Extremely iron-poor O-type stars in the Magellanic Bridge

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Table 1.

Comparison of the abundance measurements of hot massive stars and the ISM in the Magellanic Bridge.

Star	Sp. Type	$[\frac{Fe}{H}]$ $\left[ \frac{\mathrm{Fe}}{\mathrm{H}}\right]$	$[\frac{O}{H}]$ $\left[ \frac{\mathrm{O}}{\mathrm{H}}\right]$	$Δ [\frac{X}{H}]$ $\Delta \left[\frac{\mathrm{X}}{\mathrm{H}}\right]$	Z	Source
MBO2	O9V	−0.97	−1.43	−1.35	6.26 × 10⁻⁴	This work
MBO3	O9.5V	−1.44	−0.98	−1.08	1.10 × 10⁻³	This work
DI 1388	B0	−1.9	−0.5	< −0.5		Dufton et al. (2008), Hambly et al. (1994)
		−0.68				This work
ISM		−0.61	−0.96			Lehner et al. (2008)

Notes. [X/H] are the logarithmic number fractions of X and H relative to their solar values. Δ[X/H] denotes the mean overall light metals (N, C, O, Si, and Mg). Z is defined as the sum of all metal (N, C, O, Si, Mg, Ne, and Fe) mass fractions. The spectral types of MBO2 and MBO3 are taken from Ramachandran et al. (2021).

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