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Frederick Marshall
Frederick Marshall

NewsRadio Image


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NewsRadio Image


For any telescope, the resolution of its images depends on the size of its aperture. Interferometers like ASKAP simulate the aperture of a much larger telescope. With 36 relatively small dishes (each 12m in diameter) but a 6km distance connecting the farthest of these, ASKAP mimics a single telescope with a 6km wide dish.


Even with such a large dish, Parkes has rather limited resolution. By combining the information from both Parkes and ASKAP, each fills in the gaps of the other to give us the best fidelity image of this region of our Milky Way galaxy. This combination reveals the radio emission on all scales to help uncover the missing supernova remnants.


Linking the datasets from EMU and PEGASUS will allow us to reveal more hidden gems. In the next few years we will have an unprecedented view of almost the entire Milky Way, about a hundred times larger than this initial image, but with the same level of detail and sensitivity.


Radio image of Cassiopeia A supernova remnant.More about this ImageCassiopeia A is the remnant of a supernova explosion that occured over 300 years ago in our Galaxy, at a distance of about 11,000 light years from us. Its name is derived from the constellation in which it is seen: Cassiopeia, the Queen. A supernova is the explosion that occurs at the end of a massive star's life; and Cassiopeia A is the expanding shell of material that remains from such an explosion. This radio image of Cassiopeia A was created with the National Science Foundation's Very Large Array telescope in New Mexico. The image was made at three different frequencies: 1.4 GHz (L band), 5.0 GHz (C band) and 8.4 GHz (X band). Cassiopeia A is one of the brightest radio sources in the sky and has been a popular target of study for radio astronomers for decades. The material that was ejected from the supernova explosion can be seen in this image as bright filaments.Investigators involved in this research were L. Rudnick, T. Delaney, J. Keohane and B. Koralesky; image composite by T. Rector. (Date of Image: 1994)


General Restrictions: Images and other media in the National Science Foundation Multimedia Gallery are available for use in print and electronic material by NSF employees, members of the media, university staff, teachers and the general public. All media in the gallery are intended for personal, educational and nonprofit/non-commercial use only. Images credited to the National Science Foundation, a federal agency, are in the public domain. The images were created by employees of the United States Government as part of their official duties or prepared by contractors as "works for hire" for NSF. You may freely use NSF-credited images and, at your discretion, credit NSF with a "Courtesy: National Science Foundation" notation. Additional information about general usage can be found in Conditions.


Also Available:Download the high-resolution JPG version of the image. (360 KB) Use your mouse to right-click (Mac users may need to Ctrl-click) the link above and choose the option that will save the file or target to your computer.


Every time I post a radio telescope image of a near-Earth asteroid, I get at least one reader question asking me to explain how radio telescopes take photos, so I'm hereby writing a post explaining the basics of how delay-Doppler imaging works.


Radio scientists refer to time as "delay," as in "the delay between our broadcast and when we heard the return signal," and the wavelength axis of my crude graph above as "Doppler." So turn that graph on its side and you get an explanation of how radio scientists can arrive at an image like this one, the significance of which I will explain in the next post. Arecibo would be two million kilometers above your head; delay increases from top to bottom, Doppler from left to right.


In this version of the catalog, images taken in the the new EVLA configurationhave been re-reduced using shallower CLEAN thresholds in order to reduce the"CLEAN bias" in t




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