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    "title": "Several impressive filament eruptions leading up to an M 8.7 Flare at Active Region 13234 - February 27-28, 2023",
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    "release_date": "2023-06-06T00:00:00-04:00",
    "update_date": "2023-05-31T09:52:33.068028-04:00",
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        "Visualizations by": [
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                "name": "Tom Bridgman",
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            "description": "<br><br><br><h2>What is the PSF (Point Spread-Function)?</h2>Many telescopes, especially reflecting telescopes such as the ones used on SDO (<a href=\"https://en.wikipedia.org/wiki/Reflecting_telescope\" target=\"_blank\">Wikipedia</a>), have internal structures that support various optical components. These components can result in incoming light being scattered to other parts of the image. This can appear in the image as a faint haze, brightening dark areas and dimming bright areas. The point-spread function (<a href=\"https://en.wikipedia.org/wiki/Point_spread_function\" target=\"_blank\">Wikipedia</a>) is a measure of how light that would normally be received by a single camera pixel, gets scattered onto other pixels. This is often seen as the \"spikes\" seen in images of bright stars. For SDO, it manifests as a double-X shape centered over a bright flare (see <a href=\"https://svs.gsfc.nasa.gov/11383\" target=\"_blank\">Sun Emits Third Solar Flare in Two Days</a>). The effect of this scattered light can be computed, and removed, by a process called deconvolution (<a href=\"https://en.wikipedia.org/wiki/Deconvolution\" target=\"_blank\">Wikipedia</a>). This is often a very compute-intensive process which can be sped up by using a computers graphics-processing unit (GPU) for the computation.<br>",
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                    "name": "Laurence Schuler",
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