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First Resolution of Microlensed Images

MPG-Autoren

Dong,  Subo
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mérand,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Delplancke-Ströbele,  F.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Gould,  Andrew
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Chen,  Ping
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Post,  R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kochanek,  C. S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Stanek,  K. Z.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Christie,  G. W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mutel,  Robert
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Natusch,  T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Holoien,  T. W. -S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Prieto,  J. L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Shappee,  B. J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Thompson,  Todd A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Externe Ressourcen

https://ui.adsabs.harvard.edu/abs/2019ApJ...871...70D
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Zitation

Dong, S., Mérand, A., Delplancke-Ströbele, F., Gould, A., Chen, P., Post, R., et al. (2019). First Resolution of Microlensed Images. The Astrophysical Journal, 871.


Zitierlink: https://hdl.handle.net/21.11116/0000-0005-D15E-6
Zusammenfassung
We employ Very Large Telescope Interferometer GRAVITY to resolve, for the first time, the two images generated by a gravitational microlens. The measurements of the image separation {{∆ }}{θ }-,+=3.78+/- 0.05 mas, and hence the Einstein radius θ E = 1.87 ± 0.03 mas, are precise. This demonstrates the robustness of the method, provided that the source is bright enough for GRAVITY (K ≲ 10.5) and the image separation is of order of or larger than the fringe spacing. When θ E is combined with a measurement of the “microlens parallax” {π }{{E}}, the two will together yield the lens mass and lens-source relative parallax and proper motion. Because the source parallax and proper motion are well measured by Gaia, this means that the lens characteristics will be fully determined, whether or not it proves to be luminous. This method can be a powerful probe of dark, isolated objects, which are otherwise quite difficult to identify, much less characterize. Our measurement contradicts Einstein’s prediction that “the luminous circle [i.e., microlensed image] cannot be distinguished” from a star. Based on observations made with ESO telescopes at Paranal Observatory under program ID 2100.C-5014.