Ultraviolet images of the gravitationally lensed quadruple quasar Q2237+0305 with the HST

Details Ultraviolet images of the gravitationally lensed quadruple quasar Q2237+0305 with the HST Ultraviolet images of the gravitationally lensed quadruple quasar Q2237+0305 with the HST

1998-05-29

arxiv.org/abs/astro-ph/9805359v2

Pub. 1998, MNRAS, 298, 1223

Astronomy and Astrophysics

Astrophysics

16 pages, Latex, 9 figures, accepted by MNRAS, 3 tables added

Scientific paper

10.1046/j.1365-8711.1998.01720.x

We analyze observations of the quadruple lensed quasar Q2237+0305, taken with the WFPC2 camera in the F336W and F300W bands. 25 exposures were performed within 15 hours real time on 3 November 1995. On a timescale of 3--4 hours, we observe no variation in component A of greater than 0.02 mag. The other components are constant over a period of 10 hours to within about 0.05 mag. In the final 5 hours there is some evidence (not conclusive) for variation of component D by about 0.1 mag. Component A was brighter than component B by about 0.3 mag. Components C and D were fainter than component A by about 1.3 and 1.4 mag. Any fifth (central) component was at least 6.5 mag fainter than component A. Using the PC chip, we measure the relative distances of the four components with high accuracy. Our values are systematically larger than other investigators' (by 0.1% to 2.0%). The F336W filter had been chosen for the observations because it could have allowed us to see extended Ly-alpha emission from the Broad-Line Region (BLR). However, the quasar components are consistent with a point source. We conclude that there cannot be a Ly-alpha feature in the image plane brighter than about 23.5 mag in F336W and further from the quasar core than 100 mas. According to a lensing model by Rix, Scheider & Bahcall (1992), this would preclude any such features in the source plane further than 20 mas (~ 100 h^{-1} pc, assuming q_0 = 0.5) from the quasar core and brighter than 25 mag before magnification.

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