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It provides a clear representation of the flow of blood and bile within the lobule, facilitating a better understanding of liver physiology and pathology.\n\nFor medical education, anatomical studies, healthcare presentations, pharmaceutical research, liver function analysis, hepatology training, biological sciences, medical illustrations, healthcare technology, and academic projects.\n\nAnatomy of Liver Lobule is a high quality, photo real 3d model that will enhance detail and realism to any of your rendering projects. The model has a fully textured, detailed design that allows for close-up renders, and was originally modeled in 3ds Max and rendered with V-Ray. Renders have no postprocessing!\n\nHope you like it!\n\n\nFeatures:\n- High quality polygonal model, has real dimensions. Easy to merge into your scene.\n- Units: cm\n- The model was created with the optimal number of polygons. (The Meshsmooth modifier is assigned to the original mesh. 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The colors and design illustrate the liver\u0026#39;s complex anatomy, making it an exceptional educational tool for understanding liver function and structure.\n\nFor medical education, anatomical studies, healthcare training, biology research, liver function analysis, hepatology, liver disease awareness, educational displays, academic presentations, teaching resources, medical institutions, healthcare professionals, anatomy courses, liver surgery planning, and scientific exhibitions.\n\nLiver Lobule Anatomy Model with Vascular Structure on Stand is a high quality, photo real 3d model that will enhance detail and realism to any of your rendering projects. The model has a fully textured, detailed design that allows for close-up renders, and was originally modeled in 3ds Max and rendered with V-Ray. Renders have no postprocessing!\n\nHope you like it!\n\n\nFeatures:\n- High quality polygonal model, has real dimensions. 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It is designed to highlight the intricate organization of the respiratory system, making it a valuable tool for educational, medical, and artistic applications.\n\nKey features:\n\n- Detailed anatomy includes terminal bronchioles, respiratory bronchioles, alveolar ducts, alveolar sacs, and surrounding capillary networks for a comprehensive view of the gas exchange process.\n- Lobular structure accurately models the lobule’s subdivisions, including the interlobular septa and accompanying connective tissue.\n- Functional focus demonstrates the relationship between airways, blood vessels, and alveoli, essential for understanding respiratory physiology.\n\nApplications:\n\n- Medical education for teaching the microanatomy and function of the respiratory system.\n- Respiratory research useful for studying diseases such as COPD, asthma, or interstitial lung diseases.\n- Artistic and design uses provide a reference for creating medically accurate visualizations and 3D artwork.\n\nThe model is optimized for 3D printing and is available in standard file formats like STL and OBJ, ensuring compatibility with various 3D software and printing systems. This pulmonary lobule model is a versatile and reliable resource for educators, researchers, and designers.","imageAlt":"3D Model of Pulmonary Lobule","url":"https://www.cgtrader.com/3d-print-models/science/biology/3d-model-of-pulmonary-lobule","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/kwiSwy7cSnko6L4N3e1GxRbj/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/1.jpg","gridUrl":"https://media.cgtrader.com/variants/kwiSwy7cSnko6L4N3e1GxRbj/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/1.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-print-models/science/biology/3d-model-of-pulmonary-lobule","isCgtVerified":false,"types":{"printReady":true,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":5,"name":".fbx","is_native":false},{"id":21,"name":".blend","is_native":false},{"id":117,"name":".gltf","is_native":false},{"id":12,"name":".obj","is_native":false},{"id":189,"name":".ply","is_native":false},{"id":51,"name":".stl","is_native":false}],"categorySlug":"science","subcategorySlug":"biology","categoryTitle":"Science","subcategoryTitle":"Biology","schemaImageUrl":"https://img-new.cgtrader.com/items/5794786/dd135b3103/3d-model-of-pulmonary-lobule-3d-model-dd135b3103.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"premium"}},{"id":"4713659","type":"listingItem","attributes":{"id":4713659,"title":"duct sites and diseases","price":79.0,"description":"The blend file demonstrates the ducts anatomy with different parts and its disease. The model has image packed into the blend file. good model for medical school, colleges and biology.\nThe formats 3mf, ply, obj, fbx, USDZ,GLTZ \u0026 GLB with applied uv mapped textures have also been included in the downloads along with stl.\n\nI have included the various formats needed by various customer for the various 3d modelling softwares they may be using. \nThe following formats are compressed in rar formats :-\n1.\tblend\n2.\t3mf\n3.\tstl\n4.\tobj\n5.\tfbx\n6.\tglb\n7.\tgltz\n8.\tusdz\nThe downloaded files have to unpacked using any rar unpacker. After unpacking, the folder content of the respective formats will be as follows :-.\n1.\tblend :- single file with all applied and packed textures.\n2.\t3mf :- single file with all applied and packed textures.\n3.\tstl :- single file with only geometry data\n4.\tobj :- mutiple files including .obj,.mtl, images textures.\n5.\tfbx :- single file with all applied and packed textures.\n6.\tglb :- single file with all applied and packed textures.\n7.\tgltz :- mutiple files including .bin, images textures.\n8.\tusdz :- single file \n\nThe native file is blend so the open source software blender opens mostly all the files, with textures (packed with the files). The best way is to open the files named blend with blender. Other files have to be imported in blender by clicking within blender \"File \u003e\u003eImport\u003e\u003eselect the type of file you want to import\u003e\u003eopen file location of the downloaded unzipped files\u003e\u003eselect the file\u003e\u003ethe model would open in the 3d viewport of the software.\nThe other files including blender can be opened with most of the free and paid 3d modelling software. The files obj \u0026 fbx are compatible with other 3d modeling software, example maya. These software's have the open/import options similar to blender. The files stl and 3mf are compatible with 3d printing software's. The built in \"3d builder \" windows software opens all of these files including glb, \u0026 gltz. In case you don't have 3d builder installed just download it free from Microsoft store for free. \nFor 3d builder 3mf, fbx, stl, glb are standalone files (right click the model file\u003e\u003eselect open with\u003e\u003e3d builder). For obj,ply, \u0026 gltz 3d builder will prompt you to select the model files .mtl and image textures (these are packed in the rar files).\nThe textures files have been separately supplied additionally; in case one needs them.","imageAlt":"duct sites and diseases","url":"https://www.cgtrader.com/3d-models/science/medical/duct-sites-and-diseases","isCLDApplicable":false,"isSaleOffApplicable":true,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/YX9RfeLZf1nBz7kW6zCVvLsb/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/0001.jpg","gridUrl":"https://media.cgtrader.com/variants/YX9RfeLZf1nBz7kW6zCVvLsb/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/0001.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/science/medical/duct-sites-and-diseases","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":21,"name":".blend","is_native":true},{"id":127,"name":".usdz","is_native":false},{"id":117,"name":".gltf","is_native":false},{"id":189,"name":".ply","is_native":false},{"id":null,"name":null,"is_native":false},{"id":51,"name":".stl","is_native":false},{"id":5,"name":".fbx","is_native":false},{"id":12,"name":".obj","is_native":false},{"id":129,"name":".3mf","is_native":false}],"categorySlug":"science","subcategorySlug":"medical","categoryTitle":"Science","subcategoryTitle":"Medical","schemaImageUrl":"https://img-new.cgtrader.com/items/4713659/f178eb4c3e/duct-sites-and-diseases-3d-model-f178eb4c3e.webp","saleOffDiscount":30,"eligibleForSubscription":false,"subscriptionSubscribed":false,"subscriptionPotential":false,"subscriptionTierBand":null}},{"id":"6810678","type":"listingItem","attributes":{"id":6810678,"title":"Hepatitis  liver disease digestive system organs","price":29.0,"description":"This model is an accurate representation of Liver.\nThis model contains 1 separate object.\nThis model contains 102504 polygons and 102506 vertices .\nTextures Resolution 4096 x 4096 pixels. There are diffuse, roughness and normal map included (PBR workflow).\nAll textures are created from original photographs or drawings.","imageAlt":"3D Hepatitis liver disease digestive system organs","url":"https://www.cgtrader.com/3d-models/science/medical/cirrhosis-liver-disease-digestive-system-organs","isCLDApplicable":false,"isSaleOffApplicable":true,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/cnsub4azuvvtzpcb90e3kb7vx2b6/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/gan_00.jpg","gridUrl":"https://media.cgtrader.com/variants/cnsub4azuvvtzpcb90e3kb7vx2b6/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/gan_00.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/science/medical/cirrhosis-liver-disease-digestive-system-organs","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":true,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":215,"name":".png","is_native":false},{"id":5,"name":".fbx","is_native":false},{"id":12,"name":".obj","is_native":false}],"categorySlug":"science","subcategorySlug":"medical","categoryTitle":"Science","subcategoryTitle":"Medical","schemaImageUrl":"https://img-new.cgtrader.com/items/6810678/2448a4c69c/hepatitis-liver-disease-digestive-system-organs-3d-model-2448a4c69c.webp","saleOffDiscount":50,"eligibleForSubscription":true,"subscriptionSubscribed":false,"subscriptionPotential":true,"subscriptionTierBand":"premium"}},{"id":"6810572","type":"listingItem","attributes":{"id":6810572,"title":"Healthy liver digestive system organs","price":29.0,"description":"This model is an accurate representation of Liver.\nThis model contains 1 separate object.\nThis model contains 102504 polygons and 102506 vertices .\nTextures Resolution 2048 x 2048 pixels. There are diffuse, roughness and normal map included (PBR workflow).\nAll textures are created from original photographs or drawings.","imageAlt":"3D model Healthy liver digestive system organs","url":"https://www.cgtrader.com/3d-models/science/medical/healthy-liver-digestive-system-organs","isCLDApplicable":false,"isSaleOffApplicable":true,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/7gp9lk2v93essa1o53juk6790dh4/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/healthy-liver-digestive-system-organs-3d-model-99b9038d08.jpg","gridUrl":"https://media.cgtrader.com/variants/7gp9lk2v93essa1o53juk6790dh4/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/healthy-liver-digestive-system-organs-3d-model-99b9038d08.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/science/medical/healthy-liver-digestive-system-organs","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":true,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":216,"name":".jpg","is_native":false},{"id":17,"name":".max","is_native":false},{"id":5,"name":".fbx","is_native":false},{"id":12,"name":".obj","is_native":false},{"id":11,"name":".ma","is_native":false}],"categorySlug":"science","subcategorySlug":"medical","categoryTitle":"Science","subcategoryTitle":"Medical","schemaImageUrl":"https://img-new.cgtrader.com/items/6810572/99b9038d08/healthy-liver-digestive-system-organs-3d-model-99b9038d08.webp","saleOffDiscount":50,"eligibleForSubscription":true,"subscriptionSubscribed":false,"subscriptionPotential":true,"subscriptionTierBand":"premium"}},{"id":"979901","type":"listingItem","attributes":{"id":979901,"title":"hepatic liver lobule","price":39.0,"description":"The formats 3mf, obj, fbx, USDZ,GLTZ \u0026 GLB with applied uv mapped textures have also been included in the downloads along with ply \u0026 stl.\nThis a model of hepatic lobule depicting the structure of the blood vessels and bile duct along with the flow of fluid within a lobule. The structure has been labelled with texts on the view port itself. The materials are based on cycles render. I have used the array modifier, curve modifier along with empties to design the structures. In the .blend file most of the modifiers have not been applied to leave space for further modification by the designers downloading the model. Rest of the extensions (OBJ,FBX,3DS, DAE) have been exported from blender after applying modifiers\nThe blend file has 2 layers\nFirst layer :- a complete lobule\nSecond layer :- 1/6 part of a lobule\nThe short forms in outliner stand for:-\nBC :- Bezeir curve\nCyto :- mesh/ material of cytoplasm\nNuc:- mesh/ material of nucleus\nSecond layer :-\nEach structural unit has 2 meshes and a Bezier curve :- cyto (mesh), nucleus (mesh), BC (Bezier curve)\n1.\tPortal vein:-\na.\tportal v cyto\nb.\tportal v nuc\nc.\tBC portal v\n2.\tPortal branch 1\na.\tportal br 1 cyto\nb.\tportal br 1 nucleus\nc.\tBC portal br 1\n3.\tPortal branch 2\na.\tportal br2cyto\nb.\tportal br2 nucleus\nc.\tBC portal br 2\n4.\tPortal branch 3\na.\tportal br3cyto\nb.\tportal br3 nucleus\nc.\tBC portal br 3\n5.\tLobule vein \na.\tlobule v cyto\nb.\tlobule v nuc\nc.\tBC lobule v hep\n6.\tCentral vein\na.\tCentral  vcyto\nb.\tCentral  vnuc\nc.\tBC Central vein\n7.\tHepatocytes around lobule vein\na.\tlobule hep v cyto\nb.\tlobule hep v nuc\nc.\tBC lobule hep v\n8.\tHepatic artery\na.\thep art cyto\nb.\thep art nuc\nc.\tBC hepatic art\n9.\tHepatic artery br 1\na.\tHepatic art br 1 cyto\nb.\tHepatic art br 1 nuc\nc.\tBC hepatic art br 1\n10.\tHepatic artery br 2\na.\tHepatic art br2cyto\nb.\tHepatic art br2nuc\nc.\tBC hepatic art br2\n11.\tLobule artery\na.\tlobule art cyto\nb.\tlobule art nuc\nc.\tBC lobule art \n12.\tHepatocytes around lobule artery\na.\tlobule hep artcyto\nb.\tlobule hep artnuc\nc.\tBC lobule arthep\n13.\tBile duct\na.\tBile duct cyto\nb.\tBile duct nuc\nc.\tBC bile duct\n14.\tLobule bile duct\na.\tLobule bile duct cyto\nb.\tLobule bile duct nuv\nc.\tBC lobule bile duct\n15.\tArrow labels for flow\na.\tArrow bile duct \nb.\tArrow central vein \nc.\tArrow hep art \nd.\tArrow junction vein art \ne.\tArrow junction vein art label\nf.\t Arrow portal vein\n\nFirst layer :-\n\tHas similar nomenclature in outliner but with extension in name as for example\n1.\tPortal vein:-\na.\tportal v cyto (.001,.002,.003,.004,.005,.006)\nb.\tportal v nuc (.001,.002,.003,.004,.005,.006)\nc.\tBC portal v (.001,.002,.003,.004,.005,.006)\n\nThe formats 3mf, ply, obj, fbx, USDZ,GLTZ \u0026 GLB with applied uv mapped textures have also been included in the downloads along with  stl.\n\nI have included the various formats needed by various customer for the various 3d modelling softwares they may be using. \nThe following formats are compressed in rar formats :-\n1.\tblend\n2.\t3mf\n3.\tstl\n4.\tobj\n5.\tfbx\n6.\tglb\n7.\tgltz\n8.\tusdz\nThe downloaded files have to unpacked using any rar unpacker. After unpacking, the folder content of the respective formats will be as follows :-.\n1.\tblend :- single file with all applied and packed textures.\n2.\t3mf :- single file with all applied and packed textures.\n3.\tstl :- single file with only geometry data\n4.\tobj :- mutiple files including .obj,.mtl, images textures.\n5.\tfbx :- single file with all applied and packed textures.\n6.\tglb :- single file with all applied and packed textures.\n7.\tgltz :- mutiple files including .bin, images textures.\n8.\tusdz :- single file \n\nThe native file is blend so the open source software blender opens mostly all the files, with textures (packed with the files). The best way is to open the files named blend with blender. Other files have to be imported in blender by clicking within blender \"File \u003e\u003eImport\u003e\u003eselect the type of file you want to import\u003e\u003eopen file location of the downloaded unzipped files\u003e\u003eselect the file\u003e\u003ethe model would open in the 3d viewport of the software.\nThe other files including blender can be opened with most of the free and paid 3d modelling software. The files obj \u0026 fbx are compatible with other 3d modeling software, example maya. These software's have the open/import options similar to blender. The files stl and 3mf are compatible with 3d printing software's. The built in \"3d builder \" windows software opens all of these files including glb, \u0026 gltz. In case you don't have 3d builder installed just download it free from Microsoft store for free. \nFor 3d builder 3mf, fbx, stl, glb are standalone files (right click the model file\u003e\u003eselect open with\u003e\u003e3d builder). For obj,ply, \u0026 gltz 3d builder will prompt you to select the model files .mtl and image textures (these are packed in the rar files).\nThe textures files have been separately supplied additionally; in case one needs them.\n\n","imageAlt":"hepatic liver lobule 3D","url":"https://www.cgtrader.com/3d-models/science/medical/hepatic-liver-lobule","isCLDApplicable":false,"isSaleOffApplicable":true,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/cjC6dSALPL4GEZ6AvNZab93P/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/hepatic-liver-lobule-3d-model-blend.jpg","gridUrl":"https://media.cgtrader.com/variants/cjC6dSALPL4GEZ6AvNZab93P/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/hepatic-liver-lobule-3d-model-blend.