THE MORPHOLOGIES OF MASSIVE GALAXIES FROM<i>z</i>∼ 3—WITNESSING THE TWO CHANNELS OF BULGE GROWTH

Huertas-Company, M.; Pérez‐González, Pablo G.; Mei, S.; Shankar, Francesco; Bernardi, Mariangela; Daddi, E.; Barro, Guillermo; Cabrera-Vives, G.; Cattaneo, Andrea; Dimauro, Paola; Gravet, R.

doi:10.1088/0004-637x/809/1/95

Cited by 84 publications

(84 citation statements)

References 110 publications

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“…This is consistent with the idea that compact SFGs are formed from extended SFGs, which are mostly disk dominated at low z, by increasing their central densities. The evolution toward disk-like morphologies with progressively bigger cores is consistent with the prominence of disks with bulges among massive SFGs at z 1  , as reported in previous works (e.g., Bruce et al 2012Bruce et al , 2014aBuitrago et al 2013;McLure et al 2013;Mortlock et al 2013;Lang et al 2014;Huertas-Company et al 2015). Note that rejuvenation and/or the re-growth of a star-forming disk in compact SFGs is also a possibility, although the increasing number of quiescent galaxies with time suggests that the net flow of galaxies is preferentially toward compaction and quenching.…”

Section: Galaxy Morphologies In the Sfrsupporting

confidence: 90%

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Barro

Faber

Koo

et al. 2017

ApJ

270

384

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We study the evolution of the scaling relations that compare the effective density ( r r , e e S < ) and core density ( r , 1 1 S < kpc) to the stellar masses of star-forming galaxies (SFGs) and quiescent galaxies. These relations have been fully in place since z 3 and have exhibited almost constant slope and scatter since that time. For SFGs, the zero points in e S and 1 S decline by only 2 . This fact plus the narrowness of the relations suggests that galaxies could evolve roughly along the scaling relations. Quiescent galaxies follow different scaling relations that are offset to higher densities at the same mass and redshift. Furthermore, the zero point of their core density has declined by only 2 since z 3 , while the zero point of the effective density declines by 10 . When galaxies quench, they move from the star-forming relations to the quiescent relations. This involves an increase in the core and effective densities, which suggests that SFGs could experience a phase of significant core growth relative to the average evolution along the structural relations. The distribution of massive galaxies relative to the SFR-M and the quiescent M  Srelations exhibits an L-shape that is independent of redshift. The knee of this relation consists of a subset of "compact" SFGs that are the most likely precursors of quiescent galaxies forming at later times. The compactness selection threshold in 1 S exhibits a small variation from z=3 to 0.5, M 0.65 log 10.5 9.6 9.3 1 * S --> -( ) M e kpc −2 , allowing the most efficient identification of compact SFGs and quiescent galaxies at every redshift.

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Section: Galaxy Morphologies In the Sfrsupporting

confidence: 90%

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Barro

Faber

Koo

et al. 2017

ApJ

270

384

View full text Add to dashboard Cite

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“…It has been suggested that dry mergers are the main driver for this late size evolution, expanding their envelope by means of small satellite accretion (Naab et al 2009;Bell et al 2004). Indeed, z ∼ 1 has been identified as an epoch of galaxy merging (Hammer et al 2005;Kaviraj et al 2015), in which the progenitors of ETG increase in size and mass in proportion to one another, following approximately ∆ log R e ∼ 2 × ∆ log M (van Dokkum et al 2010Dokkum et al , 2015Huertas-Company et al 2015). This relation predicts that from z = 2 to 0.4 ETGs with a presentday mass of 3 × 10 11 increase their effective radii from R e ∼ 2.5 to 6 kpc, and their stellar mass by a factor of ∼ 1.5.…”

