A quasar under a microlensing caustic

Timo Anguita, Robert Schmidt

Resultado de la investigación: Conference article

Resumen

Using observations of the high magnification event seen in image C of quasar Q2237+0305 during 1999 we have obtained constraints on the structure of the quasar’s central engine. Data taken with the Apache Point Observatory 3.5 mts telescope in the g’ and the r’ bands shows a smaller amplitude of the event in the r’ filter. We compare these observations and those presented by the OGLE team with synthetic source plane microlensing magnification patterns in order to obtain constraints on the size of the accretion disk regions contributing to each band. We obtain for the Gaussian width 1.20 × 1015M/0.1M cm σg 7.96 × 1015M/0.1M cm, where M is the mean microlensing mass, and a ratio σrg = 1.25+ 0 0 45 15. With the limits on the velocity of the lensing galaxy from Gil-Merino et al. (2005)[2] as our only prior, we obtain 0.60 × 1015M/0.1M cm σg 1.57 × 1015M/0.1M cm and a ratio σrg = 1.45+ 0 0 90 25 (all values at 68 percent confidence). Additionally, from our microlensing simulations we find that, during the chromatic microlensing event observed, the continuum emitting region of the quasar crossed a caustic at ≥ 72 percent confidence. This contribution is based on the research presented in Anguita et al. (2008)[1].

Idioma originalEnglish
Número de artículo013
PublicaciónProceedings of Science
Volumen54
EstadoPublished - 1 ene 2008
EventoManchester Microlensing Conference, M2C: 12th International Conference on Gravitational Microlensing, and ANGLES Microlensing Workshop, GMC 2008 - Manchester, United Kingdom
Duración: 21 ene 200825 ene 2008

Huella dactilar

quasars
alkalies
magnification
confidence
accretion disks
engines
observatories
telescopes
galaxies
continuums
filters
simulation

ASJC Scopus subject areas

  • General

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abstract = "Using observations of the high magnification event seen in image C of quasar Q2237+0305 during 1999 we have obtained constraints on the structure of the quasar’s central engine. Data taken with the Apache Point Observatory 3.5 mts telescope in the g’ and the r’ bands shows a smaller amplitude of the event in the r’ filter. We compare these observations and those presented by the OGLE team with synthetic source plane microlensing magnification patterns in order to obtain constraints on the size of the accretion disk regions contributing to each band. We obtain for the Gaussian width 1.20 × 1015M/0.1M cm σg 7.96 × 1015M/0.1M cm, where M is the mean microlensing mass, and a ratio σr /σg = 1.25+ − 0 0 45 15. With the limits on the velocity of the lensing galaxy from Gil-Merino et al. (2005)[2] as our only prior, we obtain 0.60 × 1015M/0.1M cm σg 1.57 × 1015M/0.1M cm and a ratio σr /σg = 1.45+ − 0 0 90 25 (all values at 68 percent confidence). Additionally, from our microlensing simulations we find that, during the chromatic microlensing event observed, the continuum emitting region of the quasar crossed a caustic at ≥ 72 percent confidence. This contribution is based on the research presented in Anguita et al. (2008)[1].",
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A quasar under a microlensing caustic. / Anguita, Timo; Schmidt, Robert.

En: Proceedings of Science, Vol. 54, 013, 01.01.2008.

Resultado de la investigación: Conference article

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