54 research outputs found
Supermassive black holes as the regulators of star formation in central galaxies
We present a relationship between the black hole mass, stellar mass, and star
formation rate of a diverse group of 91 galaxies with dynamically-measured
black hole masses. For our sample of galaxies with a variety of morphologies
and other galactic properties, we find that the specific star formation rate is
a smoothly decreasing function of the ratio between black hole mass and stellar
mass, or what we call the specific black hole mass. In order to explain this
relation, we propose a physical framework where the gradual suppression of a
galaxy's star formation activity results from the adjustment to an increase in
specific black hole mass and, accordingly, an increase in the amount of
heating. From this framework, it follows that at least some galaxies with
intermediate specific black hole masses are in a steady state of partial
quiescence with intermediate specific star formation rates, implying that both
transitioning and steady-state galaxies live within this region known as the
"green valley." With respect to galaxy formation models, our results present an
important diagnostic with which to test various prescriptions of black hole
feedback and its effects on star formation activity.Comment: 15 pages, 4 figures, 2 tables. Accepted for publication in The
Astrophysical Journa
The relationship between black hole mass and galaxy properties: Examining the black hole feedback model in IllustrisTNG
Supermassive black hole feedback is thought to be responsible for the lack of
star formation, or quiescence, in a significant fraction of galaxies. We
explore how observable correlations between the specific star formation rate
(sSFR), stellar mass (M), and black hole mass (M) are
sensitive to the physics of black hole feedback in a galaxy formation model. We
use the IllustrisTNG simulation suite, specifically the TNG100 simulation and
ten model variations that alter the parameters of the black hole model.
Focusing on central galaxies at with M
M, we find that the sSFR of galaxies in IllustrisTNG decreases once
the energy from black hole kinetic winds at low accretion rates becomes larger
than the gravitational binding energy of gas within the galaxy stellar radius.
This occurs at a particular M threshold above which galaxies are
found to sharply transition from being mostly star-forming to mostly quiescent.
As a result of this behavior, the fraction of quiescent galaxies as a function
of M is sensitive to both the normalization of the
M-M relation and the M threshold for
quiescence in IllustrisTNG. Finally, we compare these model results to
observations of 91 central galaxies with dynamical M measurements
with the caveat that this sample is not representative of the whole galaxy
population. While IllustrisTNG reproduces the observed trend that quiescent
galaxies host more massive black holes, the observations exhibit a broader
scatter in M at a given M and show a smoother decline
in sSFR with M.Comment: 20 pages, submitted to MNRA
The First Quiescent Galaxies in TNG300
We identify the first quiescent galaxies in TNG300, the largest volume of the
IllustrisTNG cosmological simulation suite, and explore their quenching
processes and time evolution to z=0. We find that the first quiescent galaxies
with stellar masses M_* > 3 x 10^{10} M_sun and specific star formation rates
sSFR < 10^{-11} yr^{-1} emerge at z~4.2 in TNG300. Suppression of star
formation in these galaxies begins with a thermal mode of AGN feedback at z~6,
and a kinetic feedback mode acts in each galaxy by z~4.7 to complete the
quenching process, which occurs on a time-scale of ~0.35 Gyr. Surprisingly, we
find that the majority of these galaxies are not the main progenitors of their
z=0 descendants; instead, four of the five galaxies fall into more massive
galaxies in subsequent mergers at a range of redshifts 2.5 < z < 0.2. By z=0,
these descendants are the centres of galaxy clusters with average stellar
masses of 8 x 10^{11} M_sun. We make predictions for the first quenched
galaxies to be located by the James Webb Space Telescope (JWST).Comment: 6 pages, 4 figure
Dense stellar clump formation driven by strong quasar winds in the FIRE cosmological hydrodynamic simulations
We investigate the formation of dense stellar clumps in a suite of
high-resolution cosmological zoom-in simulations of a massive, star forming
galaxy at under the presence of strong quasar winds. Our simulations
include multi-phase ISM physics from the Feedback In Realistic Environments
(FIRE) project and a novel implementation of hyper-refined accretion disk
winds. We show that powerful quasar winds can have a global negative impact on
galaxy growth while in the strongest cases triggering the formation of an
off-center clump with stellar mass , effective radius ,
and surface density . The clump progenitor gas cloud is originally not star-forming, but
strong ram pressure gradients driven by the quasar winds (orders of magnitude
stronger than experienced in the absence of winds) lead to rapid compression
and subsequent conversion of gas into stars at densities much higher than the
average density of star-forming gas. The AGN-triggered star-forming clump
reaches and , converting
most of the progenitor gas cloud into stars in 2\,Myr, significantly
faster than its initial free-fall time and with stellar feedback unable to stop
star formation. In contrast, the same gas cloud in the absence of quasar winds
forms stars over a much longer period of time (35\,Myr), at lower
densities, and losing spatial coherency. The presence of young, ultra-dense,
