Hubble ve James Webb uzay teleskoplar\u0131, D\u00fcnya\u2019dan yakla\u015f\u0131k 7.500 \u0131\u015f\u0131k y\u0131l\u0131 uzakl\u0131kta bulunan Carina Bulutsusu\u2019nun bir b\u00f6l\u00fcm\u00fcn\u00fc ayr\u0131nt\u0131l\u0131 bi\u00e7imde g\u00f6zlemledi. Gaz ve tozdan olu\u015fan bu yap\u0131, s\u0131rt\u0131n\u0131 d\u00f6nm\u00fc\u015f ve ba\u015f\u0131n\u0131 sa\u011fa \u00e7evirmi\u015f bir kedinin siluetini and\u0131rd\u0131\u011f\u0131 i\u00e7in \u201cKedi Ba\u015f\u0131 Bulutsusu\u201d olarak an\u0131l\u0131yor. Bu ad, b\u00f6lgenin resmi bir astronomik s\u0131n\u0131fland\u0131rmas\u0131ndan \u00e7ok, g\u00f6r\u00fcnt\u00fclerde fark edilen bi\u00e7imi tarif ediyor.<\/p>\n
\u0130ki teleskop ayn\u0131 b\u00f6lgeyi farkl\u0131 \u0131\u015f\u0131k t\u00fcrlerinde inceleyerek birbirini tamamlayan g\u00f6r\u00fcnt\u00fcler elde etti. Hubble\u2019\u0131n g\u00f6r\u00fcn\u00fcr \u0131\u015f\u0131k g\u00f6zlemleri koyu renkli toz s\u00fctununu ve ayd\u0131nl\u0131k gaz s\u0131n\u0131rlar\u0131n\u0131 belirginle\u015ftirirken, James Webb\u2019in k\u0131z\u0131l\u00f6tesi g\u00f6zlemleri tozun arkas\u0131ndaki y\u0131ld\u0131zlar\u0131 ve daha \u00f6nce g\u00f6r\u00fcnmeyen ince yap\u0131lar\u0131 a\u00e7\u0131\u011fa \u00e7\u0131kar\u0131yor. Bu farkl\u0131l\u0131k, teleskoplar\u0131n yaln\u0131zca g\u00f6r\u00fcnt\u00fcleri g\u00fczelle\u015ftirmesini de\u011fil, y\u0131ld\u0131zlar\u0131n do\u011fdu\u011fu ortam\u0131n \u00e7e\u015fitli \u00f6zelliklerini ara\u015ft\u0131rmay\u0131 da sa\u011fl\u0131yor.<\/p>\n
Hubble\u2019\u0131n insan g\u00f6z\u00fcn\u00fcn alg\u0131layabildi\u011fi g\u00f6r\u00fcn\u00fcr \u0131\u015f\u0131kla kaydetti\u011fi g\u00f6r\u00fcnt\u00fcde, kahverengi ve koyu renkli bir toz s\u00fctunu \u00f6ne \u00e7\u0131k\u0131yor. Bu yo\u011fun madde, arkas\u0131ndaki \u0131\u015f\u0131\u011f\u0131 engelledi\u011fi i\u00e7in \u00e7evresindeki daha parlak gazdan kolayca ay\u0131rt ediliyor. Kedi ba\u015f\u0131n\u0131n ana hatlar\u0131n\u0131 olu\u015fturan yap\u0131 da bu gaz ve tozun uzayda ald\u0131\u011f\u0131 bi\u00e7imden kaynaklan\u0131yor.<\/p>\n
S\u00fctunun i\u00e7indeki k\u0131rm\u0131z\u0131 par\u0131lt\u0131, kedi g\u00f6z\u00fcne benzeyen bir alan olu\u015fturuyor. Bu \u0131\u015f\u0131k, toz bulutunun i\u00e7inde bulunan gen\u00e7 bir y\u0131ld\u0131zla ili\u015fkili olabilir. Ancak yaln\u0131zca g\u00f6r\u00fcnt\u00fcdeki renge bakarak y\u0131ld\u0131z\u0131n \u00f6zelliklerini kesin olarak belirlemek m\u00fcmk\u00fcn de\u011fil; bunun i\u00e7in \u0131\u015f\u0131\u011f\u0131n tayf\u0131 ve b\u00f6lgenin ba\u015fka g\u00f6zlemleri de inceleniyor. Gen\u00e7 y\u0131ld\u0131zlar\u0131n \u00e7evrelerine yayd\u0131\u011f\u0131 enerji, yak\u0131nlar\u0131ndaki gaz\u0131 ayd\u0131nlatabilir ve bulutun g\u00f6r\u00fcn\u00fcm\u00fcn\u00fc de\u011fi\u015ftirebilir.<\/p>\n
