Iteleskopu yeFermi yenze uphononongo olucocekileyo lokukhutshwa kwe-γ-ray kumbindi womnyele wethu wekhaya obonakale ungesosangqa kwaye usicaba. Ebizwa ngokuba yi-Galactic Centre Excess (GCE), oku kugqithiswa kwe-γ-ray kukusayinwa kwezinto ezimnyama ezivela njengemveliso yokuzibhubhisa ngokubuthathaka kwamasuntswana amakhulu (WIMPs), umviwa obumnyama. Nangona kunjalo, i-γ-ray engaphezulu ebonwe kwiziko le-galactic inokuthi ibe ngenxa ye-millisecond pulsars (MSPs). Ukuza kuthi ga ngoku, kwakubanjwe ukuba i-morphology ye-GCE ngenxa yezinto ezimnyama (DM) iya kuba yingqukuva. Uphononongo lwakutsha nje lokulinganisa lubonisa ukuba i-gamma-ray morphology ngenxa ye-DM inokuba yinto engaqhelekanga kwaye yacaba. Oku kuthetha ukuba zombini intshabalalo ye-dark matter (DM) kunye ne-millisecond pulsars (MSPs) ye-GCE eqatshelweyo zinokwenzeka ngokulinganayo. Imitha ye-gamma eveliswe ekutshatyalalisweni kwezinto ezimnyama (DM) iya kuba nenqanaba eliphezulu kakhulu lamandla malunga ne-0.1 tera-electron-volts (TeV). Iiteleskopu eziqhelekileyo ze-gamma-ray azikwazi ukubona ngokuthe ngqo ezi fotoni zinamandla amakhulu. Ke ngoko, ukuqinisekiswa komcimbi omnyama (DM) imodeli yeGalactic Centre Excess (GCE) iya kuba nokwenzeka ekugqityweni kwezifundo ngamaziko e-tera γ-ray afana neCherenkov Telescope Array Observatory (CTAO) kunye ne-Southern Wide-field Gamma-ray Observatory (SWGO).
Ibali lezinto ezimnyama laqala ngo-1933 xa uFritz Zwicky waphawula ukuba iminyele ehamba ngokukhawuleza kwiQela leComa ayinakubambana kwaye ihlale izinzile ngaphandle kobukho bomcimbi owongezelelweyo ongabonakaliyo ngandlel’ ithile kodwa ube nempembelelo eyaneleyo yomxhuzulane ukunqanda iminyele ukuba ingaqhekeki. Wayila ibinzana elithi “ubumnyama” ukubhekisela kwizinto ezingabonakaliyo. Ngeminyaka yoo-1960, uVera Rubin wenza igalelo elikhulu ekuqondeni kwethu umba omnyama. Uye waphawula ukuba iinkwenkwezi ezisemaphethelweni angaphandle eAndromeda kunye neminye iminyele yayijikeleza ngesantya esingesantya seenkwenkwezi esisingise embindini. Ngesimbuku esinikiweyo sazo zonke izinto ezijongiweyo, umnyele bekufanele ukuba ubhabhe ngokwahlukeneyo nto leyo ebangela ubukho benye into eyongezelelekileyo engabonakaliyo egcina iminyele ikunye ize ibangele ukuba ijikeleze ngesantya esiphezulu. Imilinganiselo yakhe yeegophe ezijikelezayo kumnyele weAndromeda ibonelele ngowona bungqina bakuqala bezinto ezimnyama.
Ngoku siyazi ukuba into emnyama ayidibani nokukhanya okanye amandla ombane. Ayifunxi, ayibonakalisi okanye ikhuphe ukukhanya okanye naziphi na ezinye iimitha zemitha ye-electromagnetic kwaye ayibonakali kungoko ibizwa ngokuba bubumnyama. Kodwa idibanisa ngokuxhuzulana kwaye ibe nefuthe lomxhuzulane kumbandela oqhelekileyo, kwaye le yindlela ubukho bayo esithubeni ngokuqhelekileyo buchazwa ngayo. Iminyele ibambene ngokulinganayo ngenxa yempembelelo yomxhuzulane yento emnyama eyenza ukuya kuthi ga kwi-26.8% yobunzima bomthamo wamandla wendalo iphela ngelixa indalo iphela enokubonwayo kuquka yonke imiba eqhelekileyo yebhayoni esibunjwe ngayo senza kuphela i-4.9% yendalo iphela. I-68.3% eseleyo yesiqulatho samandla obunzima bendalo iphela ngamandla amnyama.
