Bulge mass is king: the dominant role of the bulge in determining the fraction of passive galaxies in the Sloan Digital Sky Survey

Bluck, Asa F. L.; Mendel, J. Trevor; Ellison, Sara L.; Moreno, Jorge; Simard, Luc; Patton, David R.; Starkenburg, Else

doi:10.1093/mnras/stu594

Cited by 253 publications

(389 citation statements)

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“…Those mass estimates are based on updated SDSS photometry and bulge+disc decomposition, using dual Sérsic profiles (Simard et al 2011). In their analysis, Bluck et al (2014) consider a subsample of the full catalogue defined by the cuts 0.02 < z < 0.2, 8 < log(Mstar) < 12, dDB < 1 and PpS < 0.5. dDB represents the scatter in the relation between the estimate of the total stellar mass and the sum of the estimates of bulge and disc separately; the applied cut removes objects with problematic decomposition. PpS is the probability that a source is best-fit by a single Sérsic profile; the applied cut removes sources with possibly spurious components.…”

Section: Resultsmentioning

confidence: 99%

On the dependence of galaxy morphologies on galaxy mergers

Fontanot

Macciò

Hirschmann

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The distribution of galaxy morphological types is a key test for models of galaxy formation and evolution, providing strong constraints on the relative contribution of different physical processes responsible for the growth of the spheroidal components. In this paper, we make use of a suite of semi-analytic models to study the efficiency of galaxy mergers in disrupting galaxy discs and building galaxy bulges. In particular, we compare standard prescriptions usually adopted in semi-analytic models, with new prescriptions proposed by Kannan et al., based on results from high-resolution hydrodynamical simulations, and we show that these new implementations reduce the efficiency of bulge formation through mergers. In addition, we compare our model results with a variety of observational measurements of the fraction of spheroid-dominated galaxies as a function of stellar and halo mass, showing that the present uncertainties in the data represent an important limitation to our understanding of spheroid formation. Our results indicate that the main tension between theoretical models and observations does not stem from the survival of purely disc structures (i.e. bulgeless galaxies), rather from the distribution of galaxies of different morphological types, as a function of their stellar mass.

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Section: Resultsmentioning

confidence: 99%

On the dependence of galaxy morphologies on galaxy mergers

Fontanot

Macciò

Hirschmann

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…bulge-to-total light/ mass ratio, B/T , or Sérsic index, nS (e.g., Driver et al 2006;Wuyts et al 2011;Mendel et al 2013;Bluck et al 2014;Lang et al 2014;Omand et al 2014). Additionally, the quenched fraction depends on environment, particularly the surface density of galaxies in a given region of space, the halo mass of the group or cluster, and the distance a galaxy resides at from the centre of its group (e.g., Balogh et al 2004;van den Bosch et al 2007Peng et al 2012;Woo et al 2013;Bluck et al 2014).…”

Section: Introductionmentioning

confidence: 99%

“…It has become evident that understanding quenching processes in galaxies requires separate consideration of central and satellite galaxies, since the mechanisms for quenching star formation in these systems most likely differ (e.g., Peng et al 2012;Woo et al 2013;Bluck et al 2014;Knobel et al 2015). Central galaxies are most commonly defined as the most massive galaxy in their group or cluster, with satellites being any other group member (e.g., Yang et al 2007Yang et al , 2009).…”

Section: Introductionmentioning

confidence: 99%

“…More recent work has linked the quenched (or red) fraction of large populations of galaxies to the central density within 1 kpc (Cheung et al 2012, Fang et al 2013, the central velocity dispersion (Wake et al 2012), and to the mass of the galactic bulge (Bluck et al 2014, Lang et al 2014, Omand et al 2014). An artificial neural network (ANN) analysis performed by Teimoorinia, Bluck & Ellison (2016) established that for central galaxies the most accurate predictions for whether a galaxy will be star forming or not are given by central velocity dispersion, which outperforms all other variables considered, including bulge mass, stellar mass and halo mass.…”

Section: Introductionmentioning

confidence: 99%

“…Recent observations suggest that halo mass is more constraining of the quenched fraction of centrals than stellar mass, qualitatively in line with this view (e.g., Woo et al 2013). However, the stronger dependence of central galaxy quenching on bulge mass and central density (e.g., Bluck et al 2014 imply that this cannot be the sole, or dominant, route to quenching centrals. Further to this, elevated gas depletion and supernovae feedback in galaxy mergers, and the growth of the central potential and its stabilizing influence on giant molecular cloud collapse, have both been evoked as potential alternatives to the more commonly utilised AGN feedback (e.g., Martig et al 2009;Darg et al 2010;Moreno et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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The impact of galactic properties and environment on the quenching of central and satellite galaxies: a comparison between SDSS, Illustris and L-Galaxies

Bluck

Mendel

Ellison

et al. 2016

Mon. Not. R. Astron. Soc.

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138

226

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We quantify the impact that a variety of galactic and environmental properties have on the quenching of star formation. We collate a sample of ∼ 400,000 central and ∼ 100,000 satellite galaxies from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7). Specifically, we consider central velocity dispersion (σ c ), stellar, halo, bulge and disk mass, local density, bulge-to-total ratio, group-centric distance and galaxy-halo mass ratio. We develop and apply a new statistical technique to quantify the impact on the quenched fraction (f Quench ) of varying one parameter, while keeping the remaining parameters fixed. For centrals, we find that the f Quench − σ c relationship is tighter and steeper than for any other variable considered. We compare to the Illustris hydrodynamical simulation and the Munich semi-analytic model (L-Galaxies), finding that our results for centrals are qualitatively consistent with their predictions for quenching via radio-mode AGN feedback, hinting at the viability of this process in explaining our observational trends. However, we also find evidence that quenching in L-Galaxies is too efficient and quenching in Illustris is not efficient enough, compared to observations. For satellites, we find strong evidence that environment affects their quenched fraction at fixed central velocity dispersion, particularly at lower masses. At higher masses, satellites behave identically to centrals in their quenching. Of the environmental parameters considered, local density affects the quenched fraction of satellites the most at fixed central velocity dispersion.

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The Downfall of Massive Star-Forming Galaxies During the Last $$10\,\mathrm{Gyr}$$ 10 Gyr

Schreiber

2016

Springer Theses

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Bulge mass is king: the dominant role of the bulge in determining the fraction of passive galaxies in the Sloan Digital Sky Survey

Cited by 253 publications

References 123 publications

On the dependence of galaxy morphologies on galaxy mergers

On the dependence of galaxy morphologies on galaxy mergers

The impact of galactic properties and environment on the quenching of central and satellite galaxies: a comparison between SDSS, Illustris and L-Galaxies

The Downfall of Massive Star-Forming Galaxies During the Last $$10\,\mathrm{Gyr}$$ 10 Gyr

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