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Event Horizon Spin Coin The Event Horizon Telescope (EHT) VideoEvent Horizon Frontier: PVE Best team 最佳陣容
However, VLBI also has a lot of large blank areas that are not covered by any of the antennas. These missing parts make it difficult for VLBI to reproduce a high-fidelity image of a target object from the synthesized data.
This is a common problem for all radio interferometers, including ALMA, but it can be more serious in VLBI where the antennas are located very far apart.
It might be natural to think that a higher resolution means a higher image quality, as is the case with an ordinary digital camera, but in radio observations the resolution and image quality are quite different things.
The resolution of a telescope determines how close two objects can be to each other and yet still be resolved as separate objects, while the image quality defines the fidelity in reproducing the image of the structure of the observed object.
For example, imagine a leaf, which has a variety of veins. The resolution is the ability to see thinner vein patterns, while the image quality is the ability to capture the overall spread of the leaf.
Researchers have been studying data processing methods to improve image quality for almost as long as the history of the radio interferometer itself, so there are some established methods that are already widely used, while others are still in an experimental phase.
The observations with the EHT and the GMVA were completed in April The data collected by the antennas around the world has been sent to the United States and Germany, where data processing will be conducted with dedicated data-processing computers called correlators.
The data from the South Pole Telescope, one of the participating telescopes in the EHT, will arrive at the end of , and then data calibration and data synthesis will begin in order to produce an image, if possible.
This process might take several months to achieve the goal of obtaining the first image of a black hole, which is eagerly awaited by black hole researchers and the general astronomical community worldwide.
This lengthy time span between observations and results is normal in astronomy, as the reduction and analysis of the data is a careful, time-consuming process.
Right now, all we can do is wait patiently for success to come — for a long-held dream of astronomers to be transformed into a reality. 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.
Let's say there's a disc on a table that rotates at 60 rpm. When you are standing still it spins at 60 rpm. But if you start running around it, it will move faster or slower relative to you.
In this case, the disc has a ground speed, 60 rpm, because it has something to spin in relation to, in this case, the table. Now, let's say that there is a spinning black hole.
Because there is no control for the black hole to spin relative to, its spin must be relative to an object, for example, you.
If you stand still, it spins at a constant rate. But if you start moving around the black hole in the same direction as the rotation, according to Newtonian physics, the black hole would spin at a slower rate relative to you.
Since a faster spinning black hole has a smaller event horizon, in the first case, there would be a smaller event horizon.
Then how do scientists say that there are spinning and non-spinning black holes? Is that just in relation to Earth? First Idea My first idea is also one that is more intuitive.
When I move around the black hole, the black hole spins slower relative to me and consequently has a larger event horizon.
In this idea, the black hole would just behave like a normal object. This would mean that if you went really fast around a black hole, you could get a lot closer to the black hole that if you were standing still.
This is kind of like a satellite that orbits Earth. The slower it moves, the easier it is to fall to the Earth. I know this is a horrible analogy.
Nothing special happens here. Second Idea My second idea is that when you move faster around the black hole, the relative rotational speed of the black hole doesn't change.
This is like trying to accelerate past the speed of light. No matter how much energy you spend, your speed barely changes. I don't understand how this one would work.
Why won't the rotational speed of the black hole stay the same? What do black holes spin relative to? And what happens if you move around it?
There are lots of questions that ask how black holes spin, or how fast they spin, but as far as I know, none of them address this question.
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Press enter to see results or esc to cancel. As of December 19, all the data from each of the radio telescopes has been gathered. It is being processed to filter out background noise and interference.
For a short EHT video as of April 30, , click here. It is the most exciting time of the project. We will be sure to share what we find after we have put the data and analysis methods through "stringent tests" to convince ourselves, and independent astronomy colleagues, of what these horizon-resolving observations tell us.
Scientists have patiently waited as existing facilities were upgraded, new facilities were built, and technical conditions and weather were right to obtain a good look at a black hole.
The EHT also was peering through much less of a interstellar medium when pointed at M These factors contributed to making the neighboring black hole in M87 more accessible for imaging — and, consequently, it turned out to be the first choice for the EHT.
The EHT is an extensive virtual telescope created by combining simultaneous observations from radio arrays and dishes all around the planet. During April 5th through 11 in , the EHT observed M87 on four separate days using an array that included eight radio telescopes at six geographic locations: Arizona USA , Chile, Hawai'i USA , Mexico, the South Pole, and Spain.
The telescopes caught whatever light it was able to detect from near the black hole. By combining the data from the various telescopes from around the world, the EHT has as much magnifying power as a telescope the size of the entire earth.
The EHT was able to achieve unprecedented resolution. It can resolve down to 50 millionths of an arcsecond uas at its observing wavelength of 1.
Years of preparation and an astonishing spate of planet-wide good weather paid off with an extraordinary multi-petabyte million gigabytes yield of data.
The results were presented by a team of instrument, algorithm, software, modeling, and theoretical experts.
This followed a tremendous effort by a group of scientists that span all career stages, from undergraduates to senior members of the field.
More than members from 59 institutes in 20 countries and regions have devoted years to the effort, all unified by a common scientific vision. A defining feature of the images is an irregular but clear bright ring, whose size and shape agree closely with the expected lensed photon orbit of a 6.
The image of the shadow confines the mass of M87 to within its photon orbit, providing the strongest case for the existence of a supermassive black hole.
These observations are consistent with Doppler brightening of "relativistically" moving plasma close to the black hole. The observations produced an enormous amount of data that had to be stored on hard drives and then flown to Germany and Massachusetts where it was distilled to a more usable volume by supercomputers.
Then scientists could analyze and reconstruct the images. Previous estimates — based on models as well as spectroscopic observations of the galaxy by the Hubble Space Telescope - range between 3.
EHT scientists also deduced the radius of the event horizon to be 3. They also found that the rotation of the black hole is in a clockwise direction, and that its spin points away from us.
The brightness in the lower part of the image is due to the relativistic movement of material in a clockwise direction because that portion is moving towards us.
Why is the southern part of the ring brighter? The central axis of the spinning album or wheel is stationary, while the outer edges of the circle are traveling the circumference of the circle with each rotation, the further you move from the center of rotation, the quicker your speed.
In other words, the larger the wheel, the faster the rotation, and the more distance is covered per unit time.
If you imagine an ant crossing a spinning record album, at the edges the ant would feel the fast motion as air zoomed by, and the pull of a centrifugal force working to fling the poor ant off the spinning record album, but as the ant crawled toward the center its feeling of motion would decrease.
The same thing can be felt if you have ever been on a merry-go-round, the closer you are toward the center the less you feel the motion of your spin.
This bizarre paradox inspired Isaac Newton to study motion, and in the process, discovered gravity , and the three laws of motion that govern how all objects move in the universe.
For example, a car might have a velocity of 50 Miles per Hour Acceleration is the rate of change of velocity per unit of time. For example, if a car is traveling at 50 Miles per Hour for 50 Miles and does not change speed, then it has 0 acceleration.
A car that is stationary and not moving, also has 0 acceleration. This is because in both examples the velocity does not change.
Mathematically it is more difficult to calculate acceleration, one way to do it is to find the change of velocity for each unit of time.
For example, a car going from 0 to 50 Miles Per Hour over a 5-hour long race course, we can find the speed at each 1-hour intervals and average them.
At the starting line the car is traveling at 0 miles per hour. At 1 hour the car is traveling at 10 miles per hour. At 2 hours the car is traveling at 20 miles per hour.
At 3 hours the car is traveling at 30 miles per hour. At 4 hours the car is traveling at 40 miles per hour. At 5 hours the car is traveling at 50 miles per hour.
Each hour the car increases its velocity by 10 miles per hour. So, the average acceleration is equal to the average change in velocity divided by the average change in time, so the average of 10, 10, 10, 10, 10, in this example.
The average acceleration is equal to 10 miles per hour, per hour or hour squared. If you know a little calculus, we can find what is called instantaneous acceleration, or the acceleration using the formula:.
Basically, what this equation is stating is that acceleration is the derivative of velocity with respect to time. Objects that are set into motion and have a constant velocity are said to exhibit inertia.
These objects have zero acceleration. Acceleration is when velocity changes over time. Isaac Newton realized that objects in motion will stay in motion, unless acted upon by another force.
This is referred to as the law of inertia. In the weightless environment of outer space, an astronaut can spin a basketball and it will continue to spin at that velocity unless it hits another object, or another object acts against that motion.
However, as Isaac Newton realized , you should be feeling a centrifugal force due to this rotational force.
A force is any interaction that causes an object to be moved in a direction. Newton asked a simple question, why do objects, such as apples, fall to the Earth rather than get flung into outer space due to the rotation of the Earth?
He set about measuring the acceleration of falling objects. For example, an apple dropped from a tower.
Just before the apple is dropped its velocity is 0 meters per second, but after 1 second, the ball is traveling at 10 meters per second.
At 2 seconds the ball is traveling at 20 meters per second. At 3 seconds the ball is traveling at 30 meters per second.