Hubble Space TelescopeNICMOS Observations of Rest‐Frame Optical Continuum and \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTe

Abstract

High-resolution 1.10, 2.05, 2.12, and 2.15 km imaging of the gravitationally lensed system FSC 10214]4724 are presented. These data extend Hubble Space T elescope (HST ) observations of the lens system to redder wavelengths, thus providing the highest resolution images to date of the rest-frame optical and narrow-line (i.e., Ha ] [N II]) regions of the background quasar. The length of the arc in the wide-band continuum images increases with increasing wavelength, and the Ha ] [N II] emission has a length in between that of the 1.10 and 2.05 km emission. The structure of the arc changes from having an eastern and western peak at 1.10 km to having a single peak in the center at 2.05 km. The changing structure and length of the arc can be understood in terms of a model in which the background quasar consists of a region of scattered active galactic nucleus (AGN) light that dominates at 1.10 km (rest frame 3300 surrounded by a more extended narrow-line region. An even more extended red stellar A ), population would thus contribute light at 2.05 km (rest frame 6200In addition, the Ha ] [N II] A ). emission has structural features similar to the 1.10 km emission normalized by the (predominantly stellar) 2.05 km emission, possibly conÐrming that the 1.10 km emission is a superposition of the sources associated with the line emission (AGNs/massive stars) and the red stellar component that dominates the 2.05 km emission. The counterimage of the lensed quasar is detected in the 1.10 and 2.05 km images, and the rest frame 3300 and 6200 magniÐcations of the lensed quasar are calculated to be 50 ^11 and A 25 ^6, respectively, which translates into a rest-frame optical luminosity for the quasar of D6 ] 109 L _ . These magniÐcation values are lower than the previously measured magniÐcation of D100 at rest frame 2400If the dust in the primary lensing galaxy is not a †ecting the measurement of the counterimage A . Ñux at 2400 and 3300 the magniÐcation of the quasar appears to decrease with increasing wavelength. A , Flux measurements of the primary lensing galaxy Ðt the spectral energy distribution of an unevolving elliptical galaxy at a redshift of 0.9, consistent with previous determinations of the redshift. Subject headings : galaxies : distances and redshifts È galaxies : individual (IRAS FSC 10214]4724) È gravitational lensing È infrared : galaxies

A Chandra observation of the z= 2.285 galaxy FSC 10214+4724: evidence for a Compton-thick quasar?

“…Although somewhat uncertain, this suggests that the magnification in the X‐ray band is ≳25 (e.g. compare to the extent and magnification found in the 2.05‐μm NICMOS observations of Evans et al 1999). We can compare this estimate to the expected lensing boost from other observations.…”

“…Originally proposed to be the most luminous galaxy known (Rowan‐Robinson et al 1991), multiwavelength observations subsequently showed that it is lensed by an intervening z ≈ 0.9 galaxy, boosting its intrinsic emission by a factor of ≳10–100 (depending on the location and extent of the unlensed emission with respect to the caustic; e.g. Broadhurst & Lehar 1995; Downes, Solomon & Radford 1995; Trentham 1995; Eisenhardt et al 1996; Evans et al 1999). Optical and near‐infrared (near‐IR) spectroscopic/polarimetric observations have unambiguously shown that FSC 10214 + 4724 hosts an obscured active galactic nucleus (AGN; e.g.…”