Interpretation of microlensing events in Q2237 + 0305

Witt, Hans J.; Mao, Shude

doi:10.1086/174302

Cited by 66 publications

(76 citation statements)

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“…Graininess of the stellar distribution and dark matter sub-halos in the lens galaxy, in addition to the smooth mass profile, can cause variations to magnification without altering image locations. These milli-and micro-lensing effects (27,28), small enough not to cause additional resolved image separations, offer a plausible explanation for the deviation from the smooth lens model.…”

Section: = 156±4mentioning

confidence: 95%

iPTF16geu: A multiply imaged, gravitationally lensed type Ia supernova

Goobar

Amanullah

Kulkarni

et al. 2017

Science

228

232

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We report the discovery of a multiply-imaged gravitationally lensed Type Ia supernova, iPTF16geu (SN 2016geu), at redshift $z=0.409$. This phenomenon could be identified because the light from the stellar explosion was magnified more than fifty times by the curvature of space around matter in an intervening galaxy. We used high spatial resolution observations to resolve four images of the lensed supernova, approximately 0.3" from the center of the foreground galaxy. The observations probe a physical scale of $\sim$1 kiloparsec, smaller than what is typical in other studies of extragalactic gravitational lensing. The large magnification and symmetric image configuration implies close alignment between the line-of-sight to the supernova and the lens. The relative magnifications of the four images provide evidence for sub-structures in the lensing galaxy.Comment: Matches published versio

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Section: = 156±4mentioning

confidence: 95%

iPTF16geu: A multiply imaged, gravitationally lensed type Ia supernova

Goobar

Amanullah

Kulkarni

et al. 2017

Science

228

232

View full text Add to dashboard Cite

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“…Because the lens is relatively nearby, the image geodesics traverse the dense stellar population of the galaxy bulge. Thus the optical depths for microlensing are large for all four images (Wambsganss, & Katz 1990 ;Wambsganss, Paczyn ski, & Schneider 1990 ;Witt & Mao 1994), and Paczyn ski, microampliÐcation events are frequent. Time delays between the di †erent images are on the order of a day or less (Rix, Schneider, & Bahcall 1992 ;Wambsganss & 1994 ;Chae, Turnshek, & Khersonsky 1998), so Paczyn ski that intrinsic variations are easy to distinguish from microlensing.…”

Section: Introductionmentioning

confidence: 90%

Near‐Infrared Imaging Spectrophotometry of the Gravitational Mirage Q2237+0305

Nadeau

Racine

Doyon

et al. 1999

ApJ

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We present and discuss near-infrared broadband and spectrophotometric images (j/*j \ 60) of the gravitationally lensed quadruple image of Q2237]0305 obtained with the MONICA camera at the Canada- France-Hawaii Telescope in 1991, 1993. The spectrophotometric observations cover the wavelength range 1700 \ j (nm) \ 2400, which includes the Ha emission redshifted to 1770 nm. Our results show that microampliÐcation was achromatic from 1992 to 1994 and had similar amplitudes in the Ha and continuum emission. On the other hand, a comparison of our near-infrared continuum data with visible data from the literature shows a striking wavelength dependence of the relative ampliÐcation of components A and B at epoch 1991 September. This provides strong support to the thermal accretion disk model as a source of the UV-visible continuum emission of quasars. The Ha line proÐle changed between 1992 and 1994 but, at each epoch, di †erences in line proÐle between components are not signiÐcant (\5%). Since the time delays between images is less than one day, this sets a limit of \3% per day for proÐle evolution.

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“…This track is constrained to have identical direction and velocity in both the patterns C and B, but the starting point can be different among the different patterns. It is important to remark that the direction is set to be the same in both patterns, taking into consideration that the shear direction between images C and D is approximately perpendicular (Witt & Mao 1994).…”

Section: Ogle V Light Curvementioning

confidence: 99%

The multiple quasar Q2237+0305 under a microlensing caustic

Anguita

Schmidt

Turner

et al. 2008

A&A

115

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We use the high magnification event seen in the 1999 OGLE campaign light curve of image C of the quadruply imaged gravitational lens Q2237+0305 to study the structure of the quasar engine. We have obtained g -and r -band photometry at the Apache Point Observatory 3.5 m telescope where we find that the event has a smaller amplitude in the r -band than in the gand OGLE V-bands. By comparing the light curves with microlensing simulations we obtain constraints on the sizes of the quasar regions contributing to the g -and r -band flux. Assuming that most of the surface mass density in the central kiloparsec of the lensing galaxy is due to stars and by modeling the source with a Gaussian profile, we obtain for the Gaussian width −0.25 (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.

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Interpretation of microlensing events in Q2237 + 0305

Cited by 66 publications

References 0 publications

iPTF16geu: A multiply imaged, gravitationally lensed type Ia supernova

iPTF16geu: A multiply imaged, gravitationally lensed type Ia supernova

Near‐Infrared Imaging Spectrophotometry of the Gravitational Mirage Q2237+0305

The multiple quasar Q2237+0305 under a microlensing caustic

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