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    "results": [
        {
            "id": 31356,
            "url": "https://svs.gsfc.nasa.gov/31356/",
            "result_type": "Animation",
            "release_date": "2025-08-30T01:59:59-04:00",
            "title": "Cosmic Caverns in the Cat’s Paw Nebula",
            "description": "This visualization explores a subset of toe bean-reminiscent structures within a section of the Cat’s Paw Nebula, a massive, local star-forming region located approximately 4,000 light-years away in the constellation Scorpius.",
            "hits": 65
        },
        {
            "id": 14868,
            "url": "https://svs.gsfc.nasa.gov/14868/",
            "result_type": "Produced Video",
            "release_date": "2025-07-23T00:00:00-04:00",
            "title": "XRISM Satellite X-rays Milky Way’s Sulfur in Detail",
            "description": "An international team of scientists have provided an unprecedented tally of elemental sulfur spread between the stars using data from the Japan-led XRISM (X-ray Imaging and Spectroscopy Mission) spacecraft.Astronomers used X-rays from two binary star systems to detect sulfur in the interstellar medium, the gas and dust found in the space between stars. It’s the first direct measurement of both sulfur’s gas and solid phases, a unique capability of X-ray spectroscopy, XRISM’s (pronounced “crism”) primary method of studying the cosmos.Using ultraviolet light, researchers have found gaseous sulfur in the space between stars. In denser parts of the interstellar medium, such as the molecular clouds where stars and planets are born, this form of sulfur quickly disappears.Scientists assume the sulfur condenses into a solid, either by combining with ice or mixing with other elements.When a doctor performs an X-ray here on Earth, they place the patient between an X-ray source and a detector. Bone and tissue absorb different amounts of the light as it travels through the patient's body, creating contrast in the detector.Scientists did something similar by picking a portion of the interstellar medium with the right density — not so thin that all the X-rays would pass through unchanged, but also not so dense that they would all be absorbed.Then they selected a bright X-ray source behind that section of the medium, a binary star system called GX 340+0 located over 35,000 light-years away in the southern constellation Scorpius.Using the Resolve instrument on XRISM, the researchers were able to measure the energy of GX 340+0’s X-rays and determined that sulfur was present not only as a gas, but also as a solid, possibly mixed with iron.Iron-sulfur compounds are often found in meteorites, so scientists have long thought they might be one way sulfur solidifies out of molecular clouds to travel through the universe. XRISM’s observations could match a few of these compounds — pyrrhotite, troilite, and pyrite, which is sometimes called fool’s gold.The researchers were also able to use measurements from a second X-ray binary called 4U 1630-472 that helped confirm their findings. || ",
            "hits": 46
        },
        {
            "id": 4980,
            "url": "https://svs.gsfc.nasa.gov/4980/",
            "result_type": "Visualization",
            "release_date": "2022-03-24T01:02:00-04:00",
            "title": "May 15-16, 2022 Total Lunar Eclipse: Shadow View",
            "description": "Eastern Daylight Time (EDT). The Moon moves right to left, passing through the penumbra and umbra, leaving in its wake an eclipse diagram with the times at various stages of the eclipse. || shadow_diagram_edt_202205_print.jpg (1024x576) [85.9 KB] || moon.2355_searchweb.png (320x180) [48.4 KB] || moon.2355_thm.png (80x40) [5.0 KB] || umbracam_edt_202205_1080p30.mp4 (1920x1080) [12.2 MB] || umbracam_edt_202205_720p30.mp4 (1280x720) [6.7 MB] || umbracam_edt_202205_720p30.webm (1280x720) [9.4 MB] || umbracam_edt_202205_2160p30.mp4 (3840x2160) [35.5 MB] || umbracam_edt_202205_360p30.mp4 (640x360) [2.4 MB] || shadow_diagram_edt_202205.tif (3840x2160) [6.7 MB] || edt (3840x2160) [0 Item(s)] || umbracam_edt_202205_1080p30.mp4.hwshow [193 bytes] || ",
            "hits": 162
        },
        {
            "id": 4903,
            "url": "https://svs.gsfc.nasa.gov/4903/",
            "result_type": "Visualization",
            "release_date": "2021-04-26T09:00:00-04:00",
            "title": "May 26, 2021 Total Lunar Eclipse: Shadow View",
            "description": "Pacific Daylight Time (PDT). The Moon moves right to left, passing through the penumbra and umbra, leaving in its wake an eclipse diagram with the times at various stages of the eclipse. || pdt_print.jpg (1024x576) [72.9 KB] || pdt_searchweb.png (320x180) [45.2 KB] || pdt_thm.png (80x40) [4.9 KB] || eclipse_202105_pdt_1080p30.mp4 (1920x1080) [8.4 MB] || eclipse_202105_pdt_720p30.mp4 (1280x720) [4.6 MB] || fancy_pdt (1920x1080) [0 Item(s)] || eclipse_202105_pdt_720p30.webm (1280x720) [7.8 MB] || eclipse_202105_pdt_2160p30.mp4 (3840x2160) [26.3 MB] || eclipse_202105_pdt_360p30.mp4 (640x360) [1.7 MB] || fancy_pdt (3840x2160) [0 Item(s)] || eclipse_202105_pdt_1080p30.mp4.hwshow [192 bytes] || ",
