The rise and fall of stellar across the peak of cosmic star formation history: effects of mergers versus diffuse stellar mass acquisition

Welker, Charlotte; Dubois, Yohan; Devriendt, Julien; Pichon, Christophe; Kaviraj, Sugata; Peirani, Sébastien

doi:10.1093/mnras/stw2778

Cited by 38 publications

(41 citation statements)

References 88 publications

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“…However, it is worth mentioning that although the galaxy stellar mass functions at different redshift are consistent at the high mass end, HORIZON-AGN tend to overshoots the low-mass end (<5 × 10 10 M⊙). Similar conclusions were obtained by Welker et al (2017) by comparing galaxy stellar mass functions with observation of CANDEL-UDS and GOODS surveys. Future accurate observations will allow to confirm these theoretical predictions, but, above all, will help constraining AGN models.…”

Section: Discussionsupporting

confidence: 83%

“…Note that, at a given mass, galaxies are in general more extended at low redshifts because they experience more mergers that tend to spread material at large radii, which increase their effective radius over time (Khochfar & Silk 2006;Bournaud, Jog & Combes 2007;Naab, Johansson & Ostriker 2009;Peirani et al 2010;Oser et al 2010Oser et al , 2012Shankar et al 2013;Welker et al 2017;Rodriguez-Gomez et al 2016). This effect is more pronounced with AGN feedback since the in situ star formation is regulated by AGN activity, at the benefit of the accreted stellar mass in the overall stellar mass budget .…”

Section: General Trendsmentioning

confidence: 99%

“…This sample is extracted from our state-of-the-art hydrodynamical cosmological simulation HORIZON-AGN (Dubois et al 2014) which includes gas cooling, star formation, stellar and AGN feedback, and that we compare with two other simulations HORIZON-NOAGN (no AGN feedback) and HORIZON-DM (no baryons) stripped down in terms of modelled physical processes but featuring identical initial consitions. These simulations have been used to highlight the role of AGN feedback (Volonteri et al 2016) in regulating the baryon content of massive galaxies (Kaviraj et al 2017;Beckmann et al 2016) and their morphological transformations (Welker et al 2017;Dubois et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Peirani

Dubois

Volonteri

et al. 2017

Monthly Notices of the Royal Astronomical Society

147

141

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Using a suite of three large cosmological hydrodynamical simulations, HORIZON-AGN, HORIZON-NOAGN (no AGN feedback) and HORIZON-DM (no baryons), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the inner density profiles of massive dark matter haloes and galaxies. Based on direct object-to-object comparisons, we find that the integrated inner mass and density slope differences between objects formed in these three simulations (hereafter, H AGN , H noAGN and H DM ) significantly evolve with time. More specifically, at high redshift (z ∼ 5), the mean central density profiles of H AGN and H noAGN dark matter haloes tend to be much steeper than their H DM counterparts owing to the rapidly growing baryonic component and ensuing adiabatic contraction. By z ∼ 1.5, these mean halo density profiles in H AGN have flattened, pummelled by powerful AGN activity ("quasar mode"): the integrated inner mass difference gaps with H noAGN haloes have widened, and those with H DM haloes have narrowed. Fast forward 9.5 billion years, down to z = 0, and the trend reverses: H AGN halo mean density profiles drift back to a more cusped shape as AGN feedback efficiency dwindles ("radio mode"), and the gaps in integrated central mass difference with H noAGN and H DM close and broaden respectively. On the galaxy side, the story differs noticeably. Averaged stellar profile central densities and inner slopes are monotonically reduced by AGN activity as a function of cosmic time, resulting in better agreement with local observations.

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Section: Discussionsupporting

confidence: 83%

Section: General Trendsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Peirani

Dubois

Volonteri

et al. 2017

Monthly Notices of the Royal Astronomical Society

147

141

View full text Add to dashboard Cite

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“…The role of such mergers in driving high-mass galaxy growth at z 2 has been the subject of recent observational work (e.g., Bundy et al 2009;Lotz et al 2011;Casteels et al 2014;Mundy et al 2017) and the basis of theoretical explanations for how massive compact spheroidals at z ≈ 2 grow significantly in size by the present day (e.g., Hopkins et al 2010;Nipoti et al 2012;Hilz et al 2013;Welker et al 2017). Comparisons of the predicted growth in diffuse outer components required to drive increasing size estimates appear to be consistent with observed (minor) merger rates, at least for z 1 (Newman et al 2012;López-Sanjuan et al 2012;Ownsworth et al 2014).…”

Section: Introductionmentioning

confidence: 99%

The Stripe 82 Massive Galaxy Project. III. A Lack of Growth among Massive Galaxies

