Conventional research on distant galaxies have been carried out mainly with visible light and near infrared light. However, it is possible that many galaxies in the universe have been overlooked as much of that radiation is largely absorbed by cosmic dust. That is why millimeter and submillimeter wave observations are important. Stellar light absorbed by dust is reradiated from the dust as millimeter/submillimeter waves. Therefore galaxies, even those which it has not been possible to observe with optical telescopes, can be detected using these wavebands. Furthermore, millimeter/submillimeter waves are suitable for observation of distant galaxies. This is because the more distant the galaxy is, the more luminous part of light we can see due to the shift of wavelength of light by the expansion of the universe. This effect is called "negative K correction" and it compensates the source dimming in the distant universe.
In past observations, gigantic galaxies deeply covered in dust, where several hundreds to thousands of stars are actively forming per year, have been detected with millimeter/submillimeter waves. To capture the overall picture of galaxies in the universe, it is important to observe "general galaxies" which have moderate star-formation activities. However, it has not been possible to detect faint galaxies due to the low sensitivity of existing observation instruments.
Observations with ALMA
The research team observed a field named "Subaru/XMM-Newtown Deep Survey Field," located in the direction of the constellation Cetus, with the ALMA telescope. As a result, they succeeded in finding 15 extremely dark galaxies that were unidentified until now. "It is thanks to the high performance of ALMA, which is proudly said to be the best in the world, that observations like this have been made possible," said Hatsukade.
With the ALMA observations the team successfully measured the number density of galaxies approximately 10 times darker than the millimeter wave research results up to now. The new results agree well with the prediction by the theories of galaxy formation. That means, the galaxies detected in this research are the faint but dust-rich galaxies and they are most likely to be similar in type to normal galaxies not detected before.. In regards to this, Professor Ohta commented, "This is a big step towards getting the big picture of galaxy evolution as the objects connecting especially bright galaxies in millimeter/submillimeter waves and normal galaxies were detected with ALMA."
Furthermore, the team concluded that approximately 80% of the sources of the cosmic background radiation within the millimeter/submillimeter wavebands are more "normal galaxies" like those detected by ALMA this time.. Past observations showed the total power of signals emitted from the universe with the millimeter/submillimeter wavebands. However, spatial resolution was not sufficient to identify the sources of all the signals; only 10 -- 20% of them were identified.
To gain an overall picture of galaxies in the universe requires a much higher sensitivity for observation. For this research, only a part of the ALMA telescope, 23~25 antennas, were used. As the number of antennas in the ALMA telescope increases, its observation ability will also improve. Hatsukade expressed his hopes, saying "I want to clarify the overall picture of galaxy evolution. So, using ALMA, I would like to make observations of much fainter galaxies, and also study star formation activities and the amount of dust in those galaxies in detail." Professor Ohta also mentioned, "We are also planning to make thorough observations with visible light and infrared radiation, using the Subaru Telescope. This is in order to explore the nature of galaxies become darker due to light-absorbing dust. But for observations of extremely dark galaxies, we might need the Thirty Meter Telescope with much larger light-gathering power."
- Bunyo Hatsukade, Kouji Ohta, Akifumi Seko, Kiyoto Yabe, Masayuki Akiyama. FAINT END OF 1.3 mm NUMBER COUNTS REVEALED BY ALMA. Astrophysical Journal Letters, 2013 [link]
Cite This Page: