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ALMA was designed to work as an interferometer — a telescope made up of many individual elements. Each antenna pair creates a single baseline.
ALMA can produce as many as 1, baselines, some up to 16 kilometers long. But before ALMA could join the Event Horizon Telescope network, it first had to transform into a different kind of instrument known as a phased array.
This new version of ALMA allows its 66 antennas to function as a single radio dish 85 meters in diameter.
Shep Doeleman, the principal investigator of the ALMA Phasing Project, participated during the maser installation via remote video link.
During the upcoming observations, the signal from the phased array will be time-stamped and encoded by a dedicated atomic clock. This will allow the data to be shipped to a central processing center where it will be combined with identically timed signals from other telescopes.
The high-speed recorders that will capture the torrent of data flowing from the ALMA phased array were designed by the MIT Haystack Observatory.
National Science Foundation NSF and the National Institutes of Natural Sciences NINS of Japan in cooperation with the Republic of Chile.
ALMA is funded by ESO on behalf of its Member States, by NSF in cooperation with the National Research Council of Canada NRC and the National Science Council of Taiwan NSC and by NINS in cooperation with the Academia Sinica AS in Taiwan and the Korea Astronomy and Space Science Institute KASI.
ALMA construction and operations are led by ESO on behalf of its Member States; by the National Radio Astronomy Observatory NRAO , managed by Associated Universities, Inc.
AUI , on behalf of North America; and by the National Astronomical Observatory of Japan NAOJ on behalf of East Asia. The Joint ALMA Observatory JAO provides the unified leadership and management of the construction, commissioning and operation of ALMA.
Using ALMA, two teams of astronomers have for the first time discovered a planet-forming disk with misaligned rings around a triple star system, called GW Orionis.
Planet-forming environments can be much more complex and chaotic than previously expected. This is evidenced by a new image of the star RU Lup, made with ALMA.
NRAO and GBO are saddened at the announcement of the decommissioning of the Arecibo Telescope in Puerto Rico, which has a long and distinguished history of scientific accomplishment.
Join our host Melissa Hoffman as she talks about the history of the VLA and some of the remarkable objects it has discovered! Entries combined observational data from the VLA with data from optical, infrared, and X-ray telescopes, and from computer simulations.
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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. 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 s.
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. The Event Horizon Telescope EHT will initially be composed of 12 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 6 telescope system has been running for some time. See the image to the left which shows radio telescopes in Hawaii, California, Arizona, Mexico, France, Spain, Chile and the South Pole.
As the separation between the telescopes making up the array has increased, the array's resolution increased and it is able to discern finer and finer details.
Also, increasing the frequency of the equipment enhances the resolution. Both enhancements were implemented in The first full blown look at the Milky Way black hole will occur in the spring of 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.
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. The event horizon of Sgr. Although the Keck telescopes mentioned above have terrific resolutions for optical astronomy, they are far short of the resolution needed for detailed Sgr.
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.
With its unprecedented resolution, more than 1, 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.