We use the Illustris simulation to study relative contributions of in situ star formation and stellar accretion build-up galaxies over an unprecedentedly wide range masses (M* = 109-1012 M⊙), galaxy types, environments, assembly histories. find that 'two-phase' picture predicted by some models is a good approximation only for most massive our – namely, mass growth below few times 1011 M⊙ dominated at all redshifts. The fraction total z 0 contributed accreted stars shows strong dependence on...

Massive, quiescent galaxies at high redshift have been found to be considerably more compact than of similar mass in the local universe. How these formed has yet determined, though several progenitor populations proposed. Here we investigate formation processes and quantify assembly histories such Illustris, a suite hydrodynamical cosmological simulations encompassing sufficiently large volume include rare objects, while simultaneously resolving internal structure galaxies. We select massive...

It has recently become possible to zoom-in from cosmological sub-pc scales in galaxy simulations follow accretion onto supermassive black holes (SMBHs). However, at some point the approximations used on ISM (e.g. optically-thin cooling and stellar-population-integrated star formation [SF] feedback [FB]) break down. We therefore present first radiation-magnetohydrodynamic (RMHD) simulation which self-consistently combines FIRE physics (relevant galactic/ISM where SF/FB are ensemble-averaged)...

Massive quiescent galaxies have much smaller physical sizes at high redshift than today. The strong evolution of galaxy size may be caused by progenitor bias, major and minor mergers, adiabatic expansion, and/or renewed star formation, but it is difficult to test these theories observationally. Herein, we select a sample 35 massive, compact ($M_* = 1-3 \times 10^{11}$ M$_\odot$, $M_*/R^{1.5} > 10^{10.5}$ M$_\odot$/kpc$^{1.5}$) $z=2$ in the cosmological hydrodynamical simulation Illustris...

ABSTRACT Feedback from accreting supermassive black holes (SMBHs) is thought to be a primary driver of quenching in massive galaxies, but how best implement SMBH physics into galaxy formation simulations remains ambiguous. As part the Realistic Environments (FIRE) project, we explore effects different modelling choices for accretion and feedback suite ∼500 cosmological zoom-in across wide range halo mass (1010–1013 M⊙). Within suite, vary numerical schemes BH feedback, efficiency, strength...

Negative feedback from accreting supermassive black holes is regarded as a key ingredient in suppressing star formation and quenching massive galaxies. However, several models observations suggest that hole may have positive effect, triggering by compressing interstellar medium gas to higher densities. We investigate the dual role of using cosmological hydrodynamic simulations Feedback In Realistic Environments (FIRE) project, including novel implementation hyper-refined accretion-disc...

In a companion paper, we reported the self-consistent formation of quasar accretion disks with inflow rates $\sim 10\,{\rm M_{\odot}\,yr^{-1}}$ down to <300 Schwarzschild radii from cosmological radiation-magneto-thermochemical-hydrodynamical galaxy and star simulations. We see well-defined, steady-state disk which is stable against at sub-pc scales. The are optically thick, radiative cooling balancing accretion, but properties that distinct those assumed in most previous models. pressure...

The origin of highly magnetized white dwarfs has remained a mystery since their initial discovery. Recent observations indicate that the formation high-field magnetic is intimately related to strong binary interactions during post-main-sequence phases stellar evolution. If low-mass companion, such as planet, brown dwarf, or star, engulfed by giant, gravitational torques in envelope giant lead reduction companion's orbit. Sufficiently companions in-spiral until they are shredded tides near...

We present an analysis of the evolving comoving cumulative number density galaxy populations found in Illustris simulation. Cumulative is commonly used to link across different epochs by assuming that galaxies preserve their time. Our allows us examine extent which this assumption holds presence mergers or when rank ordering broken owing variable stellar growth rates. primary results are as follows: (1) inferred average mass evolution obtained via a constant systematically biased compared...

Without additional heating, radiative cooling of gas in the halos massive galaxies (Milky Way and above) produces cold or stars excess that observed. Previous work suggested AGN jets are likely required, but form jet energy required to quench remains unclear. This is particularly challenging for galaxy simulations, which resolution orders magnitude coarser than necessary evolve jet. On such scales, uncertain parameters include: (kinetic, thermal, cosmic ray (CR) energy), energy, momentum,...

ABSTRACT We identify the first quiescent galaxies in TNG300, largest volume of IllustrisTNG cosmological simulation suite, and explore their quenching processes time evolution to z = 0. find that with stellar masses M* &amp;gt; 3 × 1010 M⊙ specific star formation rates sSFR &amp;lt; 10−11 yr−1 emerge at ∼ 4.2 TNG300. Suppression these begins a thermal mode active galactic nucleus feedback 6, kinetic acts each galaxy by 4.7 complete process, which occurs on time-scale ∼0.35 Gyr. Surprisingly,...

Several recent simulations of galaxy formation predict two main phases supermassive black hole (BH) accretion: an early, highly intermittent phase (during which BHs are under-massive relative to local scaling relations), followed by a accelerated growth. We investigate physical factors that drive the transition in BH accretion cosmological zoom-in from FIRE project, ranging dwarf galaxies sufficiently massive host luminous quasars. The model multi-channel stellar feedback, but neglect AGN...

Recent numerical cosmological radiation-magnetohydrodynamic-thermochemical-star formation simulations have resolved the of quasar accretion disks with Eddington or super-Eddington rates onto supermassive black holes (SMBHs) down to a few hundred gravitational radii. These 'flux-frozen' and hyper-magnetized appear be qualitatively distinct from classical $\alpha$ magnetically-arrested disks: midplane pressure is dominated by toroidal magnetic fields plasma $\beta \ll 1$ powered advection flux...

