The Effect of the Stellar Size on Microlensing at the Baade Window

Witt, Hans J.

doi:10.1086/176029

Cited by 85 publications

(91 citation statements)

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“…However, as shown in several papers (e.g. Valls-Gabaud 1994;Witt 1995;Han et al 2000) blending on the one hand and differential amplification of an extended source on the other hand can lead to a chromatic, but still symmetric, lensing light curve. Under certain circumstances chromatic light curves permit to constrain the physical properties of the source-lens system (e.g.…”

Section: Observing Strategymentioning

confidence: 96%

WeCAPP -Wendelstein Calar Alto pixellensing project I

Riffeser

Fliri

Gössl

et al. 2001

A&A

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Abstract. We present WeCAPP, a long term monitoring project searching for microlensing events towards M 31. Since 1997 the bulge of M 31 was monitored in two different wavebands with the Wendelstein 0.8 m telescope. In 1999 we extended our observations to the Calar Alto 1.23 m telescope. Observing simultaneously at these two sites we obtained a time coverage of 53% during the observability of M 31. To check thousands of frames for variability of unresolved sources, we used the optimal image subtraction method (OIS) by Alard & Lupton (1998). This enabled us to minimize the residuals in the difference image analysis (DIA) and to detect variable sources with amplitudes at the photon noise level. Thus we can detect microlensing events with corresponding amplifications A > 10 of red clump giants with MI = 0.

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Section: Observing Strategymentioning

confidence: 96%

WeCAPP -Wendelstein Calar Alto pixellensing project I

Riffeser

Fliri

Gössl

et al. 2001

A&A

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“…In principle, one could also compute the image centroid for the source including occultation (as done by Witt 1995). We now provide several graphical examples of these equations.…”

Section: Extended Uniform Sourcementioning

confidence: 99%

Occultation and Microlensing

Agol

2002

ApJ

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Occultation and microlensing are different limits of the same phenomenon of one body passing in front of another body. We derive a general exact analytic expression that describes both microlensing and occultation in the case of spherical bodies with a source of uniform brightness and a nonrelativistic foreground body. We also numerically compute the case of a source with quadratic limb darkening. In the limit that the gravitational deflection angle is comparable to the angular size of the foreground body, both microlensing and occultation occur as the objects align. Such events can be used to constrain the size ratio of the lens and source stars, the limb-darkening coefficients of the source star, and the surface gravity of the lens star (if the lens and source distances are known). Application of these results to microlensing during transits in binaries and giant-star microlensing is discussed. These results unify the microlensing and occultation limits and should be useful for rapid model fitting of microlensing, eclipse, and '' micro-occultation '' events.

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“…The exceptions arise from cases in which the source colour varies spatially, so that during the course of the event the relative magnification of the blue and red source material varies. This can occur because of differential limb darkening when the lens transits the source (Witt 1995;Yoo et al 2004) or because both components of a binary source are significantly magnified during the event, but by relative factors that vary with time. The first explanation is ruled out by the lack of finite-source effects in the light curve, which would always accompany significant colour changes.…”

Section: Colour Evolution Sc5_2859mentioning

confidence: 99%

The OGLE-II event sc5_2859: a classical nova outburst?

Afonso

Glicenstein

Gould

et al. 2006

A&A

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Context. The OGLE-II event sc5_2859 was previously identified as the third longest microlensing event ever observed. Aims. Additional photometric observations from the EROS (Expérience de Recherche d'Objets Sombres) survey and spectroscopic observations of the candidate star are used to test the microlensing hypothesis. Methods. The combined OGLE and EROS data provide a high quality coverage of the light curve. The colour of the sc5_2859 event is seen to change with time. A spectrum taken in 2003 exhibits a strong H α emission line. Results. The additionnal data show that the OGLE-II sc5_2859 event is actually a classical nova outburst.

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The Effect of the Stellar Size on Microlensing at the Baade Window

Cited by 85 publications

References 0 publications

WeCAPP -Wendelstein Calar Alto pixellensing project I

WeCAPP -Wendelstein Calar Alto pixellensing project I

Occultation and Microlensing

The OGLE-II event sc5_2859: a classical nova outburst?

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