Enhancing and inhibiting star formation: high-resolution simulation studies of the impact of cold accretion, mergers and feedback on individual massive galaxies

Powell, Leila C.; Bournaud, F.; Chapon, Damien; Devriendt, Julien; Gaibler, Volker; Khochfar, Sadegh; Slyz, Adrianne; Teyssier, Romain

doi:10.1017/s1743921313004158

Cited by 2 publications

(1 citation statement)

References 9 publications

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“…Therefore, we still have to wait to properly understand how SNE feedback can possibly affect the CW emergence and dynamics. However, the findings so far, at high z, suggest that the filamentary patterns are essentially untouched by SNe feedback (Powell et al 2013). …”

Section: Discussionmentioning

confidence: 91%

Lagrangian volume deformations around simulated galaxies

Robles

Domínguez-Tenreiro

Oñorbe

et al. 2015

Monthly Notices of the Royal Astronomical Society

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El acceso a la versión del editor puede requerir la suscripción del recurso Access to the published version may require subscription ABSTRACTWe present a detailed analysis of the local evolution of 206 Lagrangian Volumes (LVs) selected at high redshift around galaxy seeds, identified in a large-volume Λ cold dark matter (ΛCDM) hydrodynamical simulation. The LVs have a mass range of 1 − 1500 × 10 10 M . We follow the dynamical evolution of the density field inside these initially spherical LVs from z = 10 up to z low = 0.05, witnessing highly non-linear, anisotropic mass rearrangements within them, leading to the emergence of the local cosmic web (CW). These mass arrangements have been analysed in terms of the reduced inertia tensor I r ij , focusing on the evolution of the principal axes of inertia and their corresponding eigendirections, and paying particular attention to the times when the evolution of these two structural elements declines. In addition, mass and component effects along this process have also been investigated. We have found that deformations are led by dark matter dynamics and they transform most of the initially spherical LVs into prolate shapes, i.e. filamentary structures. An analysis of the individual freezing-out time distributions for shapes and eigendirections shows that first most of the LVs fix their three axes of symmetry (like a skeleton) early on, while accretion flows towards them still continue. Very remarkably, we have found that more massive LVs fix their skeleton earlier on than less massive ones. We briefly discuss the astrophysical implications our findings could have, including the galaxy mass-morphology relation and the effects on the galaxy-galaxy merger parameter space, among others.

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Section: Discussionmentioning

confidence: 91%

Lagrangian volume deformations around simulated galaxies

Robles

Domínguez-Tenreiro

Oñorbe

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Deciphering an evolutionary sequence of merger stages in infrared-luminous starburst galaxies atz∼ 0.7

Calabró

Daddi

Puglisi

et al. 2019

A&A

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Based on optical/near-IR Magellan FIRE spectra of 25 starburst galaxies at 0.5 < z < 0.9, Calabrò et al. (2018) showed that their attenuation properties can be explained by a single-parameter sequence of total obscurations ranging from A V = 2 to A V = 30 towards the starburst core centers in a mixed stars and dust configuration. We investigate here the origin of this sequence for the same sample. We show that total attenuations anti-correlate with the starburst sizes in radio (3 GHz) with a significance larger than 5σ and a scatter of 0.26 dex. More obscured and compact starbursts also show enhanced N2 (=[NII]/Hα) ratios and larger line velocity widths that we attribute to an increasing shock contribution toward later merger phases, driven by deeper gravitational potential wells at the coalescence. Additionally, the attenuation is also linked to the equivalent width (EW) of hydrogen recombination lines, which is sensitive to the luminosity weighted age of the relatively unobscured stellar populations. Overall, the correlations among A V , radio size, line width, N2 and EW of Balmer/Paschen lines converge towards suggesting an evolutionary sequence of merger stages: all of these quantities are likely to be good time-tracers of the merger phenomenon, and their large spanned range appears to be characteristic of the different merger phases. Half of our sample at higher obscurations have radio sizes approximately 3 times smaller than early type galaxies at the same redshift, suggesting that, in analogy with local Ultraluminous Infrared galaxies (ULIRGs), these cores cannot be directly forming elliptical galaxies. Finally, we detect mid-IR AGN torus for half of our sample and additional X-ray emission for 6 starbursts; intriguingly, the latter have systematically more compact sizes, suggestive of emerging AGNs towards later merger stages, possibly precursors of a later QSO phase.

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Enhancing and inhibiting star formation: high-resolution simulation studies of the impact of cold accretion, mergers and feedback on individual massive galaxies

Cited by 2 publications

References 9 publications

Lagrangian volume deformations around simulated galaxies

Lagrangian volume deformations around simulated galaxies

Deciphering an evolutionary sequence of merger stages in infrared-luminous starburst galaxies atz∼ 0.7

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