The fate of high-redshift massive compact galaxies

Rosa, I. G. de la; Barbera, F. La; Ferreras, Ignacio; Alméida, J. Sánchez; Vecchia, Claudio Dalla; Martínez-Valpuesta, Inma; Stringer, Martin

doi:10.1093/mnras/stw130

Cited by 74 publications

(68 citation statements)

References 96 publications

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“…This is a simple and elegant solution which has since been supported by the results in de la Rosa et al (2016) and Margalef-Bentabol et al (2016). Moreover, it matches with evidence for nascent disks at high-z (e.g.…”

Section: Compact Massive Spheroids -Evolution or Notsupporting

confidence: 80%

“…Dullo & Graham (2013) further advocated that disks may have formed in and around these high-z mass concentrations to build the local lenticular galaxies. Nearly two dozen z ≈ 0 galaxies with massive compact spheroidal components have since been presented in Graham, Dullo & Savorgnan (2015, hereafter GDS15; see also Valentinuzzi et al 2010a,b;Poggianti et al 2013a,b;Saulder et al 2015;Carollo et al 2016;de la Rosa et al 2016). This sample included early-type galaxies in which the disk had not grown into a largescale disk that dominates the light at large radii but was instead an intermediate-scale disk 1 embedded within the spheroidal component of the galaxy 2 .…”

Section: Introductionmentioning

confidence: 99%

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Disky Elliptical Galaxies and the Allegedly Over-Massive Black Hole in the Compact Massive “Es” Galaxy NGC 1271

Graham

Ciambur

Savorgnan

2016

ApJ

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While spiral and lenticular galaxies have large-scale disks extending beyond their bulges, and most local early-type galaxies with 10 10 < M * /M < 2 × 10 11 contain a disk (e.g., ATLAS 3D ), the earlytype galaxies do possess a range of disk sizes. The edge-on, intermediate-scale disk in the 'disky elliptical' galaxy NGC 1271 has led to some uncertainty as to what is its spheroidal component. Walsh et al. reported a directly measured black hole mass of (3.09 M for this galaxy; which they remarked was an order of magnitude greater than what they expected based on their derivation of the host spheroid's luminosity. Our near-infrared image analysis supports a small embedded disk within a massive spheroidal component with M sph, * = (0.9 ± 0.2) × 10 11 M (using M * /L H = 1.4from Walsh et al.). This places NGC 1271 just 1.6-sigma above the near-linear M bh -M sph, * relation for early-type galaxies. Therefore, past speculation that there may be a systematic difference in the black hole scaling relations between compact massive early-type galaxies with intermediate-scale disks, i.e. ES galaxies such as NGC 1271, and early-type galaxies with either no substantial disk (E) or a large-scale disk (S0) is not strongly supported by NGC 1271. We additionally (i) show how ES galaxies fit naturally in the ('bulge'-to-total)-(morphological type) diagram, while noting a complication with recent revisions to the Hubble-Jeans tuning-fork diagram, (ii) caution about claims of over-massive black holes in other ES galaxies if incorrectly modelled as S0 galaxies, and (iii) reveal that the compact massive spheroid in NGC 1271 has properties similar to bright bulges in other galaxies which have grown larger-scale disks.

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Section: Compact Massive Spheroids -Evolution or Notsupporting

confidence: 80%

Section: Introductionmentioning

confidence: 99%

Disky Elliptical Galaxies and the Allegedly Over-Massive Black Hole in the Compact Massive “Es” Galaxy NGC 1271

Graham

Ciambur

Savorgnan

2016

ApJ

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“…Because r eff > r h here, our models have a somewhat massive central region, which may stem from the formation process, as the galaxies do not grow, but form in practically one monolithic collapse. These compact bulges may also be related to the observed red nuggets (de la Rosa et al 2016). This feature of our models will also be important in Section 4.6, where we show that they slightly lack stellar angular momentum.…”

