{
    "count": 11,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 4851,
            "url": "https://svs.gsfc.nasa.gov/4851/",
            "result_type": "Visualization",
            "release_date": "2020-09-09T13:15:00-04:00",
            "title": "Deep Star Maps 2020",
            "description": "The star map in celestial coordinates, at five different resolutions. The map is centered at 0h right ascension, and r.a. increases to the left. || starmap_2020_4k_print.jpg (1024x512) [41.8 KB] || starmap_2020_4k_searchweb.png (320x180) [53.9 KB] || starmap_2020_4k_thm.png (80x40) [5.5 KB] || starmap_2020_4k.exr (4096x2048) [34.3 MB] || starmap_2020_8k.exr (8192x4096) [124.5 MB] || starmap_2020_16k.exr (16384x8192) [422.9 MB] || starmap_2020_32k.exr (32768x16384) [1.4 GB] || starmap_2020_64k.exr (65536x32768) [3.8 GB] || ",
            "hits": 3381
        },
        {
            "id": 4451,
            "url": "https://svs.gsfc.nasa.gov/4451/",
            "result_type": "Visualization",
            "release_date": "2017-08-01T00:00:00-04:00",
            "title": "The Alternative Night Sky - Another Time - Another Place",
            "description": "A low-magnitude threshold version of the skymap. The threshold magnitude is 3.0 so the galactic disk is very faint.  Good for when you just want the brighter stars and have a wide field of view. || RandomizedSkymap.t3_04096x02048_print.jpg (1024x512) [157.4 KB] || RandomizedSkymap.t3_04096x02048_searchweb.png (320x180) [78.0 KB] || RandomizedSkymap.t3_04096x02048_thm.png (80x40) [4.1 KB] || RandomizedSkymap.t3_04096x02048.tif (4096x2048) [24.0 MB] || RandomizedSkymap.t3_08192x04096.tif (8192x4096) [96.0 MB] || ",
            "hits": 320
        },
        {
            "id": 3595,
            "url": "https://svs.gsfc.nasa.gov/3595/",
            "result_type": "Visualization",
            "release_date": "2009-07-27T00:00:00-04:00",
            "title": "Sentinels of the Heliosphere",
            "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point, a point between the Earth and the Sun where the gravitational pull is approximately equal. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageThis enhanced, narrated visualization was shown at the SIGGRAPH 2009 Computer Animation Festival in New Orleans, LA in August 2009; an eariler version created for AGU was called NASA's Heliophysics Observatories Study the Sun and Geospace. || ",
            "hits": 97
        },
        {
            "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": 208
        },
        {
            "id": 3569,
            "url": "https://svs.gsfc.nasa.gov/3569/",
            "result_type": "Visualization",
            "release_date": "2008-12-16T00:00:00-05:00",
            "title": "THEMIS Dayside Science - Sampling the Bow Shock",
            "description": "In the early part of the mission, the five THEMIS satellites follow the same orbit single-file. The apogee of the orbit takes the spacecraft just beyond the bow shock of Earth's magnetosphere. This enables the closely spaced satellites to measure the thickness of the different regions that they encounter. || ",
            "hits": 23
        },
        {
            "id": 3570,
            "url": "https://svs.gsfc.nasa.gov/3570/",
            "result_type": "Visualization",
            "release_date": "2008-12-15T00:00:00-05:00",
            "title": "NASA's Heliophysics Observatories Study the Sun and Geospace",
            "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point between the Sun and the Earth. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageA refined and narrated version of this visualization, Sentinels of the Heliosphere, is now available. || ",
            "hits": 79
        },
        {
            "id": 3525,
            "url": "https://svs.gsfc.nasa.gov/3525/",
            "result_type": "Visualization",
            "release_date": "2008-12-01T00:00:00-05:00",
            "title": "Two Posters of Earth with Sea Ice and Clouds over a Star Background",
            "description": "These very high resolution images show a global view of the Earth at different orientations with Arctic sea ice on December 8,2008 and September 15, 2008. The extent of the sea ice was determined by the AMSR-E sea ice concentration data. The terrain shows the average land cover for the related months over the continents. (See Blue Marble Next Generation) The global cloud cover shown was obtained from the original Blue Marble cloud data distributed in 2002. (See Blue Marble:Clouds) A matching star background is provided. || ",
            "hits": 44
        },
        {
            "id": 3539,
            "url": "https://svs.gsfc.nasa.gov/3539/",
            "result_type": "Visualization",
            "release_date": "2008-08-29T00:00:00-04:00",
            "title": "Blue Marble Next Generation Images from Terra/MODIS",
            "description": "The Blue Marble Next Generation (BMNG) data set provides a monthly global cloud-free true-color picture of the Earth's landcover at a 500-meter spatial resolution. This data set, shown on a globe, is derived from monthly data collected in 2004. The ocean color is derived from applying a depth shading to the bathymetry data. The Antarctica coverage snown is the Landsat Image Mosaic of Antarctica. Behind the Earth is a skymap from the Tycho and Hipparcos star catalogs. This skymap is 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. || ",
            "hits": 180
        },
        {
            "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": 155
        },
        {
            "id": 3402,
            "url": "https://svs.gsfc.nasa.gov/3402/",
            "result_type": "Visualization",
            "release_date": "2007-02-15T00:00:00-05:00",
            "title": "Global View of the Arctic and Antarctic on September 21, 2005",
            "description": "In support of International Polar Year, this matching pair of images showing a global view of the Arctic and Antarctic were generated in poster-size resolution. Both images show the sea ice on September 21, 2005, the date at which the sea ice was at its minimum extent in the northern hemisphere. The color of the sea ice is derived from the AMSR-E 89 GHz brightness temperature while the extent of the sea ice was determined by the AMSR-E sea ice concentration. Over the continents, the terrain shows the average land cover for September, 2004. (See Blue Marble Next Generation) The global cloud cover shown was obtained from the original Blue Marble cloud data distributed in 2002. (See Blue Marble:Clouds) A matching star background is provided for each view. All images include transparency, allowing them to be composited on a background. || ",
            "hits": 88
        },
        {
            "id": 3379,
            "url": "https://svs.gsfc.nasa.gov/3379/",
            "result_type": "Visualization",
            "release_date": "2006-10-23T00:00:00-04:00",
            "title": "Arrange for Change Poster",
            "description": "As part of the Earth to Sky project, this graphic is being used by the National Park Service (NPS) as a 7.5 X 9.8 foot traveling exhibition booth. Earth to Sky is a partnership between NASA and NPS that gives NASA content to NPS interpreters to help park visitors connect with the natural and cultural heritage of the U.S. The 'Arrange for Change' theme, provides information about the climate change and its consequences for National Parks. The  'Blue Marble' Earth image and star field provided by the Scientific Visualization Studio are used to evoke the emotional connection that this is the only planet we can call home. || ",
            "hits": 39
        }
    ]
}