What Is Very Long Baseline Interferometry (VLBI)?
Very Long Baseline Interferometry (VLBI) is a technique where a signal from an astronomical radio source, such as a quasar, is collected at multiple radio telescopes on earth. The distances between the radio telescopes is then calculated using the time difference between the arrivals of the radio signal at different telescopes. This allows the observations of a different object by several radio telescopes to be combined, creating a "virtual telescope" with a size equal to the "maximum separation between the telescopes". A minimum of three antennae is required.
Data received at each antenna in the array includes its arrival time as measured by a local atomic clock such as a hydrogen maser. The data is stored on local hard drives. At a later time, all the data is collected on a super-computer and correlated with each other to produce a very high resolution image.
The resolution achievable using interferometry is proportional to the observed frequency, i.e. the higher the frequency, the higher the resolution of the final image. The EHT started out at 16 Gb/s in 2015, then 32 Gb/s in 2016, and finally 64 Gb/s in several years.
The VLBI technique enables the distance between telescopes to be much greater than that possible with conventional interferometry, which requires antennae to be physically connected by coaxial cables or other types of transmission lines.
The very large telescope separations are possible in VLBI due to the invention of the "closure phase imaging" technique by Roger Jennison in the 1950s. This technique adjusts individual image phase cycles to eliminate small delay errors from the various antennae. Closure phase imaging was a brilliant development enabling today's super radio telescopes. Top
The Event Horizon Telescope (EHT)
The Event Horizon Telescope (EHT) will initially be composed of nine radio observatories based all around the world with the objective of observing up close the black hole at the center of the Milky Way. A prototype of six telescope system has been running for some time. See the image to the left which shows telescopes in Hawaii, California, Arizona, Mexico, Chile and the South Pole. The final nine observatories are listed here.
Through the technique of VLBI many independent radio antennae separated by thousands of miles can be operated in concert to create a “virtual” telescope with a diameter of almost the size of the planet. As the separation between the telescopes making up the array is increased, the array's resolution increases and it is able to discern finer and finer details. Also, increasing the frequency of the equipment enhances the resolution. Both enhancements are being implemented in 2016. The first full blown look at the Milky Way black hole is expected to occur in the spring of 2017.
Massive in weight, black holes are extremely compact, appearing as a tiny point in the sky through the most powerful single telescopes. Left by themselves black holes, like our Milky Way black hole, lie dormant with their mouths open. But when a passing star or gas cloud does come into their vicinity drawn in by the black hole's gravity, the gas or star is heated to billions of degrees as it swirls in the doughnut accretion disk. Black holes are sloppy eaters, and when they feed, jets of x-rays and other radiation are violently expelled into the surrounding area.
Most people think of black holes as giant vacuum cleaners sucking in everything that gets too close. But the supermassive black holes at the centers of galaxies are more like cosmic engines, converting energy from in-falling matter into intense radiation. Jets of x-rays and other radiation are violently expelled into the surrounding areas.
The Event Horizon Telescope was named after the point of no return "event horizon" of a black hole. Its job is to "see" what has been until now unseeable - a small, dark sphere of nothing, a tiny speck in the glow of radiation coming from the center of our galaxy. See Sagittarius A* (pronounced Sagittarius A Star and abbreviated Sgr. A*) to the left.
Sgr. A* is the location of the black hole buried in dust and gas in the middle of our Milky Way galaxy 26,000 light-years away (150,000 trillion miles away). It is not visible in normal light. It can only be seen in infrared and x-ray light. It is there that astronomers believe a supermassive black hole lurks, a tiny trap hole into which the equivalent of four million suns have disappeared.