Section: Discussion: Sfh Constraints On Galaxy Formation Scenariosmentioning

confidence: 99%

Spatially-resolved star formation histories of CALIFA galaxies

Delgado

Pérez

Fernandes

et al. 2017

A&A

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This paper presents the spatially resolved star formation history (SFH) of nearby galaxies with the aim of furthering our understanding of the different processes involved in the formation and evolution of galaxies. To this end, we apply the fossil record method of stellar population synthesis to a rich and diverse data set of 436 galaxies observed with integral field spectroscopy in the CALIFA survey. The sample covers a wide range of Hubble types, with stellar masses ranging from M ∼ 10 9 to 7 × 10 11 M . Spectral synthesis techniques are applied to the datacubes to retrieve the spatially resolved time evolution of the star formation rate (SFR), its intensity (Σ SFR ), and other descriptors of the 2D-SFH in seven bins of galaxy morphology (E, S0, Sa, Sb, Sbc, Sc, and Sd), and five bins of stellar mass. Our main results are: (a) Galaxies form very fast independently of their current stellar mass, with the peak of star formation at high redshift (z > 2). Subsequent star formation is driven by M and morphology, with less massive and later type spirals showing more prolonged periods of star formation. (b) At any epoch in the past the SFR is proportional to M , with most massive galaxies having the highest absolute (but lowest specific) SFRs. (c) While nowadays Σ SFR is similar for all spirals, and significantly lower in early type galaxies (ETG), in the past Σ SFR scales well with morphology. The central regions of today's ETGs are where Σ SFR reached the highest values (> 10 3 M Gyr −1 pc −2 ), similar to those measured in high redshift star forming galaxies. (d) The evolution of Σ SFR in Sbc systems matches that of models for Milky-Way-like galaxies, suggesting that the formation of a thick disk may be a common phase in spirals at early epochs. (e) The SFR and Σ SFR in outer regions of E's and S0's show that they have undergone an extended phase of growth in mass between z = 2 and 0.4. The mass assembled in this phase is in agreement with the two-phase scenario proposed for the formation of ETG. (f) Evidence of an early and fast quenching is found only in the most massive (M > 2 × 10 11 M ) E galaxies of the sample, but not in spirals of similar mass, suggesting that halo-quenching is not the main mechanism for the shut down of star formation in galaxies. Less massive E and disk galaxies show more extended SFHs and a slow quenching. (g) Evidence of fast quenching is also found in the nuclei of ETG and early spirals, with SFR and Σ SFR indicating that they can be the relic of the "red nuggets" detected at high redshift.

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“…In this respect, mounting evidence for a nearly environment-independent flattening in the star formation rate-stellar mass relation at high Mstar (e.g., Erfanianfar et al 2016, and references therein), paralleling an increased incidence of bulge-dominated galaxies, is also suggestive. The increase in host velocity dispersion may in fact be correlated with the growth of a central black hole; the associated feedback can reduce star formation, though alternative explanations in terms of, e.g., morphological transformations, may still be viable solutions (e.g., Martig et al 2009;Huertas-Company et al 2015).…”

Section: Implications For the Co-evolution Of Black Holes And Galaxiesmentioning

confidence: 99%

Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation

Shankar¹,

Bernardi²,

Sheth³

et al. 2016

Mon. Not. R. Astron. Soc.

250

369

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We compare the set of local galaxies having dynamically measured black holes with a large, unbiased sample of galaxies extracted from the Sloan Digital Sky Survey. We confirm earlier work showing that the majority of black hole hosts have significantly higher velocity dispersions σ than local galaxies of similar stellar mass. We use Monte-Carlo simulations to illustrate the effect on black hole scaling relations if this bias arises from the requirement that the black hole sphere of influence must be resolved to measure black hole masses with spatially resolved kinematics. We find that this selection effect artificially increases the normalization of the M bh -σ relation by a factor of at least ∼ 3; the bias for the M bh -M star relation is even larger. Our Monte Carlo simulations and analysis of the residuals from scaling relations both indicate that σ is more fundamental than M star or effective radius. In particular, the M bh -M star relation is mostly a consequence of the M bh -σ and σ-M star relations, and is heavily biased by up to a factor of 50 at small masses. This helps resolve the discrepancy between dynamically-based black hole-galaxy scaling relations versus those of active galaxies. Our simulations also disfavour broad distributions of black hole masses at fixed σ. Correcting for this bias suggests that the calibration factor used to estimate black hole masses in active galaxies should be reduced to values of f vir ∼ 1. Black hole mass densities should also be proportionally smaller, perhaps implying significantly higher radiative efficiencies/black hole spins. Reducing black hole masses also reduces the gravitational wave signal expected from black hole mergers.

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THE MORPHOLOGIES OF MASSIVE GALAXIES FROMz∼ 3—WITNESSING THE TWO CHANNELS OF BULGE GROWTH

Cited by 84 publications

References 110 publications

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Spatially-resolved star formation histories of CALIFA galaxies

Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation

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