S\u00fctunun sa\u011f kenar\u0131nda g\u00f6r\u00fclen sar\u0131ms\u0131 \u0131\u015f\u0131k \u00e7izgisi, \u00e7evredeki b\u00fcy\u00fck y\u0131ld\u0131zlar\u0131n etkisini yans\u0131t\u0131yor olabilir. Bu y\u0131ld\u0131zlardan yay\u0131lan mor\u00f6tesi \u0131\u015f\u0131n\u0131m, gaz\u0131 \u0131s\u0131t\u0131p parlat\u0131rken bulutun d\u0131\u015f katmanlar\u0131n\u0131n zamanla a\u015f\u0131nmas\u0131na da yol a\u00e7abilir. Y\u0131ld\u0131zlar\u0131n \u00e7evreye savurdu\u011fu madde ve enerji, gaz\u0131 s\u0131k\u0131\u015ft\u0131rabilir, itebilir ya da da\u011f\u0131tabilir. Bu s\u00fcre\u00e7lerin birlikte etkisi, s\u00fctunun kediyi and\u0131ran s\u0131n\u0131rlar\u0131n\u0131n olu\u015fmas\u0131na katk\u0131da bulunmu\u015f olabilir. Yo\u011funlu\u011fu daha y\u00fcksek olan b\u00f6l\u00fcmler ise \u00e7evresindeki maddeye g\u00f6re daha dayan\u0131kl\u0131 olduklar\u0131ndan bi\u00e7imlerini bir s\u00fcre koruyabilir.<\/p>\n
James Webb Uzay Teleskobu, g\u00f6r\u00fcn\u00fcr \u0131\u015f\u0131\u011f\u0131n \u00f6tesindeki k\u0131z\u0131l\u00f6tesi \u0131\u015f\u0131n\u0131m\u0131 alg\u0131layabiliyor. Bu \u00f6zellik, gaz ve toz bulutlar\u0131n\u0131n i\u00e7indeki baz\u0131 kaynaklar\u0131 incelemeyi kolayla\u015ft\u0131r\u0131yor; \u00e7\u00fcnk\u00fc k\u0131z\u0131l\u00f6tesi \u0131\u015f\u0131k tozdan g\u00f6r\u00fcn\u00fcr \u0131\u015f\u0131\u011fa k\u0131yasla daha etkili bi\u00e7imde ge\u00e7ebiliyor. Webb\u2019in yak\u0131n k\u0131z\u0131l\u00f6tesi g\u00f6r\u00fcnt\u00fcs\u00fcnde bu nedenle toz s\u00fctunu daha ge\u00e7irgen g\u00f6r\u00fcn\u00fcr ve bulutun gerisindeki \u00e7ok say\u0131da y\u0131ld\u0131z belirginle\u015fir. G\u00f6r\u00fc\u015f do\u011frultusunda yer alan baz\u0131 uzak galaksiler de arka planda se\u00e7ilebilir.<\/p>\n
Yine de k\u0131z\u0131l\u00f6tesi g\u00f6zlemler b\u00fct\u00fcn tozu ortadan kald\u0131rmaz. \u00d6zellikle yo\u011fun ve kal\u0131n b\u00f6lgeler y\u0131ld\u0131z \u0131\u015f\u0131\u011f\u0131n\u0131 h\u00e2l\u00e2 engelleyebilir. Webb\u2019in g\u00f6r\u00fcnt\u00fcs\u00fc, bu nedenle bulutun her noktas\u0131n\u0131 ayn\u0131 a\u00e7\u0131kl\u0131kta g\u00f6stermez; farkl\u0131 \u0131\u015f\u0131k dalga boylar\u0131 yap\u0131n\u0131n farkl\u0131 katmanlar\u0131na ve \u00f6zelliklerine duyarl\u0131d\u0131r. Yak\u0131n k\u0131z\u0131l\u00f6tesi g\u00f6zlemler y\u0131ld\u0131zlar\u0131 ve s\u0131cak gaz\u0131 ortaya \u00e7\u0131kar\u0131rken, orta k\u0131z\u0131l\u00f6tesi g\u00f6zlemler daha \u00e7ok tozun ve belirli molek\u00fcllerin yayd\u0131\u011f\u0131 \u0131\u015f\u0131\u011fa odaklan\u0131r.<\/p>\n
Webb\u2019in orta k\u0131z\u0131l\u00f6tesi g\u00f6r\u00fcnt\u00fcs\u00fcnde s\u0131cak toz ile karbon i\u00e7eren baz\u0131 molek\u00fcllerin yayd\u0131\u011f\u0131 \u0131\u015f\u0131k \u00f6ne \u00e7\u0131kar. Bu g\u00f6r\u00fcn\u00fcm, toz s\u00fctununun sol taraf\u0131ndaki k\u00fc\u00e7\u00fck gaz ve toz k\u00fcmelerini ve ince uzant\u0131lar\u0131 daha belirgin h\u00e2le getirir. B\u00f6ylece ara\u015ft\u0131rmac\u0131lar, b\u00fcy\u00fck yap\u0131n\u0131n yan\u0131 s\u0131ra \u00e7evresindeki daha k\u00fc\u00e7\u00fck ayr\u0131nt\u0131lar\u0131 da inceleyebilir. Bu t\u00fcr ayr\u0131nt\u0131lar, gaz\u0131n nas\u0131l yo\u011funla\u015ft\u0131\u011f\u0131 ve y\u0131ld\u0131z olu\u015fumunun hangi ko\u015fullarda ger\u00e7ekle\u015fti\u011fi hakk\u0131nda ipu\u00e7lar\u0131 sa\u011flayabilir.<\/p>\n
