Close-up view of Einstein Cross
Macro and microlensing, coupled with the giant eye of the European Southern Observatory's Very Large Telescope, enabled astronomers to probe regions on scales as small as a millionth of an arcsecond.
December 15, 2008
Provided by ESO, Garching, Germany
December 15, 2008
Photo by ESO, F. Courbin et al.
Combining a double natural "magnifying glass" with the power of European Southern Observatory's (ESO) Very Large Telescope (VLT), astronomers have scrutinized the inner parts of the disk around a super-massive black hole 10 billion light-years away. They were able to study the disk with a level of detail a thousand times better than that of the best telescopes in the world, providing the first observational confirmation of the prevalent theoretical models of such disks.
The team of astronomers from Europe and the United States studied the "Einstein Cross," a famous cosmic mirage. This cross-shaped configuration consists of four images of a distant source. The multiple images are a result of gravitational lensing by a foreground galaxy, an effect that was predicted by Albert Einstein as a consequence of his theory of general relativity. The light source in the Einstein Cross is a quasar approximately 10 billion light-years away, whereas the foreground-lensing galaxy is 10 times closer. The lensing galaxy's gravitational field bends and magnifies the quasar's light.
This magnification effect, known as "microlensing," in which a galaxy plays the role of a cosmic magnifying glass or a natural telescope, proves useful in astronomy as it allows us to observe distant objects that would otherwise be too faint to explore using currently available telescopes. "The combination of this natural magnification with the use of a big telescope provides us with the sharpest details ever obtained," said Frederic Courbin, leader of the program studying the Einstein Cross with ESO's VLT
In addition to macrolensing by the galaxy, stars in the lensing galaxy act as secondary lenses to produce an additional magnification. This secondary magnification is based on the same principle as macrolensing, but on a smaller scale, and because stars are much smaller than galaxies, it is known as "microlensing." As the stars are moving in the lensing galaxy, the microlensing magnification also changes with time. From Earth, the brightness of the quasar images (four in the case of the Einstein Cross) flickers around a mean value, due to microlensing. The size of the area magnified by the moving stars is a few light-days, or comparable in size to the quasar's accretion disk.
Microlensing affects various emission regions of the disk in different ways, with smaller regions being more magnified. Because differently sized regions have different colors (or temperatures), the net effect of the microlensing is to produce color variations in the quasar images, in addition to the brightness variations. By observing these variations in detail for several years, astronomers can measure how matter and energy are distributed about the super-massive black hole that lurks inside the quasar. Astronomers observed the Einstein Cross three times per month during a period of 3 years using the VLT, monitoring all the brightness and color changes of the four images.
"Thanks to this unique dataset, we could show that the most energetic radiation is emitted in the central light-day away from the super-massive black hole and, more importantly, that the energy decreases with distance to the black hole almost exactly in the way predicted by theory," said Alexander Eigenbrod, who completed the analysis of the data.
The use of the macro and microlensing, coupled with the giant eye of the VLT, enabled astronomers to probe regions on scales as small as a millionth of an arcsecond. This corresponds to the size of a quarter seen at a distance of 3.1 million miles (5 million kilometers), i.e., about 13 times the distance to the Moon. "This is 1,000 times better than can be achieved using normal techniques with any existing telescope," said Courbin.
Measuring the way the temperature is distributed around the central black hole is a unique achievement. Various theories exist for the formation and fuelling of quasars, each of which predicts a different profile. So far, no direct and model-independent observation has allowed scientists to validate or invalidate any of these existing theories, particularly for the central regions of the quasar. "This is the first accurate and direct measurement of the size of a quasar accretion disk with wavelength (color), independent of any model," said team member Georges Meylan.