ALMAs hul i Universet
Alt det, der skete lige efter Big Bang var så voldsomt, at det efterlod et uudsletteligt aftryk på selve Universets struktur. Vi kan måle disse ar idag ved at observere det ældste lys i Universet. Det lys, som blev dannet for næsten 14 milliarder år siden, har nu spredt sig i takt med rummets udvidelse, så det stadig fylder hele Universet. Nu måler vi det som svag mikrobølgestråling og derfor kaldes det den kosmiske mikrobølge baggrund, eller cosmic microwave background (CMB).
CMB-strålingen kan bruges til at undersøge kosmos via en effekt, som kaldes Sunyaev-Zel’dovich (SZ) effekten, opdaget over 30 år siden. Her på Jorden modtager vi CMB-strålingen som mikrobølger, der undervejs til os har passeret igennem for eksempel galaxehobe, som kan indeholde højenergielektroner. Disse elektroner giver fotonerne et lille energitilskud ved passagen. Med vore teleskoper kan vi finde disse energirige elektroner. Det er svært, men det er vigtigt, for det kan hjælpe astronomerne til at forstå nogle af de grundliggende egenskaber ved Universet, som for eksempel placeringen og fordelingen af galaksehobe.
Billedet viser de første målinger af termisk Sunyaev-Zel’dovich effekt fra Atacama Large Millimeter/submillimeter Array (ALMA) i Chile (i blåt). Astronomerne har kombineret data fra ALMAs 7- og 12 meterantenner for at opnå de skarpest mulige billede. Målområdet er den af de tungeste kendte galaksehobe, RX J1347.5–1145, hvis centrale område kan ses her som et mørkt "hul" i ALMA-målingerne. Energifordelingen af CMBfotonerne ændrer sig, og det måler vi som en nedgang i temperatur ved de bølgelængder, som ALMA observerer. Det er det, som optræder som en mørk plet i billedet her.
Links
Kilde:ALMA (ESO/NAOJ/NRAO)/T. Kitayama (Toho University, Japan)/ESA/Hubble & NASA
Om billedet
| Id: | potw1708a |
| Sprog: | da |
| Type: | Observation |
| Udgivelsesdato: | 20. februar 2017 06:00 |
| Størrelse: | 3816 x 3559 px |
Om objektet
| Type: | Early Universe : Cosmology |
| Constellation: | Virgo |
Baggrundsbilleder
Koordinater
| Position (RA): | 13 47 30.65 |
| Position (Dec): | -11° 45' 18.95" |
| Field of view: | 1.91 x 1.78 arcminutes |
| Orientering: | Nord er 130.7° droite fra lodret |
Farver & filtre
| Bånd | Bølgelængde | Teleskop |
|---|---|---|
| Milimeter 92 GHz | 3.258613 mm | Atacama Large Millimeter/submillimeter Array Band 3 |
| Optisk g | 475 nm | Hubble Space Telescope ACS |
| Optisk B | 435 nm | Hubble Space Telescope ACS |
| Optisk V | 606 nm | Hubble Space Telescope ACS |
| Optisk r | 625 nm | Hubble Space Telescope ACS |
| Optisk i | 775 nm | Hubble Space Telescope ACS |
| Optisk z | 850 nm | Hubble Space Telescope ACS |
| Infrarød J | 1.1 μm | Hubble Space Telescope WFC3 |
| Infrarød H short | 1.6 μm | Hubble Space Telescope WFC3 |
| Optisk I | 814 nm | Hubble Space Telescope ACS |
| Infrarød J | 1.1 μm | Hubble Space Telescope WFC3 |
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