Author

Kauffmann, Guinevere
Kauffmann, Guinevere
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Original publication

1.
Kauffmann, Guinevere
The physical properties of galaxies with unusually red mid-infrared colours

Highlight: May 2018

Finding needles in a haystack

May 01, 2018

Previous studies of large AGN samples both a low and at high redshifts seemed to rule out galaxy mergers as the drivers for black hole growth. A new technique developed at MPA for selecting a rare type of active galactic nuclei now show that it is possible to identify a new class of AGN in which more than  80% of the galaxies turn out to be merging or interacting systems, with clear indications of an accreting black hole. A detailed statistical analysis then reveals that mergers drive  black hole formation in the most massive galaxies in the local Universe.

Figure 1: This illustration shows the different features of an active galactic nucleus (AGN). The extreme luminosity of an AGN is powered by accretion onto a supermassive black hole. In addition to the accretion disk, models of active galaxies also include a region of cold gas and dust, the torus. Viewed edge-on, the torus blocks out the light from the accretion disk and the system is a Type II AGN. Viewed face-on, the accretion disk dominates the luminosity and the system is a quasar. Zoom Image
Figure 1: This illustration shows the different features of an active galactic nucleus (AGN). The extreme luminosity of an AGN is powered by accretion onto a supermassive black hole. In addition to the accretion disk, models of active galaxies also include a region of cold gas and dust, the torus. Viewed edge-on, the torus blocks out the light from the accretion disk and the system is a Type II AGN. Viewed face-on, the accretion disk dominates the luminosity and the system is a quasar. [less]

Our understanding of the formation paths of supermassive black holes is still very sketchy. In 1982, Andrzej Soltan showed that the summed emission from all observed quasars yields a remarkably accurate estimate of the total mass of present-day black holes. His argument was based on the expected conversion efficiency of the rest mass energy of matter in an accretion disk falling into a black hole at the centre of a quasar - these distant objects are thus believed to signpost the main sites of black hole growth across the Universe.

Unfortunately, quasars are not ideal objects to study the mechanisms by which black holes grow. The emission from the central nucleus is more luminous than the underlying host galaxy by many orders of magnitude, making detailed studies of the host system extremely difficult. For this reason, studies to constrain possible triggering mechanisms for black hole growth focus on so called Type II active galactic nuclei (AGN). In these systems, the radiation from the accretion disk is believed to be blocked by a very dense layer of gas and dust (the so-called torus, see Figure 1). Large spectroscopic galaxy surveys such as the Sloan Digital Sky Survey have yielded samples of hundreds of thousands of nearby Type II AGN, which are selected according to their optical emission line ratios. At higher redshifts, Type II AGN are commonly selected at X-ray wavelengths.

Figure 2: SDSS colour images (g,r,i-band) of typical AGN host galaxies in our sample. Many are interacting or have disturbed morphologies. Zoom Image
Figure 2: SDSS colour images (g,r,i-band) of typical AGN host galaxies in our sample. Many are interacting or have disturbed morphologies. [less]

So far, studies of the host galaxies of these systems appear to rule out theoretical scenarios in which black hole growth occurs when two or more galaxies merge together. Simulations of the gravitational interactions and gas dynamics of two merging galaxies show that tidal torques during the merger cause the gas to shock, lose energy and flow towards the centre of the merger remnant. Energetic processes that act on the gas very close to the black hole are, however, very difficult to simulate in a reliable way.

In recent work at MPA, a new technique combined data from several observing programmes using the Wide-field Infrared Survey Explorer satellite, the Very Large Array (VLA) FIRST Survey (Radio Images of the Sky at Twenty-Centimeters) and the Sloan Digital Sky Survey. This combination of data permits a more reliable selection of a large sample of active galaxies where there is strong hot dust emission from a central torus. The radio data turned out to be a critical element of the selection technique, because there are large number of galaxies where the hot dust extends over a large area and is probably not being heated by the black hole. This had not been accounted for in previous work.

Figure 3: Line ratio diagnostic diagrams illustrating that the AGN in our sample (red dots) have gas in a higher ionization state than ordinary AGN (black dots). Zoom Image

Figure 3: Line ratio diagnostic diagrams illustrating that the AGN in our sample (red dots) have gas in a higher ionization state than ordinary AGN (black dots).

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Follow-up work demonstrated that the new selection, which includes only 1.6% of the sources in previous AGN samples, yields galaxies with properties that are very different. More than 80% of the galaxies in the new sample turn out to be merging or interacting systems. For many of them, their stellar spectra show strong bursts of star formation in their central regions. The emission lines indicate that the gas is highly ionized, with the main source of ionization likely being an accreting black hole rather than the young stars in the nucleus. The radio emission is usually compact and centrally located and is too luminous to be explained by the observed young stars in the nucleus. With 1300 galaxies the new sample is large enough to show conclusively that these AGN currently signpost the bulk of black hole formation in the most massive galaxies in the local Universe - with the "normal" AGN population dominant in lower mass galaxies.

The challenge now is to go back in time to younger galaxies, i.e. to extend this study to higher redshifts. Pulling similar samples out of surveys of galaxies at higher redshifts, however, will need comparable data sets in different wavelength bands. Then we can investigate how the accreting black holes in these younger systems are influencing the gas in and around their host galaxies.

 
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