            "hits": 60
        },
        {
            "id": 4177,
            "url": "https://svs.gsfc.nasa.gov/4177/",
            "result_type": "Visualization",
            "release_date": "2014-07-23T00:00:00-04:00",
            "title": "As Seen by STEREO-A: The Carrington-Class CME of 2012",
            "description": "STEREO-A, at a position along Earth's orbit where it has an unobstructed view of the far side of the Sun, could clearly observe possibly the most powerful coronal mass ejection (CME) of solar cyle 24 on July 23, 2012.  The visualizations on this page cover the entire day.We see the flare erupt in the lower right quadrant of the solar disk from a large active region.  The material is launched into space in a direction towards STEREO-A.  This creates the ring-like 'halo' CME visible in the STEREO-A coronagraph, COR-2 (blue circular image).As the CME expands beyond the field of view of the COR-2 imager, the high energy particles reach STEREO-A, creating the snow-like noise in the image.  The particles also strike the HI-2 imager (blue square) brightening the image.The HI-1 imager has had 'bloom removal' enabled and filled with contents of the immediately previous HI-1 image, which creates a linear artifact above and below bright stars and planets. || ",
            "hits": 199
        },
        {
            "id": 11422,
            "url": "https://svs.gsfc.nasa.gov/11422/",
            "result_type": "Produced Video",
            "release_date": "2013-11-22T11:00:00-05:00",
            "title": "NASA's Solar Observing Fleet Watch Comet ISON's Journey Around the Sun",
            "description": "After several days of continued observations, scientists continue to work to determine and to understand the fate of Comet ISON: There's no doubt that the comet shrank in size considerably as it rounded the sun and there's no doubt that something made it out on the other side to shoot back into space. The question remains as to whether the bright spot seen moving away from the sun was simply debris, or whether a small nucleus of the original ball of ice was still there. Regardless, it is likely that it is now only dust.  The comet was visible in instruments on NASA's Solar Terrestrial Relations Observatory, or STEREO, and the joint European Space Agency/NASA Solar and Heliospheric Observatory, or SOHO, via images called coronagraphs.Watch this video on the NASA Goddard YouTube channel.Credit:NASA/STEREO/ESA/SOHO/SDOGSFC || STEREO_A_Cor2_Still.jpg (1280x720) [494.6 KB] || STEREO_A_Cor2_Still_web.png (320x180) [67.2 KB] || ISON_Full_FINAL_1280x720.wmv (1280x720) [49.4 MB] || ISON_Full_FINAL_appletv.m4v (960x540) [46.4 MB] || ISON_Full_H264_1280x720_30.mov (1280x720) [43.1 MB] || ISON_Full_MPEG4_1280X720_29.97.mp4 (1280x720) [28.0 MB] || ISON_Full_FINAL_appletv.webmhd.webm (960x540) [16.6 MB] || ISON_Full_FINAL_ipod_lg.m4v (640x360) [17.5 MB] || ISON_Full_FINAL.mp4 (320x240) [8.3 MB] || ISON_Full_FINAL_ipod_sm.mp4 (320x240) [8.3 MB] || ISON_Full_ProRes_1280x720_29.97.mov (1280x720) [810.6 MB] || ISON_Full_H264_Best_1280x720_29.97.mov (1280x720) [517.2 MB] || ISON_Full_H264_Good_1280x720_29.97.mov (1280x720) [124.1 MB] || ISON_Full_FINAL_youtube_hq.mov (1280x720) [124.1 MB] || ",
            "hits": 51
        },
        {
            "id": 10869,
            "url": "https://svs.gsfc.nasa.gov/10869/",
            "result_type": "Produced Video",
            "release_date": "2012-01-10T11:00:00-05:00",
            "title": "NASA's RXTE Helps Pinpoint Launch of 'Bullets' in a Black Hole's Jet",
            "description": "Using observations from NASA's Rossi X-ray Timing Explorer (RXTE) satellite and the National Science Foundation's (NSF) Very Long Baseline Array (VLBA) radio telescope, an international team of astronomers has identified the moment when a black hole in our galaxy launched superfast knots of gas into space. Racing outward at about one-quarter the speed of light, these \"bullets\" of ionized gas are thought to arise from a region located just outside the black hole's event horizon, the point beyond which nothing can escape.The research centered on the mid-2009 outburst of a binary system known as H1743-322, located about 28,000 light-years away toward the constellation Scorpius. Discovered by NASA's HEAO-1 satellite in 1977, the system is composed of a normal star and a black hole of modest but unknown masses. Their orbit around each other is measured in days, which puts them so close together that the black hole pulls a continuous stream of matter from its stellar companion. The flowing gas forms a flattened accretion disk millions of miles across, several times wider than our sun, centered on the black hole. As matter swirls inward, it is compressed and heated to tens of millions of degrees, so hot that it emits X-rays.Some of the infalling matter becomes re-directed out of the accretion disk as dual, oppositely directed jets. Most of the time, the jets consist of a steady flow of particles. Occasionally, though, they morph into more powerful outflows that hurl massive gas blobs at significant fractions of the speed of light. || ",
