Identification and characterization of optical companions to the population of millisecond pulsars in the globular cluster M3

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Table A.1

Inferred NS mass and orbital inclination for M3B, M3D and M3F.

	M3B	M3D		M3F

Parameter		Young	Old	Young	Old
M_NS (M_⊙)	${1.22}_{- 0.04}^{+ 0.04}$ $1.22_{ - 0.04}^{ + 0.04}$	${1.47}_{- 0.11}^{+ 0.48}$ $1.47_{ - 0.11}^{ + 0.48}$	${1.34}_{- 0.05}^{+ 0.06}$ $1.34_{ - 0.05}^{ + 0.06}$	${1.46}_{- 0.10}^{+ 0.47}$ $1.46_{ - 0.10}^{ + 0.47}$	${1.48}_{- 0.12}^{+ 0.46}$ $1.48_{ - 0.12}^{ + 0.46}$
i (deg)	${88.75}_{- 7.44}^{+ 1.25}$ $88.75_{ - 7.44}^{ + 1.25}$	${44.44}_{- 5.40}^{+ 8.86}$ $44.44_{ - 5.40}^{ + 8.86}$	${83.27}_{- 6.70}^{+ 4.67}$ $83.27_{ - 6.70}^{ + 4.67}$	${30.70}_{- 3.31}^{+ 5.14}$ $30.70_{ - 3.31}^{ + 5.14}$	${48.97}_{- 4.00}^{12.43}$ $48.97_{ - 4.00}^{12.43}$

Notes. Here we assume a bimodal Gaussian distribution for the prior on M_NS. For M3D and M3F, we show both the young and old solutions.

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