The UV--mid-IR Spectral Energy Distribution of a z=1.7 Quasar Host Galaxy

Details The UV--mid-IR Spectral Energy Distribution of a z=1.7 Quasar Host Galaxy The UV--mid-IR Spectral Energy Distribution of a z=1.7 Quasar Host Galaxy

2009-04-10

arxiv.org/abs/0904.1708v2

Astrophys.J.702:472-479,2009

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

v2, 19 pages, 5 figures, added image depths to Table 1, added UV SFR estimates, corrected misquoted X-ray luminosity

Scientific paper

10.1088/0004-637X/702/1/472

We have measured the spectral energy distribution (SED) of the host galaxy of the z_s=1.7 gravitationally lensed quasar SDSS J1004+4112 from 0.44-8.0 micron (0.16-3.0 micron in the rest frame). The large angular extent of the lensed images and their separation from the centralgalaxy of this cluster lens allows the images to be resolved even with the Spitzer Space Telescope. Based on the SED, the host galaxy is a mixture of relatively old and intermediate age stars with an inferred stellar mass of log(M_stars/M_sun)=11.09+/-0.28 and a star formation rate of log(Mdot/1 M_sun per yr)=1.21+/-0.26. Given the estimated black hole mass of M_BH ~10^8.6 M_sun from locally-calibrated correlations of black hole masses with line widths and luminosities, the black hole represents a fraction log(M_BH/M_stars) = -2.49+/-0.28 of the stellar mass and it is radiating at 0.24+/-0.05 of the Eddington limit. The ratio of the host stellar mass to the black hole mass is only marginally consistent with the locally observed ratio.

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