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tokens: component of Fe K α emission (log ξ = 0). A very similar result is reached by performing the same test on the 2014 mean EPIC-pn + NuSTAR spectrum (Δ χ 2 = 52), resulting in a modest reflection strength, R ∼ 0.6, while the photon index and Fe abundance remain unchanged: Γ ∼ 1.8; A Fe ∼ 3. The remaining key parameters in the relxill model are largely consistent with those reported in Table 2 ; i.e., log ξ ∼ 1.2, q ∼ 3, θ ∼ 40, r in 6. The black hole spin, a *, is unconstrained although we find a lower-limit on the high-energy cutoff of E cut > 130 keV. Finally, we return to check for the presence of highly-ionized absorption in the contemporaneous NuSTAR data. In terms of the EPIC-pn analysis, the two absorption grids modeling the highly-ionized two-velocity outflow are highly significant, with a combined contribution to the fit statistic of Δ χ 2 = 42 (for six additional parameters; meanwhile, the highly-ionized emission and soft-band absorption grids improve the fit by Δ χ 2 = 39 and Δ χ 2 = 44, respectively). Zoghbi et al. ( 2015 ) detected no significant discrete absorption features in the NuSTAR spectrum. We now find, in direct comparison with XMM-Newton , including the same two xstar absorption zones to the same baseline model fitted to just the contemporaneous NuSTAR observations offers a far less significant improvement to the fit statistic, with Δ χ 2 = 9. As such, even though the highly-ionized outflow is now well established thanks to XMM-Newton , we also confirm the main result from Zoghbi et al. ( 2015 ) that it was not detectable by NuSTAR alone. This demonstrates the importance of long-look observations with XMM-Newton in addition to the broad-band coverage of NuSTAR . 4. DISCUSSION AND CONCLUSIONS An extended XMM-Newton observation of PG 1211+143 has revealed spectral structure in the Fe K band, unseen in previous (shorter) observations. Utilizing the high throughput of the EPIC-pn, Pounds et al. ( 2016a ) showed that highly-ionized outflow resolved two velocity components ( and ), while an analysis of the high-resolution RGS data in Pounds et al. ( 2016b ) found lower-ionization co-moving counterparts of that dual-velocity flow. Here, we have extended our modeling over a wider energy range, incorporating contemporaneous NuSTAR data. The power of this approach—i.e., combining XMM-Newton and NuSTAR data—has previously been demonstrated in a precise measurement of the higher-energy continuum and thereby helping to disentangle absorption and reflection in a number of AGNs—e.g., NGC 1365 (Risaliti et al. 2013 ; Walton et al. 2014 ; Rivers et al. 2015 ), NGC 5548 (Kaastra et al. 2014 ; Ursini et al. 2015 ; Cappi et al. 2016 ) and PDS 456 (Nardini et al. 2015 ). In Section 3.1 , we fitted the hard X-ray spectrum with relativistic reflection, following the recent analysis of Zoghbi et al. ( 2015 ). Using the NuSTAR data alone, we confirm their solution, finding a steep photon index (Γ ∼ 2.4) and high reflection fraction ( R ∼