Ultraviolet images of the gravitationally lensed quadruple quasar Q2237+0305 with the HST WFPC2

Michael Blanton, Edwin L. Turner, Joachim Wambsganss

    Research output: Contribution to journalArticle

    Abstract

    We present and analyse observations of the quadruple lensed quasar Q2237+0305, obtained with the HST WFPC2 camera in the F336W and F300W filters. 25 exposures were performed within 15 h real time on 1995 November 3. On a time-scale of 3-4 h, we observe no variation in component A greater than 0.02 mag. The other components remain constant over a period of 10 h to within about 0.05 mag. In the final 5 h there is some evidence (not conclusive) for variation of component D by about 0.1 mag. The exposures indicate that component A is brighter than component B by about 0.3 mag. Components C and D are fainter than component A by about 1.3 and 1.4 mag respectively. Our results place an upper limit on any fifth (central) component of 6.5 mag fainter than component A. We determine the astrometric properties of the lens system, using only the exposures of the higher resolution Planetary Camera chip. We measure the relative distances of the four components with high accuracy. Our values are systematically larger than those of other investigators (by 0.1-2.0 per cent). We discuss the reasons why we believe our results are reliable. The F336W filter had been chosen for the observations because it corresponds to the redshifted Lyα line of the quasar. This filter might have allowed us to see extended Lyα emission from the broad-line region (BLR) of the quasar as Lyα arcs, and hence to determine the physical size of the BLR. However, the quasar components seen in this filter are consistent with a point source. We conclude that there cannot be any Lyα 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, Schieder & Bahcall, this would preclude any such features in the source plane further than 20 mas (∼100 h-1 pc, assuming q0 = 0.5) from the quasar core and brighter than 25 mag before magnification.

    Original languageEnglish (US)
    Pages (from-to)1223-1232
    Number of pages10
    JournalMonthly Notices of the Royal Astronomical Society
    Volume298
    Issue number4
    StatePublished - Aug 21 1998

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    Keywords

    • Gravitational lensing
    • Quasars: individual: Q2237+0305
    • Ultraviolet: galaxies

    ASJC Scopus subject areas

    • Space and Planetary Science

    Cite this

    Ultraviolet images of the gravitationally lensed quadruple quasar Q2237+0305 with the HST WFPC2. / Blanton, Michael; Turner, Edwin L.; Wambsganss, Joachim.

    In: Monthly Notices of the Royal Astronomical Society, Vol. 298, No. 4, 21.08.1998, p. 1223-1232.

    Research output: Contribution to journalArticle

    Blanton, Michael ; Turner, Edwin L. ; Wambsganss, Joachim. / Ultraviolet images of the gravitationally lensed quadruple quasar Q2237+0305 with the HST WFPC2. In: Monthly Notices of the Royal Astronomical Society. 1998 ; Vol. 298, No. 4. pp. 1223-1232.
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    abstract = "We present and analyse observations of the quadruple lensed quasar Q2237+0305, obtained with the HST WFPC2 camera in the F336W and F300W filters. 25 exposures were performed within 15 h real time on 1995 November 3. On a time-scale of 3-4 h, we observe no variation in component A greater than 0.02 mag. The other components remain constant over a period of 10 h to within about 0.05 mag. In the final 5 h there is some evidence (not conclusive) for variation of component D by about 0.1 mag. The exposures indicate that component A is brighter than component B by about 0.3 mag. Components C and D are fainter than component A by about 1.3 and 1.4 mag respectively. Our results place an upper limit on any fifth (central) component of 6.5 mag fainter than component A. We determine the astrometric properties of the lens system, using only the exposures of the higher resolution Planetary Camera chip. We measure the relative distances of the four components with high accuracy. Our values are systematically larger than those of other investigators (by 0.1-2.0 per cent). We discuss the reasons why we believe our results are reliable. The F336W filter had been chosen for the observations because it corresponds to the redshifted Lyα line of the quasar. This filter might have allowed us to see extended Lyα emission from the broad-line region (BLR) of the quasar as Lyα arcs, and hence to determine the physical size of the BLR. However, the quasar components seen in this filter are consistent with a point source. We conclude that there cannot be any Lyα 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, Schieder & Bahcall, this would preclude any such features in the source plane further than 20 mas (∼100 h-1 pc, assuming q0 = 0.5) from the quasar core and brighter than 25 mag before magnification.",
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    N2 - We present and analyse observations of the quadruple lensed quasar Q2237+0305, obtained with the HST WFPC2 camera in the F336W and F300W filters. 25 exposures were performed within 15 h real time on 1995 November 3. On a time-scale of 3-4 h, we observe no variation in component A greater than 0.02 mag. The other components remain constant over a period of 10 h to within about 0.05 mag. In the final 5 h there is some evidence (not conclusive) for variation of component D by about 0.1 mag. The exposures indicate that component A is brighter than component B by about 0.3 mag. Components C and D are fainter than component A by about 1.3 and 1.4 mag respectively. Our results place an upper limit on any fifth (central) component of 6.5 mag fainter than component A. We determine the astrometric properties of the lens system, using only the exposures of the higher resolution Planetary Camera chip. We measure the relative distances of the four components with high accuracy. Our values are systematically larger than those of other investigators (by 0.1-2.0 per cent). We discuss the reasons why we believe our results are reliable. The F336W filter had been chosen for the observations because it corresponds to the redshifted Lyα line of the quasar. This filter might have allowed us to see extended Lyα emission from the broad-line region (BLR) of the quasar as Lyα arcs, and hence to determine the physical size of the BLR. However, the quasar components seen in this filter are consistent with a point source. We conclude that there cannot be any Lyα 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, Schieder & Bahcall, this would preclude any such features in the source plane further than 20 mas (∼100 h-1 pc, assuming q0 = 0.5) from the quasar core and brighter than 25 mag before magnification.

    AB - We present and analyse observations of the quadruple lensed quasar Q2237+0305, obtained with the HST WFPC2 camera in the F336W and F300W filters. 25 exposures were performed within 15 h real time on 1995 November 3. On a time-scale of 3-4 h, we observe no variation in component A greater than 0.02 mag. The other components remain constant over a period of 10 h to within about 0.05 mag. In the final 5 h there is some evidence (not conclusive) for variation of component D by about 0.1 mag. The exposures indicate that component A is brighter than component B by about 0.3 mag. Components C and D are fainter than component A by about 1.3 and 1.4 mag respectively. Our results place an upper limit on any fifth (central) component of 6.5 mag fainter than component A. We determine the astrometric properties of the lens system, using only the exposures of the higher resolution Planetary Camera chip. We measure the relative distances of the four components with high accuracy. Our values are systematically larger than those of other investigators (by 0.1-2.0 per cent). We discuss the reasons why we believe our results are reliable. The F336W filter had been chosen for the observations because it corresponds to the redshifted Lyα line of the quasar. This filter might have allowed us to see extended Lyα emission from the broad-line region (BLR) of the quasar as Lyα arcs, and hence to determine the physical size of the BLR. However, the quasar components seen in this filter are consistent with a point source. We conclude that there cannot be any Lyα 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, Schieder & Bahcall, this would preclude any such features in the source plane further than 20 mas (∼100 h-1 pc, assuming q0 = 0.5) from the quasar core and brighter than 25 mag before magnification.

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    KW - Ultraviolet: galaxies

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