We present extensive radio observations of the nearby Type Ibc supernovae 2004cc, 2004dk, and 2004gq spanning 8-1900 days after explosion. Using a dynamical model developed for synchrotron emission from slightly decelerated shockwave, we estimate velocity energy fastest ejecta density profile circumstellar medium. The shockwaves all three are characterized by non-relativistic velocities v ~ (0.1-25)c associated energies E (2-10) * 1e47 erg, in line with expectations typical homologous Smooth...

Pressure balance plays a central role in models of the interstellar medium (ISM), but whether and how pressure is realized realistic multiphase ISM not yet well understood. We address this question using set FIRE-2 cosmological zoom-in simulations Milky Way-mass disk galaxies, which self-consistently shaped by gravity, cooling, stellar feedback. analyze gravity determines vertical profile as total partitioned between different phases components (thermal, dispersion/turbulence, bulk flows)....

ABSTRACT Without active galactic nucleus (AGN) feedback, simulated massive, star-forming galaxies become too compact relative to observed at z ≲ 2. In this paper, we perform high-resolution re-simulations of a massive ($M_{\star }\sim 10^{11}\, \rm {{\rm M}_{\odot }}$) galaxy ∼ 2.3, drawn from the Feedback in Realistic Environments (FIRE) project. simulation without AGN experiences rapid starburst and shrinking its half-mass radius. We experiment with driving mechanical winds, using...

Abstract The far-infrared–radio correlation (FRC) is one of the most promising empirical constraints on role cosmic rays (CRs) and magnetic fields in galaxy formation evolution. While many theories have been proposed order to explain emergence maintenance FRC across a gamut properties redshift, nonlinear physics at play remain unexplored full complexity within cosmological context. We present first reproduction z ∼ 0 using detailed synthetic observations state-of-the-art zoom-in simulations...

Recent radiation-thermochemical-magnetohydrodynamic simulations resolved formation of quasar accretion disks from cosmological scales down to ~300 gravitational radii $R_{g}$, arguing they were 'hyper-magnetized' (plasma $\beta\ll1$ supported by toroidal magnetic fields) and distinct traditional $\alpha$-disks. We extend these, refining $\approx 3\,R_{g}$ around a $10^{7}\,{\rm M_{\odot}}$ BH with multi-channel radiation thermochemistry, exploring factor 1000 range rates...

ABSTRACT The galaxy size–stellar mass and central surface density–stellar relationships are fundamental observational constraints on formation models. However, inferring the physical size of a from observed stellar emission is non-trivial due to various effects, such as mass-to-light ratio variations that can be caused by non-uniform ages, metallicities, dust attenuation. Consequently, forward-modelling light-based sizes simulations desirable. In this work, we use skirt radiative transfer...

Advances in instrumentation have recently extended detailed measurements of gas kinematics to large samples high-redshift galaxies. Relative most nearby, thin disk galaxies, which rotation accurately traces the gravitational potential, interstellar medium (ISM) z>1 galaxies is typically more dynamic and exhibits elevated turbulence. If not properly modeled, these effects can strongly bias dynamical mass measurements. We use high-resolution FIRE-2 cosmological zoom-in simulations analyze...

ABSTRACT We investigate the formation of dense stellar clumps in a suite high-resolution cosmological zoom-in simulations massive, star-forming galaxy at z ∼ 2 under presence strong quasar winds. Our include multiphase ISM physics from Feedback In Realistic Environments (FIRE) project and novel implementation hyper-refined accretion disc show that powerful winds can have global negative impact on growth while strongest cases triggering an off-centre clump with mass ${\rm M}_{\star }\sim...

While galaxy rotation curves provide one of the most powerful methods for measuring dark matter profiles in inner regions rotation-supported galaxies, at dwarf scale there are factors that can complicate this analysis. Given expectation a universal profile matter-only simulations, diversity observed has become an often-discussed issue Lambda Cold Dark Matter cosmology on galactic scales. We analyze suite Feedback Realistic Environments (FIRE) simulations $10^{10}-10^{12}$ $M_\odot$ halos...

Abstract Feedback from supermassive black holes is believed to be a critical driver of the observed color bimodality galaxies above Milky Way mass scale. Active galactic nuclei (AGN) feedback has been modeled in many galaxy formation simulations, but most implementations have involved simplified prescriptions or coarse-grained interstellar medium (ISM). We present first set In Realistic Environments (FIRE)-3 cosmological zoom-in simulations with AGN evolved z ∼ 0, examining impact on halos...

Galaxy comoving number density is commonly used to forge progenitor/descendant links between observed galaxy populations at different epochs. However, this method breaks down in the presence of mergers, or when galaxies experience stochastic growth rates. We present a simple analytic framework treat physical processes that drive evolution and diffusion within space. The mass rank order population with time influenced by coagulation rate "mass scatter" rate. quantify relative contribution...

Previous studies of fueling black holes (BHs) in galactic nuclei have argued (on scales ~0.01-1000pc) accretion is dynamical with inflow rates $\dot{M}\simη\,M_{\rm gas}/t_{\rm dyn}$ terms gas mass $M_{\rm gas}$, time $t_{\rm dyn}$, and some $η$. But these models generally neglected expulsion by stellar feedback, or considered extremely high densities where inefficient. Studies star formation, however, shown on sub-kpc the efficiency $f_{\rm wind}=M_{\rm ejected}/M_{\rm total}$ gravitational...