Free Astronomy Magazine March-April 2026 ARABIC VERSION

MARCH-APRIL2026 42 ASTROPUBLISHING sistsoftheGeminiNorthtelescope inHawai’iandtheGeminiSouthtel- escopeinChile.Itispartlyfundedby NSF and operated by NSF NOIRLab. “The ability to rapidly point the Blanco and Gemini telescopes on short notice is crucial to capturing transienteventssuchasgamma-ray bursts,” saysCarney. “Withoutthis ability,wewouldbelimitedinour understanding of distant events in the dynamic night sky.” Theteamusedasuiteofinstruments for their investigation: the NEW-FIRM wide-field infrared imager and the 570-megapixel DOE-fabricated Dark Energy Camera (DECam), both mounted on the Blanco telescope, and the Gemini Multi-Object Spec- trographs (GMOS) mounted onGemini North and Gemini South. Analysis of the observations re-vealed that GRB 250702B could not beseeninvisiblelight,partlydueto interstellar dust in our own Milky WayGalaxy,butmoresoduetodust in the GRB’s host galaxy. In fact, Gemini North, which provided the only close-to-visible-wavelength de- tectionofthehostgalaxy,required nearly two hours of observations to capture the faint signal from beneath the swaths of dust. Car- ney and his team then combined these