Figure 3 from NuSTAR and XMM-Newton Observations of Luminous, Heavily Obscured, WISE-selected Quasars at z ∼ 2

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NuSTAR and XMM-Newton Observations of Luminous, Heavily Obscured, WISE-selected Quasars at z ∼ 2

Authors: D. Stern, G. B. Lansbury, R. J. Assef, W. N. Brandt, D. M. Alexander, D. R. Ballantyne, M. Baloković, F. E. Bauer, D. Benford, A. Blain, S. E. Boggs, C. Bridge, M. Brightman, F. E. Christensen, A. Comastri, W. W. Craig, A. Del Moro, P. R. M. Eisenhardt, P. Gandhi, R. L. Griffith, C. J. Hailey, F. A. Harrison, R. C. Hickox, T. H. Jarrett, M. Koss, S. Lake, S. M. LaMassa, B. Luo, C.-W. Tsai, C. M. Urry, D. J. Walton, E. L. Wright, J. Wu, L. Yan, and W. W. Zhang

Stern et al. 2014 The Astrophysical Journal 794 102.

Provider: AAS Journals

Caption: Figure 3.

Best-fitting SED template models (heavy gray line) to the WISE photometry (shown by green symbols) for WISE J2207+1939 and WISE J2357+0328. The fits use the Sbc spiral (green) and type-1 AGN (blue) empirical templates from Assef et al. (2010), with the amount of reddening for the AGN component a free parameter. The host galaxy dominates at observed λ ≲ 5 μm, while the heavily obscured AGN dominates at longer wavelengths. Note that the best-fit models shown here find the stellar light dominated by the spiral template, while the modeling (and associated uncertainties listed in Table 1) use all three galaxy templates from Assef et al. (2010; see Section 4.1).

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