Open Access2016+112: a gravitationally lensed type II quasar
Author(s) -
Koopmans L. V. E.,
Garrett M. A.,
Blandford R. D.,
Lawrence C. R.,
Patnaik A. R.,
Porcas R. W.
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.05438.x
Subject(s) - physics , quasar , astrophysics , gravitational lens , very long baseline interferometry , radio galaxy , astronomy , galaxy , einstein ring , x shaped radio galaxy , brightness , active galactic nucleus , lens (geology) , redshift , optics
A single‐screen model of the gravitational lens system 2016+112 is proposed, that explains recent Hubble Space Telescope ( HST ) infrared (NICMOS–F160W) observations and new high‐resolution European VLBI Network (EVN) 5‐GHz radio observations, presented in this paper. In particular, we find that a massive ‘dark’ structure at the lens position, previously suggested by X‐ray, optical and spectroscopic observations of the field around 2016+112, is not necessarily required to accommodate the strong‐lensing constraints. A massive structure to the north‐west of the lens system, suggested from a weak‐lensing analysis of the field, is included in the model. The lensed source is an X‐ray bright active galaxy at z = 3.273 with a central bright optical continuum core and strong narrow emission lines, suggestive of a type II quasar. The EVN 5‐GHz radio maps show a radio jet structure with at least two compact subcomponents. We propose that the diamond caustic crosses the counter‐jet of the radio source, so that part of the counter‐jet, host galaxy and narrow‐line emission regions are quadruply imaged. The remainder of the radio source, including the core, is doubly imaged. Our lens model predicts a very high magnification (μ∼ 300) at the brightness peaks of the inner two radio components of complex C. If the jet exhibits relativistic velocities on microarsecond scales, it might result in apparent hyperluminal motion. However, the lack of strong radio variability and the peaked radio spectrum imply that these motions need not be present in the source. Our model furthermore implies that the optical spectrum of C′ can only show features of the active galactic nuclei and its host galaxy.