masses and stellar abundances from NIRPS reveal tentative evidence for water-rich formation around M dwarfs

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Table 1

Calculated WMFs.

Planet	WMF (sequestered)	WMF (differentiated)
GJ 1132 b	<0.07	0.02 ± 0.01
GJ 1252b	<0.03	${0.012}_{- 0.007}^{+ 0.009}$ $Mathematical equation: $\[0.012_{-0.007}^{+0.009}\]$$
LTT 3780 b	<0.04	${0.013}_{- 0.008}^{+ 0.010}$ $Mathematical equation: $\[0.013_{-0.008}^{+0.010}\]$$
GJ 357 b	<0.08	<0.04
HD 260655 b	<0.11	${0.02}_{- 0.01}^{+ 0.02}$ $Mathematical equation: $\[0.02_{-0.01}^{+0.02}\]$$
L 98-59 b	0.023 ± 0.004	0.005 ± 0.003
L 98-59 c	<0.14	0.03 ± 0.01
LHS 1140 c	<0.12	0.02 ± 0.01
TOI-270 b	<0.19	0.04 ± 0.01

Notes. The distributions of the two sets of WMF estimates. The 95th percentile upper limits on the WMF estimates are reported instead of error bars where the WMF posterior is consistent with 0 for the differentiated WMFs, or 0.01 for the sequestered WMFs.

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