ALMA i dziura we Wszechświecie
Wydarzenia wokół Wielkiego Wybuchu były tak kataklizmiczne, że pozostawiły niezatarty ślad w kosmosie. Możemy dzisiaj wykryć te blizny obserwując najstarsze światło we Wszechświecie. Ponieważ powstało prawie 14 miliardów lat temu, światło to — istniejące obecnie jako słabe promieniowanie mikrofalowe i dlatego nazwane kosmicznym mikrofalowym promieniowanie tła (CMB) — rozszerzyło się tak, że przenika cały kosmos, wypełniając do wykrywalnymi fotonami.
Promieniowanie tła może być używane do badania kosmosu przez tzw. efekt Suniajewa-Zeldowicza (SZ), po raz pierwszy zaobserwowany 30 lat temu. Kosmiczne promieniowanie tła wykrywamy tutaj na Ziemi gdy wchodzące w jego skład fotony mikrofalowe podróżują do nas przez przestrzeń kosmiczną. W trakcie tej podróży mogą przemieszczać się przez gromady galaktyk zawierające wysokoenergetyczne elektrony. Elektrony te dają fotonom niewielki dodatek energii. Wykrywanie takich "zdopingowanych" fotonów poprzez teleskopy stanowi wyzwanie, ale jest ważne — pomagają one bowiem astronomom w zrozumieniu niektórych fundamentalnych własności Wszechświata, takich jak położenie i rozmieszczenie gęstych gromad galaktyk.
Zdjęcie pokazuje pierwsze pomiary termicznego efektu Suniajewa-Zeldowicza przy pomocy Atacama Large Millimeter/submillimeter Array (ALMA) w Chile (kolor niebieski). Astronomowie połączyli dane z 7 i 12 metrowych anten ALMA, aby uzyskać najostrzejszy możliwy obraz. Celem była jedna z najmasywniejszych znanych gromad galaktyk, RX J1347.5–1145,której centrum widać jako ciemną "dziurę" w obserwacjach ALMA. Rozkład energii fotonów promieniowania tła przesuwa się i wygląda jak wzrost temperatury na falach o długości obserwowanej przez ALMA, dlatego widać ciemny obszar na zdjęciu w miejscu gromady.
Linki
Źródło:ALMA (ESO/NAOJ/NRAO)/T. Kitayama (Toho University, Japan)/ESA/Hubble & NASA
O zdjęciu
| Identyfikator: | potw1708a |
| Język: | pl |
| Typ: | Obserwacje |
| Data publikacji: | 20 lutego 2017 06:00 |
| Rozmiar: | 3816 x 3559 px |
O obiekcie
| Typ: | Early Universe : Cosmology |
| Constellation: | Virgo |
Współrzędne
| Pozycja (RA): | 13 47 30.65 |
| Pozycja (Dec): | -11° 45' 18.95" |
| Pole widzenia: | 1.91 x 1.78 arcminutes |
| Orientacja: | North is 130.7° prawo of vertical |
Kolory i filtry
| Pasmo | Długość fali | Teleskop |
|---|---|---|
| Milimetrowy 92 GHz | 3.258613 mm | Atacama Large Millimeter/submillimeter Array Band 3 |
| Optyczny g | 475 nm | Hubble Space Telescope ACS |
| Optyczny B | 435 nm | Hubble Space Telescope ACS |
| Optyczny V | 606 nm | Hubble Space Telescope ACS |
| Optyczny r | 625 nm | Hubble Space Telescope ACS |
| Optyczny i | 775 nm | Hubble Space Telescope ACS |
| Optyczny z | 850 nm | Hubble Space Telescope ACS |
| Podczerwony J | 1.1 μm | Hubble Space Telescope WFC3 |
| Podczerwony H short | 1.6 μm | Hubble Space Telescope WFC3 |
| Optyczny I | 814 nm | Hubble Space Telescope ACS |
| Podczerwony J | 1.1 μm | Hubble Space Telescope WFC3 |
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