data with new observations taken with the Keck I Telescope at W. M. Keck Observatory, the Magellan Baade Telescope, and the Fraunhofer Telescope at Wen- delstein Observatory, as well as publicly available data from VLT, NASA’s Hubble Space Telescope (HST), and X-ray and radio observatories. They then compared this robust dataset with theoreti- calmodels,whichareframeworksthatexplain thebehavior ofastronom- icalphenom- ena. Models can be used to make pre- dictionsthatcanthenbetestedagainst observationaldatatorefinescientists’ understanding. The team’s analysis established that the initial gamma-ray signal likely camefrom a narrow, high-speed jet of ma-terial crashing into the surrounding ma-terial, known as a relativistic jet. The analysisalsohelpedcharacterizetheen- vironment around the GRB and the host galaxy overall. They found that there isa large amount of dust surrounding the location of the burst, and that the host galaxy is extremely massive comparedto most GRB hosts. The data support a picture in which the GRB source resides in a dense, dusty environment, possiblyathicklaneofdustpresentinthehos t https://noirlab.edu/public/videos/noirlab2531a/?nocache=true& ﻣﺠﻠﺔ FreeAstronomy ﺎﻟﻌﺮ ﺔ 42 ﻈﻬــﺮ ﻋﻠـــﻰ اﻟ ﻤـــ ـ اﻟــ : ـــﺎﻟﻤﺠﺮة اﻟﻤﻀـــ ﻔﺔ ﺤﻘﻞ اﻟﻨ ﻤـــﻲ اﻟﻤﺤــ ﻂ ﻻﻧﻔﺠــﺎر أﺷــﻌﺔ ﻏﺎﻣــﺎ GRB 250702B - أﻃــﻮل اﻧﻔﺠــﺎر أﺷــﻌﺔ ﻏﺎﻣــﺎ رﺻـــﺪﻩ ﻋﻠﻤـــﺎء اﻟﻔﻠـــﻚ ﻋﻠـــﻰ اﻹ . ﻃـــﻼق ﺘﻀـــﻤﻦ ﻫـــﺬا اﻟـــ ـ ﺤﻘﻞ رﺻـــﺪ اً ﻣـــﻦ ــ ﺗﻠﺴـ ﻮبﺟ ﻤ ﻧـﻮر وﻫـﻮ أﺣـﺪ ﺗﻠﺴـ ﻮﺑﻲ اﻟــﺪوﻟﻲ ـ ﻣﺮﺻـﺪ ﺟ ﻤ ﺗﻤﻮﻟــﮫ اﻟـﺬ اﻟﻤﺆﺳﺴـ ــﺔ واﻟـ ــﺔ ﻟﻠﻌﻠـﻮم اﻷﻣﺮ ﻜ ﺔ اﻟﻮﻃﻨ ﺬ ﺸـﻐﻠﮫ ﻣﺨﺘ ﻧﻮﻳﺮﻻب ـﺎﻣ ا اﻟﻄﺎﻗـﺔ اﻟﻤﻈﻠﻤـﺔ اﻟﻤﺼـﻨﻌﺔ ﻣـﻦ ﺎﻹﺿﺎﻓﺔ إﻟﻰ ــﺔ اﻟﻤﺜ ﺘـــﺔ ﻋﻠــﻰ ﺗﻠﺴـــ ﻮب ﻓ ﻜﺘــﻮر ﻗﺒــﻞ وزارة اﻟﻄﺎﻗـــﺔ اﻷﻣﺮ ﻜ ـــﻮ ﻼﻧ ﻘﻄـﺮ 4 ــﺔ ﻟﻠﻌﻠــﻮم ﻓــﻲﻣﺮﺻــﺪ ﺳــ و أﻣﺘــﺎراﻟﺘــﺎﺑﻊ ﻟﻠﻤﺆﺳﺴــﺔ اﻟﻮﻃﻨ ﺗﻮﻟﻮﻟﻮ وﻫﻮ ﺑﺮﺎﻣﺞ ﺗﺎﺑﻊ ﻟﻤﺨﺘ أﺑﺤﺎث ﻋﻠﻢ اﻟﻔﻠﻚ اﻟ ﺼﺮيواﻷﺷﻌﺔ ﺗﺤـــــــﺖ اﻟـــــــ ـ ) ﻤﺮاء ﻧـــــــﻮﻳﺮﻻب ( . ﻋﻠــــــــﻰ اﻟ ﺴـــــــﺎر : ﺻـــــــﻮرة ﻣﻘﺮ ـــــــﺔ ﻟﻠﻤﺠــــــــﺮة اﻟﻤﻀ ﻔﺔ اﻟﺘﻘ ﺎﻄﻬ ﺗﻠﺴ ﻮبﺟ ﻤ ﻧﻮر . ﻫﺬﻩ اﻟﺼـﻮرة ﻫـ ﻲ ﻧﺘﻴﺠـﺔ ﻣﻦ اﻟﺮﺻـﺪ أﻛ ﻣﻦﺳﺎﻋﺘ ـﺪو اﻟﻤﺠـﺮة اﻟﻤﻀـ ﻔﺔ ﺧﺎﻓﺘـﺔ وﻣـﻊ ذﻟـﻚ ﺗ ﻟﻠﻐﺎ ﺔ ﺴ ﺐ اﻟ ﻤ ﺔ اﻟﻜﺒ ة ﻣﻦ اﻟﻐ ﺎراﻟﻤﺤ ﻂ ﺑﻬﺎ . [International Gemini Observatory /CTIO/NOIRLab /DOE/NSF/AURA. Image processing: J. Miller (International Gemini Observatory /NSFNOIRLab), M. Zamani & D. de Martin (NSF NOIRLab)] ﻳﻮﺿﺢ ﻫﺬا اﻟﺮﺳﻢ اﻟﺘﻮﺿﻴﺤﻲ ﻋﻤ ﺣﺪثﻓﻲ ﻠ ﺔ ﺗﺤﺪ ﺪ ﻣﻮﻗﻊ اﻻﻧﻔﺠﺎراﻟﺬ 2 ﻳﻮﻟﻴﻮوﻣﺠﺮﮫ اﻟﻤﻀ ﻔﺔ . وﻗــﺪ ﺳـــﺎﻋﺪت ﺗﻠﺴـــ ﻮ ﺎت ـــﻒ ﻣﺘﻌــﺪدة