G\u00f6r\u00fcnt\u00fcn\u00fcn sa\u011f\u0131ndaki sar\u0131 \u0131\u015f\u0131k kayna\u011f\u0131 da tozun i\u00e7inde olu\u015fan gen\u00e7 bir y\u0131ld\u0131z aday\u0131 olabilir. \u00d6n\u00fcnden ge\u00e7iyor gibi g\u00f6r\u00fcnen ince \u015feritle ayn\u0131 b\u00f6lgede bulunmas\u0131, ikisi aras\u0131nda fiziksel bir ba\u011flant\u0131 oldu\u011fu anlam\u0131na gelmez. \u0130ki yap\u0131n\u0131n ger\u00e7ekten ili\u015fkili olup olmad\u0131\u011f\u0131n\u0131 anlamak i\u00e7in konum, uzakl\u0131k ve hareket bilgileri gibi ek veriler gerekir. Tek bir g\u00f6r\u00fcnt\u00fc, g\u00f6ky\u00fcz\u00fcndeki iki nesnenin birbirine yak\u0131n g\u00f6r\u00fcnmesini g\u00f6sterebilir; ancak bu g\u00f6r\u00fcn\u00fc\u015f tek ba\u015f\u0131na aralar\u0131nda bir ba\u011f oldu\u011funu kan\u0131tlamaz.<\/p>\n
Hubble ve Webb\u2019in g\u00f6zlemleri, ayn\u0131 g\u00f6k b\u00f6lgesinin farkl\u0131 bile\u015fenlerini ortaya \u00e7\u0131kararak tamamlay\u0131c\u0131 bir ara\u015ft\u0131rma olana\u011f\u0131 sunuyor. Hubble, g\u00f6r\u00fcn\u00fcr \u0131\u015f\u0131kta ayd\u0131nl\u0131k gaz ile \u0131\u015f\u0131\u011f\u0131 engelleyen koyu tozu \u00f6ne \u00e7\u0131kar\u0131yor. Webb ise k\u0131z\u0131l\u00f6tesi \u0131\u015f\u0131k sayesinde bulutun i\u00e7indeki y\u0131ld\u0131zlar\u0131, s\u0131cak tozu ve ince yap\u0131lar\u0131 daha ayr\u0131nt\u0131l\u0131 bi\u00e7imde incelemeye yard\u0131mc\u0131 oluyor. Bu verilerin birlikte de\u011ferlendirilmesi, y\u0131ld\u0131zlar\u0131n hangi ko\u015fullarda do\u011fdu\u011funu ve \u00e7evrelerindeki maddeyle nas\u0131l etkile\u015fime girdi\u011fini ara\u015ft\u0131rmay\u0131 destekliyor.<\/p>\n
Kedi ba\u015f\u0131 bi\u00e7imi kal\u0131c\u0131 de\u011fil.<\/b> B\u00fcy\u00fck y\u0131ld\u0131zlardan gelen \u0131\u015f\u0131n\u0131m ve y\u0131ld\u0131z r\u00fczg\u00e2rlar\u0131 \u00e7evredeki gaz\u0131 zaman i\u00e7inde \u0131s\u0131t\u0131p da\u011f\u0131tabilir. Buna kar\u015f\u0131l\u0131k, yo\u011fun gaz ve toz k\u00fcmeleri daha uzun s\u00fcre varl\u0131\u011f\u0131n\u0131 s\u00fcrd\u00fcrebilir; baz\u0131lar\u0131 kendi k\u00fctle\u00e7ekimi alt\u0131nda \u00e7\u00f6kmeye ba\u015flayarak yeni y\u0131ld\u0131zlar\u0131n olu\u015fmas\u0131na zemin haz\u0131rlayabilir. Bu nedenle b\u00f6lgenin bug\u00fcnk\u00fc g\u00f6r\u00fcn\u00fcm\u00fc, devam eden fiziksel s\u00fcre\u00e7lerin ge\u00e7ici bir a\u015famas\u0131n\u0131 yans\u0131t\u0131yor. Yeterince uzun zaman i\u00e7inde gaz ve toz da\u011f\u0131ld\u0131k\u00e7a kediyi and\u0131ran siluet de de\u011fi\u015fecek ve sonunda tan\u0131nmaz h\u00e2le gelecek.<\/p>\n