Physics of Galactic Metals: Evolutionary Effects due to Production, Distribution, Feedback, and Interaction with Black Holes

Choi, Ena; Ostriker, Jeremiah P.; Naab, Thorsten; Somerville, Rachel S.; Hirschmann, Michaela; Núñez, Alejandro; Hu, Chia-Yu; Oser, Ludwig

doi:10.3847/1538-4357/aa7849

Cited by 67 publications

(121 citation statements)

References 148 publications

(194 reference statements)

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“…Additionally, the investment in computational time for higher-resolution simulations appears justifiable only after an improvement of contemporary models, which in some respects suffer from significant deficits. For instance, simulations on larger spatial scales (out to R eff ) by Hirschmann et al (2013) and Choi et al (2017) always predict strongly positive age gradients in massive (log(M ,T /M )>10) galaxies (Hirschmann et al 2015), which indicates that better prescriptions or additional physical processes need to be implemented.…”

Section: Discussionmentioning

confidence: 99%

Stellar age gradients and inside-out star formation quenching in galaxy bulges

Breda

Papaderos

Gomes

et al. 2020

A&A

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Radial age gradients hold the cumulative record of the multitude of physical processes driving the build-up of stellar populations and the ensuing star formation (SF) quenching process in galaxy bulges, therefore potentially sensitive discriminators between competing theoretical concepts on bulge formation and evolution. Based on spectral modeling of integral field spectroscopy (IFS) data from the CALIFA survey, we derive mass-and light-weighted stellar age gradients (∇(t ,B ) L,M ) within the photometrically determined bulge radius (R B ) of a representative sample of local face-on late-type galaxies that span 2.6 dex in stellar mass (8.9 ≤ logM ,T ≤ 11.5). Our analysis documents a trend for decreasing ∇(t ,B ) L,M with increasing M ,T , with high-mass bulges predominantly showing negative age gradients and vice versa. The inversion from positive to negative ∇(t ,B ) L,M occurs at logM ,T 10, which roughly coincides with the transition from lower-mass bulges whose gas excitation is powered by SF to bulges classified as Composite, LINER or Seyfert. We discuss two simple limiting cases for the origin of radial age gradients in massive LTG bulges. The first one assumes that the stellar age in the bulge is initially spatially uniform (∇(t ,B ) L,M ≈ 0), thus the observed age gradients (∼ -3 Gyr/R B ) arise from an inside-out SF quenching (ioSFQ) front that is radially expanding with a mean velocity v q . In this case, the age gradients for massive bulges translate into a slow (v q ∼1-2 km s −1 ) ioSFQ that lasts until z ∼ 2, suggesting mild negative feedback by SF or an AGN. If, on the other hand, negative age gradients in massive bulges are not due to ioSFQ but primarily due to their inside-out formation process, then the standard hypothesis of quasi-monolithic bulge formation has to be discarded in favor of a scenario that involves gradual buildup of stellar mass over 2-3 Gyr through, e.g., inside-out SF and inward migration of SF clumps from the disk. In this case, rapid ( 1 Gyr) AGN-driven ioSFQ cannot be ruled out. While the M ,T vs. ∇(t ,B ) L,M relation suggests that the assembly history of bulges is primarily regulated by galaxy mass, its large scatter (∼1.7 Gyr/R B ) reflects a considerable diversity that calls for an in-depth examination of the role of various processes (e.g., negative and positive AGN feedback, bar-driven gas inflows) with higher-quality IFS data in conjunction with advanced spectral modeling codes.

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Section: Discussionmentioning

confidence: 99%

Stellar age gradients and inside-out star formation quenching in galaxy bulges

Breda

Papaderos

Gomes

et al. 2020

A&A

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“…3). This high rate of BH accretion in turn results in a phase of significant gas heating and ejection, so that the total galaxy stellar mass remains constant after z ∼ 1, as in-situ star formation is strongly suppressed due to the lack of available dense gas (see also Choi et al 2017). Also the warm gas fractions are strongly reduced after z ∼ 1, causing subsequent fluctuations in all three irregularity parameters.…”

Section: Galaxy 0094mentioning

confidence: 99%

“…The sets of simulated galaxies, examined in this work, have been introduced by Hirschmann et al (2017) and Choi et al (2017), and we urge readers to consult these works for more details beyond the brief summary we provide here.…”

Section: Simulation Samplementioning

confidence: 99%

Ionized gas kinematics of massive elliptical galaxies in CALIFA and in cosmological zoom-in simulations

Florian

Ziegler

Hirschmann

et al. 2020

A&A

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Context. Powerful Active Galactic Nuclei (AGN) are supposed to play a key regulatory role on the evolution of their host galaxies by shaping the thermodynamic properties of their gas component. However, little is known as to the nature and the visibility timescale of the kinematical imprints of AGN-driven feedback. Gaining theoretical and observational insights into this subject is indispensable for a thorough understanding of the AGN-galaxy co-evolution and could yield empirical diagnostics for the identification of galaxies that have experienced a major AGN episode in the past. Aims. We present an investigation of kinematical imprints of AGN feedback on the Warm Ionized gas Medium (WIM) of massive early-type galaxies (ETGs). To this end, we take a two-fold approach that involves a comparative analysis of Hα velocity fields in 123 local ETGs from the CALIFA integral field spectroscopy survey with 20 simulated galaxies from high-resolution hydrodynamic cosmological SPHgal simulations. The latter were re-simulated for two modeling setups, one with and another without AGN feedback. Methods. In order to quantify the effects of AGN feedback on gas kinematics we measure three parameters that probe deviations from simple regular rotation using the kinemetry package. These indicators trace the possible presence of distinct kinematic components in Fourier space (k3,5/k1), variations in the radial profile of the kinematic major axis (σPA), and offsets between the stellar and gas velocity fields (∆φ). These quantities are monitored in the simulations from a redshift 3 to 0.2 to assess the connection between black hole accretion history, stellar mass growth and kinematical perturbation of the WIM. Results. Observed local massive galaxies show a broad range of irregularities, indicating disturbed warm gas motions, irrespective of being classified via diagnostic lines as AGN or not. Simulations of massive galaxies with AGN feedback generally exhibit higher irregularity parameters than without AGN feedback, more consistent with observations. Besides AGN feedback, other processes like major merger events or infalling gas clouds can lead to elevated irregularity parameters, but they are typically of shorter duration. More specifically, k3,5/k1 is most sensitive to AGN feedback, whereas ∆φ is most strongly affected by gas infall. Conclusions. We conclude that even if the general disturbance of the WIM velocity is not a unique indicator for AGN feedback, irregularity parameters, high enough to be consistent with observations, can only be reproduced in simulations with AGN feedback. Specifically, an elevated value for the deviation from simple ordered motion is a strong sign for previous events of AGN activity and feedback.

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“…They can reproduce the observational results and compare the X-ray properties in detail [5][6][7][8]. References [5,6] applied 2D high-resolution hydro simulations and considered stellar feedback, dynamical (rotation), and structural (flattening) parameters as well as AGN feedback, and References [7,8] applied 3D cosmological simulations. While the differences among different simulations and different parameters/recipes are to yet be understood, in general they can reproduce the observed relations among L X,GAS , T GAS , M TOTAL (or M within 5 Re).…”

Section: Comparison With Simulationsmentioning

confidence: 99%

“…Recent numerical simulation studies [5][6][7][8] have further attempted to reproduce the observed scaling relations, in order to constrain the physical mechanisms that shape the hot ISM.…”

Section: X-ray Scaling Relationsmentioning

confidence: 99%

Hot Gaseous Halos in Early Type Galaxies

Kim

2017

Galaxies

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The hot gas in early type galaxies (ETGs) plays a crucial role in their formation and evolution. As the hot gas is often extended to the outskirts beyond the optical size, the large scale structural features identified by Chandra (including cavities, cold fronts, filaments, and tails) point to key evolutionary mechanisms, e.g., AGN feedback, merging history, accretion/stripping, as well as star formation and quenching. We systematically analyze the archival Chandra data of ETGs to study the hot ISM. Using uniformly derived data products with spatially resolved spectral information, we revisit the X-ray scaling relations of ETGs and address their implications by comparing them with those of groups/clusters and simulations.

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Physics of Galactic Metals: Evolutionary Effects due to Production, Distribution, Feedback, and Interaction with Black Holes

Cited by 67 publications

References 148 publications

Stellar age gradients and inside-out star formation quenching in galaxy bulges

Stellar age gradients and inside-out star formation quenching in galaxy bulges

Ionized gas kinematics of massive elliptical galaxies in CALIFA and in cosmological zoom-in simulations

Hot Gaseous Halos in Early Type Galaxies

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