Bundy

Leauthaud

Saito

et al. 2017

ApJ

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The average stellar mass (M * ) of high-mass galaxies (log M * /M ⊙ > 11.5) is expected to grow by ∼30% since z ∼ 1, largely through ongoing mergers that are also invoked to explain the observed increase in galaxy sizes. Direct evidence for the corresponding growth in stellar mass has been elusive, however, in part because the volumes sampled by previous redshift surveys have been too small to yield reliable statistics. In this work, we make use of the Stripe 82 Massive Galaxy Catalog (s82-mgc) to build a mass-limited sample of 41,770 galaxies (log M * /M ⊙ > 11.2) with optical to near-IR photometry and a large fraction (>55%) of spectroscopic redshifts. Our sample spans 139 deg 2 , significantly larger than previous efforts. After accounting for a number of potential systematic errors, including the effects of M * scatter, we measure galaxy stellar mass functions over 0.3 < z < 0.65 and detect no growth in the typical M * of massive galaxies with an uncertainty of 9%. This confidence level is dominated by uncertainties in the star formation history assumed for M * estimates, although our inability to characterize low surface-brightness outskirts may be the most important limitation of our study. Even among these high-mass galaxies, we find evidence for differential evolution when splitting the sample by recent star formation (SF) activity. While low-SF systems appear to become completely passive, we find a mostly sub-dominant population of galaxies with residual, but low rates of star formation (∼1 M ⊙ /yr) number density does not evolve. Interestingly, these galaxies become more prominent at higher M * , representing ∼10% of all galaxies at 10 12 M ⊙ and perhaps dominating at even larger masses.

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“…Central "seed" black holes are thought to gradually grow via mainly gas accretion, eventually becoming massive enough to shine as quasars or Seyfert galaxies and trigger powerful winds and/or jets capable of removing gas and quenching star formation in the host galaxy. This feedback from active black holes has become a key ingredient in almost all galaxy evolution models (e.g., Granato et al 2004;Cirasuolo et al 2005;Vittorini et may further increase their mass (and size) via mergers with other galaxies/black holes, which could contribute up to ∼ 80% of their final mass (e.g., De Lucia & Blaizot 2007;Malbon et al 2007;Oser et al 2010;Shankar et al 2010;Oser et al 2012;González et al 2011;Shankar et al 2013;Dubois et al 2013Dubois et al , 2016Rodriguez-Gomez et al 2016;Welker et al 2017). Additional mechanisms, besides mergers, can also contribute to the growth of the stellar bulge and feeding of the central black hole, most notably disc instabilities (e.g., Bower et al 2006;Bournaud et al 2011;Di Matteo et al 2012;Barausse 2012;Dubois et al 2012b).…”

Section: Introductionmentioning

confidence: 99%

Selection bias in dynamically measured supermassive black hole samples: scaling relations and correlations between residuals in semi-analytic galaxy formation models

Barausse

Shankar

Bernardi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Recent work has confirmed that the scaling relations between the masses of supermassive black holes and host-galaxy properties such as stellar masses and velocity dispersions may be biased high. Much of this may be caused by the requirement that the black-hole sphere of influence must be resolved for the black-hole mass to be reliably estimated. We revisit this issue with a comprehensive galaxy evolution semi-analytic model. Once tuned to reproduce the (mean) correlation of black-hole mass with velocity dispersion, the model cannot account for the correlation with stellar mass. This is independent of the model's parameters, thus suggesting an internal inconsistency in the data. The predicted distributions, especially at the low-mass end, are also much broader than observed. However, if selection effects are included, the model's predictions tend to align with the observations. We also demonstrate that the correlations between the residuals of the scaling relations are more effective than the relations themselves at constraining AGN feedback models. In fact, we find that our model, while in apparent broad agreement with the scaling relations when accounting for selection biases, yields very weak correlations between their residuals at fixed stellar mass, in stark contrast with observations. This problem persists when changing the AGN feedback strength, and is also present in the hydrodynamic cosmological simulation Horizon-AGN, which includes state-of-the-art treatments of AGN feedback. This suggests that current AGN feedback models are too weak or simply not capturing the effect of the black hole on the stellar velocity dispersion.

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The rise and fall of stellar across the peak of cosmic star formation history: effects of mergers versus diffuse stellar mass acquisition

Cited by 38 publications

References 88 publications

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

The Stripe 82 Massive Galaxy Project. III. A Lack of Growth among Massive Galaxies

Selection bias in dynamically measured supermassive black hole samples: scaling relations and correlations between residuals in semi-analytic galaxy formation models

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