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/science/medical/hepatic-liver-lobule","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":21,"name":".blend","is_native":true},{"id":117,"name":".gltf","is_native":false},{"id":127,"name":".usdz","is_native":false},{"id":12,"name":".obj","is_native":false},{"id":5,"name":".fbx","is_native":false},{"id":129,"name":".3mf","is_native":false},{"id":51,"name":".stl","is_native":false}],"categorySlug":"science","subcategorySlug":"medical","categoryTitle":"Science","subcategoryTitle":"Medical","schemaImageUrl":"https://img-new.cgtrader.com/items/979901/2d35411dd5/hepatic-liver-lobule-3d-model-2d35411dd5.webp","saleOffDiscount":30,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"premium"}},{"id":"2874957","type":"listingItem","attributes":{"id":2874957,"title":"Liver lobule histology","price":29.0,"description":"A blend model of liver depicting its microscopic details as well as its direction of blood and bile flow along with its anatomical lobule, portal triad, bile duct and fibrous boundries.\nThe formats 3mf, ply, obj, fbx, USDZ,GLTZ \u0026 GLB with applied uv mapped textures have also been included in the downloads along with  stl.\n\nI have included the various formats needed by various customer for the various 3d modelling softwares they may be using. \nThe following formats are compressed in rar formats :-\n1.\tblend\n2.\t3mf\n3.\tstl\n4.\tobj\n\n6.\tglb\n7.\tgltz\n8.\tusdz\nThe downloaded files have to unpacked using any rar unpacker. After unpacking, the folder content of the respective formats will be as follows :-.\n1.\tblend :- single file with all applied and packed textures.\n2.\t3mf :- single file with all applied and packed textures.\n3.\tstl :- single file with only geometry data\n4.\tobj :- mutiple files including .obj,.mtl, images textures.\n\n6.\tglb :- single file with all applied and packed textures.\n7.\tgltz :- mutiple files including .bin, images textures.\n8.\tusdz :- single file \n\nThe native file is blend so the open source software blender opens mostly all the files, with textures (packed with the files). The best way is to open the files named blend with blender. Other files have to be imported in blender by clicking within blender \"File \u003e\u003eImport\u003e\u003eselect the type of file you want to import\u003e\u003eopen file location of the downloaded unzipped files\u003e\u003eselect the file\u003e\u003ethe model would open in the 3d viewport of the software.\nThe other files including blender can be opened with most of the free and paid 3d modelling software. The files obj \u0026 fbx are compatible with other 3d modeling software, example maya. These software's have the open/import options similar to blender. The files stl and 3mf are compatible with 3d printing software's. The built in \"3d builder \" windows software opens all of these files including glb, \u0026 gltz. In case you don't have 3d builder installed just download it free from Microsoft store for free. \nFor 3d builder 3mf, fbx, stl, glb are standalone files (right click the model file\u003e\u003eselect open with\u003e\u003e3d builder). For obj,ply, \u0026 gltz 3d builder will prompt you to select the model files .mtl and image textures (these are packed in the rar files).\nThe textures files have been separately supplied additionally; in case one needs them.\n\n\n","imageAlt":"3D model Liver lobule histology","url":"https://www.cgtrader.com/3d-models/science/medical/liver-lobule-histology","isCLDApplicable":false,"isSaleOffApplicable":true,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/vaAScw37q1KdnVpFcxFWpQpG/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/0001.jpg","gridUrl":"https://media.cgtrader.com/variants/vaAScw37q1KdnVpFcxFWpQpG/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/0001.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/science/medical/liver-lobule-histology","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":21,"name":".blend","is_native":true},{"id":127,"name":".usdz","is_native":false},{"id":189,"name":".ply","is_native":false},{"id":117,"name":".gltf","is_native":false},{"id":51,"name":".stl","is_native":false},{"id":12,"name":".obj","is_native":false},{"id":129,"name":".3mf","is_native":false}],"categorySlug":"science","subcategorySlug":"medical","categoryTitle":"Science","subcategoryTitle":"Medical","schemaImageUrl":"https://img-new.cgtrader.com/items/2874957/da1ba35b26/liver-lobule-histology-3d-model-da1ba35b26.webp","saleOffDiscount":30,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"premium"}},{"id":"5005684","type":"listingItem","attributes":{"id":5005684,"title":"Liver histology anatomy labelled","price":23.0,"description":"A blend model of liver depicting its microscopic details as well as its direction of blood and bile flow along with its anatomical lobule, functional lobule , portal triad, bile duct and fibrous boundries.\n\nThe formats 3mf, ply, obj, fbx, USDZ,GLTZ \u0026 GLB with applied uv mapped textures have also been included in the downloads along with  stl.\n\n\n\nI have included the various formats needed by various customer for the various 3d modelling softwares they may be using. \n\nThe following formats are compressed in rar formats :-\n\n1.    blend\n\n2.    3mf\n\n3.    stl\n\n4.    obj\n\n5.    fbx\n\n6.    glb\n\n7.    gltz\n\n8.    usdz\n\nThe downloaded files have to unpacked using any rar unpacker. After unpacking, the folder content of the respective formats will be as follows :-.\n\n1.    blend :- single file with all applied and packed textures.\n\n2.    3mf :- single file with all applied and packed textures.\n\n3.    stl :- single file with only geometry data\n\n4.    obj :- mutiple files including .obj,.mtl, images textures.\n\n5.    fbx :- single file with all applied and packed textures.\n\n6.    glb :- single file with all applied and packed textures.\n\n7.    gltz :- mutiple files including .bin, images textures.\n\n8.    usdz :- single file \n\n\n\nThe native file is blend so the open source software blender opens mostly all the files, with textures (packed with the files). The best way is to open the files named blend with blender. 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THE MODELS ARE  OF A SIMILAR  SCALE  AND STYLE AND POSED WITH AN EXPRESSIVE LOOK ON THE FACE TO ADD BOTH CHARACTER AND EMOTION TO EACH MODEL.\n\n\n ALL FILES ARE CLEAN AND READY TO GO, ALL OF THE MESH'S HAVE BEEN RUN THROUGH MESHMIXERS 'ANALYSIS/INSPECTOR'  TOOLS TO FIX ANY BAD TOPOLOGY AFTER SCULPTING (NON-MANIFOLD); AND ALL OF THE OBJ/STL FILES WERE GENERATED WITHIN MESHMIXER.\n    \n          1.    THE MODELS ARE IN BOTH STL \u0026 OBJ FORMATS\n\n\t2. EACH  MODEL SIZE IS 150MM TALL AS STANDARD, THIS CAN OBVIOUSLY BE RE-SCALED IN YOUR OWN SLICER SOFTWARE TO YOUR OWN PREFERENCES.\n\t\n\t3. THE MODELS ARE IDEAL FOR PEOPLE WITH HD RESIN PRINTERS, BUT EXCELLENT DETAILED RESULTS CAN ALSO BE ACHIEVED WITH FDM PRINTERS IF THE MODELS ARE PRINTED IN A LARGER SCALE  SO THE DETAILS OF THE MODELS CAN STILL BE CAPTURED WITHIN THE SLICING SOFTWARE.\n\t\n\t4. 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The Bootes Void is like a boot or sock. In astronomy, Bootes Void are isolated and relatively small dark nebulae containing dense cosmic dust and gas from which star formation may take place. Bootes Void are found within H II regions, and typically have a mass of about two to 50 solar masses contained within a region about a light year or so across (about 4.5×1047 m3). They contain molecular hydrogen (H2), carbon oxides and helium, and around 1% (by mass) silicate dust. Bok globules most commonly result in the formation of double- or multiple-star systems. An analysis of near-infrared observations published in 1990 confirmed that stars were being born inside Bootes Void. Further observations have revealed that some Bok globules contain embedded warm sources, some contain Herbig–Haro objects, and some show outflows of molecular gas. Millimeter-wave emission line studies have provided evidence for the infall of material onto an accreting protostar. 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For the psychologist, see Star Vega (psychologist). For other uses, see Vega (disambiguation). Vega is the brightest star in the northern constellation of Lyra. It has the Bayer designation α Lyrae, which is Latinised to Alpha Lyrae and abbreviated Alpha Lyr or α Lyr. This star is relatively close at only 25 light-years (7.7 parsecs) from the Sun, and one of the most luminous stars in the Sun's neighborhood. It is the fifth-brightest star in the night sky, and the second-brightest star in the northern celestial hemisphere, after Arcturus. Vega has been extensively studied by astronomers, leading it to be termed arguably the next most important star in the sky after the Sun. Vega was the northern pole star around 12,000 BCE and will be so again around the year 13,727, when its declination will be +86° 14′. Vega was the first star other than the Sun to have its image and spectrum photographed. It was one of the first stars whose distance was estimated through parallax measurements. Vega has functioned as the baseline for calibrating the photometric brightness scale and was one of the stars used to define the zero point for the UBV photometric system. Vega is only about a tenth of the age of the Sun, but since it is 2.1 times as massive, its expected lifetime is also one tenth of that of the Sun; both stars are at present approaching the midpoint of their main sequence lifetimes. Compared with the Sun, Vega has a lower abundance of elements heavier than helium. Vega is also a variable star—that is, a star whose brightness fluctuates. It is rotating rapidly with a speed of 236 km/s at the equator. This causes the equator to bulge outward due to centrifugal effects, and, as a result, there is a variation of temperature across the star's photosphere that reaches a maximum at the poles. From Earth, Vega is observed from the direction of one of these poles. Based on observations of more infrared radiation than expected, Vega appears to have a circumstellar disk of dust. This dust is likely to be the result of collisions between objects in an orbiting debris disk, which is analogous to the Kuiper belt in the Solar System. Stars that display an infrared excess due to dust emission are termed Vega-like stars. 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The Giant GRB Ring is like a rock or cloud. The Giant GRB Ring is a ring of 9 gamma-ray bursts (GRBs) that may be associated with one of the largest known cosmic structures. It was discovered in July 2015 by a team of Hungarian and American astronomers led by L.G. Balazs while analyzing data from different gamma-ray and X-ray telescopes, in particular the Swift Spacecraft. The ring of GRBs lies at a distance of about 2.8 gigaparsecs (9.1 billion light years) from Earth at the redshift between 0.78 and 0.86 and measures about 1.72 gigaparsecs (5.6 billion light years) in diameter, making it one of the largest structures known. Typically, the distribution of GRBs in the universe appears in the sets of less than the 2σ distribution, or with fewer than two GRBs in the average data of the point-radius system. Thus, such a concentration as this appears extremely unlikely, given accepted theoretical models. Proposals include the existence of a giant supergalactic structure. This would be an extremely huge structure of the universe, with a mean size of about 5.6 billion light years. Such a supercluster can explain the significant distribution of GRBs because of its tie to star formation. If such a structure did exist, it would be one of the largest structures of the observable universe.\n\nTexture Resolution: 1102 x 1102","imageAlt":"Giant GRB Ring 3D","url":"https://www.cgtrader.com/3d-models/space/other/giant-grb-ring","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/hU9UPvVw9nGvxHcu9KHMdVM8/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/giant%20GRB%20ring.jpg","gridUrl":"https://media.cgtrader.com/variants/hU9UPvVw9nGvxHcu9KHMdVM8/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/giant%20GRB%20ring.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/giant-grb-ring","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5801879/f624576d4a/giant-grb-ring-3d-model-f624576d4a.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5819160","type":"listingItem","attributes":{"id":5819160,"title":"Boss Great Wall","price":3.0,"description":"Description\nDescription\n\nThe Boss Great Wall. The Boss Great Wall is like a spider web. The Boss Great Wall contains nebulas, including saturn nebula, hourglass nebula, cat eye nebula, stingray nebula, eskimo nebula, ring nebula, dumbbell nebula, twin-jet nebula, shrimp nebula, red spider nebula and etc. The Boss Great Wall also includes galaxies. The BOSS Great Wall is a supercluster complex that was identified, using the Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey (SDSS), in early 2016. It was discovered by a research team from several institutions, consisting of: Heidi Lietzen, Elmo Tempel, Lauri Juhan Liivamägi, Antonio Montero-Dorta, Maret Einasto, Alina Streblyanska, Claudia Maraston, Jose Alberto Rubiño-Martín and Enn Saar. The BOSS Great Wall is one of the largest superstructures in the observable universe, though there are even larger structures known. The large complex has a mean redshift of z ~ 0.47 (z times Hubble length ≈ 6.8 billion light years). It consists of two elongated superclusters, two large superclusters, and several smaller superclusters as well. The elongated superclusters form galaxy walls, with the larger of the two having a diameter of 186/h Mpc (supercluster A in the figure); the second wall's being 173/h Mpc (supercluster B). The other two main superclusters are moderately large, having diameters of 91/h Mpc and 64/h Mpc (superclusters D and C, respectively). The superstructure is roughly 1 billion light years in diameter, and has a total mass approximately 10,000 times the Milky Way galaxy. It contains at least 830 visible galaxies (represented in the figure within their respective superclusters), as well as many others that are not visible (dark galaxies). The researchers used Minkowski functionals to verify the structure's overall shape and size; the first three quantifying the thickness, width, and length followed by the fourth determining the structure's overall curvature. The research team compared the luminosities and stellar masses within the superstructure to known high stellar mass galaxies within the SDSS's 7th data release, DR7. This allowed the team to scale the data using known values, from local superclusters, to determine the overall morphology of the BOSS Great Wall. It is currently debated amongst astronomers if the BOSS Great Wall may be considered a structure, due to the intricacies of its shape and overall size. The question of whether the supercluster complex is moving together or being slowly separated by the expanding universe is a key factor to this discussion. Nevertheless, when compared to several other chain structures, such as the Sloan Great Wall, the BOSS Great Wall's superclusters are far richer, containing more dense, high stellar mass galaxies. The BOSS Great Wall's discovery, and the data gained therein, should prove very beneficial for astronomers who study the overall structure of the cosmic web.\n\nTexture Resolution: 736 x 915","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/boss-great-wall-90b806b7-8c8e-4c4f-8628-896ac03518dc","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/kD2yZ8QTWn3Tq8JW1XVoVzvj/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/boss%20great%20wall-2.jpg","gridUrl":"https://media.cgtrader.com/variants/kD2yZ8QTWn3Tq8JW1XVoVzvj/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/boss%20great%20wall-2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/boss-great-wall-90b806b7-8c8e-4c4f-8628-896ac03518dc","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5819160/c93b8fb9c1/boss-great-wall-3d-model-c93b8fb9c1.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5971725","type":"listingItem","attributes":{"id":5971725,"title":"GRB 090423","price":3.0,"description":"Description\nGRB 090423. This GRB 090423 is like a comet that's passing through the supernova explosion. GRB 090423 was a gamma-ray burst (GRB) detected by the Swift Gamma-Ray Burst Mission on April 23, 2009, at 07:55:19 UTC whose afterglow was detected in the infrared and enabled astronomers to determine that its redshift is z = 8.2, making it one of the most distant objects detected at that time with a spectroscopic redshift (GN-z11, discovered in 2016, has a redshift of 11). A gamma-ray burst is an extremely luminous event flash of gamma rays that occurs as the result of an explosion, and is thought to be associated with the formation of a black hole. The burst itself typically only lasts for a few seconds, but gamma-ray bursts frequently produce an \"afterglow\" at longer wavelengths that can be observed for many hours or even days after the burst. Measurements at these wavelengths, which include X-ray, ultraviolet, optical, infrared, and radio, enable follow-up study of the event. The finite speed of light means that GRB 090423 is also one of the earliest objects ever detected for which a spectroscopic redshift has been measured. The universe was only 630 million years old when the GRB occurred, and its detection confirms that massive stars were born and dying even very early on in the life of the universe. GRB 090423 and similar events provide a unique means of studying the early universe, as few other objects of that era are bright enough to be seen with today's telescopes. On April 23, 2009, at 07:55:19 UTC the Swift satellite detected a burst that lasted about 10 seconds and was located in the direction of the constellation Leo. Swift localized the field in which GRB 090423 occurred, and 77 seconds after the burst, the Swift UVOT Photometric System took a 150-second exposure of the field, but was unable to detect an optical or ultraviolet afterglow. A few minutes after its discovery, ground-based telescopes began observing the field. Within 20 minutes of the burst, Nial Tanvir and his team found an infrared source at the Swift position using the United Kingdom Infrared Telescope (UKIRT) on Mauna Kea, Hawaii. The initial observations taken by UKIRT were triggered autonomously via the eSTAR Project. They observed a drop off in flux beyond 1.13 micrometres with the VLT. Attributing this drop off to Lyman alpha absorption by neutral hydrogen in the intergalactic medium, they calculated a redshift of 8.2 for GRB 090423. The team of C.C. Thöne and Paolo D'Avanzo observed the afterglow of GRB 090423 using the Italian TNG 3.6m telescope located in the Canary Islands, Spain. They obtained two hours of spectra, which when combined, suggested a very weak signal at the position of the afterglow. They too saw a drop off in flux near 1.1 micrometres, and reported a redshift of 8.1 for GRB 090423, which is consistent, within error, of the redshift reported by Tanvir et al. The redshift of 8.1 suggest the burst may have lasted approximately 1.2 seconds in the local frame of the emitter, its duration being redshifted accordingly to the observed 10 seconds. The intergovernmental astronomy organisation, European Southern Observatory (ESO) operates the Very Large Telescope that obtained the spectrum reported by Tanvir et al. The GRB was not visible in Chile when Swift first detected the burst at 07:55 UTC, but was the following day at 03:00 UTC, which enabled the Gamma-Ray Burst Optical/Near-Infrared Detector (GROND) at La Silla Observatory to make observations of the burst, and find a photometric redshift consistent with the value reported elsewhere. The last observers to gather data during the event was the Combined Array for Research in Millimeter-wave Astronomy (CARMA) observatory. The observation of GRB 090423 by CARMA was taken at a frequency of 92.5 GHz. While the afterglow was not detected, they were able to place a 3-sigma upper limit of 0.7 mJy on the flux density of the afterglow.