Akwaziwa ukuba yintoni kanye kanye into emnyama. Akukho masuntswana asisiseko kwi Model Model zineempawu ezifunekayo ukuze zibe mnyama. Mhlawumbi, i-hypothetical "supersymmetric particles" ezingamaqabane kwiinqununu kwiModeli esemgangathweni yenza into emnyama. Mhlawumbi kukho ihlabathi elifanayo lezinto ezimnyama. I-WIMPs (I-Weakly Interacting Massive Particles), i-axion, okanye i-neutrinos engabonakaliyo ngamasuntswana acingelwayo angaphaya koMgangatho oMgangatho okhokela abaviwa. Nangona kunjalo, akukho mpumelelo ifunyenweyo okwangoku ekufumaneni amasuntswana anjalo.
Kukho iiprojekthi ezininzi (ezifana ne Uvavanyo lwe-XENON, Iprojekthi ye-DarkSide-20k, EURECA Rxperiment, kwaye I-RES-NOVA) kungoku nje kuyaqhubeka ukuchongwa ngokuthe ngqo kwamasuntswana ezinto ezimnyama. Ezi ubukhulu becala zizichongi zerhasi ezinolwelo okanye izixhobo ze-cryogenic eziyilelwe ukukhangela imiqondiso ebuthathaka ekudibaneni kwamasuntswana obumnyama. Nangona kunjalo, ngaphandle kweendlela ezininzi zenoveli, akukho projekthi ikwazile ukubona ngokuthe ngqo nayiphi na into emnyama okwangoku.
Ngobungqina obungathanga ngqo bomcimbi omnyama, umntu unokukhangela iziphumo zomxhuzulane womcimbi omnyama, njengoko uFritz Zwicky kunye noVera Rubin benzayo ukufumana umba omnyama ngokufunda indlela igalaksi ebanjwa ngayo kunye nangona inezantya eziphakamileyo ngokungafaniyo kumcimbi oqhelekileyo ojongweyo. Ifuthe lomxhuzulane lelensing (ukugoba kokukhanya) kunye neziphumo zokuhamba kweenkwenkwezi esithubeni nako kunokubonelela ngobungqina obungathanga ngqo bobukho bezinto ezimnyama. Ukongeza, iimveliso zembubhiso (ezifana ne-gamma-ray, i-neutrinos, kunye ne-cosmic ray) zidalwe xa amasuntswana ezinto ezimnyama engqubana kunye esithubeni zinokubonisa ubukho bento emnyama. Enye indawo apho kwaqikelelwa ukuba izinto ezimnyama zaqikelelwa ngokusekelwe kwimveliso yokutshatyalaliswa kwamasuntswana amnyama ngumbindi wekhaya lethu kumnyele iMilky Way.
Ukufunyanwa kwezinto ezimnyama kumbindi womnyele wekhaya lethu iMilky Way
Bekukho imiqondiso yokukhanya okugqithisileyo okuphakathi kwe microwave kumbindi we Milky Way (MW). Ukukhanya okugqithisileyo kwacetywa ukuba kube ngenxa yokukhutshwa kwe-synchrotron kwii-electron ezihambelanayo kunye neepositrons eziveliswe kwi-WIMP yokutshatyalaliswa kwezinto ezimnyama, kungoko isignali eyandisiweyo ye-γ-ray kuluhlu lwamandla ukuya kumakhulu ambalwa e-GeV yaqikelelwa kwangaphambili. Emva koko, i-Fermi-Large Area Telescope (LAT) yafumanisa i-γ-ray yesignali echongwe njenge-Galactic Centre Excess (GCE). Kungekudala, kwaqondwa ukuba i-Galactic Centre Excess (GCE) inokuba nayo ngenxa yeenkwenkwezi ze-neutron ezindala (i-millisecond pulsars). Kwakucingelwa ukuba i-morphology ye-GCE yayiza kubaluleka - i-GCE ye-symmetrical spherical-shaped spherical-shaped GCE yayiza kubonisa ukukhutshwa kwe-γ-ray ekutshatyalalisweni kwezinto ezimnyama (DM) ngelixa i-morphology ethe tyaba ye-GCE iya kuba nesiphakamiso se-γ-ray ephuma kwi-millisecond pulsars (MSP).
