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We present the integrated VLT-MUSE spectrum of the central 2'x2' (30x30pc$^{2}$) of NGC 2070, the dominant giant HII region of the Tarantula Nebula inthe Large Magellanic Cloud, together withan empirical far-ultraviolet spectrumconstructed via LMC template stars from the ULLYSES survey and Hubble TarantulaTreasury Project UV photometry. NGC 2070 provides a unique opportunity tocompare results from individual stellar populations (e.g. VLT FLAMES TarantulaSurvey) in a metal-poor starburst region to the integrated results from thepopulation synthesis tools Starburst99, Charlot & Bruzual and BPASS. Themetallicity of NGC 2070 inferred from standard nebular strong line calibrationsis 0.4$\pm$0.1 dex lower than obtained from direct methods. The Halpha inferredage of 4.2 Myr from Starburst99 is close to the median age of OB stars withinthe region, although individual stars span a broad range of 1-7 Myr. Theinferred stellar mass is close to that obtained for the rich star cluster R136within NGC 2070, although this contributes only 21% to the integrated far-UVcontinuum. HeII 1640 emission is dominated by classical WR stars and mainsequence WNh+Of/WN stars. 18% of the NGC~2070 far UV continuum flux arises fromvery massive stars with >100 Msun, including several very luminous Ofsupergiants. None of the predicted population synthesis models at lowmetallicities are able to successfully reproduce the far-UV spectrum of NGC2070. We attribute issues to the treatment of mass-loss in very massive stars,the lack of contemporary empirical metal-poor templates, plus WR stars producedvia binary evolution.

Mapping the core of the Tarantula Nebula with VLT-MUSE. III. A template for metal-poor starburst regions in the visual and far-ultraviolet