\n\nTexture Resolution: 1200 x 686","imageAlt":"GRB 090423 3D","url":"https://www.cgtrader.com/3d-models/space/other/grb-090423","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/jt3jsf4i6au5x2345rgq1eq5ef3m/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/grb%20090423.jpg","gridUrl":"https://media.cgtrader.com/variants/jt3jsf4i6au5x2345rgq1eq5ef3m/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/grb%20090423.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/grb-090423","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5971725/68cefe40d2/grb-090423-3d-model-68cefe40d2.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5806377","type":"listingItem","attributes":{"id":5806377,"title":"Giant Void","price":3.0,"description":"Description\n\nGiant Void. Giant Void is like a skull. The Giant Void (also known as the Giant Void in NGH, Canes Venatici Supervoid, and AR-Lp 36) is an extremely large region of space with an underdensity of galaxies and located in the constellation Canes Venatici. It is the second-largest-confirmed void to date, with an estimated diameter of 300 to 400 Mpc (1 to 1.3 billion light-years) and its centre is approximately 1.5 billion light-years away (z = 0.116). It was discovered in 1988 and was the largest void in the Northern Galactic Hemisphere, and possibly the second-largest ever detected. Even the hypothesized \"Eridanus Supervoid\" corresponding to the location of the WMAP cold spot is dwarfed by this void, although the Giant Void does not correspond to any significant cooling to the cosmic microwave background. Inside this vast void there are 17 galaxy clusters, concentrated in a spherically shaped region 50 Mpc in diameter. Studies of the motion of these clusters show that they have no interaction to each other, meaning the density of the clusters is very low resulting in weak gravitational interaction. The void's location in the sky is close to the Boötes Void. In a series of papers published between 2004 and 2006, cosmologist and theoretical physicist Laura Mersini-Houghton presented a theory that the universe arose from a multiverse, and made a series of testable predictions which included the existence of the Giant Void.\n\nTexture Resolution: 1360 x 1372","imageAlt":"3D model Giant Void","url":"https://www.cgtrader.com/3d-models/space/other/giant-void","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/KVjEEDFRoShCCRGhRtubFSUj/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/giant%20void.jpg","gridUrl":"https://media.cgtrader.com/variants/KVjEEDFRoShCCRGhRtubFSUj/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/giant%20void.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/giant-void","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5806377/ef94927ed6/giant-void-3d-model-ef94927ed6.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5806344","type":"listingItem","attributes":{"id":5806344,"title":"Southern Local Supervoid","price":3.0,"description":"Description\nDescription\n\nSouthern Local Supervoid. The Southern Local Supervoid is like a fish. The Southern Local Supervoid is a tremendously large, nearly empty region of space (a void). It lies next to the Local Supercluster, which contains our galaxy the Milky Way. Its center is 96 megaparsecs away and the void is 112 megaparsecs in diameter across its narrowest width. Its volume is very approximately 600 billion times that of the Milky Way. See volumes of similar orders of magnitude.\n\nTexture Resolution: 1103 x 1103","imageAlt":"Southern Local Supervoid 3D model","url":"https://www.cgtrader.com/3d-models/space/other/southern-local-supervoid","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/HfB7q5oby76zzLkhcu3wH7kG/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/southern%20local%20supervoid.jpg","gridUrl":"https://media.cgtrader.com/variants/HfB7q5oby76zzLkhcu3wH7kG/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/southern%20local%20supervoid.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/southern-local-supervoid","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5806344/ea2ad8232c/southern-local-supervoid-3d-model-ea2ad8232c.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"6719599","type":"listingItem","attributes":{"id":6719599,"title":"The Little Horse Doesnt Know How to Quit","price":5.0,"description":"Small in size yet unwavering in spirit, the model captures a moment of continuous motion—running not toward visible success, but away from surrender.\nBe resilient, even if the destination remains unseen.\nInspired by the little horse “Ma Xiao Ye”.\nThis 3D model is an original reinterpretation and not an official reproduction.","imageAlt":"3D print model The Little Horse Doesnt Know How to","url":"https://www.cgtrader.com/3d-print-models/art/other/the-little-horse-doesnt-know-how-to-quit","isCLDApplicable":false,"isSaleOffApplicable":true,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/4vu7ahith8eqxcj5ir0bofagbos9/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/z7378503513474_fea2923247788d5ac8e6d0c6b44aa327.jpg","gridUrl":"https://media.cgtrader.com/variants/4vu7ahith8eqxcj5ir0bofagbos9/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/z7378503513474_fea2923247788d5ac8e6d0c6b44aa327.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-print-models/art/other/the-little-horse-doesnt-know-how-to-quit","isCgtVerified":false,"types":{"printReady":true,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":51,"name":".stl","is_native":false}],"categorySlug":"art","subcategorySlug":"other","categoryTitle":"Art \u0026 Design","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/6719599/c872502c56/the-little-horse-doesnt-know-how-to-quit-3d-model-c872502c56.webp","saleOffDiscount":50,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5806410","type":"listingItem","attributes":{"id":5806410,"title":"Giant Void","price":3.0,"description":"Description\nDescription\n\nGiant Void. Giant Void is like a circle or teleportation portal. The Giant Void (also known as the Giant Void in NGH, Canes Venatici Supervoid, and AR-Lp 36) is an extremely large region of space with an underdensity of galaxies and located in the constellation Canes Venatici. It is the second-largest-confirmed void to date, with an estimated diameter of 300 to 400 Mpc (1 to 1.3 billion light-years) and its centre is approximately 1.5 billion light-years away (z = 0.116). It was discovered in 1988 and was the largest void in the Northern Galactic Hemisphere, and possibly the second-largest ever detected. Even the hypothesized Eridanus Supervoid corresponding to the location of the WMAP cold spot is dwarfed by this void, although the Giant Void does not correspond to any significant cooling to the cosmic microwave background. Inside this vast void there are 17 galaxy clusters, concentrated in a spherically shaped region 50 Mpc in diameter. Studies of the motion of these clusters show that they have no interaction to each other, meaning the density of the clusters is very low resulting in weak gravitational interaction. The void's location in the sky is close to the Boötes Void. 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The Bok Globules is like a boot or sock. In astronomy, Bok globules are isolated and relatively small dark nebulae containing dense cosmic dust and gas from which star formation may take place. Bok globules are found within H II regions, and typically have a mass of about two to 50 solar masses contained within a region about a light year or so across (about 4.5×1047 m3). They contain molecular hydrogen (H2), carbon oxides and helium, and around 1% (by mass) silicate dust. Bok globules most commonly result in the formation of double- or multiple-star systems. An analysis of near-infrared observations published in 1990 confirmed that stars were being born inside Bok globules. Further observations have revealed that some Bok globules contain embedded warm sources, some contain Herbig–Haro objects, and some show outflows of molecular gas. Millimeter-wave emission line studies have provided evidence for the infall of material onto an accreting protostar. 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Henize 70 was first observed in 1950 in a survey of bright planetary nebulae. Based on appearance it was proposed that it might be a supernova remnant. In 1956, it was added to a catalogue of Hα emission stars and nebulae by Karl Gordon Henize, where it was described as an emission nebula rather than a planetary nebula. A paper published in 1978 proposed that the formations of Henize 70 and other emission nebulae could be due to stellar winds. Later in 1981, a scientific article mentioned a higher likeliness of a supernova explosion forming the nebula instead of stellar winds. A 2014 study measured that Henize 70 featured high SII and Hα ratios, indicating that it is not a supernova remnant. 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For the psychologist, see Star Vega (psychologist). For other uses, see Vega (disambiguation). Vega is the brightest star in the northern constellation of Lyra. It has the Bayer designation α Lyrae, which is Latinised to Alpha Lyrae and abbreviated Alpha Lyr or α Lyr. This star is relatively close at only 25 light-years (7.7 parsecs) from the Sun, and one of the most luminous stars in the Sun's neighborhood. It is the fifth-brightest star in the night sky, and the second-brightest star in the northern celestial hemisphere, after Arcturus. Vega has been extensively studied by astronomers, leading it to be termed \"arguably the next most important star in the sky after the Sun\". Vega was the northern pole star around 12,000 BCE and will be so again around the year 13,727, when its declination will be +86° 14′. Vega was the first star other than the Sun to have its image and spectrum photographed. It was one of the first stars whose distance was estimated through parallax measurements. Vega has functioned as the baseline for calibrating the photometric brightness scale and was one of the stars used to define the zero point for the UBV photometric system. Vega is only about a tenth of the age of the Sun, but since it is 2.1 times as massive, its expected lifetime is also one tenth of that of the Sun; both stars are at present approaching the midpoint of their main sequence lifetimes. Compared with the Sun, Vega has a lower abundance of elements heavier than helium. Vega is also a variable star—that is, a star whose brightness fluctuates. It is rotating rapidly with a speed of 236 km/s at the equator. This causes the equator to bulge outward due to centrifugal effects, and, as a result, there is a variation of temperature across the star's photosphere that reaches a maximum at the poles. From Earth, Vega is observed from the direction of one of these poles. Based on observations of more infrared radiation than expected, Vega appears to have a circumstellar disk of dust. This dust is likely to be the result of collisions between objects in an orbiting debris disk, which is analogous to the Kuiper belt in the Solar System. Stars that display an infrared excess due to dust emission are termed Vega-like stars. 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This meticulously crafted 3D model is perfect for printing and adding to your fantasy collection.\n\nDesign:\nChibi Style: The dragons are depicted in an adorable style, with exaggerated proportions that bring out their cuteness and playful nature.\nDynamic Pose: The dragons are shown in a joyful and energetic pose, with expressions full of character and their iconic bubbles swirling around.\nRound Base: The model comes with a round base, ideal for display on desks, shelves, or vitrines.\nFeatures:\nHigh-Quality STL File: Designed with precision to ensure sharp details and smooth surfaces during printing.\nPerfect for Collectors: A unique addition for fans of retro gaming, 3D models, and fantasy characters.\nIdeal for 3D Printing: Sized to be easily printable with stunning results.\nWhat’s Included:\nDetailed STL file including:\nThe Bubble Bobble dragons in Chibi style.\nA round base designed for stability and aesthetics.\nPrinting Recommendations:\nUse high-resolution settings for the best quality of detail.\nSupports recommended for printing intricate details like bubbles and the dragon's features.\nImportant Notes:\nThis is a digital download. No physical product will be shipped.\nThe file is intended for personal use only. For commercial use, please contact the creator.\nAdd a touch of retro gaming nostalgia to your collection with these charming Bubble Bobble Dragons in Chibi style. Perfect for lovers of classic arcade games, fantasy art, and 3D printing!\n\nHashtags\nBubbleBobble, 3DPrinting, STLFile, ChibiStyle, FantasyArt, CollectorItem, DigitalDownload, RetroGaming, AdorableDragons, 3DPrintArt","imageAlt":"Bubble Bobble Dragons - 3D Model - Chibi Style - STL File","url":"https://www.cgtrader.com/3d-print-models/miniatures/figurines/bubble-bobble-dragons-3d-model-chibi-style-stl-file","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/NdFdETX8HBxEGtFoFQENAP1X/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/Copia%20di%20Copia%20di%20Copia%20di%20Futuro%20-%201.jpg","gridUrl":"https://media.cgtrader.com/variants/NdFdETX8HBxEGtFoFQENAP1X/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/Copia%20di%20Copia%20di%20Copia%20di%20Futuro%20-%201.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-print-models/miniatures/figurines/bubble-bobble-dragons-3d-model-chibi-style-stl-file","isCgtVerified":false,"types":{"printReady":true,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":51,"name":".stl","is_native":false}],"categorySlug":"miniatures","subcategorySlug":"figurines","categoryTitle":"Miniatures","subcategoryTitle":"Action Figures \u0026 Statues","schemaImageUrl":"https://img-new.cgtrader.com/items/5792930/f3ff926133/bubble-bobble-dragons-3d-model-chibi-style-stl-file-3d-model-f3ff926133.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5817834","type":"listingItem","attributes":{"id":5817834,"title":"Vega Star","price":3.0,"description":"Description\n\nStar Vega redirects here. For the psychologist, see Star Vega (psychologist). For other uses, see Vega (disambiguation). Vega is the brightest star in the northern constellation of Lyra. It has the Bayer designation α Lyrae, which is Latinised to Alpha Lyrae and abbreviated Alpha Lyr or α Lyr. This star is relatively close at only 25 light-years (7.7 parsecs) from the Sun, and one of the most luminous stars in the Sun's neighborhood. It is the fifth-brightest star in the night sky, and the second-brightest star in the northern celestial hemisphere, after Arcturus. Vega has been extensively studied by astronomers, leading it to be termed arguably the next most important star in the sky after the Sun. Vega was the northern pole star around 12,000 BCE and will be so again around the year 13,727, when its declination will be +86° 14′. Vega was the first star other than the Sun to have its image and spectrum photographed. It was one of the first stars whose distance was estimated through parallax measurements. Vega has functioned as the baseline for calibrating the photometric brightness scale and was one of the stars used to define the zero point for the UBV photometric system. Vega is only about a tenth of the age of the Sun, but since it is 2.1 times as massive, its expected lifetime is also one tenth of that of the Sun; both stars are at present approaching the midpoint of their main sequence lifetimes. Compared with the Sun, Vega has a lower abundance of elements heavier than helium. Vega is also a variable star—that is, a star whose brightness fluctuates. It is rotating rapidly with a speed of 236 km/s at the equator. This causes the equator to bulge outward due to centrifugal effects, and, as a result, there is a variation of temperature across the star's photosphere that reaches a maximum at the poles. From Earth, Vega is observed from the direction of one of these poles. Based on observations of more infrared radiation than expected, Vega appears to have a circumstellar disk of dust. This dust is likely to be the result of collisions between objects in an orbiting debris disk, which is analogous to the Kuiper belt in the Solar System. Stars that display an infrared excess due to dust emission are termed Vega-like stars. 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The Hercules Corona Borealis Great Wall is like a blue space sky with stars and white large dots. The Hercules–Corona Borealis Great Wall (HCB) or simply the Great Wall is a galaxy filament that is the largest known structure in the observable universe, measuring approximately 10 billion light-years in length (the observable universe is about 93 billion light-years in diameter). This massive superstructure is a region of the sky seen in the data set mapping of gamma-ray bursts (GRBs) that has been found to have a concentration of similarly distanced GRBs that is unusually higher than the expected average distribution. It was discovered in early November 2013 by a team of American and Hungarian astronomers led by István Horváth, Jon Hakkila and Zsolt Bagoly while analyzing data from the Swift Gamma-Ray Burst Mission, together with other data from ground-based telescopes. It is the largest known formation in the universe, exceeding the size of the Huge-LQG by about a factor of two. The overdensity lies at the Second, Third and Fourth Galactic Quadrants (NGQ2, NGQ3 and NGQ4) of the sky. Thus, it lies in the Northern Hemisphere, centered on the border of the constellations Draco and Hercules. The entire clustering consists of around 19 GRBs with the redshift ranges between 1.6 and 2.1. Typically, the distribution of GRBs in the universe appears in the sets of less than the 2σ distribution, or with less than two GRBs in the average data of the point-radius system.[clarification needed] One possible explanation of this concentration is the Hercules–Corona Borealis Great Wall. The wall has a mean size in excess of 2 billion to 3 billion parsecs (6 to 10 billion light-years). Such a supercluster can explain the significant distribution of GRBs because of its tie to star formation. Doubt has been placed on the existence of the structure in other studies, positing that the structure was found through biases in certain statistical tests, without considering the full effects of extinction. 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For the psychologist, see Star Vega (psychologist). For other uses, see Vega (disambiguation). Vega is the brightest star in the northern constellation of Lyra. It has the Bayer designation α Lyrae, which is Latinised to Alpha Lyrae and abbreviated Alpha Lyr or α Lyr. This star is relatively close at only 25 light-years (7.7 parsecs) from the Sun, and one of the most luminous stars in the Sun's neighborhood. It is the fifth-brightest star in the night sky, and the second-brightest star in the northern celestial hemisphere, after Arcturus. Vega has been extensively studied by astronomers, leading it to be termed arguably the next most important star in the sky after the Sun. Vega was the northern pole star around 12,000 BCE and will be so again around the year 13,727, when its declination will be +86° 14′. Vega was the first star other than the Sun to have its image and spectrum photographed. It was one of the first stars whose distance was estimated through parallax measurements. Vega has functioned as the baseline for calibrating the photometric brightness scale and was one of the stars used to define the zero point for the UBV photometric system. Vega is only about a tenth of the age of the Sun, but since it is 2.1 times as massive, its expected lifetime is also one tenth of that of the Sun; both stars are at present approaching the midpoint of their main sequence lifetimes. Compared with the Sun, Vega has a lower abundance of elements heavier than helium. Vega is also a variable star—that is, a star whose brightness fluctuates. It is rotating rapidly with a speed of 236 km/s at the equator. This causes the equator to bulge outward due to centrifugal effects, and, as a result, there is a variation of temperature across the star's photosphere that reaches a maximum at the poles. From Earth, Vega is observed from the direction of one of these poles. Based on observations of more infrared radiation than expected, Vega appears to have a circumstellar disk of dust. This dust is likely to be the result of collisions between objects in an orbiting debris disk, which is analogous to the Kuiper belt in the Solar System. Stars that display an infrared excess due to dust emission are termed Vega-like stars. Observations by the James Webb Space Telescope show that the disk is exceptionally smooth, with no evidence of shaping by massive planets, though there is some evidence that there may be one or more Neptune-mass planets closer to the star.\n\nTexture Resolution: 1600 x 1037","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/vega-star","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/j07vissqioyxhakt5nuh4w5gk0zu/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/vega%20star-2.jpg","gridUrl":"https://media.cgtrader.com/variants/j07vissqioyxhakt5nuh4w5gk0zu/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/vega%20star-2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/vega-star","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/6018027/f1bf08782f/vega-star-3d-model-f1bf08782f.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5813566","type":"listingItem","attributes":{"id":5813566,"title":"Vega Cluster","price":3.0,"description":"Description\nDescriptionDescription\n\nStar Vega redirects here. For the psychologist, see Star Vega (psychologist). For other uses, see Vega (disambiguation). Vega is the brightest star in the northern constellation of Lyra. It has the Bayer designation α Lyrae, which is Latinised to Alpha Lyrae and abbreviated Alpha Lyr or α Lyr. This star is relatively close at only 25 light-years (7.7 parsecs) from the Sun, and one of the most luminous stars in the Sun's neighborhood. It is the fifth-brightest star in the night sky, and the second-brightest star in the northern celestial hemisphere, after Arcturus. Vega has been extensively studied by astronomers, leading it to be termed arguably the next most important star in the sky after the Sun. Vega was the northern pole star around 12,000 BCE and will be so again around the year 13,727, when its declination will be +86° 14′. Vega was the first star other than the Sun to have its image and spectrum photographed. It was one of the first stars whose distance was estimated through parallax measurements. Vega has functioned as the baseline for calibrating the photometric brightness scale and was one of the stars used to define the zero point for the UBV photometric system. Vega is only about a tenth of the age of the Sun, but since it is 2.1 times as massive, its expected lifetime is also one tenth of that of the Sun; both stars are at present approaching the midpoint of their main sequence lifetimes. Compared with the Sun, Vega has a lower abundance of elements heavier than helium. Vega is also a variable star—that is, a star whose brightness fluctuates. It is rotating rapidly with a speed of 236 km/s at the equator. This causes the equator to bulge outward due to centrifugal effects, and, as a result, there is a variation of temperature across the star's photosphere that reaches a maximum at the poles. From Earth, Vega is observed from the direction of one of these poles. Based on observations of more infrared radiation than expected, Vega appears to have a circumstellar disk of dust. This dust is likely to be the result of collisions between objects in an orbiting debris disk, which is analogous to the Kuiper belt in the Solar System. Stars that display an infrared excess due to dust emission are termed Vega-like stars. 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This Shapley Supercluster is like a gas cloud or nebula. The Shapley Supercluster or Shapley Concentration (SCl 124) is the largest concentration of galaxies in our nearby universe that forms a gravitationally interacting unit, thereby pulling itself together instead of expanding with the universe. It appears as a striking overdensity in the distribution of galaxies in the constellation of Centaurus. It is 650 million light-years away (z=0.046). In 1930, Harlow Shapley and his colleagues at the Harvard College Observatory started a survey of galaxies in the southern sky, using photographic plates obtained at the 24-inch Bruce telescope at Bloemfontein, South Africa. By 1932, Shapley reported the discovery of 76,000 galaxies brighter than 18th apparent magnitude in a third of the southern sky, based on galaxy counts from his plates. Some of this data was later published as part of the Harvard galaxy counts, intended to map galactic obscuration and to find the space density of galaxies. In this catalog, Shapley could see most of the 'Coma-Virgo cloud' (now known to be a superposition of the Coma Supercluster and the Virgo Supercluster), but found a 'cloud' in the constellation of Centaurus to be the most striking concentration of galaxies. He found it particularly interesting because of its great linear dimension, the numerous population and distinctly elongated form. This can be identified with what we now know as the core of the Shapley Supercluster. Shapley estimated the distance to this cloud to be 14 times that to the Virgo Cluster, from the average diameters of the galaxies. This would place the Shapley Supercluster at a distance of 231 Mpc, based on the current estimate of the distance to Virgo. In recent times, the Shapley Supercluster was named by Somak Raychaudhury, from a survey of galaxies from UK Schmidt Telescope Sky survey plates, using the Automated Plate Measuring Facility (APM) at the University of Cambridge in England. In this paper, the supercluster was named after Harlow Shapley, in recognition of his pioneering survey of galaxies in which this concentration of galaxies was first seen. 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The Hercules Corona Borealis Great Wall is like a dragon. The Hercules–Corona Borealis Great Wall (HCB) or simply the Great Wall is a galaxy filament that is the largest known structure in the observable universe, measuring approximately 10 billion light-years in length (the observable universe is about 93 billion light-years in diameter). This massive superstructure is a region of the sky seen in the data set mapping of gamma-ray bursts (GRBs) that has been found to have a concentration of similarly distanced GRBs that is unusually higher than the expected average distribution. It was discovered in early November 2013 by a team of American and Hungarian astronomers led by István Horváth, Jon Hakkila and Zsolt Bagoly while analyzing data from the Swift Gamma-Ray Burst Mission, together with other data from ground-based telescopes. It is the largest known formation in the universe, exceeding the size of the Huge-LQG by about a factor of two. The overdensity lies at the Second, Third and Fourth Galactic Quadrants (NGQ2, NGQ3 and NGQ4) of the sky. Thus, it lies in the Northern Hemisphere, centered on the border of the constellations Draco and Hercules. The entire clustering consists of around 19 GRBs with the redshift ranges between 1.6 and 2.1. Typically, the distribution of GRBs in the universe appears in the sets of less than the 2σ distribution, or with less than two GRBs in the average data of the point-radius system.[clarification needed] One possible explanation of this concentration is the Hercules–Corona Borealis Great Wall. The wall has a mean size in excess of 2 billion to 3 billion parsecs (6 to 10 billion light-years). Such a supercluster can explain the significant distribution of GRBs because of its tie to star formation. Doubt has been placed on the existence of the structure in other studies, positing that the structure was found through biases in certain statistical tests, without considering the full effects of extinction. 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This Saraswati Supercluster is like a lizard. The Saraswati Supercluster is a massive galaxy supercluster about 1.2 gigaparsecs (4 billion light years) away within the Stripe 82 region of SDSS, in the direction of the constellation Pisces. It is one of the largest structures found in the universe, with a major axis in diameter of about 200 Mpc (652 million light years). It consists of at least 43 galaxy clusters, and has the mass of 2 × 1016 MO, forming a galaxy filament. The Saraswati supercluster was discovered by a team of astrophysicists from the Inter-University Centre for Astronomy and Astrophysics and Indian Institute of Science Education and Research led by Joydeep Bagchi and colleagues in Pune, India in 2017. Analyzing the data of Stripe 82 of the comprehensive Sloan Digital Sky Survey, particularly the sets of LOWZ data from the Baryon Oscillation Spectroscopic Survey, part of the DR12 catalogue of the SDSS, the team discovered an overdensity of the sampled 625 galaxies from LOWZ and 3,016 from the LEGACY-BOSS-SOUTHERN, a survey of the southern sky that is also a part of SDSS DR12. It was named after the Hindu goddess of knowledge Saraswati, as well as the mythological Sarasvati river; since the Sanskrit name also means “ever flowing stream with many pools”, and the supercluster has many clusters and groups moving and merging together. The Saraswati Supercluster is one of the largest and most massive superclusters known, comparable to the massive Shapley Concentration in the nearby universe. The supercluster consists of 43 massive galaxy clusters, the most massive being Abell 2631 and ZwCL 2341.1+0000 respectively. It is surrounded by a network of galaxy filaments, clusters, and voids. The Saraswati supercluster and its environs reveal that some extreme large-scale, prominent matter density enhancements had formed in the past when dark energy had just started to dominate structure formation. 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The Centaurus Cluster is like a flying fish or albatross bird. The Centaurus Cluster (A3526) is a cluster of hundreds of galaxies, located approximately 170 million light-years away in the Centaurus constellation. The brightest member galaxy is the elliptical galaxy NGC 4696 (~11m). The Centaurus cluster shares its supercluster, the Hydra–Centaurus Supercluster, with IC4329 Cluster and Hydra Cluster. The cluster consists of two different sub-groups of galaxies with different velocities. Cen 30 is the main subgroup containing NGC 4696. Cen 45 which is centered on NGC 4709, is moving at 1500 km/s relative to Cen 30, and is believed to be merging with the main cluster.\n\nTexture Resolution: 2808 x 2957","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/centaurus-cluster","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/Z83oYdLt5RRb7PdWgi5tuU6C/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/centaurus%20cluster.jpg","gridUrl":"https://media.cgtrader.com/variants/Z83oYdLt5RRb7PdWgi5tuU6C/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/centaurus%20cluster.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/centaurus-cluster","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5823059/b0cb425c6b/centaurus-cluster-3d-model-b0cb425c6b.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5811547","type":"listingItem","attributes":{"id":5811547,"title":"Vega Cluster","price":3.0,"description":"Description\nDescription\n\nStar Vega redirects here. For the psychologist, see Star Vega (psychologist). For other uses, see Vega (disambiguation). Vega is the brightest star in the northern constellation of Lyra. It has the Bayer designation α Lyrae, which is Latinised to Alpha Lyrae and abbreviated Alpha Lyr or α Lyr. This star is relatively close at only 25 light-years (7.7 parsecs) from the Sun, and one of the most luminous stars in the Sun's neighborhood. It is the fifth-brightest star in the night sky, and the second-brightest star in the northern celestial hemisphere, after Arcturus. Vega has been extensively studied by astronomers, leading it to be termed arguably the next most important star in the sky after the Sun. Vega was the northern pole star around 12,000 BCE and will be so again around the year 13,727, when its declination will be +86° 14′. Vega was the first star other than the Sun to have its image and spectrum photographed. It was one of the first stars whose distance was estimated through parallax measurements. Vega has functioned as the baseline for calibrating the photometric brightness scale and was one of the stars used to define the zero point for the UBV photometric system. Vega is only about a tenth of the age of the Sun, but since it is 2.1 times as massive, its expected lifetime is also one tenth of that of the Sun; both stars are at present approaching the midpoint of their main sequence lifetimes. Compared with the Sun, Vega has a lower abundance of elements heavier than helium. Vega is also a variable star—that is, a star whose brightness fluctuates. It is rotating rapidly with a speed of 236 km/s at the equator. This causes the equator to bulge outward due to centrifugal effects, and, as a result, there is a variation of temperature across the star's photosphere that reaches a maximum at the poles. From Earth, Vega is observed from the direction of one of these poles. Based on observations of more infrared radiation than expected, Vega appears to have a circumstellar disk of dust. This dust is likely to be the result of collisions between objects in an orbiting debris disk, which is analogous to the Kuiper belt in the Solar System. Stars that display an infrared excess due to dust emission are termed Vega-like stars. Observations by the James Webb Space Telescope show that the disk is exceptionally smooth, with no evidence of shaping by massive planets, though there is some evidence that there may be one or more Neptune-mass planets closer to the star.