The structure of the BAL QSO 1700 + 518

Abstract

ABSTRACT. We present 0.5 arcsec resolution optical images of the low-redshift, bright, broad-absorption-line (BAL) QSO 1700+518. We find a bright arc 2 arcsec to the NE of the nucleus which is redder than the surrounding host galaxy. There is also a faint radial structure to the SE, which is aligned with the core radio structure. The principal radio structure is a slightly resolved component coincident with the optical nucleus and an unresolved lobe 1 arcsec to the W which has no corresponding optical structure. We discuss the morphological and other properties of the QSO.

The Host Galaxy of the Broad Absorption Line QSO PG 1700+518 and Its Ring Galaxy Companion: NICMOS 1.6 Micron Imaging

“…Di †use emission surrounding the QSO extends to D5A in deep (3 p \ 25 mag arcsec~2), ground-based V -band images (Hickson & Hutchings 1987 ;Hutchings et al 1992). This structure is presumably associated with the QSO host galaxy, and not the ring galaxy, given the sharpness of the ring edge seen in our images (Fig.…”

“…The double radio source associated with PG 1700]518 Hutchings et al 1992) is apparently not directly associated with the QSO host galaxy or PG 1700]518R, since the position angle di †ers by D50¡.…”

“…Previous ground-based optical and near-IR images of PG 1700]518 reveal a slight extension southwest and an arclike feature northeast of the bright point source B2A .5 (Hickson & Hutchings 1987 ;Hutchings, Ne †, & Gower 1992 ;Stickel et al 1995). The "" E ] A ÏÏ optical spectrum of the arc implies an old population of stars plus an 85 Myr old starburst (Canalizo & Stockton 1997 ;Stockton, Canalizo, & Close 1998), and the small velocity o †set between the arc and the QSO (140 km s~1) suggests that the two are physically associated.…”

“…It was originally identiÐed in the Palomar-Green Survey (Schmidt & Green 1983) and subsequently found to be one of only B2% of QSOs that show broad absorption lines (BALs) from low-ionization species such as Al III j1860 and Mg II j2800 (Wampler 1985 ;Pettini & Boksenberg 1985 ;Turnshek et al 1985). Its IR luminosity, warm far-IR colors indicative of dust heated by a QSO UV continuum km) ¹ 3 : 60 Low et al 198860 Low et al , 1989, and its polarization properties Schmidt & Hines 1999 ;Schmidt, Hines, & Smith 1997), all suggest a strong connection with the ultra-and hyperluminous infrared galaxies (Sanders et al 1988a ;Cutri et al 1994 ;Hines et al 1995).Previous ground-based optical and near-IR images of PG 1700]518 reveal a slight extension southwest and an arclike feature northeast of the bright point source B2A .5 (Hickson & Hutchings 1987 ;Hutchings, Ne †, & Gower 1992 ;Stickel et al 1995). The "" E ] A ÏÏ optical spectrum of the arc implies an old population of stars plus an 85 Myr old starburst (Canalizo & Stockton 1997 ;Stockton, Canalizo, & Close 1998), and the small velocity o †set between the arc and the QSO (140 km s~1) suggests that the two are physically associated.…”

Adaptive-Optics Imaging of Low and Intermediate Redshift Quasars

“…The comparison between the HST and CFHT images of PG 1700+514 shows how powerful AO can be, and bodes well for the use of the technique on 10 m-class telescopes. No obvious relation is found between the near-IR image and the radio map (Hutchings et al 1992). …”