Evolution of density profiles in high-<i>z</i>galaxies: compaction and quenching inside-out

Tacchella, Sandro; Dekel, Avishai; Carollo, C. M.; Ceverino, Daniel; DeGraf, Colin; Lapiner, Sharon; Mandelker, Nir; Primack, Joel R.

doi:10.1093/mnras/stw303

Cited by 262 publications

(285 citation statements)

References 151 publications

(256 reference statements)

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“…Cheung et al 2012;Fang et al 2013; and suggests that the immediate starforming progenitors of quiescent galaxies experience a phase of stronger core growth that increases their concentration with respect to galaxies growing along the M  Srelations. At high redshifts, this phase is consistent with the compaction evolutionary tracks predicted in hydrodynamical simulations (Ceverino et al 2015;Zolotov et al 2015;Tacchella et al 2016), which are typically associated with strongly dissipational (gas-rich) processes such as major mergers and interaction driven gravitational instabilities (Dekel et al 2009a;Ceverino et al 2010;. At lower redshifts, these gas-rich processes probably coexist with minor mergers and secular instabilities (e.g., bars and spiral arms; Kormendy & Kennicutt 2004).…”

Section: Discussionsupporting

confidence: 80%

“…The evolution of these tracks at lower redshift, however, differs substantially from that of fully quenched galaxies, which are expected to grow in mass only by merging. These massive simulations have quenched cores, but they still exhibit star formation (and therefore mass growth) in a regrown disk (Zolotov et al 2015;Tacchella et al 2016). The newly formed disk causes a sudden increase in size, which leads to decreasing tracks with mass in e S , but nearly flat tracks in 1 S (see also Figure 19 of Zolotov et al 2015).…”

Section: B~) the Steep Increase In Ementioning

confidence: 99%

“…Some of these processes, like mergers and disk instabilities, are indeed expected to be more frequent at earlier times due to the higher gas-to-total mass ratios in SFGs (Daddi et al 2010;Tacconi et al 2010Tacconi et al , 2013. The increased gas mass relative to the SFR makes such systems prone to gravitational collapse on scales of ∼1 kpc, causing substantial core growth resulting from a gasfed central starburst and/or an inward migration of clumps (Dekel et al 2009b;Ceverino et al 2010Ceverino et al , 2015Genel et al 2014;Wellons et al 2015Wellons et al , 2016Zolotov et al 2015;Bournaud 2016;Tacchella et al 2016). At lower redshifts, SFGs with dense cores have clearly recognizable disk structures, but their profiles are dominated by a central bulge (Bruce et al 2012(Bruce et al , 2014aWuyts et al 2012;Mortlock et al 2013;Lang et al 2014;Morishita et al 2015;Abramson et al 2016;Margalef-Bentabol et al 2016;Schreiber et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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

Barro

Faber

Koo

et al. 2017

ApJ

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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: Discussionsupporting

confidence: 80%

Section: B~) the Steep Increase In Ementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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

Barro

Faber

Koo

et al. 2017

ApJ

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270

384

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“…This behavior suggests that galaxies are quenched inside-out and that this process is faster in the bulge-dominated regions than in the disks. A similar result is found by Tacchella et al (2016) analyzing a sample of star forming galaxies at z ∼ 2.2. These results are interpreted as evidence of the morphological quenching that these galaxies experience in the growth of their central bulges.…”

Section: Previous Worksupporting

confidence: 85%

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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“…The compactions produce compact starforming blue nuggets and may activate central AGNs. These trigger gas depletion from the centre and lead to inside-out quenching (Tacchella et al 2015b;Zolotov et al 2015). The sequence of compaction and quenching attempts can explain the confinement of star-forming galaxies into a narrow main sequence (Tacchella et al 2015c).…”

Section: Discussionmentioning

confidence: 99%

Evolution of galaxy shapes from prolate to oblate through compaction events

Tomassetti

Dekel²,

Mandelker³

et al. 2016

Mon. Not. R. Astron. Soc.

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We study the evolution of global shapes of galaxies using cosmological simulations. The shapes refer to the components of dark matter (DM), stars and gas at the stellar half-mass radius. Most galaxies undergo a characteristic compaction event into a blue nugget at z ∼ 2 − 4, which marks the transition from a DM-dominated central body to a self-gravitating baryonic core. We find that in the high-z, DM-dominated phase, the stellar and DM systems tend to be triaxial, preferentially prolate and mutually aligned. The elongation is supported by an anisotropic velocity dispersion that originates from the assembly of the galaxy along a dominant large-scale filament. We estimate that torques by the dominant halo are capable of inducing the elongation of the stellar system and its alignment with the halo. Then, in association with the transition to self-gravity, small-pericenter orbits puff up and the DM and stellar systems evolve into a more spherical and oblate configuration, aligned with the gas disc and associated with rotation. This transition typically occurs when the stellar mass is ∼ 10 9 M and the escape velocity in the core is ∼ 100 km s −1 , indicating that supernova feedback may be effective in keeping the core DM-dominated and the system prolate. The early elongated phase itself may be responsible for the compaction event, and the transition to the oblate phase may be associated with the subsequent quenching in the core.

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Evolution of density profiles in high-zgalaxies: compaction and quenching inside-out

Cited by 262 publications

References 151 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

Evolution of galaxy shapes from prolate to oblate through compaction events

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