\n\nTexture Resolution: 1001 x 1024","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/vega-cluster-60665dd8-2c1e-4d89-a543-3d0f73f9c9c0","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/Zo3YziS9yzpd6aXE92qN92EA/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/vega%20cluster-2.jpg","gridUrl":"https://media.cgtrader.com/variants/Zo3YziS9yzpd6aXE92qN92EA/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/vega%20cluster-2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/vega-cluster-60665dd8-2c1e-4d89-a543-3d0f73f9c9c0","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5811547/305c95866d/vega-cluster-3d-model-305c95866d.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"6015323","type":"listingItem","attributes":{"id":6015323,"title":"Cosmic Walls and Clusters Collection","price":15.0,"description":"Description\nThis is a collection of 49 Cosmic Walls and Clusters Models. Each asset is a high end, photorealistic 3D model, that is created to help you add the realism to your project. Each model is suitable for any visual production - broadcast, high-res film close-ups, advertising, games, design visualization, forensic presentation, etc.\n\nEach model was originally created in 3Ds Max 2022, then fully textured and rendered using V-Ray.\n\nAll geometry and visual aspects of the model are optimized to give you highest possible quality for up to 2k renders. There is no post-production used on any of the renders you see.\n\nThis collection contains:\n\n1 El Gordo Cluster(1st) - $3 2 El Gordo Cluster(2nd)- $3 3 El Gordo Cluster(3rd) - $3 4 Pavo Indus Supercluster - $3 5 Boss Great Wall(1st) - $3 6 Boss Great Wall(2nd) - $3 7 GRB 090423(1st) - $3 8 GRB 090423(2nd) - $3 9 Cosmic Web(1st) - $3 10 Cosmic Web(2nd) - $3 11 Cosmic Web(3rd) - $3 12 Shapley Supercluster(1st) - $3 Shapley Supercluster(2nd) - $3 14 Shapley Supercluster(3rd) - $3 15 Shapley Supercluster(4th) - $3 16 Shapley Supercluster(5th) - $3 17 Bullet Cluster - $3 18 Giant Void(1st) - $3 19 Giant Void(2nd) - $3 20 Clowes Campusano LQG - $3 21 U1 11 LQG - $3 22 Saraswati Supercluster - $3 23 Bok Globules - $3 24 Bootes Void - $3 25 Horologium Supercluster(1st) - $3 26 Horologium Supercluster(2nd) - $3 27Horologium Supercluster(3rd) - $3 28 Pandoras Cluster(1st) - $3 29 Pandoras Cluster(2nd) - $3 30 Centaurus Cluster - $3 31 Finger of God Globule - $3 32 KBC Void - $3 33 Hercules Corona Borealis Great Wall(1st) - $3 34 Hercules Corona Borealis Great Wall(2nd) - $3 35 Hercules Corona Borealis Great Wall(3rd) - $3 36 ASASSN 15lh - $3 37 Cosmic Filament - $3 38 Corona Borealis(1st) - $3 39 Corona Borealis(2nd) - $3 40 Southern Local Supervoid - $3 41 Giant GRB Ring - $3 42 Virgo Cluster - $3 43 Tonantzintla 618(1st) - $3 44 Tonantzintla 618(2nd) - $3 45 Ulas J1342 - $3 46 Leo Supercluster - $3 47 Coma Wall - $3 You save - $147 Features: -Each model is accurately sized to match the real object. -Clean and optimized topology is used for maximum polygon efficiency. -Each model is fully sub-dividable to allow Turbosmooth Iterations to increase mesh smoothness if needed. -All textures and materials are tailored and applied for high quality render results. -All objects have fully unwrapped UVs. -No extra plugins are needed for this model. -Lights and cameras are included in the scenes.\n\nSpecifications:\n\n-Each model is included in 1 file format. -3ds Max V-Ray\n\n-Units in all formats: #generic -All Textures are JPG and PNG format with the following resolutions: - 1089 x 580 px, 1679 x 1679 px, 400 x 400 px, 1200 x 686 px, 1600 x 1600 px, 500 x 500 px, 1446 x 1446 px, 800 x 800 px, 1200 x 720 px, 512 x 386 px, 512 x 386 px, 1280 x 720 px, 1023 x 685 px, 1150 x 1132 px, 736 x 915 px, 1530 x 1182 px, 768 x 768 px, 512 x 414 px, 1000 x 532 px, 1354 x 768 px, 3997 x 3861 px, 1156 x 1156 px, 1526 x 1526 px\n\nAdditional Notes:\n\nThis collection was created for 1 day form our Leading 3D artists to ensure you get the best quality model and save precious production time.\n\nIf you have any questions, you can contact us trough support. 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This El Gordo Cluster is like a starfield with comets. El Gordo (lit. The Fat One) (ACT-CL J0102-4915 or SPT-CL J0102-4915) is the largest distant galaxy cluster observed at its distance or beyond, as of 2011. As of 2014, it held the record for being the largest distant galaxy cluster to have been discovered with a mass of slightly less than three quadrillion solar masses although later its mass was reduced to about 2.1×1015 (2.1 quadrillion) solar masses with a 10% uncertainty. It was found by NASA's Chandra X-ray Observatory, the Atacama Cosmology Telescope (funded by the National Science Foundation) and the European Southern Observatory's Very Large Telescope. This galaxy cluster, officially named as, 'ACT-CL J0102-4915', has been given a 'nickname' by the researchers as 'El Gordo', which stands for the Fat One or the Big One in Spanish. It is located more than 7 billion light-years from Earth. Findings and results on 'El Gordo' were announced at the 219th meeting of American Astronomical Society in Austin, Texas.\n\nTexture Resolution: 2000 x 2000","imageAlt":"3D model ray El Gordo Cluster","url":"https://www.cgtrader.com/3d-models/space/other/el-gordo-cluster-e13f4f78-e8cf-47b4-9f2d-d392b8d1aa90","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/C2EaNpu2mpntHLpgzBTuKftZ/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/el%20gordo%20cluster-2.jpg","gridUrl":"https://media.cgtrader.com/variants/C2EaNpu2mpntHLpgzBTuKftZ/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/el%20gordo%20cluster-2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/el-gordo-cluster-e13f4f78-e8cf-47b4-9f2d-d392b8d1aa90","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5862315/98fa6f1bc2/el-gordo-cluster-3d-model-98fa6f1bc2.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5864705","type":"listingItem","attributes":{"id":5864705,"title":"Bullet Cluster","price":3.0,"description":"Description\nBullet Cluster. This Bullet Cluster is like a gas cloud with blue and pink colors. The Bullet Cluster (1E 0657-56) consists of two colliding clusters of galaxies. Strictly speaking, the name Bullet Cluster refers to the smaller subcluster, moving away from the larger one. It is at a comoving radial distance of 1.141 Gpc (3.72 billion light-years). The object is of a particular note for astrophysicists, because gravitational lensing studies of the Bullet Cluster are claimed to provide strong evidence for the existence of dark matter. Observations of other galaxy cluster collisions, such as MACS J0025.4-1222, similarly support the existence of dark matter. The major components of the cluster pair—stars, gas and the putative dark matter—behave differently during collision, allowing them to be studied separately. The stars of the galaxies, observable in visible light, were not greatly affected by the collision, and most passed right through, gravitationally slowed but not otherwise altered. The hot gas of the two colliding components, seen in X-rays, represents most of the baryonic, or \"ordinary\", matter in the cluster pair. The gases of the intracluster medium interact electromagnetically, causing the gases of both clusters to slow much more than the stars.\n\nThe third component, the dark matter, was detected indirectly by the gravitational lensing of background objects. In theories without dark matter, such as modified Newtonian dynamics (MOND), the lensing would be expected to follow the baryonic matter; i.e. the X-ray gas. However, the lensing is strongest in two separated regions near (possibly coincident with) the visible galaxies. This provides support for the idea that most of the gravitation in the cluster pair is in the form of two regions of dark matter, which bypassed the gas regions during the collision. 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The galaxies in the cluster make up less than five percent of its mass. The gas (around 20 percent) is so hot that it shines only in X-rays. Dark matter makes up around 75 percent of the cluster's mass. This cluster also shows a radio halo along with several other Abell clusters. It has a strong central halo, along with an extended tail, which could either be relic radiation, or an extension of the central halo. Renato Dupke, a member of the team that discovered the Cluster, explained the origin of the name in an interview: \"We nicknamed it ‘Pandora's Cluster’ because so many different and strange phenomena were unleashed by the collision.\" In February 2023, NASA's James Webb Space Telescope captured unprecedented details of Abell 2744, revealing previously unseen galaxies and offering insights into the early universe. This remarkable observation underscores the ongoing exploration of Pandora's Cluster and its significance in understanding cosmic evolution.\n\nTexture Resolution: 8068 x 8067","imageAlt":"3D model Pandoras Cluster","url":"https://www.cgtrader.com/3d-models/space/other/pandoras-cluster","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/tE5KRrVY5H4ckFW7JYd4USnM/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/pandoras%20cluster.jpg","gridUrl":"https://media.cgtrader.com/variants/tE5KRrVY5H4ckFW7JYd4USnM/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/pandoras%20cluster.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/pandoras-cluster","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5850766/59c16768b2/pandoras-cluster-3d-model-59c16768b2.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"6453820","type":"listingItem","attributes":{"id":6453820,"title":"Henize 70","price":3.0,"description":"Description\nHenize 70 (N70) is a faint emission nebula and superbubble located in the Large Magellanic Cloud in the constellation of Dorado. Henize 70 was first observed in 1950 in a survey of bright planetary nebulae. Based on appearance it was proposed that it might be a supernova remnant. In 1956, it was added to a catalogue of Hα emission stars and nebulae by Karl Gordon Henize, where it was described as an emission nebula rather than a planetary nebula. A paper published in 1978 proposed that the formations of Henize 70 and other emission nebulae could be due to stellar winds. Later in 1981, a scientific article mentioned a higher likeliness of a supernova explosion forming the nebula instead of stellar winds. A 2014 study measured that Henize 70 featured high SII and Hα ratios, indicating that it is not a supernova remnant. Henize 70 has spectral line ratios relatively similar to that of supernova remnants due to having similar SII/Hα line ratios although most supernova remnants have higher NII/Hα line ratios.\n\nTexture Resolution: 2048 x 1615","imageAlt":"3D Henize 70","url":"https://www.cgtrader.com/3d-models/space/other/henize-70","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/tyb34z90wp37lkb5w2n9m3zounam/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/henize%2070.jpg","gridUrl":"https://media.cgtrader.com/variants/tyb34z90wp37lkb5w2n9m3zounam/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/henize%2070.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/henize-70","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/6453820/a059861812/henize-70-3d-model-a059861812.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5862070","type":"listingItem","attributes":{"id":5862070,"title":"Shapley Supercluster","price":3.0,"description":"Description\nShapley Supercluster. This Shapley Supercluster is like a steam logo. The Shapley Supercluster or Shapley Concentration (SCl 124) is the largest concentration of galaxies in our nearby universe that forms a gravitationally interacting unit, thereby pulling itself together instead of expanding with the universe. It appears as a striking overdensity in the distribution of galaxies in the constellation of Centaurus. It is 650 million light-years away (z=0.046). In 1930, Harlow Shapley and his colleagues at the Harvard College Observatory started a survey of galaxies in the southern sky, using photographic plates obtained at the 24-inch Bruce telescope at Bloemfontein, South Africa. By 1932, Shapley reported the discovery of 76,000 galaxies brighter than 18th apparent magnitude in a third of the southern sky, based on galaxy counts from his plates. Some of this data was later published as part of the Harvard galaxy counts, intended to map galactic obscuration and to find the space density of galaxies. In this catalog, Shapley could see most of the 'Coma-Virgo cloud' (now known to be a superposition of the Coma Supercluster and the Virgo Supercluster), but found a 'cloud' in the constellation of Centaurus to be the most striking concentration of galaxies. He found it particularly interesting because of its great linear dimension, the numerous population and distinctly elongated form. This can be identified with what we now know as the core of the Shapley Supercluster. Shapley estimated the distance to this cloud to be 14 times that to the Virgo Cluster, from the average diameters of the galaxies. This would place the Shapley Supercluster at a distance of 231 Mpc, based on the current estimate of the distance to Virgo. In recent times, the Shapley Supercluster was named by Somak Raychaudhury, from a survey of galaxies from UK Schmidt Telescope Sky survey plates, using the Automated Plate Measuring Facility (APM) at the University of Cambridge in England. In this paper, the supercluster was named after Harlow Shapley, in recognition of his pioneering survey of galaxies in which this concentration of galaxies was first seen. Around the same time, Roberto Scaramella and co-workers had also noticed the Shapley Supercluster in the Abell catalogue of clusters of galaxies: they had named it the Alpha concentration.\n\nTexture Resolution: 768 x 768","imageAlt":"other 3D Shapley Supercluster","url":"https://www.cgtrader.com/3d-models/space/other/shapley-supercluster-4316c3be-7dab-4de1-b4c1-1fa930a9a0f9","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/RgTB2evv9mwszD2hdLUeo4uR/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/shapley%20supercluster----2.jpg","gridUrl":"https://media.cgtrader.com/variants/RgTB2evv9mwszD2hdLUeo4uR/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/shapley%20supercluster----2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/shapley-supercluster-4316c3be-7dab-4de1-b4c1-1fa930a9a0f9","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5862070/1ec5709655/shapley-supercluster-3d-model-1ec5709655.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"6456310","type":"listingItem","attributes":{"id":6456310,"title":"Musica Star","price":3.0,"description":"Description\n18 Delphini, also named Musica is a single star in the constellation of Delphinus of the low northern hemisphere. It has a Sun-like golden hue and is faintly visible to the eye with an apparent visual magnitude of 5.506. The star is located at a distance of approximately 245 light-years from the Sun based on parallax, and it is drifting further away with a radial velocity of +4 km/s. An object believed to be an extrasolar planet (designated 18 Delphini b or Arion) orbits the star. 18 Delphini is the star's Flamsteed designation, abbreviated 18 Del. Following its discovery the planet was designated 18 Delphini b. As part of the NameExoWorlds program by the International Astronomical Union, in 2015 the name Musica, Latin for 'music', was selected for this star by Tokushima Prefectural Jonan High School Science Club of Japan. The planet was given the name Arion, after a genius of poetry and music in ancient Greece. According to legend, his life was saved at sea by dolphins after attracting their attention by the playing of his kithara. The constellation 'Delphinus' is Latin for 'dolphin'. The stellar classification of 18 Delphini is G6III, which means it is an evolved star that has cooled and expanded off the main sequence. It is a suspected red clump giant that is generating energy from core helium fusion. A moderate level of X-ray emission has been detected from this star, which suggests it has a mildly active chromosphere. The star is 650 million years old with more than double the mass of the Sun, and has expanded to seven times the Sun's radius. It is radiating 34 times the luminosity of the Sun from its photosphere at an effective temperature of 5,071 K. The Washington Double Star Catalogue lists a pair of visual companions for this star. Component B is magnitude 9.88 and lies at an angular separation of 197.5 arcseconds along a position angle (PA) of 162° from the brighter star as of 2003. Component C has a magnitude of 12.77 with a separation of 129.3 arcseconds as of 2000. The proper motion of both stars are diverging significantly from 18 Delphini, so they can be ruled out as physical companions. However, a faint star located 29.2″ away appears to be a co-moving companion. This has a projected separation of 2,199 AU and a mass estimated as 19% that of the Sun. It is a small red dwarf star with a class of M4–5.\n\nTexture Resolution: 800 x 800","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/musica-star","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/hiw1fkq4hycyoqdkgjoaezha986o/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/musica%20star.jpg","gridUrl":"https://media.cgtrader.com/variants/hiw1fkq4hycyoqdkgjoaezha986o/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/musica%20star.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/musica-star","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/6456310/de78d076b0/musica-star-3d-model-de78d076b0.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"6016850","type":"listingItem","attributes":{"id":6016850,"title":"Sirius Star","price":3.0,"description":"Description\nSirius Star. Sirius is the brightest star in the night sky. Its name is derived from the Greek word Σείριος (Latin script: Seirios), meaning lit. 