However, to observe Sgr. A*’s event horizon, one needs an instrument with an extremely tiny resolution. The event horizon of Sgr. A* is estimated to be about 50 micro arc-seconds (μas) in diameter. (An arc-second is 1/3600 of a degree, a measure of angular resolution used by astronomers.) One of the most powerful optical observatories on the planet, the twin Keck telescopes atop Mauna Kea in Hawaii, can only resolve down to 20,000 μas. Trying to see something of 50 μas is like being in Los Angeles and trying to read the date on a coin in New York City. Wow! Top
What Does The Milky Way Black Hole Look Like?
Although the Keck telescopes mentioned above have terrific resolutions for optical astronomy, they are far short of the resolution needed for detailed Sgr. A* observation. Hence the need to join many worldwide radio telescopes into one family and attempt to get down to a resolution of about 10 μas. However, getting all the family members in synch using atomic clocks is very tricky and time consuming. Also, processing all the data takes a fair amount of time because each telescope's data has to be tweaked to get all of the remote telescopes in exact time synch.
The EHT has some intriguing possibilities for not only producing the first image of a black hole, but it will also test Einstein’s general relativity at extremes and might uncover physics beyond general relativity. With its unprecedented resolution, more than 1,000 times better than the Hubble Telescope, the EHT will see swirling gas on its final plunge over the event horizon, never to again be in contact with the rest of the universe. If the theory of general relativity is correct, the black hole itself will be a shadow because not even light can escape its immense gravity.
The image to the left is from a simulation of what the black hole might look like to the EHT. It will be somewhat fuzzy due to some distortions from the gas and dust around it. The light surrounding the black hole's shadow will also be distorted by the extreme force of the black hole's gravity. If some of the light is coming towards us, it will be bent by gravity and may cover up some of the black hole's shadow as shown in the simulation. Top
A Few EHT Telescopes
Arizona Radio Observatory (ARO). The ARO is located on Kitt Peak, a 6,900 foot mountain in southern Arizona. In the 40 years since it was first built, the 12 meter ARO has been at the forefront of millimeter molecular astronomy: studying molecules in space through the use of molecular spectroscopy at millimeter wavelengths. Many of the molecules that have been discovered in the interstellar medium were discovered by the ARO. In 2013, the dish was replaced with ESA's ALMA "prototype" antenna, which had been located in New Mexico.
Only very recent technological advances have made it possible to not only record radio waves at just the right wavelengths where they don’t interfere with water vapor in the atmosphere but also to ensure the ultra-precise timing necessary to combine observations from multiple telescopes thousands of miles apart into one exposure.
Large Millimeter Telescope (LMT). The LMT is a 20 story facility with a 50 meter (165 foot) bowl antenna (the largest in the world) on one of the highest southern Mexican mountains and one of the main components of the EHT. It is a joint project consisting of 80% Mexican and 20% American funding by the Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE) and the University of Massachusetts Amherst.
Perhaps the most stunning application of the EHT will come when studying the flares Sgr. A* is known to periodically generate. Approximately once a day, multiple observatories have observed a flaring event that not only causes a brightening of Sgr. A*’s emission, but it also changes the structure of the emission region. These flares have been interpreted as “hotspots” in the accretion flow close to the event horizon. When the EHT is fully operational, it will be able to track these hotspots, tracing their origin and watch them diminish. Not only that, astronomers hope to use hotspots as a tracer to map out the "structure of spacetime" in this strong gravity environment.
James Clerk Maxwell Telescope (JCMT). Its 15 meter (50-foot) dish looks at the sky with instruments that tell us about the cold universe in several different ways. Operating between the infrared and radio waves, observing at wavelengths between 1.4 and 0.4mm, it uses some of the most sensitive and sophisticated instrumentation to detect the coldest material in the universe only a few tens of degrees above absolute zero. Water vapor in the Earth’s atmosphere intercepts this radiation, making the high and dry site of Mauna Kea, Hawaii vitally important for the research performed at the JCMT.
