The dependence of mass and environment on the secular processes of AGNs in terms of morphology, colour, and specific star-formation rate

Argudo-Fernández, M.; Lacerna, Iván; Puertas, S. Duarte

doi:10.1051/0004-6361/201833328

Cited by 25 publications

(23 citation statements)

References 93 publications

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“…In the voids, somewhat surprisingly, F SFG first flattens out and then declines at the lowest masses. Both the increase of the AGN fraction and the decrease of the SFG fraction with increasing stellar mass in dense environments agree with the results by Argudo-Fernández et al (2018). Figure 6 shows the average AGN and SFG fractions in clusters versus the distance from the brightest cluster galaxy, assumed to be located close to the cluster center.…”

Section: Lsmsupporting

confidence: 83%

“…Colors of the symbols correspond to the stellar mass according to the scale on the right of the figure. est stellar masses. The finding of a higher AGN fraction in dense environments is consistent with the results by Manzer & De Robertis (2014) and by Argudo-Fernández et al (2018), but disagrees with the results of many other studies (see Sect. 1).…”

Section: Lsmsupporting

confidence: 66%

“…The mass dependence is, however, quite different: it is mild in voids where F AGN reaches 30% at most; in clusters it is steeper, particularly above M 10 10.1 M ; F AGN reaches 70% at the highest masses. The higher F AGN in clusters, compared to voids, agrees with the results by Manzer & De Robertis (2014) and by Argudo-Fernández et al (2018), but disagrees with the results of many other studies which however have used different selection criteria. The average SFG fraction in clusters is higher in the less dense outer regions, where the fraction of star-forming galaxies is lower.…”

Section: Lsmcontrasting

confidence: 49%

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Role of Environment on Nuclear Activity

Amiri

Tavasoli

Zotti

2019

ApJ

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Motivated by the apparently conflicting results reported in the literature on the effect of environment on nuclear activity, we have carried out a new analysis by comparing the fraction of galaxies hosting active galactic nuclei (AGNs) in the most overdense regions (rich galaxy clusters) and the most underdense ones (voids) in the local universe. Exploiting the classical BPT diagnostics, we have extracted volume limited samples of star forming and AGN galaxies. We find that, at variance with star-forming galaxies, AGN galaxies have similar distributions of specific star formation rates and of galactic ages (as indicated by the D n 4000 parameter) both in clusters and in voids. In both environments galaxies hosting AGNs are generally old, with low star formation activity. The AGN fraction increases faster with stellar mass in clusters than in voids, especially above 10 10.2 M . Our results indicate that, in the local universe, the nuclear activity correlates with stellar mass and galaxy morphology and is weakly, if at all, affected by the local galaxy density.

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Section: Lsmsupporting

confidence: 83%

Section: Lsmsupporting

confidence: 66%

Section: Lsmcontrasting

confidence: 49%

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Role of Environment on Nuclear Activity

Amiri

Tavasoli

Zotti

2019

ApJ

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“…With new instruments and more dedicated observations in this century, it has been possible to learn new information. In particular, the number of local early-type (i.e., E and lenticular) galaxies with integrated properties different from the classical "red and dead" massive ones increases as the stellar mass is smaller and the environment becomes less dense (e.g., Kuntschner et al 2002;Bernardi et al 2006;Lee et al 2006;Schawinski et al 2007Schawinski et al , 2009Kannappan et al 2009;Suh et al 2010;Thomas et al 2010;McIntosh et al 2014;Schawinski et al 2014;George & Zingade 2015;Vulcani et al 2015;Lacerna et al 2016Lacerna et al , 2018Spector & Brosch 2017;Argudo-Fernández et al 2018). Two examples of these early-type galaxies are the recently quenched ellipticals (RQEs) and the blue, star-forming (BSF) ellipticals.…”

Section: Introductionmentioning

confidence: 99%

SDSS-IV MaNGA: Global and local stellar population properties of elliptical galaxies

Lacerna

Ibarra-Medel

Ávila-Reese

et al. 2020

A&A

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Context. We study the spatially resolved properties of 343 elliptical galaxies with the Mapping Nearby Galaxies at the Apache Point Observatory (MaNGA) survey. Aims. Our goal is to understand the fundamental processes of formation and quenching of elliptical galaxies. Methods. We used the DESI Legacy Imaging Surveys for accurate morphological classification. Based on integrated spectroscopic properties and colors, we classified seven classes of elliptical galaxies. We inferred the stellar age and metallicity gradients out to a 1.5 effective radius (Reff) of classical “red and dead”, recently quenched, and blue star-forming ellipticals (CLEs, RQEs, and BSFs), corresponding to 73%, 10%, and 4% of the sample, respectively. Additionally, we reconstructed their global and radial histories of star formation and mass growth. Results. The mass- and luminosity-weighted age gradients of CLEs are nearly flat or mildly negative, with small differences between both ages. The respective metallicity gradients are negative (∇log[Zmw] = −0.11−0.08+0.07 dex/Reff and ∇log[Zlw] = −0.11−0.07+0.06 dex/Reff, respectively), being flatter as the mass is smaller. The more massive CLEs formed stars earlier and quenched faster than the less massive ones. The CLEs show a weak inside-out growth and a clear inside-out quenching. They finished their quenching globally 3.8 ± 1.2 Gyr ago on average, with quenching time-scales of 3.4 ± 0.8 Gyr. At M⋆ < 1011 M⊙, the age and Z gradients of the RQEs and BSFs are flatter than those of the CLEs, but with larger scatters. They show very weak inside-out growth and quenching, which is slow and not even completed at z ∼ 0 for the BSFs. Instead, the massive RQEs show an outside-in quenching and positive gradients in the luminosity-weighted age and stellar metallicities. The RQEs of all masses quenched 1.2 ± 0.9 Gyr ago on average. Conclusions. Our results for the CLEs are consistent with a two-phase scenario where their inner parts formed by an early and coeval dissipative collapse with a consequent burst of star formation and further quenching, whereas the outer parts continued their assembly, likely by dry mergers. We also discuss some evolutionary scenarios for the RQE and BSF galaxies that would agree with the generic results.

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“…The massive SDSS galaxies with M * > 3 × 10 10 M ⊙ are found to be more concentrated and dominated by older stellar populations, whereas the low-mass galaxies are likely to have lower concentrations and younger stellar ages. Many previous studies discuss the mass dependence of galaxy structure between QGs and SFGs (e.g., van der Wel et al 2014;Lang et al 2014;Whitaker et al 2015Whitaker et al , 2017Argudo-Fernández et al 2018;Mowla et al 2018;Matharu et al 2019;Miller et al 2019). For two main classes of galaxies at high redshifts, their stellar masses have also been found to be correlated with structure parameters (e.g., the size -mass relation and the density -mass relation) (Barro et al 2017;Lee et al 2018).…”

Section: Introductionmentioning

confidence: 99%

The Mass Dependence of Structure, Star Formation Rate, and Mass Assembly Mode at 0.5 < z < 2.5

Fang

Yuan

et al. 2019

ApJ

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To investigate the mass dependence of structural transformation and star formation quenching, we construct three galaxy samples using massive (M * > 10 10 M ⊙ ) red, green, and blue galaxy populations at 0.5 < z < 2.5 in five 3D-HST/CANDELS fields. The structural parameters, including effective radius (r e ), galaxy compactness (Σ 1.5 ), and second order moment of 20% brightest pixels (M 20 ) are found to be correlated with stellar mass. Sérsic index (n), concentration (C), and Gini coefficient (G) seem to be insensitive to stellar mass. The morphological distinction between blue and red galaxies is found at a fixed mass bin, suggesting that quenching processes should be accompanied with transformations of galaxy structure and morphology. Except for r e and Σ 1.5 at high mass end, structural parameters of green galaxies are intermediate between red and blue galaxies in each stellar mass bin at z < 2, indicating green galaxies are at a transitional phase when blue galaxies are being quenched into quiescent statuses. The similar sizes and compactness for the blue and green galaxies at high-mass end implies that these galaxies will not appear to be significantly shrunk until they are completely quenched into red QGs. For the green galaxies at 0.5 < z < 1.5, a morphological transformation sequence of bulge buildup can be seen as they are gradually shut down their star formation activities, while a faster morphological transformation is verified for the green galaxies at 1.5 < z < 2.5.

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The dependence of mass and environment on the secular processes of AGNs in terms of morphology, colour, and specific star-formation rate

Cited by 25 publications

References 93 publications

Role of Environment on Nuclear Activity

Role of Environment on Nuclear Activity

SDSS-IV MaNGA: Global and local stellar population properties of elliptical galaxies

The Mass Dependence of Structure, Star Formation Rate, and Mass Assembly Mode at 0.5 < z < 2.5

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