On the Contribution of the X-Ray Source to the Extended Nebular He ii Emission in IZW18

Nebular He ii emission implies the presence of energetic photons (E ≥ 54 eV). Despite the great deal of effort dedicated to understanding He ii ionization, its origin has remained mysterious, particularly in metal-deficient star-forming (SF) galaxies. Unfolding He ii-emitting, metal-poor starbursts at z ~ 0 can yield insight into the powerful ionization processes occurring in the primordial universe. Here we present a new study on the effects that X-ray sources have on the He ii ionization in the extremely metal-poor galaxy IZw18 (Z ~ 3% Z⊙), whose X-ray emission is dominated by a single high-mass X-ray binary (HMXB). This study uses optical integral field spectroscopy, archival Hubble Space Telescope observations, and all of the X-ray data sets publicly available for IZw18. We investigate the time-variability of the IZw18 HMXB for the first time; its emission shows small variations on timescales from days to decades. The best-fit models for the HMXB X-ray spectra cannot reproduce the observed He ii ionization budget of IZw18, nor can recent photoionization models that combine the spectra of both very low metallicity massive stars and the emission from HMXB. We also find that the IZw18 HMXB and the He ii-emission peak are spatially displaced at a projected distance of sime200 pc. These results reduce the relevance of X-ray photons as the dominant He ii ionizing mode in IZw18, which leaves uncertain what process is responsible for the bulk of its He ii ionization. This is in line with recent work discarding X-ray binaries as the main source responsible for He ii ionization in SF galaxies. © 2021. The American Astronomical Society. All rights reserved.
This work has been partially funded by projects AYA2016-79724-C4-4-P and PID2019-107408GB-C44 from the Spanish PNAYA. C.K., M.A.G., and J.V.M. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). M.A.G. acknowledges support from MCIU grant PGC2018-102184-B-I00 cofunded with FEDER funds. G.R.-L. acknowledges support from CONACyT (grant 263373) and PRODEP (Mexico). This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC.