Effect of the interactions and environment on nuclear activity

Sabater, J.; Best, P. N.; Argudo-Fernández, M.

doi:10.1093/mnras/sts675

Cited by 131 publications

(205 citation statements)

References 97 publications

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“…On the topic of merger incidence, the higher merger rates we find among AGNs at z < 1 is consistent with the level of enhancement of AGN activity in low redshift mergers (Silverman et al 2011;Sabater et al 2013). In addition, the weakening of a merger connection at z ∼ 2 is consistent with Kocevski et al (2012).…”

Section: Comparison With Existing Studies Of X-ray Selected Agnssupporting

confidence: 88%

The host galaxies of X-ray selected active galactic nuclei toz= 2.5: Structure, star formation, and their relationships from CANDELS andHerschel/PACS

Rosario

McIntosh

Wel

et al. 2014

A&A

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We study the relationship between the structure and star formation rate (SFR) of X-ray selected low and moderate luminosity active galactic nuclei (AGNs) in the two Chandra Deep Fields, using Hubble Space Telescope imaging from the Cosmic Assembly Near Infrared Extragalactic Legacy Survey (CANDELS) and deep far-infrared maps from the PEP+GOODS-Herschel survey. We derive detailed distributions of structural parameters and FIR luminosities from carefully constructed control samples of galaxies, which we then compare to those of the AGNs. At z ∼ 1, AGNs show slightly diskier light profiles than massive inactive (non-AGN) galaxies, as well as modestly higher levels of gross galaxy disturbance (as measured by visual signatures of interactions and clumpy structure). In contrast, at z ∼ 2, AGNs show similar levels of galaxy disturbance as inactive galaxies, but display a red central light enhancement, which may arise from a more pronounced bulge in AGN hosts or extinguished nuclear light. We undertake a number of tests of both these alternatives, but our results do not strongly favor one interpretation over the other. The mean SFR and its distribution among AGNs and inactive galaxies are similar at z > 1.5. At z < 1, however, clear and significant enhancements are seen in the SFRs of AGNs with bulge-dominated light profiles. These trends suggest an evolution in the relation between nuclear activity and host properties with redshift, towards a minor role for mergers and interactions at z > 1.5.

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Section: Comparison With Existing Studies Of X-ray Selected Agnssupporting

confidence: 88%

The host galaxies of X-ray selected active galactic nuclei toz= 2.5: Structure, star formation, and their relationships from CANDELS andHerschel/PACS

Rosario

McIntosh

Wel

et al. 2014

A&A

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“…Sabater et al 2013). In this scenario, the interaction is responsible for the morphological disturbance and inflow of gas towards the centre, which first triggers star formation (e.g.…”

Section: Dependence Of Relative Frequencies Of Sne Types On Host Actimentioning

confidence: 99%

“…Storchi-Bergmann et al 2001; Kuo et al 2008;Sabater, Best & Argudo-Fernández 2013). The produced gas inflow not only forms massive stars in the central region, but also fuels the SMBH in the centre of galaxies (e.g.…”

Section: Introductionmentioning

confidence: 99%

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Hakobyan¹,

Nazaryan²,

Adibekyan³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the relative frequencies of different supernova (SN) types in spirals with various morphologies and in barred or unbarred galaxies. We use a well-defined and homogeneous sample of spiral host galaxies of 692 SNe from the Sloan Digital Sky Survey in different stages of galaxy-galaxy interaction and activity classes of nucleus. We propose that the underlying mechanisms shaping the number ratios of SNe types can be interpreted within the framework of interaction-induced star formation, in addition to the known relations between morphologies and stellar populations. We find a strong trend in behaviour of the N Ia /N CC ratio depending on host morphology, such that early spirals include more Type Ia SNe. The N Ibc /N II ratio is higher in a broad bin of early-type hosts. The N Ia /N CC ratio is nearly constant when changing from normal, perturbed to interacting galaxies, then declines in merging galaxies, whereas it jumps to the highest value in post-merging/remnant galaxies. In contrast, the N Ibc /N II ratio jumps to the highest value in merging galaxies and slightly declines in post-merging/remnant subsample. The interpretation is that the star formation rates and morphologies of galaxies, which are strongly affected in the final stages of interaction, have an impact on the number ratios of SNe types. The N Ia /N CC (N Ibc /N II ) ratio increases (decreases) from star-forming to active galactic nuclei (AGN) classes of galaxies. These variations are consistent with the scenario of an interaction-triggered starburst evolving into AGN during the later stages of interaction, accompanied with the change of star formation and transformation of the galaxy morphology into an earlier type.

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“…We then added the requirement that more than 80% of the neighbours within a projected radius of 1 Mpc possess a spectroscopic redshift in either the main galaxy sample (Strauss et al 2002), with magnitudes between 14.5 < m r,Petrosian < 17.77, or in the Baryon Oscillation Spectroscopic Survey (BOSS; Dawson et al 2013), which uses a new spectrograph (Smee et al 2013) to obtain spectra of galaxies with 0.15 < z < 0.8 and quasars with 2.15 < z < 3.5, which is useful to reject background objects in our study. To correct for redshift incompleteness in the field, we used the photometric redshift z p provided by the SDSS (z of the table Photoz, for galaxies at magnitudes m r < 17.77 according to Sabater et al 2013). After a first rejection of neighbours with z p > 0.1 as background galaxies, we selected as potential companions neighbour galaxies with |z CIG − z p | < 2.5 z p,Err (Guo et al 2011), where z CIG is the spectroscopic redshift of the CIG galaxy and z p,Err is the photometric redshift error.…”

Section: Sample and Datamentioning

confidence: 99%

Effects of the environment on galaxies in the Catalogue of Isolated Galaxies: physical satellites and large scale structure

Argudo-Fernández

Verley

Bergond

et al. 2014

A&A

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Context. We present a study of the 3D environment for a sample of 386 galaxies in the Catalogue of Isolated Galaxies (CIG, Karachentseva 1973) using the Ninth Data Release of the Sloan Digital Sky Survey (SDSS-DR9). Aims. We aim to identify and quantify the effects of the satellite distribution around a sample of galaxies in the CIG, as well as the effects of the large-scale structure (LSS). Methods. To recover the physically bound galaxies we first focused on the satellites that are within the escape speed of each CIG galaxy. We also propose a more conservative method using the stacked Gaussian distribution of the velocity difference of the neighbours. The tidal strengths affecting the primary galaxy were estimated to quantify the effects of the local and LSS environments. We also defined the projected number density parameter at the fifth nearest neighbour to characterise the LSS around the CIG galaxies. Results. Out of the 386 CIG galaxies considered in this study, at least 340 (88% of the sample) have no physically linked satellite. Following the more conservative Gaussian distribution of physical satellites around the CIG galaxies leads to upper limits. Out of the 386 CIG galaxies, 327 (85% of the sample) have no physical companion within a projected distance of 0.3 Mpc. The CIG galaxies are distributed following the LSS of the local Universe, although presenting a large heterogeneity in their degree of connection with it. When present around a CIG galaxy, the effect of physically bound galaxies largely dominates (typically by more than 90%) the tidal strengths generated by the LSS. Conclusions. The CIG samples a variety of environments, from galaxies with physical satellites to galaxies without neighbours within 3 Mpc. A clear segregation appears between early-type CIG galaxies with companions and isolated late-type CIG galaxies. Isolated galaxies are in general bluer, with probably younger stellar populations and very high star formation compared with older, redder CIG galaxies with companions. Reciprocally, the satellites are redder and with an older stellar populations around massive early-type CIG galaxies, while they have a younger stellar content around massive late-type CIG galaxies. This suggests that the CIG is composed of a heterogeneous population of galaxies, sampling from old to more recent, dynamical systems of galaxies. CIG galaxies with companions might have a mild tendency (0.3−0.4 dex) to be more massive, and may indicate a higher frequency of having suffered a merger in the past.

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Effect of the interactions and environment on nuclear activity

Cited by 131 publications

References 97 publications

The host galaxies of X-ray selected active galactic nuclei toz= 2.5: Structure, star formation, and their relationships from CANDELS andHerschel/PACS

The host galaxies of X-ray selected active galactic nuclei toz= 2.5: Structure, star formation, and their relationships from CANDELS andHerschel/PACS

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Effects of the environment on galaxies in the Catalogue of Isolated Galaxies: physical satellites and large scale structure

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