'glowing' or 'scorching'. The star is designated α Canis Majoris, Latinized to Alpha Canis Majoris, and abbreviated α CMa or Alpha CMa. With a visual apparent magnitude of −1.46, Sirius is almost twice as bright as Canopus, the next brightest star. Sirius is a binary star consisting of a main-sequence star of spectral type A0 or A1, termed Sirius A, and a faint white dwarf companion of spectral type DA2, termed Sirius B. The distance between the two varies between 8.2 and 31.5 astronomical units as they orbit every 50 years. Sirius appears bright because of its intrinsic luminosity and its proximity to the Solar System. At a distance of 2.64 parsecs (8.6 ly), the Sirius system is one of Earth's nearest neighbours. Sirius is gradually moving closer to the Solar System and it is expected to increase in brightness slightly over the next 60,000 years to reach a peak magnitude of −1.68. Coincidentally, at about the same time, Sirius will take its turn as the southern Pole Star, around the year 66,270 AD. In that year, Sirius will come to within 1.6 degrees of the south celestial pole. This is due to axial precession and proper motion of Sirius itself which moves slowly in the SSW direction, so it will be visible from the southern hemisphere only. After that time, its distance will begin to increase, and it will become fainter, but it will continue to be the brightest star in the Earth's night sky for approximately the next 210,000 years, at which point Vega, another A-type star that is intrinsically more luminous than Sirius, becomes the brightest star. Sirius A is about twice as massive as the Sun (MO) and has an absolute visual magnitude of +1.43. It is 25 times as luminous as the Sun, but has a significantly lower luminosity than other bright stars such as Canopus, Betelgeuse, or Rigel. The system is between 200 and 300 million years old. It was originally composed of two bright bluish stars. The initially more massive of these, Sirius B, consumed its hydrogen fuel and became a red giant before shedding its outer layers and collapsing into its current state as a white dwarf around 120 million years ago. Sirius is colloquially known as the \"Dog Star\", reflecting its prominence in its constellation, Canis Major (the Greater Dog). The heliacal rising of Sirius marked the flooding of the Nile in Ancient Egypt and the \"dog days\" of summer for the ancient Greeks, while to the Polynesians, mostly in the Southern Hemisphere, the star marked winter and was an important reference for their navigation around the Pacific Ocean.\n\nTexture Resolution: 1010 x 1112","imageAlt":"Sirius Star 3D model","url":"https://www.cgtrader.com/3d-models/space/other/sirius-star-70a04588-38a7-4a6e-94f9-a33febaaa443","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/ypvpcmjuoqfkj7dkq37c7yduu4ia/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/sirius%20star.jpg","gridUrl":"https://media.cgtrader.com/variants/ypvpcmjuoqfkj7dkq37c7yduu4ia/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/sirius%20star.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/sirius-star-70a04588-38a7-4a6e-94f9-a33febaaa443","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/6016850/dd9ce08af4/sirius-star-3d-model-dd9ce08af4.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5863393","type":"listingItem","attributes":{"id":5863393,"title":"Coma Wall","price":3.0,"description":"Description\nComa Wall also known CfA2 Great Wall. This Coma Wall is like a firework. The Great Wall (also called Coma Wall), sometimes specifically referred to as the CfA2 Great Wall, is an immense galaxy filament. It is one of the largest known superstructures in the observable universe.\n\nThis structure was discovered c. 1989 by a team of American astronomers led by Margaret J. Geller and John Huchra while analyzing data gathered by the second CfA Redshift Survey of the Center for Astrophysics | Harvard \u0026 Smithsonian (CfA). The term \"Great\" has been added to distinguish it as an even larger type compared to standard galaxy walls.\n\nThe CfA2 Great Wall has the maximum dimensions of either 500 million or 750 million light years depending on the figure and the reference used.[citation needed] It is 200 million light years in width and about 16 million light years in thickness. Its nearest point is about 300 million light years from Earth, while its furthest point is 550 million light years away. 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This Virgo Cluster is like a stars in space. The Virgo Cluster is a cluster of galaxies whose center is 53.8 ± 0.3 Mly (16.5 ± 0.1 Mpc) away in the constellation Virgo. Comprising approximately 1,300 (and possibly up to 2,000) member galaxies, the cluster forms the heart of the larger Virgo Supercluster, of which the Local Group (containing the Milky Way galaxy) is a member. The Local Group actually experiences the mass of the Virgo Supercluster as the Virgocentric flow. It is estimated that the Virgo Cluster's mass is 1.2×1015 MO out to 8 degrees of the cluster's center or a radius of about 2.2 Mpc.\n\nMany of the brighter galaxies in this cluster, including the giant elliptical galaxy Messier 87, were discovered in the late 1770s and early 1780s and subsequently included in Charles Messier's catalogue of non-cometary fuzzy objects. Described by Messier as nebulae without stars, their true nature was not recognized until the 1920s.\n\nThe cluster extends across approximately 8 degrees centered in the constellation Virgo. Some of its most prominent members can be seen with binoculars and small telescopes, while a 6-inch telescope will reveal about 160 of the cluster's galaxies on a clear night. Its brightest member is the elliptical galaxy Messier 49.\n\nTexture Resolution: 1023 x 685","imageAlt":"Virgo Cluster 3D model","url":"https://www.cgtrader.com/3d-models/space/other/virgo-cluster","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/Ao2THDUuPKwSWZdJr67w9mDj/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/virgo%20cluster.jpg","gridUrl":"https://media.cgtrader.com/variants/Ao2THDUuPKwSWZdJr67w9mDj/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/virgo%20cluster.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/virgo-cluster","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5863610/d0cb98beb4/virgo-cluster-3d-model-d0cb98beb4.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5862935","type":"listingItem","attributes":{"id":5862935,"title":"Fornax Cluster","price":3.0,"description":"Description\nFornax Cluster. The Fornax Cluster is a cluster of galaxies lying at a distance of 19 megaparsecs (62 million light-years). It has an estimated mass of (7±2)×1013 solar masses, making it the second richest galaxy cluster within 100 million light-years, after the considerably larger Virgo Cluster. It may be associated with the nearby Eridanus Group. It lies primarily in the constellation Fornax, with its southern boundaries partially crossing into the constellation of Eridanus, and covers an area of sky about 6° across or about 28 sq degrees. The Fornax Cluster is a particularly valuable source of information about the evolution of such clusters due to its relatively close proximity to the Sun. It also shows the gravitational effects of a merger of a galaxy subgroup with the main galaxy group, which in turn lends clues about the associated galactic superstructure. At the centre of the cluster lies NGC 1399. Other cluster members include NGC 1316 (the group's brightest galaxy), NGC 1365, NGC 1427A, NGC 1427 and NGC 1404. Fornax can be divided into two subclusters: the main cluster, centered on NGC 1399, and a subgroup 3 degrees to the southwest centered on the lenticular galaxy NGC 1316 that is currently in the process of infalling with the largest subcluster to merge with it, and whose galaxies are experiencing relatively strong star formation activity.\n\nTexture Resolution: 702 x 336","imageAlt":"Fornax Cluster 3D","url":"https://www.cgtrader.com/3d-models/space/other/fornax-cluster-4027c3e8-e9af-4fa0-81fe-9d53b90cb94f","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/RCnRtYVxJvz5G7fV97jC4zCZ/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/fornax%20cluster--2.jpg","gridUrl":"https://media.cgtrader.com/variants/RCnRtYVxJvz5G7fV97jC4zCZ/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/fornax%20cluster--2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/fornax-cluster-4027c3e8-e9af-4fa0-81fe-9d53b90cb94f","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5862935/7331be6fd9/fornax-cluster-3d-model-7331be6fd9.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5818016","type":"listingItem","attributes":{"id":5818016,"title":"Boss Great Wall","price":3.0,"description":"Description\n\nThe Boss Great Wall. The Boss Great Wall is like a bird. The BOSS Great Wall is a supercluster complex that was identified, using the Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey (SDSS), in early 2016. It was discovered by a research team from several institutions, consisting of: Heidi Lietzen, Elmo Tempel, Lauri Juhan Liivamägi, Antonio Montero-Dorta, Maret Einasto, Alina Streblyanska, Claudia Maraston, Jose Alberto Rubiño-Martín and Enn Saar. The BOSS Great Wall is one of the largest superstructures in the observable universe, though there are even larger structures known. The large complex has a mean redshift of z ~ 0.47 (z times Hubble length ≈ 6.8 billion light years). It consists of two elongated superclusters, two large superclusters, and several smaller superclusters as well. The elongated superclusters form galaxy walls, with the larger of the two having a diameter of 186/h Mpc (supercluster A in the figure); the second wall's being 173/h Mpc (supercluster B). The other two main superclusters are moderately large, having diameters of 91/h Mpc and 64/h Mpc (superclusters D and C, respectively). The superstructure is roughly 1 billion light years in diameter, and has a total mass approximately 10,000 times the Milky Way galaxy. It contains at least 830 visible galaxies (represented in the figure within their respective superclusters), as well as many others that are not visible (dark galaxies). The researchers used Minkowski functionals to verify the structure's overall shape and size; the first three quantifying the thickness, width, and length followed by the fourth determining the structure's overall curvature. The research team compared the luminosities and stellar masses within the superstructure to known high stellar mass galaxies within the SDSS's 7th data release, DR7. This allowed the team to scale the data using known values, from local superclusters, to determine the overall morphology of the BOSS Great Wall. It is currently debated amongst astronomers if the BOSS Great Wall may be considered a structure, due to the intricacies of its shape and overall size. The question of whether the supercluster complex is moving together or being slowly separated by the expanding universe is a key factor to this discussion. Nevertheless, when compared to several other chain structures, such as the Sloan Great Wall, the BOSS Great Wall's superclusters are far richer, containing more dense, high stellar mass galaxies. The BOSS Great Wall's discovery, and the data gained therein, should prove very beneficial for astronomers who study the overall structure of the cosmic web.\n\nTexture Resolution: 1080 x 1080","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/boss-great-wall","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/vU8EwTM5MbzKDyKsV1xq7V6Y/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/boss%20great%20wall.jpg","gridUrl":"https://media.cgtrader.com/variants/vU8EwTM5MbzKDyKsV1xq7V6Y/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/boss%20great%20wall.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/boss-great-wall","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5818016/aaf1c28d49/boss-great-wall-3d-model-aaf1c28d49.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"6455952","type":"listingItem","attributes":{"id":6455952,"title":"Alcor and Mizar Stars","price":3.0,"description":"Description\nMizar and Alcor are two stars forming a eye double in the handle of the Big Dipper (or Plough) asterism in the constellation of Ursa Major. Their magnitudes are 2.2 and 3.9, and the pair can easily be seen without the aid of a telescope. Mizar and its fainter companion Alcor are actually a four-star binary system consisting of two pairs of double stars that are gravitationally bound to each other. The traditional name Mizar derives from the Arabic المئزر or mi'zar, meaning 'apron; wrapper, cover'. Alcor was originally the Arabic سها or suhā/sohā, meaning either 'the forgotten' or 'neglected one'. The ancient Persians and the Bedouins used distinguishing Mizar and Alcor as a test of vision.\nMizar, also designated Zeta Ursae Majoris (ζ Ursae Majoris, abbreviated Zeta UMa, ζ UMa), is itself a quadruple system and Alcor, also designated 80 Ursae Majoris (80 UMa), is a binary star, the pair together forming a sextuple system. Mizar was the first known binary star system, claimed to be discovered by Italian astronomer Giovanni Battista Riccioli in 1650. The whole system lies about 83 light-years away from the Sun, as measured by the Hipparcos astrometry satellite.\nWith normal eyesight Alcor appears at about 12 arcminutes from Mizar. Alcor is of magnitude 3.99 and spectral class A5V. It has a faint red dwarf companion separated by 1 arcsecond. Mizar and Alcor's proper motions show they move together, along with most of the other stars of the Big Dipper except Alpha Ursae Majoris and Eta Ursae Majoris, as members of the Ursa Major moving group, a mostly dispersed group of stars sharing a common birth. However, it has yet to be demonstrated conclusively that they are gravitationally bound. Parallax measurements by Gaia indicate that Alcor and Mizar are somewhat closer together than previously thought: 0.36±0.19 pc. The uncertainty is due to not knowing exactly how far away the stars are. If they are exactly the same distance from us then the distance between them is only 17800 AU (0.281 ly). Between Mizar and Alcor, the 8th-magnitude star Sidus Ludoviciana is a distant background object.\nAlcor Star is located on lower left and Mizar Star is located on upper center.\n\nTexture Resolution: 1172 x 896","imageAlt":"Alcor and Mizar Stars 3D","url":"https://www.cgtrader.com/3d-models/space/other/alcor-and-mizar-stars","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/k2ioklp18bltei3yvmsvw0mxt3xq/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/alcor%20and%20mizar%20stars.jpg","gridUrl":"https://media.cgtrader.com/variants/k2ioklp18bltei3yvmsvw0mxt3xq/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/alcor%20and%20mizar%20stars.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/alcor-and-mizar-stars","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/6455952/23fdf693ee/alcor-and-mizar-stars-3d-model-23fdf693ee.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5842771","type":"listingItem","attributes":{"id":5842771,"title":"Phoenix Cluser","price":3.0,"description":"Description\nPhoenix Cluster. The Phoenix Cluster is like an ant. The Phoenix Cluster (SPT-CL J2344-4243) is a massive, Abell class type I galaxy cluster located at its namesake, southern constellation of Phoenix. It was initially detected in 2010 during a 2,500 square degree survey of the southern sky using the Sunyaev–Zeldovich effect by the South Pole Telescope collaboration. It is one of the most massive galaxy clusters known, with the mass on the order of 2×1015 MO, and is the most luminous X-ray cluster discovered, producing more X-rays than any other known massive cluster. It is located at a comoving distance of 8.61 billion light-years (2.64 gigaparsecs) from Earth. About 42 member galaxies were identified and currently listed in the SIMBAD Astronomical Database, though the real number may be as high as 1,000 galaxies. The Phoenix Cluster was first reported in a paper by R. Williamson and colleagues during a survey by the South Pole Telescope in Antarctica, being one of the 26 galaxy clusters identified by the survey. The detection has been conducted at frequencies between 95, 150, and 220 GHz, with 14 of the galaxy clusters detected have been previously identified, while 12 – including Phoenix Cluster, being new discoveries. The would-be named Phoenix Cluster (still identified by its numerical catalogue entry SPT-CL J2344–4243) has been remarked to be having the largest X-ray luminosity of any cluster described by the survey. A bright, type-2 Seyfert galaxy has also been pronounced lying 19 arcseconds from the apparent center of the cluster that has been identified as 2MASX J23444387-4243124, which would later be named Phoenix A, the cluster's central galaxy.\n\nTexture Resolution: 864 x 864","imageAlt":"Phoenix Cluser 3D","url":"https://www.cgtrader.com/3d-models/space/other/phoenix-cluser","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/Pho23N1BJVhLKw5XH9Wk6nBA/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/phoenix%20cluster--2.jpg","gridUrl":"https://media.cgtrader.com/variants/Pho23N1BJVhLKw5XH9Wk6nBA/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/phoenix%20cluster--2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/phoenix-cluser","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5842771/ca4c824ce9/phoenix-cluser-3d-model-ca4c824ce9.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5862136","type":"listingItem","attributes":{"id":5862136,"title":"El Gordo Cluster","price":3.0,"description":"Description\nEl Gordo Cluster. This El Gordo Cluster is like a comet. El Gordo (lit. The Fat One) (ACT-CL J0102-4915 or SPT-CL J0102-4915) is the largest distant galaxy cluster observed at its distance or beyond, as of 2011. As of 2014, it held the record for being the largest distant galaxy cluster to have been discovered with a mass of slightly less than three quadrillion solar masses although later its mass was reduced to about 2.1×1015 (2.1 quadrillion) solar masses with a 10% uncertainty. It was found by NASA's Chandra X-ray Observatory, the Atacama Cosmology Telescope (funded by the National Science Foundation) and the European Southern Observatory's Very Large Telescope. This galaxy cluster, officially named as, 'ACT-CL J0102-4915', has been given a 'nickname' by the researchers as 'El Gordo', which stands for \"the Fat One\" or \"the Big One\" in Spanish. It is located more than 7 billion light-years from Earth. Findings and results on 'El Gordo' were announced at the 219th meeting of American Astronomical Society in Austin, Texas.