[ITAL]Hubble Space Telescope[/ITAL] Imaging Polarimetry of the Gravitational Lens FSC 10214+4724

Abstract

We present imaging polarimetry of the extremely luminous, redshift 2.3 IRAS source FSC 10214]4724. The observations were obtained with HST Ïs Faint Object Camera in the F437M Ðlter, which is free of strong emission lines. The long arc is unresolved to FWHM in the transverse 0A .7 0A .04 direction and has an integrated polarization of 28%^3%, in good agreement with ground-based observations. The polarization position angle varies along the arc by up to 35¡. The overall position angle is 62¡^3¡ east of north. No counterimage is detected to B \ 27.5 mag (3 p), giving an observed arc to counterimage Ñux ratio greater than 250, considerably greater than the Ñux ratio of 100 measured previously in the I band. This implies that the conÐguration of the object in the source plane at the B band is di †erent from that at I band and/or that the lensing galaxy is dusty.

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

“…We can compare this estimate to the expected lensing boost from other observations. The HST observations and source model of Nguyen et al (1999) suggest that the central source (i.e. the X‐ray emitting AGN) is ≈100 pc from the caustic, indicating that the magnification of the AGN emission is likely to be ≈100.…”

Ultraviolet Spectropolarimetry of Narrow‐Line Radio Galaxies

“…For the former two galaxies, the spectral shape of the polarized Ñux is again similar to that of a typical QSO (the continuum shape would not be too di †erent from quasars ; e.g., Cristiani & Vio 1990) : a \ [0.5 for IRAS P09104]4109 at jj rest \ 3900È5500 A (excluding the 3000 bump region ; Hines et al 1999 ;Hines A & Wills 1993), and a \ [0.5 for IRAS F15307]3252 at (Hines et al 1995). For IRAS jj rest \ 2200È4200 A F10214]4724, which is a gravitationally lensed galaxy (Nguyen et al 1999), the polarized Ñux is rather red : a \ [1.4 at (Goodrich et al 1996). jj rest \ 1200È2700 A For IRAS P09104]4109, the spatial polarized Ñux distribution has been found to be extended (a few kiloparsecs ; Hines et al 1999).…”

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

“…A of D100, and Nguyen et al (1999) have computed a lower limit of the rest-frame 1300 magniÐcation of D250. Thus, A the magniÐcation of the lensed quasar appears to be decreasing with increasing wavelength.…”

“…Thus, A the magniÐcation of the lensed quasar appears to be decreasing with increasing wavelength. However, as Nguyen et al (1999) point out, while the arc is most likely too far from the primary lensing galaxy (source 2) for its measured Ñux to be diminished by dust in the lensing galaxy, the proximity of the counterimage to the nucleus of source 2 may mean that the Ñux of the 1300È3300 A counterimage, and thus the Ñux ratio of the arc to counterimage at 1300È3300 are heavily a †ected by dust in the A , primary lensing galaxy. By the same argument, the radiation from the lensed quasar that is detected in the 2.05 km Ðlter has a wavelength of 1.1 km as it passes near the primary lensing galaxy, and is thus una †ected by dust.…”