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Space-Warping Planets: The Microlensing Method

Microlensing is the only known method capable of discovering planets at truly great distances from Earth. Whereas radial velocity searches look for planets in our immediate galactic neighborhood, up to 100 light years from Earth, and transit photometry can potentially detect planets at a distance of hundreds of light years from Earth, microlensing can find planets orbiting stars near the center of the galaxy, thousands of light-years away.

How We Detect Exoplanets: The Microlensing Method

The Planetary Society

How We Detect Exoplanets: The Microlensing Method
Star gravity makes space bend near it. When a star passes in front of another star, it bends the distant starlight like a lens, making it brighter. If the lensing star has an exoplanet, it acts like another lens, making the star even brighter.
Planet Detection through Microlensing

OGLE

Planet Detection through Microlensing
The microlensing process in stages, from right to left. The lensing star (white) moves in front of the source star (yellow) magnifying its image and creating a microlensing event. In the fourth image from the right the planet adds its own microlensing effect, creating the two characteristic spikes in the light curve.

Microlensing is an astronomical effect predicted by Einstein's General Theory of Relativity. According to Einstein, when the light emanating from a star passes very close to another star on its way to an observer on Earth, the gravity of the intermediary star will slightly bend the light rays from the source star, causing the two stars to appear farther apart than they normally would. This effect was used by Sir Arthur Eddington in 1919 to provide the first empirical evidence for General Relativity.

Now, if the source star is positioned not just close to the intermediary star when seen from Earth, but precisely behind it, this effect is multiplied. Light rays from the source star pass on all sides of the intermediary, or "lensing" star, creating what is known as an "Einstein ring." Even the most powerful Earth-bound telescope cannot resolve the separate images of the source star and the lensing star between them, seeing instead a single giant disk of light, known as the "Einstein disk," where a star had previously been. The resulting effect is a sudden dramatic increase in the brightness of the lensing star, by as much as 1,000 times. This typically lasts for a few weeks or months before the source star moves out of alignment with the lensing star and the brightness subsides.

While this is the normal pattern of a microlensing event, things are substantially different when the lensing star has a smaller companion. If a planet is positioned close enough to the lensing star so that it crosses one of the two light streams emanating from the source star, the planet's own gravity bends the light stream and temporarily produces a third image of the source star. When measured from Earth, this effect appears as a temporary spike of brightness, lasting several hours to several days, superimposed upon the regular pattern of the microlensing event. For planet hunters, such spikes are the telltale signs of the presence of a planet. Furthermore, the precise characteristics of the microlensing light-curve, its intensity and length, tell scientists a great deal about the planet itself. Its total mass, its orbit, and its period can all be deduced with a high degree of accuracy and probablity from the microlensing event.

Visit the NASA Exoplanet Archive for a current list of planets discovered through microlensing.

Advantages

Microlensing is capable of finding the most distant and the smallest planets of any currently available method for detecting extrasolar planets. In January 2006 scientists announced the discovery through microlensing of a planet of only five Earth masses, orbiting a star near the center of our galaxy, 22,000 light-years away! It was the lowest mass planet detected up to that time, and also the farthest from Earth.

Microlensing, furthermore, is most sensitive to planets that orbit in moderate to large distances from their star. This makes it complementary to the radial velocity and transit detection methods, both of which are most effective at detecting planets orbiting very close to their stars. In fact, microlensing events can reveal the presence of free-floating or rogue planets that don't orbit stars at all.

Finally, like transit photometry, microlensing searches are massive, targeting tens of thousands of planets simultaneously. If a microlensing event takes place anywhere within the observed starfield, it will be detected.

Because of its sensitivity to low-mass planets that orbit at relatively large distances from their stars, microlensing surveys can yield discoveries of Earth-sized (and smaller) worlds orbiting at Earth-like distances from Sun-like and larger stars.

The microlensing light curve of planet OGLE–2005-BLG-390Lb

European Southern Observatory

The microlensing light curve of planet OGLE–2005-BLG-390Lb
The general curve shows the microlensing event peaking on July 31, 2005, and then diminishing. The disturbance around August 10 indicates the presence of a planet.

Drawbacks

Unlike planets detected by other methods, which are associated with particular stars and can be observed repeatedly, planets detected by microlensing will never be observed again. This is because microlensing events are unique and do not repeat themselves. Thanks to a microlensing event we know, for example, that the planet known as OGLE–2005-BLG-390Lb is a cold, rocky world orbiting a small, cool star near the center of the galaxy. After several years have passed and the background star has moved away, astronomers can sometimes observe the lensing star again and learn more about it. As for the alien world itself, we will probably never know anything more about it, since it will never be observed again.

Another problem with microlensing is that the distance of the detected planet from the Earth is known only by rough approximation. When dealing with planets tens of thousands of light-years away, this could mean errors of thousands of light-years!

Finally, microlensing is dependent on rare and random events - the passage of one star precisely in front of another, as seen from Earth, with a planet orbiting the lensing star positioned relatively close by. This makes the discovery of planets by this method both difficult and unpredictable.

The 1.3 meter

OGLE

The 1.3 meter "Warsaw" telescope at Las Campanas, Chile, used by OGLE

Microlensing Projects

The Optical Gravitational Lensing Experiment (OGLE), led by Andrzej Udalski of Warsaw University, found the first 3 planets ever detected through microlensing. The international project makes use of the 1.3-meter Warsaw telescope at Las Campanas, Chile, to search for microlensing events. Every night the telescope is pointed toward the same dense field of 100 million stars in the vicinity of the galactic bulge, while the telescope's complex CCD cameras note any change in brightness of any point in the starfield. Every year OGLE detects about 500 microlensing events, but planet detections are extremely rare. As of February 2020, it had found 49 exoplanets.

Microlensing Observations in Astrophysics (MOA), led by Yasushi Muraki of Nagoya University, is a Japanese-New Zealand collaboration that uses a 1.8-meter telescope in New Zealand. As of February 2020 it had yielded 24 exoplanets.

The Korea Microlensing Telescope Network (KMTNet) runs CCD-equipped, 2-meter telescopes at 3 southern observatories. As of February 2020 it had discovered 10 exoplanets.

Whenever OGLE and MOA detect a microlensing event, it contacts a network of telescopes that specialize in searching for signs of the presence of a planet. The networks, known as Robonet, MicroFUN (the Microlensing Follow-Up Network), and PLANET (the Probing Lensing Anomalies NETwork), include 1- and 2- meter telescopes across the globe. Together, the telescopes are able to continuously cover each microlensing event, providing an accurate light curve and indicating whether a planet is present or not.

Acknowledgments

This page was originally written in 2002 by staff writers for The Planetary Society. The Society most recently revised and updated it in February 2020 and thanks Emily Sandford for helpful comments.

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