ﻓـــﻲ اﻟﻔﻀـــﺎء وﻋﻠــﻰ اﻷرض ﺗ ﻤـــﻊ اﻟﻀـــﻮء ﻋــ اﻟﻄ اﻟﻔﻠﻜﻴـــ ﻓـــﻲ ﺗﺤﺪ ﺪ اﻟﻤﺼﺪر . [NASA’s Goddard Space Flight Center an A. Mellinger, CMU] - ﻣﺎﺭﺱ ﺃﺑﺮﻳﻞ 2 0 2 6 ﻳﻤﻮﱠ ل ﻫﺬا ا ﴩو ع ﺟﺰﺋﻴﺎً ﻣﻦ ﻗِﺒَﻞ ﻣﺆﺳﺴﺔ اﻟﻌﻠﻮم اﻟﻮﻃﻨﻴﺔ اﻷﻣﺮﻳﻜﻴ ﺔ وﻳﺸﻐّ ﻠﻪ ﻣﺨﺘـﱪ ﻧﻮﻳﺮﻻب . ﻳﻘـﻮل ﻛـﺎرﻧﻲ " : إن اﻟﻘـﺪرة ﻋـﲆ ﺗﻮﺟﻴﻪ ﺗﻠﺴﻜﻮﺑﻲ ﺑﻼﻧﻜﻮ وﺟﻴﻤﻴﻨﻲ ﺑﴪـﻋﺔ وﺑﺈﺷﻌﺎر ﻗﺼ أﻣﺮ ﺑـﺎﻟﻎ اﻷﻫﻤﻴـﺔ ﻟﺮﺻـﺪ اﻷﺣﺪاث اﻟﻌﺎﺑﺮة ﻣﺜﻞ اﻧﻔﺠﺎرات أﺷﻌﺔ ﻏﺎﻣﺎ و ﺑﺪون ﻫﺬه اﻟﻘﺪرة ﺳﺘﻜﻮن ﻗﺪرﺗﻨﺎ ﻋﲆ ﻓﻬﻢ ودراﺳﺔ اﻷﺣﺪاث اﻟﺒﻌﻴـﺪة ﰲ ﺳـﻤﺎء اﻟﻠﻴـﻞ اﻟﺪﻳﻨﺎﻣﻴﻜﻴﺔ ﻣﺤﺪودة ﻟﻘﺪ ". اﺳﺘﺨﺪم اﻟﻔﺮﻳﻖ ﻣﺠﻤﻮﻋﺔ ﻣﻦ اﻷﺟﻬﺰة ﻹﺟﺮاء ﺑﺤﺜﻬﻢ : ﺟﻬﺎز اﻟﺘﺼﻮﻳﺮ ﺑﺎﻷﺷـﻌﺔ ﺗﺤـﺖ اﻟﺤﻤـﺮاء واﺳـﻊ ا ﺠ ـﺎل ) ﻧﻴ ـﻮﻓ م ( ﺑﺎﻻﺿـﺎﻓﺔ اﱃ ﻛ ـﺎﻣ ا اﻟﻄﺎﻗﺔ ا ﻈﻠﻤﺔ ) دي ﻛﺎم ( ا ﺼﻨﻌﺔ ﻣﻦ ﻗِﺒَﻞ وزارة اﻟﻄﺎﻗ ــ ﺔ اﻷﻣﺮﻳﻜﻴ ــﺔ ﺑﺪﻗ ــﺔ 570 ﻣﻴﺠﺎﺑﻜﺴﻞ وﻛﻼﻫﻤﺎ ﻣﺜﺒﺖ ﻋـﲆ ﺗﻠﺴـﻜﻮب ﺑﻼﻧﻜﻮ وﻣﻄﻴﺎف ﺟﻴﻤﻴﻨﻲ ﻣﺘﻌﺪد اﻷﺟﺴـﺎم ) ( ﺟﻲ ﻣﻮس ا ﺜﺒﺖ ﻋﲆ ﺗﻠﺴﻜﻮﺑﻲ ﺟﻴﻤﻴﻨﻲ ﻧﻮرث وﺟﻴﻤﻴﻨﻲ . ﺳﺎوث ﻟﻘﺪ ﻛﺸﻒ ﺗﺤﻠﻴـﻞ اﻷرﺻـﺎد أن اﻧﻔﺠـﺎر أﺷـﻌﺔ ﻏﺎﻣـﺎ GRB 250702B ﻟﻢ ﻳﻜﻦ ﻣﺮﺋﻴﺎً وﻳﻌﻮد ذﻟﻚ ﺟﺰﺋﻴ ﺎً إﱃ اﻟﻐﺒﺎر ﺑ اﻟﻨﺠﻮم ﰲ ﻣﺠ ﺮﺗﻨﺎ درب اﻟﺘﺒﺎﻧﺔ وإﱃ ﺣﺪ ﻛﺒ إﱃ اﻟﻐﺒﺎر ﰲ ا ﺠـﺮة ا ﻀـﻴ ﻔﺔ ﻻﻧﻔﺠﺎر أﺷﻌﺔ ﻏﺎﻣﺎ . ﰲ اﻟﻮاﻗﻊ اﺣﺘﺎج ﻣﺮﺻﺪ ﺟﻴﻤﻴﻨﻲ ﻧﻮرث اﻟﺬي وﻓّﺮ اﻟﻜﺸـﻒ اﻟﻮﺣﻴـﺪ اﻟﻘﺮﻳﺐ ﻣﻦ اﻟﻄ ﻮل ا ﻮﺟﻲ ا ﺮﺋـﻲ ﻟﻠﻤﺠـﺮة ا ﻀﻴﻔﺔ إﱃ ﻣـﺎ ﻳﻘـﺮب ﻣـﻦ ﺳـﺎﻋﺘ ﻣـﻦ اﻹﺷﺎرة اﻟﺨﺎﻓﺘﺔ ﻣﻦ ﺗﺤﺖ ﻃﺒﻘـﺎت اﻟﻐﺒـﺎر . ﺛـﻢ ﻗـﺎم ﻛـﺎرﻧﻲ وﻓﺮﻳﻘﻪ ﺑـﺪﻣﺞ ﻫـﺬه اﻟﺒﻴﺎﻧـﺎت ﻣـﻊ أرﺻـﺎد ﺟﺪﻳـﺪة أُﺟﺮﻳـﺖ ﺑﺎﺳـﺘﺨﺪام ﺗﻠﺴـﻜﻮب ﻛﻴـﻚ اﻷول ﰲ ﻣﺮﺻـﺪ دﺑﻠﻴـﻮ إم ﻛﻴـﻚ وﺗﻠﺴـﻜﻮب ﻣـﺎﺟﻼن ﺑـﺎد وﺗﻠﺴـﻜﻮ ب ﻓﺮاوﻧﻬـﻮﻓﺮ ﰲ ﻣﺮﺻـﺪ ﻓﻴﻨﺪﻟﺸﺘﺎﻳﻦ ﺑﺎﻹﺿـﺎﻓﺔ إﱃ اﻟ ﺒﻴﺎﻧـﺎت ا ﺘﺎﺣـﺔ ﻟﻠﺠﻤﻬـﻮر ﻣـﻦ اﻟ ﺘﻠﺴﻜﻮب اﻟﻜﺒ ﺟﺪاً وﺗﻠﺴﻜﻮب ﻫﺎﺑﻞ اﻟﻔﻀﺎﺋﻲ اﻟﺘﺎﺑﻊ ﻟﻨﺎﺳﺎ وﻣﺮاﺻﺪ اﻷﺷﻌﺔ اﻟﺴﻴﻨﻴﺔ واﻟﺮادﻳﻮ . ﻳﺔ ﺛﻢ ﻗﺎرﻧﻮا ﻫﺬه ا ﺠﻤﻮﻋﺔ اﻟﻘﻮ ﻳﺔ ﻣﻦ اﻟﺒﻴﺎﻧﺎت ﺑﺎﻟﻨﻤﺎذج اﻟﻨﻈﺮﻳـﺔ وﻫـﻲ أﻃـﺮ ﺗـ ﴩح ـ ﺳﻠﻮك اﻟﻈﻮاﻫﺮ اﻟﻔﻠﻜﻴـﺔ . ﻳﻤﻜـﻦ اﺳـﺘﺨﺪام اﻟﻨﻤـﺎذج ﻟﻠﺘﻨﺒـﺆ ﺑﺎﻟﻈﻮاﻫﺮ اﻟﻔﻠﻜﻴﺔ واﻟﺘﻲ ﻳﻤﻜـﻦ اﺧﺘﺒﺎرﻫـﺎ ﻣﻘﺎﺑـﻞ اﻟﺒﻴﺎﻧـﺎت اﻟﺮﺻﺪﻳﺔ ــــــ ﻟﺘﺤﺴـ ﻓﻬ ـﻢ اﻟﻌﻠﻤ ـﺎء . أﺛﺒ ـﺖ ﻫﻨــﺎك ﻛﻤﻴــﺔ ﺗﺤﻠﻴﻞ اﻟﻔﺮﻳﻖ أن إﺷﺎرة أﺷﻌﺔ ﻏﺎﻣﺎ اﻷوﻟﻴﺔ رﺑﻤـﺎ ﺟﺎءت ﻣﻦ ﻧﻔﺎﺛﺔ ﺿﻴﻘﺔ وﻋﺎﻟﻴﺔ اﻟﴪﻋﺔ ﻣﻦ ا ﺎدة اﺻـﻄﺪﻣﺖ ﺑﺎ ـﺎدة ا ﺤﻴﻄـﺔ وا ﻌﺮوﻓـﺔ ﺑﺎﺳـﻢ اﻟﻨﻔﺎﺛﺔ اﻟﻨﺴﺒﻴﺔ . ﻛﻤﺎ ﺳـﺎﻋﺪ اﻟﺘﺤﻠﻴـﻞ ﰲ ﺗﺤﺪﻳـﺪ ﺧﺼﺎﺋﺺ اﻟﺒﻴﺌﺔ ا ﺤﻴﻄﺔ ﺑﺎﻧﻔﺠـﺎر أﺷـﻌ ﺔ ﻏﺎﻣـﺎ وا ﺠﺮة ا ﻀﻴﻔﺔ ووﺟﺪوا أن ﻫﻨ ﺎك ﻛﻤﻴﺔ ﻛﺒ ة ﻣﻦ اﻟﻐﺒﺎر ﺗﺤﻴﻂ ﺑﻤﻮﻗﻊ اﻻﻧﻔﺠﺎر وأن ا ﺠﺮة ا ﻀﻴﻔﺔ ﺿﺨﻤﺔ ﻟﻠﻐﺎﻳﺔ ﻣﻘﺎرﻧﺔ ﺑﻤﻌﻈﻢ ا ﺠﺮات ا ﻀـﻴﻔﺔ ﻻﻧﻔﺠـﺎرات أﺷـﻌﺔ ﻏﺎﻣـﺎ . ﻛﻤـﺎ ﺗﺸـ اﻟﻨﻤـﺎذج اﻟﻌﺪدﻳﺔ إﱃ ﺗﻔﺎﻋﻞ ﻣﻌﻘﺪ ﺑـ اﻟﺼـﺪﻣﺔ اﻷﻣﺎﻣﻴـﺔ واﻟﺮﻳﺎح اﻟﻨﺠﻤﻴـﺔ اﻟﺴـﺎﺑﻘﺔ ﻟﻼﻧﻔﺠـﺎر اﻟﻌﻨﻴﻔـﺔ . ﺗﺪﻋﻢ اﻟﺒﻴﺎﻧﺎت ﺻﻮرة ﻣﻔﺎدﻫﺎ أن ﻣﺼﺪر اﻧﻔﺠـﺎر أﺷﻌﺔ ﻏﺎﻣﺎ ﻳﻘﻊ ﰲ ﺑﻴﺌـﺔ ﻛﺜﻴﻔـﺔ ﻣﻠﻴﺌـﺔ ﺑﺎﻟﻐﺒـﺎر ورﺑﻤﺎ ﻳﻜﻮن ﻋﺒﺎرة ﻋﻦ ﴍﻳﻂ ﺳﻤﻴﻚ ﻣﻦ اﻟﻐﺒـﺎر ﻣﻮﺟﻮد ﰲ ا ﺠﺮة ا ﻀﻴﻔﺔ ﻋﲆ ﻃﻮل ﺧﻂ اﻟﺮؤﻳـﺔ ﺑ اﻷرض وﻣﺼﺪر اﻧﻔﺠﺎر أﺷﻌﺔ ﻏﺎﻣﺎ .