Uqwalaselo olubanzi lweziko legalaksi iMilky Way yiFermi-Large Area Telescope (LAT) ibonise iasphericity ecaba. Ngokuqhelekileyo, umntu anganxulumanisa i-asphericity ebonwayo kwiinkwenkwezi ezindala (MSP) nangona kunjalo uphononongo lwakutsha nje olupapashwe nge-16 ka-Okthobha ka-2025 lugqibe ekubeni i-GCE morphologies eqikelelwe ziinkwenkwezi ezindala (MSP) kunye neemodeli zokubhangisa izinto ezimnyama (DM) azibonakali.
Ukufunda ukuhanjiswa komcimbi omnyama, abaphandi baqhube ukulinganisa i-morphology ye-MW (Milky Way) efana neminyele. Bafumanise ukuba i-halos emnyama ejikeleze iminyele kunye nakwimimandla esembindini yeminyele yayingafane ibengqukuva njengoko kucingelwa kwimodeli ye-anisotropic. Endaweni yoko, uhlalutyo lubonise intelekelelo yoxinano lwemiba emnyama kuyo yonke iminyele. Olu sasazo lwe-non-axisymmetric dark matter (DM) lwaboniswa nangokudityaniswa kwembali yomnyele iMilky Way kwiminyaka eyibhiliyoni yokuqala emithathu kwimbali yendalo iphela. I-morphology eqatshelweyo ye-GCE ithe tyaba phezu kommandla osembindini, ocingelwa ngokubanzi ukuba luphawu losasazo lwenkwenkwezi endala (MSP). Uphononongo olutsha luye lwabonisa ukuba umcimbi omnyama (DM) uvelisa ukuhanjiswa kwebhokisi efanayo. Ngaloo ndlela, ukutshatyalaliswa kwezinto ezimnyama (DM) kunye ne-millisecond pulsars (MSPs) iingqikelelo ze-GCE eziqatshelweyo zinokwenzeka ngokulinganayo.
Nokuba i-GCE eqatshelweyo ibangelwa yinto emnyama (DM) okanye ngenxa ye-millisecond pulsars (MSPs) iya kwaziwa xa ii-γ-ray observatories ezifana ne-Cherenkov Telescope Array Observatory (CTAO) kunye ne-Southern Wide-field Gamma-ray Observatory (SWGO) zigqibezela izifundo zazo zemitha ye-tera-gamma kwixa elizayo. Imitha ye-gamma eveliswe njengemveliso yokubhangisa yento emnyama (DM) kwiziko le-galactic iya kuba ziifotoni ze-ultra-high-energy ezinezinga eliphezulu kakhulu lamandla elimalunga ne-0.1 tera-electron-volts (TeV). Iiteleskopu eziqhelekileyo zegamma-ray azikwazi ukubona ngokuthe ngqo ezi fotoni zinamandla amakhulu. Imitha ye-Tera-gamma iya kuba yinto ekujoliswe kuyo ebalulekileyo kwixa elizayo i-γ-reyi yokuphonononga njengeCTAO kunye ne-SWGO.
