The ionizing continuum from active galactic nuclei is fundamental for interpreting their broad emission lines and understanding their impact on the surrounding gas. Furthermore, it provides hints on how matter accretes on to supermassive black holes. Using Hubble Space Telescope's Wide Field Camera 3, we have constructed the first stacked ultraviolet (rest-frame wavelengths 600-2500 angstrom) spectrum of 53 luminous quasars at z similar or equal to 2.4, with a state-of-the-art correction for the intervening Lyman forest and Lyman continuum absorption. The continuum slope (f nu proportional to nu(alpha nu)) of the full sample shows a break at similar to 912 angstrom with spectral index alpha(nu) = -0.61 +/- 0.01 lambda > 912 angstrom and a softening at shorter wavelengths (alpha(nu) = -1.70 +/- 0.61 lambda <= 912 angstrom). Our analysis proves that a proper intergalactic medium absorption correction is required to establish the intrinsic continuum emission of quasars. We interpret our average ultraviolet spectrum in the context of photoionization, accretion disc models, and quasar contribution to the ultraviolet background. We find that observed broad line ratios are consistent with those predicted assuming an ionizing slope of alpha(ion) = -2.0, similar to the observed ionizing spectrum in the same wavelength range. The continuum break and softening are consistent with accretion disc plus X-ray corona models when black hole spin is taken into account. Our spectral energy distribution yields a 30 per cent increase to previous estimates of the specific quasar emissivity, such that quasars may contribute significantly to the total specific Lyman limit emissivity estimated from the Ly alpha forest at z < 3.2.

Lusso, E., Worseck, G., Hennawi, J., Prochaska, J., Vignali, C., Stern, J., et al. (2015). The first ultraviolet quasar-stacked spectrum at z ≃ 2.4 from WFC3. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 449(4), 4204-4220 [10.1093/mnras/stv516].

The first ultraviolet quasar-stacked spectrum at z ≃ 2.4 from WFC3

VIGNALI, CRISTIAN;
2015

Abstract

The ionizing continuum from active galactic nuclei is fundamental for interpreting their broad emission lines and understanding their impact on the surrounding gas. Furthermore, it provides hints on how matter accretes on to supermassive black holes. Using Hubble Space Telescope's Wide Field Camera 3, we have constructed the first stacked ultraviolet (rest-frame wavelengths 600-2500 angstrom) spectrum of 53 luminous quasars at z similar or equal to 2.4, with a state-of-the-art correction for the intervening Lyman forest and Lyman continuum absorption. The continuum slope (f nu proportional to nu(alpha nu)) of the full sample shows a break at similar to 912 angstrom with spectral index alpha(nu) = -0.61 +/- 0.01 lambda > 912 angstrom and a softening at shorter wavelengths (alpha(nu) = -1.70 +/- 0.61 lambda <= 912 angstrom). Our analysis proves that a proper intergalactic medium absorption correction is required to establish the intrinsic continuum emission of quasars. We interpret our average ultraviolet spectrum in the context of photoionization, accretion disc models, and quasar contribution to the ultraviolet background. We find that observed broad line ratios are consistent with those predicted assuming an ionizing slope of alpha(ion) = -2.0, similar to the observed ionizing spectrum in the same wavelength range. The continuum break and softening are consistent with accretion disc plus X-ray corona models when black hole spin is taken into account. Our spectral energy distribution yields a 30 per cent increase to previous estimates of the specific quasar emissivity, such that quasars may contribute significantly to the total specific Lyman limit emissivity estimated from the Ly alpha forest at z < 3.2.
2015
Lusso, E., Worseck, G., Hennawi, J., Prochaska, J., Vignali, C., Stern, J., et al. (2015). The first ultraviolet quasar-stacked spectrum at z ≃ 2.4 from WFC3. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 449(4), 4204-4220 [10.1093/mnras/stv516].
Lusso, E.; Worseck, G.; Hennawi, J.F.; Prochaska, J.X.; Vignali, C.; Stern, J.; O'Meara, J.M.
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