            "hits": 66
        },
        {
            "id": 3572,
            "url": "https://svs.gsfc.nasa.gov/3572/",
            "result_type": "Visualization",
            "release_date": "2009-01-26T00:00:00-05:00",
            "title": "The Tycho Catalog Skymap - Version 2.0",
            "description": "This image set is a skymap of stars from the Tycho and Hipparcos star catalogs, provided by the ESO/ECF generic catalog server. The maps are plotted in plate carrée projection (Cylindrical-Equidistant) using celestial coordinates making them suitable for mapping onto spheres in many popular animation programs. The stars are plotted as gaussian point-spread functions (PSF) so the size and amplitude of the stars corresponds to their relative intensity. The stars are also elongated in Right Ascension (celestial longitude) based on declination (celestial latitude) so stars in the polar regions will still be round when projected on a sphere. Stars fainter than the threshold magnitude, usually selected as 5th magnitude, have their magnitude-intensity curve adjusted so they appear brighter than they really are. This makes the band of the Milky Way more visible. Stellar colors are assigned based on B and V magnitudes (B and V are stellar magnitudes measured through different filters). If Johnson B and V magnitudes are unavailable, Tycho B and V magnitudes are used instead. From these, an effective stellar temperature is derived using the algorithms described in Flower (ApJ 469, 355 1996). Corrections were noted from Siobahn Morgan (UNI). The effective temperature was then converted to CIE tristimulus X,Y,Z triples assuming a black-body emission distribution. The X,Y,Z values are then converted to red-green-blue color pixels. About 2.4 million stars are plotted, but many may be below the pixel intensity resolution. The three most conspicuously missing objects on these maps are the Andromeda galaxy (M31) and the two Magellanic Clouds. Changes from the first version #3442, The Tycho Catalog Skymap: The star generation algorithm now favors use of the Johnson magnitudes when available. This improves the star colors over the previous method. The star intensity profiles are also slightly modified to make the cores brighter with a faster intensity falloff. We have also set the color standard to SMPTE with a gamma of 1.8.Update: This skymap has been revised.  The newer version is available at Deep Star Maps. || ",
            "hits": 225
        },
        {
            "id": 3442,
            "url": "https://svs.gsfc.nasa.gov/3442/",
            "result_type": "Visualization",
            "release_date": "2007-08-20T00:00:00-04:00",
            "title": "The Tycho Catalog Skymap",
            "description": "This image set is a skymap of stars from the Tycho and Hipparcos star catalogs. The maps are plotted in plate carrée projection (Cylindrical-Equidistant) using celestial coordinates making them suitable for mapping onto spheres in many popular animation programs. The stars are plotted as gaussian point-spread functions (PSF) so the size and amplitude of the stars corresponds to their relative intensity. The stars are also elongated in Right Ascension (celestial longitude) based on declination (celestial latitude) so stars in the polar regions will still be round when projected on a sphere. Stars fainter than the threshold magnitude, usually selected as 5th magnitude, have their magnitude-intensity curve adjusted so they appear brighter than they really are. This makes the band of the Milky Way more visible. Stellar colors are assigned based on B and V magnitudes (B and V are stellar magnitudes measured through different filters). If Tycho B and V magnitudes are unavailable, Johnson B and V magnitudes are used instead. From these, an effective stellar temperature is derived using the algorithms described in Flower (ApJ 469, 355 1996). Corrections were noted from Siobahn Morgan (UNI). The effective temperature was then converted to CIE tristimulus X,Y,Z triples assuming a black-body emission distribution. The X,Y,Z values are then converted to red-green-blue color pixels. About 2.4 million stars are plotted, but many may be below the pixel intensity resolution. The three most conspicuously missing objects on these maps are the Andromeda galaxy (M31) and the two Magellanic Clouds. [The images in this visualization were updated August 28, 2007 to fix a bug in the star generation algorithm.]This skymap has been superseded by #3572, The Tycho Catalog Skymap - Version 2.0. || ",
            "hits": 161
        }
    ]
}