In between the stars are giant clouds where stars and solar systems are born. They are made of gas (mostly molecular hydrogen – H2) and cosmic dust (tiny particles of silicate and carbon). The clouds are some of the coldest objects in the universe – so cold that their “heat glow” is invisible to human eyes. We need specialised telescopes and instruments to see this submillimeter radiation. Top
Processing The Data
Processing the data from the nine high altitude observatories is not an easy task. First off, when conventional hard drives were used at the remote sites, 85% of them failed due to the low air pressure at extreme heights. The low air pressure at 15,000 feet caused the magnetic heads to crash into the platters. The replacement hard drives had to be helium filled which are hermetically sealed from the outside air. The new drives not only solved the low-pressure problem, but also offered double the storage capacity.
An enormous amout of data is collected for each 5 day run. Each radio telescope typically collects 900TB of data per 5 day run. That data is then stored on from 1,000 to 2,000 hard drives, which amounts to about 7 petabytes (PB) of total stored data.
Data collected on the hard drives must be transported via jet airliner from the various telescopes to the MIT Haystack Observatory in Westford, Mass. There the images/data are cross-compared and analyzed on a special grid computer, pictured above, made of about 800 CPUs all connected through a high speed network. (For a comparison, EHT is processing about ten times the amount of data than the Large Hadron Collider (LHC) does in Switzerland.) The 800 CPUs use application-specific software to create a virtual telescope that instead of light, culls the astronomical data samples into a single image that's just gigabytes in capacity. The Perimeter Institute at the University of Waterloo in Canada is also one of the prime institutions that will be analyzing the data from the EHT. Top
In theory these black holes were thought to be powered by magnetic fields. For the first time EHT astronomers, using only three telescopes, have detected magnetic fields just outside the event horizon of the black hole at the center of our Milky Way. In Sgr. A* polarized light is emitted by electrons spiraling around magnetic field lines. As a result, this light directly traces the structure of the magnetic fields. "These magnetic fields have been predicted to exist, but no one has seen them before. Our data puts decades of theoretical work on solid observational ground," adds principal investigator Shep Doeleman, who is assistant director of MIT's Haystack Observatory. See an artist's conception of the Milky Way Black Hole to the left. The object in the upper center of the black hole diagram is a corona (never seen by a human, only hard x-rays have been observed).
The EHT team found that magnetic fields in some regions near the black hole are disorderly, with jumbled loops and whorls resembling intertwined spaghetti. They also found that the some magnetic fields fluctuated on short time scales of only 15 minutes or so. In contrast, other regions showed a much more organized pattern. The results appear in the December 2015 issue of the journal Science.
"Understanding these magnetic fields is critical. Nobody has been able to resolve magnetic fields near the event horizon until now," says lead author Michael Johnson of the Harvard-Smithsonian Center for Astrophysics (CfA). "Once again, the galactic center is proving to be a more dynamic place than we might have guessed," says Johnson. "Those magnetic fields are dancing all over the place."
As of August, 2015, the current EHT system resolution was about 60 μas. The first images will probably "not" be at 10 μas as multiple refinements have to be implemented to achieve 10 μas. One of the most important decisions was choosing which wavelength of light would be used. Radio waves were the obvious place to start because they are scattered much less by gas and dust than visible or infra-red light. Then it took a lot of theoretical calculations to settle on the specific wavelength of 1.3mm. "We've run upwards of a million simulations, for many different configurations of what the gas might look like. And in all cases, we think that the 1.3mm wavelength is the right choice to see down to the event horizon," said Professor Ozel of the University of Arizona.
In the spring of 2017, the complete Event Horizon Project, all nine telescopes, are going to produce data from the black hole at the center of the Milky Way. The goal is to directly image the black hole's event horizon for the first time. Given all the data researchers will need to process, we shouldn't expect the first images of a black hole until the end of the year, or even the start of 2018. And that's assuming there's good enough weather to get a clear picture in the viewing window. The Event Horizon Telescope is expected to produce data and images of Sgr. A* and M87 (the next closest black hole to earth) well into the early 2020s.