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Based on assumptions concerning the quasar mechanism it was assumed that quasars are turned on due to mergers.
Observationally for z<1 where it is possible to determine if the quasar's associated galaxy is or is not merging it has been found that the quasar turn on does not correlate with mergers.
This means from a that mechanism that turns what quasar on is related to something internal to the galaxy or to the quasar.
Supporting that conclusion is the finding that quasars occur more commonly in voids rather than in high dense regions.
Supporting this conclusion is for z<1 mergers are not common.
The above finding makes it difficult to explain why there are clusters of quasars that are anomalies at 6 sigma in z<1.2.
http://arxiv.org/abs/1009.3265v2
http://arxiv.org/abs/1108.6221v1
Observationally for z<1 where it is possible to determine if the quasar's associated galaxy is or is not merging it has been found that the quasar turn on does not correlate with mergers.
This means from a that mechanism that turns what quasar on is related to something internal to the galaxy or to the quasar.
Supporting that conclusion is the finding that quasars occur more commonly in voids rather than in high dense regions.
Supporting this conclusion is for z<1 mergers are not common.
The above finding makes it difficult to explain why there are clusters of quasars that are anomalies at 6 sigma in z<1.2.
http://arxiv.org/abs/1009.3265v2
http://arxiv.org/abs/0710.1631v1THE BULK OF THE BLACK HOLE GROWTH SINCE z ∼ 1 OCCURS IN A SECULAR UNIVERSE:
NO MAJOR MERGER-AGN CONNECTION⋆What is the relevance of major mergers and interactions as triggering mechanisms for active galactic nuclei (AGN) activity? To answer this long-standing question, we analyze 140 XMM-Newton-selected AGN host galaxies and a matched control sample of 1264 inactive galaxies over z ∼ 0.3–1.0 and M∗ < 1011.7M⊙ with high-resolution HST/ACS imaging from the COSMOS field. The visual analysis of their morphologies by 10 independent human classifiers yields a measure of the fraction of distorted morphologies in the AGN and control samples, i.e., quantifying the signature of recent mergers which might potentially be responsible for fueling/triggering the AGN. We find that (1) the vast majority (>85%) of the AGN host galaxies do not show strong distortions, and (2) there is no significant difference in the distortion fractions between active and inactive galaxies. Our findings provide the best direct evidence that, since z ∼ 1, the bulk of black hole (BH) accretion has not been triggered by major galaxy mergers, therefore arguing that the alternative mechanisms, i.e., internal secular processes and minor interactions, are the leading triggers for the episodes of major BH growth. We also exclude an alternative interpretation of our results: a substantial time lag between merging and the observability of the AGN phase could wash out the most significant merging signatures, explaining the lack of enhancement of strong distortions on the AGN hosts. We show that this alternative scenario is unlikely due to: (1) recent major mergers being ruled out for the majority of sources due to the high fraction of disk-hosted AGN, (2) the lack of a significant X-ray signal in merging inactive galaxies as a signature of a potential buried AGN, and (3) the low levels of soft X-ray obscuration for AGN hosted by interacting galaxies, in contrast to model predictions.
ACTIVE GALACTIC NUCLEI IN VOID REGIONS
We present a comprehensive study of accretion activity in the most underdense environments in the universe, the voids, based on the SDSS DR2 data. Based on investigations of multiple void regions, we show that Active Galactic Nuclei (AGN) are definitely common in voids, but that their occurrence rate and properties differ from those in walls. AGN are more common in voids than in walls, but only among moderately luminous and massive galaxies (Mr < −20, log M∗/M⊙ < 10.5), and this enhancement is more pronounced for the relatively weak accreting systems (i.e., L[OIII] < 1039 erg s−1). Void AGN hosted by moderately massive and luminous galaxies are accreting at equal or lower rates than their wall counterparts, show lower levels of obscuration than in walls, and similarly aged stellar populations. The very few void AGN in massive bright hosts accrete more strongly, are more obscured, and are associated with younger stellar emission than wall AGN. These trends suggest that the accretion strength is connected to the availability of fuel supply, and that accretion and starformation co-evolve and rely on the same source of fuel.
http://arxiv.org/abs/1108.6221v1
Two close Large Quasar Groups of size approx. 350 Mpc at z = 1.2
What is the relevance of major mergers and interactions as triggering mechanisms for active galactic nuclei (AGN) activity? To answer this long-standing question, we analyze 140 XMM-Newton-selected AGN host galaxies and a matched control sample of 1264 inactive galaxies over z ∼ 0.3–1.0 and M∗ < 1011.7M⊙ with high-resolution HST/ACS imaging from the COSMOS field. The visual analysis of their morphologies by 10 independent human classifiers yields a measure of the fraction of distorted morphologies in the AGN and control samples, i.e., quantifying the signature of recent mergers which might potentially be responsible for fueling/triggering the AGN. We find that (1) the vast majority (>85%) of the AGN host galaxies do not show strong distortions, and (2) there is no significant difference in the distortion fractions between active and inactive galaxies. Our findings provide the best direct evidence that, since z ∼ 1, the bulk of black hole (BH) accretion has not been triggered by major galaxy mergers, therefore arguing that the alternative mechanisms, i.e., internal secular processes and minor interactions, are the leading triggers for the episodes of major BH growth. We also exclude an alternative interpretation of our results: a substantial time lag between merging and the observability of the AGN phase could wash out the most significant merging signatures, explaining the lack of enhancement of strong distortions on the AGN hosts. We show that this alternative scenario is unlikely due to: (1) recent major mergers being ruled out for the majority of sources due to the high fraction of disk-hosted AGN, (2) the lack of a significant X-ray signal in merging inactive galaxies as a signature of a potential buried AGN, and (3) the low levels of soft X-ray obscuration for AGN hosted by interacting galaxies, in contrast to model predictions.