\n\nTexture Resolution: 1530 x 1182","imageAlt":"3D El Gordo Cluster","url":"https://www.cgtrader.com/3d-models/space/other/el-gordo-cluster","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/VPoWQapD2Khrna8yo6jLj7hW/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/el%20gordo%20cluster.jpg","gridUrl":"https://media.cgtrader.com/variants/VPoWQapD2Khrna8yo6jLj7hW/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/el%20gordo%20cluster.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/el-gordo-cluster","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5862136/b16122d3db/el-gordo-cluster-3d-model-b16122d3db.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5825208","type":"listingItem","attributes":{"id":5825208,"title":"Sculptor Wall","price":3.0,"description":"Description\nSculptor Wall. The Sculptor Wall is like a dinosaur or falling turtle. The Sculptor Wall is a superstructure of galaxies (\"wall of galaxies\") relatively near to the Milky Way Galaxy (redshift of approximately z=0.03), also known as the Sculptor superclusters. The superstructure is also called the Southern Great Wall, the Great Southern Wall, or just the Southern Wall, in reference to the Northern Great Wall. The structure is 8000 km/s long (where km/s indicates the rate of expansion between two objects at the extents of a superstructure), 5000 km/s wide, 1000 km/s deep, in redshift space dimensions. Because these structures are so large, it is convenient to estimate their size by measuring their redshift; using a value of 67.8 for Hubble's constant, the size of the structure is approximately 100 Mpc long by 70 Mpc wide by 10 Mpc deep. The Grus Wall is \"perpendicular\" to the Fornax Wall and Sculptor Wall.\n\nTexture Resolution: 1156 x 1156","imageAlt":"3D model Sculptor Wall","url":"https://www.cgtrader.com/3d-models/space/other/sculptor-wall","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/1qoj53iKq49SZHHcQxJufjaS/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/sculptor%20wall.jpg","gridUrl":"https://media.cgtrader.com/variants/1qoj53iKq49SZHHcQxJufjaS/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/sculptor%20wall.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/sculptor-wall","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5825208/174439a9dc/sculptor-wall-3d-model-174439a9dc.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5862880","type":"listingItem","attributes":{"id":5862880,"title":"Fornax Cluster","price":3.0,"description":"Description\nFornax Cluster. The Fornax Cluster is a cluster of galaxies lying at a distance of 19 megaparsecs (62 million light-years). It has an estimated mass of (7±2)×1013 solar masses, making it the second richest galaxy cluster within 100 million light-years, after the considerably larger Virgo Cluster. It may be associated with the nearby Eridanus Group. It lies primarily in the constellation Fornax, with its southern boundaries partially crossing into the constellation of Eridanus, and covers an area of sky about 6° across or about 28 sq degrees. The Fornax Cluster is a particularly valuable source of information about the evolution of such clusters due to its relatively close proximity to the Sun. It also shows the gravitational effects of a merger of a galaxy subgroup with the main galaxy group, which in turn lends clues about the associated galactic superstructure. At the centre of the cluster lies NGC 1399. Other cluster members include NGC 1316 (the group's brightest galaxy), NGC 1365, NGC 1427A, NGC 1427 and NGC 1404. Fornax can be divided into two subclusters: the main cluster, centered on NGC 1399, and a subgroup 3 degrees to the southwest centered on the lenticular galaxy NGC 1316 that is currently in the process of infalling with the largest subcluster to merge with it, and whose galaxies are experiencing relatively strong star formation activity.\n\nTexture Resolution: 1280 x 640","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/fornax-cluster-a19b2b76-6055-4d17-ac35-975c66b3cd26","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/B2RZdnBnFRfhCDK61P2DZQWw/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/fornax%20cluster-2.jpg","gridUrl":"https://media.cgtrader.com/variants/B2RZdnBnFRfhCDK61P2DZQWw/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/fornax%20cluster-2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/fornax-cluster-a19b2b76-6055-4d17-ac35-975c66b3cd26","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5862880/65bb7919f4/fornax-cluster-3d-model-65bb7919f4.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"6455408","type":"listingItem","attributes":{"id":6455408,"title":"Henize 2-10","price":3.0,"description":"Description\nHen 2-10, also known as He 2-10 and Henize 2-10, is a dwarf starburst galaxy located 34 million light years away in the constellation of Pyxis. The galaxy is believed to be an early stage starburst galaxy. A black hole was later discovered near the center of the dwarf galaxy, suggesting that the black holes found at the center of most large galaxies may have formed before the galaxies themselves. Recent estimates have placed the mass of this black hole around 3×106 MO, and the mass of the entire dwarf galaxy at about 1×1010 MO. Henize 2-10 draws its name from a catalog of planetary nebulae assembled by astronomer Karl Henize. Henize additionally noted that the object was identified in an unpublished paper by Rudolph Minkowski. The object was likely misidentified as a planetary nebula due to the galaxy's strong emission lines, a feature common of planetary nebulas. It was not until the 1970s when observations of Hen 2-10 indicated that the center of the object was a strong source of radio waves that it was shown that Hen 2-10 was a dwarf galaxy rather than a planetary nebula. Supporting evidence for the reclassification came in the form of excess infrared emission and a higher than usual density of neutral hydrogen. Hen 2-10 is a starburst galaxy featuring at least two star-forming regions near the center of the galaxy. These regions feature a variety of different substances, and multiple super star clusters. A study of some of these SSCs estimates their age to be between 4 and 5 megayears. The galaxy also features emission typical of that in a Wolf–Rayet star, further providing evidence for the starburst region of the galaxy. It was one of the first galaxies found to feature this emission. The strong prevalence of this emission has led to its classification as a Wolf–Rayet galaxy, a special subclass of starburst galaxy that features a higher than normal number of Wolf–Rayet stars. Furthermore, observations have shown irregularities in the southeast portion of the galaxy which could be interpreted as a tidal tail. This tidal tail suggests that Hen 2-10 may have had past interactions with other galaxies, possibly even a merger event. In 2011, a team of researchers studied the non-thermal emission of the galaxy center and indicated that the source strengths of radio waves are too strong to come from x-ray binaries while the source strengths of x-rays are too strong to be supernova remnants. However, these sources do align with known data for black holes. This original paper postulated the mass of the black hole to be ~1×106 MO, but a newer study has refined the estimate to 3×106 MO. The presence of SSCs near the center of the galaxy, and not a singular nuclear star cluster (NSC) has led some to believe that Hen 2-10 is a galaxy in its early years. The presence of the black hole is seen to be evidence of the dissipationless model of NSC formation. In this model, the SSCs will move to the center and form a singular NSC. Due to the black hole's relatively small mass, it is not believed to have a major effect on the timescale of this motion, although it is not yet understood how the black hole will affect the NSC formation. Ignoring the black hole indicates that the NSC should be fully formed in a few hundred million years.\n\nTexture Resolution: 3600 x 2569","imageAlt":"Henize 2-10 3D","url":"https://www.cgtrader.com/3d-models/space/other/henize-2-10","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/xw39m1y3jlprwkq0ffbtklp7pu05/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/henize%202-10.jpg","gridUrl":"https://media.cgtrader.com/variants/xw39m1y3jlprwkq0ffbtklp7pu05/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/henize%202-10.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/henize-2-10","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/6455408/851e236d9a/henize-2-10-3d-model-851e236d9a.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5862820","type":"listingItem","attributes":{"id":5862820,"title":"Fornax Cluster","price":3.0,"description":"Description\nFornax Cluster. The Fornax Cluster is a cluster of galaxies lying at a distance of 19 megaparsecs (62 million light-years). It has an estimated mass of (7±2)×1013 solar masses, making it the second richest galaxy cluster within 100 million light-years, after the considerably larger Virgo Cluster. It may be associated with the nearby Eridanus Group. It lies primarily in the constellation Fornax, with its southern boundaries partially crossing into the constellation of Eridanus, and covers an area of sky about 6° across or about 28 sq degrees. The Fornax Cluster is a particularly valuable source of information about the evolution of such clusters due to its relatively close proximity to the Sun. It also shows the gravitational effects of a merger of a galaxy subgroup with the main galaxy group, which in turn lends clues about the associated galactic superstructure. At the centre of the cluster lies NGC 1399. Other cluster members include NGC 1316 (the group's brightest galaxy), NGC 1365, NGC 1427A, NGC 1427 and NGC 1404. Fornax can be divided into two subclusters: the main cluster, centered on NGC 1399, and a subgroup 3 degrees to the southwest centered on the lenticular galaxy NGC 1316 that is currently in the process of infalling with the largest subcluster to merge with it, and whose galaxies are experiencing relatively strong star formation activity.\n\nTexture Resolution: 1200 x 839","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/fornax-cluster","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/fo2YX3F9mURPvG6Qh97Z6nL2/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/fornax%20cluster.jpg","gridUrl":"https://media.cgtrader.com/variants/fo2YX3F9mURPvG6Qh97Z6nL2/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/fornax%20cluster.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/fornax-cluster","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5862820/1e0306910b/fornax-cluster-3d-model-1e0306910b.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5975777","type":"listingItem","attributes":{"id":5975777,"title":"GRB 090423","price":3.0,"description":"Description\nGRB 090423. This GRB 090423 is like a comet that's passing through the supernova explosion. GRB 090423 was a gamma-ray burst (GRB) detected by the Swift Gamma-Ray Burst Mission on April 23, 2009, at 07:55:19 UTC whose afterglow was detected in the infrared and enabled astronomers to determine that its redshift is z = 8.2, making it one of the most distant objects detected at that time with a spectroscopic redshift (GN-z11, discovered in 2016, has a redshift of 11). A gamma-ray burst is an extremely luminous event flash of gamma rays that occurs as the result of an explosion, and is thought to be associated with the formation of a black hole. The burst itself typically only lasts for a few seconds, but gamma-ray bursts frequently produce an afterglow at longer wavelengths that can be observed for many hours or even days after the burst. Measurements at these wavelengths, which include X-ray, ultraviolet, optical, infrared, and radio, enable follow-up study of the event. The finite speed of light means that GRB 090423 is also one of the earliest objects ever detected for which a spectroscopic redshift has been measured. The universe was only 630 million years old when the GRB occurred, and its detection confirms that massive stars were born and dying even very early on in the life of the universe. GRB 090423 and similar events provide a unique means of studying the early universe, as few other objects of that era are bright enough to be seen with today's telescopes. On April 23, 2009, at 07:55:19 UTC the Swift satellite detected a burst that lasted about 10 seconds and was located in the direction of the constellation Leo. Swift localized the field in which GRB 090423 occurred, and 77 seconds after the burst, the Swift UVOT Photometric System took a 150-second exposure of the field, but was unable to detect an optical or ultraviolet afterglow. A few minutes after its discovery, ground-based telescopes began observing the field. Within 20 minutes of the burst, Nial Tanvir and his team found an infrared source at the Swift position using the United Kingdom Infrared Telescope (UKIRT) on Mauna Kea, Hawaii. The initial observations taken by UKIRT were triggered autonomously via the eSTAR Project. They observed a drop off in flux beyond 1.13 micrometres with the VLT. Attributing this drop off to Lyman alpha absorption by neutral hydrogen in the intergalactic medium, they calculated a redshift of 8.2 for GRB 090423. The team of C.C. Thöne and Paolo D'Avanzo observed the afterglow of GRB 090423 using the Italian TNG 3.6m telescope located in the Canary Islands, Spain. They obtained two hours of spectra, which when combined, suggested a very weak signal at the position of the afterglow. They too saw a drop off in flux near 1.1 micrometres, and reported a redshift of 8.1 for GRB 090423, which is consistent, within error, of the redshift reported by Tanvir et al. The redshift of 8.1 suggest the burst may have lasted approximately 1.2 seconds in the local frame of the emitter, its duration being redshifted accordingly to the observed 10 seconds. The intergovernmental astronomy organisation, European Southern Observatory (ESO) operates the Very Large Telescope that obtained the spectrum reported by Tanvir et al. The GRB was not visible in Chile when Swift first detected the burst at 07:55 UTC, but was the following day at 03:00 UTC, which enabled the Gamma-Ray Burst Optical/Near-Infrared Detector (GROND) at La Silla Observatory to make observations of the burst, and find a photometric redshift consistent with the value reported elsewhere. The last observers to gather data during the event was the Combined Array for Research in Millimeter-wave Astronomy (CARMA) observatory. The observation of GRB 090423 by CARMA was taken at a frequency of 92.5 GHz. While the afterglow was not detected, they were able to place a 3-sigma upper limit of 0.7 mJy on the flux density of the afterglow.\n\nTexture Resolution: 400 x 400","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/grb-090423-5c573446-307e-4e56-8243-0e5d414d734a","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/yvshgrq4qqf54y19qgz3o1mr94hz/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/grb%20090423%20%282%29.jpg","gridUrl":"https://media.cgtrader.com/variants/yvshgrq4qqf54y19qgz3o1mr94hz/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/grb%20090423%20%282%29.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/grb-090423-5c573446-307e-4e56-8243-0e5d414d734a","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5975777/7a994367a9/grb-090423-3d-model-7a994367a9.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5857245","type":"listingItem","attributes":{"id":5857245,"title":"Pandoras Cluster","price":3.0,"description":"Description\nDescription\n\nPandora's Cluster(Abell 2744), nicknamed Pandora's Cluster, is a giant galaxy cluster resulting from the simultaneous pile-up of at least four separate, smaller galaxy clusters that took place over a span of 350 million years, and is located approximately 4 billion light years from Earth. The galaxies in the cluster make up less than five percent of its mass. The gas (around 20 percent) is so hot that it shines only in X-rays. Dark matter makes up around 75 percent of the cluster's mass. This cluster also shows a radio halo along with several other Abell clusters. It has a strong central halo, along with an extended tail, which could either be relic radiation, or an extension of the central halo. Renato Dupke, a member of the team that discovered the Cluster, explained the origin of the name in an interview: We nicknamed it ‘Pandora's Cluster’ because so many different and strange phenomena were unleashed by the collision. In February 2023, NASA's James Webb Space Telescope captured unprecedented details of Abell 2744, revealing previously unseen galaxies and offering insights into the early universe. This remarkable observation underscores the ongoing exploration of Pandora's Cluster and its significance in understanding cosmic evolution.\n\nTexture Resolution: 1280 x 720","imageAlt":"3D Pandoras Cluster","url":"https://www.cgtrader.com/3d-models/space/other/pandoras-cluster-dd427f19-bc0a-45ae-9fd8-077d229901d9","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/nXLAm2LLaK9S9xvY8C8rF8FR/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/pandoras%20cluster-2.jpg","gridUrl":"https://media.cgtrader.com/variants/nXLAm2LLaK9S9xvY8C8rF8FR/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/pandoras%20cluster-2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/pandoras-cluster-dd427f19-bc0a-45ae-9fd8-077d229901d9","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5857245/45754db9d1/pandoras-cluster-3d-model-45754db9d1.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5806262","type":"listingItem","attributes":{"id":5806262,"title":"Cosmic Web","price":3.0,"description":"Description\nDescriptionDescription\n\nCosmic Web. In cosmology, galaxy filaments are the largest known structures in the universe, consisting of walls of galactic superclusters. These massive, thread-like formations can commonly reach 50 to 80 megaparsecs (160 to 260 megalight-years)—with the largest found to date being the Hercules-Corona Borealis Great Wall at around 3 gigaparsecs (9.8 Gly) in length—and form the boundaries between voids. Due to the accelerating expansion of the universe, the individual clusters of gravitationally bound galaxies that make up galaxy filaments are moving away from each other at an accelerated rate; in the far future they will dissolve. Galaxy filaments form the cosmic web and define the overall structure of the observable universe.\n\nTexture Resolution: 640 x 426","imageAlt":"Cosmic Web 3D model","url":"https://www.cgtrader.com/3d-models/space/other/cosmic-web-e6588cac-f219-4280-9ffe-b3dd7075adcb","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/ELyvsdBRfuMrWgsKN5eMau35/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/cosmic%20web--2.jpg","gridUrl":"https://media.cgtrader.com/variants/ELyvsdBRfuMrWgsKN5eMau35/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/cosmic%20web--2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/cosmic-web-e6588cac-f219-4280-9ffe-b3dd7075adcb","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5806262/95a3bfc43a/cosmic-web-3d-model-95a3bfc43a.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5826609","type":"listingItem","attributes":{"id":5826609,"title":"Phoenix Cluster","price":3.0,"description":"Description\nPhoenix Cluster. The Phoenix Cluster is like a blue bright star. The Phoenix Cluster (SPT-CL J2344-4243) is a massive, Abell class type I galaxy cluster located at its namesake, southern constellation of Phoenix. It was initially detected in 2010 during a 2,500 square degree survey of the southern sky using the Sunyaev–Zeldovich effect by the South Pole Telescope collaboration. It is one of the most massive galaxy clusters known, with the mass on the order of 2×1015 MO, and is the most luminous X-ray cluster discovered, producing more X-rays than any other known massive cluster. It is located at a comoving distance of 8.61 billion light-years (2.64 gigaparsecs) from Earth. About 42 member galaxies were identified and currently listed in the SIMBAD Astronomical Database, though the real number may be as high as 1,000 galaxies. The Phoenix Cluster was first reported in a paper by R. Williamson and colleagues during a survey by the South Pole Telescope in Antarctica, being one of the 26 galaxy clusters identified by the survey. The detection has been conducted at frequencies between 95, 150, and 220 GHz, with 14 of the galaxy clusters detected have been previously identified, while 12 – including Phoenix Cluster, being new discoveries. The would-be named Phoenix Cluster (still identified by its numerical catalogue entry SPT-CL J2344–4243) has been remarked to be having \"the largest X-ray luminosity of any cluster\" described by the survey. A bright, type-2 Seyfert galaxy has also been pronounced lying 19 arcseconds from the apparent center of the cluster that has been identified as 2MASX J23444387-4243124, which would later be named Phoenix A, the cluster's central galaxy.\n\nTexture Resolution: 3600 x 3600","imageAlt":null,"url":"https://www.cgtrader.com/3d-models/space/other/phoenix-cluster","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/JKZxoFxwH5A6fAqYKpH6DQd7/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/phoenix%20cluster.jpg","gridUrl":"https://media.cgtrader.com/variants/JKZxoFxwH5A6fAqYKpH6DQd7/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/phoenix%20cluster.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/phoenix-cluster","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5826609/dadd321641/phoenix-cluster-3d-model-dadd321641.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5866081","type":"listingItem","attributes":{"id":5866081,"title":"LL Pegasi","price":3.0,"description":"Description\nDescriptionLL Pegasi. LL Pegasi (AFGL 3068) is a Mira variable star surrounded by a pinwheel-shaped nebula, IRAS 23166+1655, thought to be a preplanetary nebula. It is a binary system that includes an extreme carbon star. The pair is hidden by the dust cloud ejected from the carbon star and is only visible in infrared light.\n\nTexture Resolution: 1280 x 1280","imageAlt":"LL Pegasi 3D model","url":"https://www.cgtrader.com/3d-models/space/other/ll-pegasi-00752081-6b5f-4fe5-b2a7-4e5fbbe5766b","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/8ow8qZkgwFrMmNyoFZKzxXFu/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/ll%20pegasi-2.jpg","gridUrl":"https://media.cgtrader.com/variants/8ow8qZkgwFrMmNyoFZKzxXFu/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/ll%20pegasi-2.webp","isAdultContent":false},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/ll-pegasi-00752081-6b5f-4fe5-b2a7-4e5fbbe5766b","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":216,"name":".jpg","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5866081/5c14591592/ll-pegasi-3d-model-5c14591592.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5843534","type":"listingItem","attributes":{"id":5843534,"title":"Phoenix Cluster","price":3.0,"description":"Description\nPhoenix Cluster. The Phoenix Cluster is like a chromosome X. The Phoenix Cluster (SPT-CL J2344-4243) is a massive, Abell class type I galaxy cluster located at its namesake, southern constellation of Phoenix. It was initially detected in 2010 during a 2,500 square degree survey of the southern sky using the Sunyaev–Zeldovich effect by the South Pole Telescope collaboration. It is one of the most massive galaxy clusters known, with the mass on the order of 2×1015 MO, and is the most luminous X-ray cluster discovered, producing more X-rays than any other known massive cluster. It is located at a comoving distance of 8.61 billion light-years (2.64 gigaparsecs) from Earth. About 42 member galaxies were identified and currently listed in the SIMBAD Astronomical Database, though the real number may be as high as 1,000 galaxies. The Phoenix Cluster was first reported in a paper by R. Williamson and colleagues during a survey by the South Pole Telescope in Antarctica, being one of the 26 galaxy clusters identified by the survey. The detection has been conducted at frequencies between 95, 150, and 220 GHz, with 14 of the galaxy clusters detected have been previously identified, while 12 – including Phoenix Cluster, being new discoveries. The would-be named Phoenix Cluster (still identified by its numerical catalogue entry SPT-CL J2344–4243) has been remarked to be having the largest X-ray luminosity of any cluster described by the survey. 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The Phoenix Cluster is like a orange bright star. The Phoenix Cluster (SPT-CL J2344-4243) is a massive, Abell class type I galaxy cluster located at its namesake, southern constellation of Phoenix. It was initially detected in 2010 during a 2,500 square degree survey of the southern sky using the Sunyaev–Zeldovich effect by the South Pole Telescope collaboration. It is one of the most massive galaxy clusters known, with the mass on the order of 2×1015 MO, and is the most luminous X-ray cluster discovered, producing more X-rays than any other known massive cluster. It is located at a comoving distance of 8.61 billion light-years (2.64 gigaparsecs) from Earth. About 42 member galaxies were identified and currently listed in the SIMBAD Astronomical Database, though the real number may be as high as 1,000 galaxies. The Phoenix Cluster was first reported in a paper by R. 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This El Gordo Cluster is like a latin N letter. El Gordo (lit. The Fat One) (ACT-CL J0102-4915 or SPT-CL J0102-4915) is the largest distant galaxy cluster observed at its distance or beyond, as of 2011. As of 2014, it held the record for being the largest distant galaxy cluster to have been discovered with a mass of slightly less than three quadrillion solar masses although later its mass was reduced to about 2.1×1015 (2.1 quadrillion) solar masses with a 10% uncertainty. It was found by NASA's Chandra X-ray Observatory, the Atacama Cosmology Telescope (funded by the National Science Foundation) and the European Southern Observatory's Very Large Telescope. This galaxy cluster, officially named as, 'ACT-CL J0102-4915', has been given a 'nickname' by the researchers as 'El Gordo', which stands for the Fat One or the Big One in Spanish. It is located more than 7 billion light-years from Earth. 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This Shapley Supercluster is like a space with stars in black and white background. The Shapley Supercluster or Shapley Concentration (SCl 124) is the largest concentration of galaxies in our nearby universe that forms a gravitationally interacting unit, thereby pulling itself together instead of expanding with the universe. It appears as a striking overdensity in the distribution of galaxies in the constellation of Centaurus. It is 650 million light-years away (z=0.046). In 1930, Harlow Shapley and his colleagues at the Harvard College Observatory started a survey of galaxies in the southern sky, using photographic plates obtained at the 24-inch Bruce telescope at Bloemfontein, South Africa. By 1932, Shapley reported the discovery of 76,000 galaxies brighter than 18th apparent magnitude in a third of the southern sky, based on galaxy counts from his plates. 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In cosmology, galaxy filaments are the largest known structures in the universe, consisting of walls of galactic superclusters. These massive, thread-like formations can commonly reach 50 to 80 megaparsecs (160 to 260 megalight-years)—with the largest found to date being the Hercules-Corona Borealis Great Wall at around 3 gigaparsecs (9.8 Gly) in length—and form the boundaries between voids. Due to the accelerating expansion of the universe, the individual clusters of gravitationally bound galaxies that make up galaxy filaments are moving away from each other at an accelerated rate; in the far future they will dissolve. 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The Clowes Campusano LQG is like a chinese hieroglyph (cna). The Clowes–Campusano LQG (CCLQG; also called LQG 3 and U1.28) is a large quasar group, consisting of 34 quasars and measuring about 2 billion light-years across. It is one of the largest known superstructures in the observable universe. It is located near the larger Huge-LQG. It was discovered by the astronomers Roger Clowes and Luis Campusano in 1991. Lying at a distance of 9.5 billion light years away, the CCLQG is a cosmic decoupling of 34 individual quasars (highly luminous active galactic nuclei powered by supermassive black holes) spanning a region roughly 2 billion light-years in length, and about 1 billion light years wide, making it one of the largest and most exotic cosmic structures known in the observable universe. It was named U1.28 because of its average redshift of 1.28, and is located in the constellation of Leo. It was also notable because it is located in the ecliptic, the line where the Sun seems to travel in the entire year. It was 1.8 billion light-years away from the Huge-LQG, a group of 73 quasars discovered in 2012. Its proximity to the Huge-LQG has attracted the attention of scientists. First, because it was very close to the Huge-LQG, the region where the two LQG's are located are different, or \"lumpy\", when compared to other regions in the universe with the same size and redshift. Second, because of their close locations, it has been suggested that the two structures are really a single structure in itself, and only connected by hidden intergalactic filament; however, no such evidence has been found.\n\nTexture Resolution: 1526 x 1526","imageAlt":"Clowes Campusano LQG 3D model","url":"https://www.cgtrader.com/3d-models/space/other/clowes-campusano-lqg","isCLDApplicable":false,"isSaleOffApplicable":false,"gaAttributes":{},"primaryImage":{"gridFallbackUrl":"https://media.cgtrader.com/variants/5Q7wSmBLBPcuYPqFYZSAVzqf/a26e47dab5f2d22c43d6c5ce4b4b46ecc30c70918878397cba1a10c1e35d7bfc/clowes%20campusano%20LQG.jpg","gridUrl":"https://media.cgtrader.com/variants/5Q7wSmBLBPcuYPqFYZSAVzqf/78add9c2f02fbd73a43ffb3970be38683c5f15eff6ca849dc78c644f4ff9ce1b/clowes%20campusano%20LQG.webp","isAdultContent":true},"modelInfo":{"modelUrl":"https://www.cgtrader.com/3d-models/space/other/clowes-campusano-lqg","isCgtVerified":false,"types":{"printReady":false,"animated":false,"pbr":false,"rigged":false,"lowPoly":false}},"metaverseFormatsList":[{"id":17,"name":".max","is_native":true},{"id":215,"name":".png","is_native":false}],"categorySlug":"space","subcategorySlug":"other","categoryTitle":"Space","subcategoryTitle":"Other","schemaImageUrl":"https://img-new.cgtrader.com/items/5823494/2ef711162a/clowes-campusano-lqg-3d-model-2ef711162a.webp","saleOffDiscount":0,"eligibleForSubscription":true,"subscriptionSubscribed":true,"subscriptionPotential":false,"subscriptionTierBand":"essentials"}},{"id":"5806785","type":"listingItem","attributes":{"id":5806785,"title":"Hercules Corona Borealis Great Wall","price":3.0,"description":"Description\n\nHercules Corona Borealis Great Wall. The Hercules Corona Borealis Great Wall is like a dragon. The Hercules–Corona Borealis Great Wall (HCB) or simply the Great Wall is a galaxy filament that is the largest known structure in the observable universe, measuring approximately 10 billion light-years in length (the observable universe is about 93 billion light-years in diameter). This massive superstructure is a region of the sky seen in the data set mapping of gamma-ray bursts (GRBs) that has been found to have a concentration of similarly distanced GRBs that is unusually higher than the expected average distribution. It was discovered in early November 2013 by a team of American and Hungarian astronomers led by István Horváth, Jon Hakkila and Zsolt Bagoly while analyzing data from the Swift Gamma-Ray Burst Mission, together with other data from ground-based telescopes. It is the largest known formation in the universe, exceeding the size of the Huge-LQG by about a factor of two. The overdensity lies at the Second, Third and Fourth Galactic Quadrants (NGQ2, NGQ3 and NGQ4) of the sky. Thus, it lies in the Northern Hemisphere, centered on the border of the constellations Draco and Hercules. The entire clustering consists of around 19 GRBs with the redshift ranges between 1.6 and 2.1. Typically, the distribution of GRBs in the universe appears in the sets of less than the 2σ distribution, or with less than two GRBs in the average data of the point-radius system.[clarification needed] One possible explanation of this concentration is the Hercules–Corona Borealis Great Wall. The wall has a mean size in excess of 2 billion to 3 billion parsecs (6 to 10 billion light-years). Such a supercluster can explain the significant distribution of GRBs because of its tie to star formation. Doubt has been placed on the existence of the structure in other studies, positing that the structure was found through biases in certain statistical tests, without considering the full effects of extinction. 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ULAS J1342+0928 is the third-most distant known quasar detected and contains the second-most distant and oldest known supermassive black hole, at a reported redshift of z = 7.54. The ULAS J1342+0928 quasar is located in the Boötes constellation. The related supermassive black hole is reported to be \"780 million times the mass of the Sun\". At its discovery, it was the most distant known quasar. In 2021 it was eclipsed by QSO J0313-1806 as the most distant quasar. On 6 December 2017, astronomers published that they had found the quasar using data from the Wide-field Infrared Survey Explorer (WISE) combined with ground-based surveys from the United Kingdom Infrared Telescope and the DECam Legacy Survey. It was spectroscopically confirmed using data from the Magellan Telescopes at Las Campanas Observatory in Chile, as well as the Large Binocular Telescope in Arizona and the Gemini North telescope in Hawaii. The related black hole of the quasar existed when the universe was about 690 million years old (about 5 percent of its currently known age of 13.80 billion years). The quasar comes from a time known as \"the epoch of reionization\", when the universe emerged from its Dark Ages. Extensive amounts of dust and gas have been detected to be released from the quasar into the interstellar medium of its host galaxy. ULAS J1342+0928 has a measured redshift of 7.54, which corresponds to a comoving distance of 29.36 billion light-years from Earth. When it was reported in 2017, it was the most distant quasar yet observed. The quasar emitted the light observed on Earth today less than 690 million years after the Big Bang, about 13.1 billion years ago. The quasar's luminosity is estimated at 4×1013 solar luminosities. This energy output is generated by a supermassive black hole estimated at 7.8×108 solar masses. According to lead astronomer Bañados, \"This particular quasar is so bright that it will become a gold mine for follow-up studies and will be a crucial laboratory to study the early universe.\" The light from ULAS J1342+0928 was emitted before the end of the theoretically predicted transition of the intergalactic medium from an electrically neutral to an ionized state (the epoch of reionization). Quasars may have been an important energy source in this process, which marked the end of the cosmic Dark Ages, so observing a quasar from before the transition is of major interest to theoreticians. Because of their high ultraviolet luminosity, quasars also are some of the best sources for studying the reionization process. 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LL Pegasi (AFGL 3068) is a Mira variable star surrounded by a pinwheel-shaped nebula, IRAS 23166+1655, thought to be a preplanetary nebula. It is a binary system that includes an extreme carbon star. 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