Olu phononongo linyathelo eliya phambili ekubhaqweni kwezinto ezimnyama esithubeni ngeemveliso zayo zokutshabalalisa nangona kunjalo ubukho bezinto ezimnyama kwiziko le-galactic buya kufuna ukuqinisekiswa yi-ultra-high energy γ-ray observatories ezifana ne-CTAO okanye i-SWGO kwixesha elizayo. Inkqubela phambili ebaluleke ngakumbi kwinzululwazi yomba omnyama inokuba kubhaqwa ngqo naliphi na isuntswana leDM.
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Iingxelo:
- Hochberg, Y., Kahn, YF, Leane, RK et al. Iindlela ezintsha zokubona into emnyama. UNat Rev Phys 4, 637–641 (2022). https://doi.org/10.1038/s42254-022-00509-4
- I-Misiaszeka M. kunye noRossib N. 2024. Ukufunyanwa ngokuthe ngqo kwezinto ezimnyama: ukuphononongwa okubalulekileyo. Symmetry 2024, 16(2), 201; DOI: https://doi.org/10.3390/sym16020201
- Instituto de Física Corpuscular. Ukukhangela into emnyama: indlela entsha yokufumanisa into engabonakaliyo. 22 Agasti 2025. Iyafumaneka e https://webific.ific.uv.es/web/en/content/search-dark-matter-new-approach-detecting-invisible
- Muru MM, et al 2025. Fermi-LAT Galactic Centre Excess Morphology of Dark Matter in Simulations of the Milky Way Galaxy. Iileta zokuphonononga ngokwasemzimbeni. 135, 161005. Ipapashwe nge-16 kaOktobha 2025. DOI: https://doi.org/10.1103/g9qz-h8wd . Ushicilelo lwangaphambili kwi-arXiv. Ingeniswe nge-8 ka-Agasti 2025. DOI: https://doi.org/10.48550/arXiv.2508.06314
- IYunivesithi yaseJohns Hopkins. Iindaba - Ukukhanya okungaqondakaliyo kwindlela yobisi kunokuba bubungqina bezinto ezimnyama. Ithunyelwe nge-16 ka-Okthobha 2025. Iyafumaneka e https://hub.jhu.edu/2025/10/16/mysterious-glow-in-milky-way-dark-matter/
- Leibniz Institute for Astrophysics. Iindaba - I-Milky Way ibonisa ukugqithisa kwe-gamma ray ngenxa yokutshatyalaliswa kwezinto ezimnyama. Ithunyelwe nge-17 ka-Okthobha 2025. Iyafumaneka e https://www.aip.de/en/news/milkyway-gammaray-darkmatter-annihilation/
- I-Fermi Gamma-ray Space Telescope. Ifumaneka e https://science.nasa.gov/mission/fermi/
- ICherenkov Telescope Array Observatory (CTAO). Ifumaneka e https://www.ctao.org/emission-to-discovery/science/
- I-Southern Wide-field Gamma-ray Observatory (SWGO). Ifumaneka e https://www.swgo.org/SWGOWiki/doku.php?id=swgo_rel_pub
- Tartu Observatory. Icala elimnyama leNdalo yonke. Ifumaneka e https://kosmos.ut.ee/en/dark-side-of-the-universe
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, this excess γ-ray is a possible signature of dark matter arising as a product of self-annihilations of weakly interacting massive particles (WIMPs), a dark matter particle candidate. However, the excess γ-ray observed at the galactic centre may also be due to old millisecond pulsars (MSPs). Hitherto, it was held that the morphology GCE due to dark matter (DM) would be spherical. A recent simulation study reveals that gamma-ray morphology due to DM could be significantly nonspherical and flattened. This means both dark matter (DM) annihilations and millisecond pulsars (MSPs) hypotheses for the observed GCE are equally possible. The gamma rays produced in the annihilation of dark matter (DM) would have an extremely high energy level of approximately 0.1 tera-electron-volts (TeV). The standard gamma-ray telescopes cannot detect these high-energy photons directly. Hence, confirmation of dark matter (DM) model of Galactic Centre Excess (GCE) would be possible upon completion of studies by the tera γ-ray observatories like CTAO and SWGO.){kind=link}