Section: Comparison Between Newtonian and Mondian Modelsmentioning

confidence: 76%

The Formation of Exponential Disk Galaxies in MOND

Wittenburg

Kroupa

Famaey

2020

ApJ

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The formation and evolution of galaxies is highly dependent on the dynamics of stars and gas, which is governed by the underlying law of gravity. To investigate how the formation and evolution of galaxies takes place in Milgromian gravity (MOND), we present full hydrodynamical simulations with the Phantom of Ramses (POR) code. These are the first-ever galaxy formation simulations done in MOND with detailed hydrodynamics, including star formation, stellar feedback, radiative transfer and supernovae. These models start from simplified initial conditions, in the form of isolated, rotating gas spheres in the early Universe. These collapse and form late-type galaxies obeying several scaling relations, which was not a priori expected. The formed galaxies have a compact bulge and a disk with exponentially decreasing surface mass density profiles and scale lengths consistent with observed galaxies, and vertical stellar mass distributions with distinct exponential profiles (thin and thick disk). This work thus shows for the first time that disk galaxies with exponential profiles in both gas and stars are a generic outcome of collapsing gas clouds in MOND. These models have a slight lack of stellar angular momentum because of their somewhat compact stellar bulge, which is connected to the simple initial conditions and the negligible later gas accretion. We also analyse how the addition of more complex baryonic physics changes the main resulting properties of the models and find this to be negligibly so in the Milgromian framework.

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“…As far as the remaining 25% of dense ETGs possibly missing in the local Universe, stochastic merger events could have transformed them into non-dense systems (Σ ≤ 2500 M pc −2 ), contributing to the increase of the mean size and the number density of the whole population of ultramassive ETGs at z < 1.5. In fact, de la Rosa et al (2016) have found that a portion of presentday massive galaxies host in the centre a compact core with the same structural and dynamical properties as high-z compact galaxies. Numerically, the contribution of these size-evolved ultramassive dense ETGs to the total number density of local ultramassive ETGs is ∼2 × 10 −5 gal/Mpc3 (see Fig.…”

Section: Discussionmentioning

confidence: 99%

Ultramassive dense early-type galaxies: Velocity dispersions and number density evolution sincez= 1.6

Gargiulo

Saracco

Tamburri

et al. 2016

A&A

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Aims. We investigate the stellar mass assembly history of ultramassive (M 10 11 M ) dense (Σ = M /2πR 2 e > 2500 M pc −2 ) early-type galaxies (ETGs, elliptical and spheroidal galaxies) selected on basis of visual classification over the last 9 Gyr. Methods. We traced the evolution of the comoving number density ρ of ultramassive dense ETGs and compared their structural (effective radius R e and stellar mass M ) and dynamical (velocity dispersion σ e ) parameters over the redshift range 0 < z < 1.6. We derived the number density ρ at 1.6 < z < 1 from the MUNICS and GOODS-South surveys, while we took advantage of the COSMOS spectroscopic survey to probe the intermediate redshift range [0.2−1.0]. We derived the number density of ultramassive dense local ETGs from the SDSS sample taking all of the selection bias affecting the spectroscopic sample into account. To compare the dynamical and structural parameters, we collected a sample of 11 ultramassive dense ETGs at 1.2 < z < 1.6 for which velocity dispersion measurements are available. For four of these ETGs (plus one at z = 1.91), we present previously unpublished estimates of velocity dispersion, based on optical VLT-FORS2 spectra. We probe the intermediate redshift range (0.2 < ∼ z < ∼ 0.9) and the local Universe with different ETGs samples. Results. We find that the comoving number density of ultramassive dense ETGs evolves with z as ρ(z) ∝ (1 + z) 0.3 ± 0.8 implying a decrease of ∼25% of the population of ultramassive dense ETGs since z = 1.6. By comparing the structural and dynamical properties of high-z ultramassive dense ETGs over the range 0 < ∼ z < 1.6 in the [R e , M , σ e ] plane, we find that all of the ETGs of the high-z sample have counterparts with similar properties in the local Universe. This implies either that the majority (∼70%) of ultramassive dense ETGs already completed the assembly and shaping at z = 1.4, or that, if a significant portion of dense ETGs evolves in size, new ultramassive dense ETGs must form at z < 1.5 to maintain their number density at almost constant. The difficulty in identify good progenitors for these new dense ETGs at z < ∼ 1.5 and the stellar populations properties of local ultramassive dense ETGs point towards the first hypothesis. In this case, the ultramassive dense galaxies missing in the local Universe could have joined, in the last 9 Gyr, the so colled non-dense ETGs population through minor mergers, thus contributing to mean size growth. In any case, the comparison between their number density and the number density of the whole population of ultramassive ETGs relegates their contribution to the mean size evolution to a secondary process.

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The fate of high-redshift massive compact galaxies

Cited by 74 publications

References 96 publications

Disky Elliptical Galaxies and the Allegedly Over-Massive Black Hole in the Compact Massive “Es” Galaxy NGC 1271

Disky Elliptical Galaxies and the Allegedly Over-Massive Black Hole in the Compact Massive “Es” Galaxy NGC 1271

The Formation of Exponential Disk Galaxies in MOND

Ultramassive dense early-type galaxies: Velocity dispersions and number density evolution sincez= 1.6

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