gravitationally bound stellar clumps in recently quenched galaxies could thus
indicate local positive feedback acting alongside the strong negative impact of
powerful quasar winds, providing a plausible formation scenario for globular
clusters.Comment: 14 pages, 12 figure
Dense stellar clump formation driven by strong quasar winds in the FIRE cosmological hydrodynamic simulations
We investigate the formation of dense stellar clumps in a suite of high-resolution cosmological zoom-in simulations of a massive, star-forming galaxy at z ⌠2 under the presence of strong quasar winds. Our simulations include multiphase ISM physics from the Feedback In Realistic Environments (FIRE) project and a no v el implementation of hyper-refined accretion disc winds. We show that powerful quasar winds can have a global negative impact on galaxy growth while in the strongest cases triggering the formation of an off-centre clump with stellar mass M ⌠10 7 M , effective radius R 1 / 2 Clump ⌠20 pc , and surface density âŒ10 4 M pc â2 . The clump progenitor gas cloud is originally not star -forming, b ut strong ram pressure gradients driven by the quasar winds (orders of magnitude stronger than experienced in the absence of winds) lead to rapid compression and subsequent conversion of gas into stars at densities much higher than the average density of star-forming gas. The AGN-triggered star-forming clump reaches SFR ⌠50 M yr â1 and SFR ⌠10 4 M yr â1 kpc â2 , converting most of the progenitor gas cloud into stars in âŒ2 Myr, significantly faster than its initial free-fall time and with stellar feedback unable to stop star formation. In contrast, the same gas cloud in the absence of quasar winds forms stars over a much longer period of time ( âŒ35 Myr), at lower densities, and losing spatial coherency. The presence of young, ultra-dense, gravitationally bound stellar clumps in recently quenched galaxies could thus indicate local positive feedback acting alongside the strong negative impact of powerful quasar winds, providing a plausible formation scenario for globular clusters
Local positive feedback in the overall negative: the impact of quasar winds on star formation in the FIRE cosmological simulations
Negative feedback from accreting supermassive black holes is regarded as a
key ingredient in suppressing star formation and quenching massive galaxies.
However, several models and observations suggest that black hole feedback may
have a positive effect, triggering star formation by compressing interstellar
medium gas to higher densities. We investigate the dual role of black hole
feedback using cosmological hydrodynamic simulations from the Feedback In
Realistic Environments (FIRE) project, including a novel implementation of
hyper-refined accretion-disc winds. Focusing on a massive, star-forming galaxy
at (), we show that
strong quasar winds with kinetic power 10 erg/s acting for
20Myr drive the formation of a central gas cavity and can dramatically
reduce the star formation rate surface density across the galaxy disc. The
suppression of star formation is primarily driven by reducing the amount of gas
that can become star-forming, compared to directly evacuating the pre-existing
star-forming gas reservoir (preventive feedback dominates over ejective
feedback). Despite the global negative impact of quasar winds, we identify
several plausible signatures of local positive feedback, including: (1) spatial
anti-correlation of wind-dominated regions and star-forming clumps, (2) higher
local star formation efficiency in compressed gas near the edge of the cavity,
and (3) increased local contribution of outflowing material to star formation.
Stars forming under the presence of quasar winds tend to do so at larger radial
distances. Our results suggest that positive and negative AGN feedback can
coexist in galaxies, but local positive triggering of star formation plays a
minor role in global galaxy growth.Comment: 17 pages, 12 figure
JWST Reveals Widespread AGN-Driven Neutral Gas Outflows in Massive z ~ 2 Galaxies
We use deep JWST/NIRSpec R~1000 slit spectra of 113 galaxies at 1.7 < z <
3.5, selected from the mass-complete Blue Jay survey, to investigate the
prevalence and typical properties of neutral gas outflows at cosmic noon. We
detect excess Na I D absorption (beyond the stellar contribution) in 46% of
massive galaxies ( M/M 10), with similar incidence rates in
star-forming and quenching systems. Half of the absorption profiles are
blueshifted by at least 100 km/s, providing unambiguous evidence for neutral
gas outflows. Galaxies with strong Na I D absorption are distinguished by
enhanced emission line ratios consistent with AGN ionization. We conservatively
measure mass outflow rates of 3 - 100 yr; comparable to or
exceeding ionized gas outflow rates measured for galaxies at similar stellar
mass and redshift. The outflows from the quenching systems
(log(sSFR)[yr] -10) have mass loading factors of 4 - 360, and
the energy and momentum outflow rates exceed the expected injection rates from
supernova explosions, suggesting that these galaxies could possibly be caught
in a rapid blowout phase powered by the AGN. Our findings suggest that
AGN-driven ejection of cold gas may be a dominant mechanism for fast quenching
of star formation at z~2.Comment: 16 pages, 8 figures, submitted to MNRA
Spatially resolved star formation and inside-out quenching in the TNG50 simulation and 3D-HST observations
We compare the star-forming main sequence (SFMS) of galaxies â both integrated and resolved on 1âkpc scales â between the high-resolution TNG50 simulation of IllustrisTNG and observations from the 3D-HST slitless spectroscopic survey at z ⌠1. Contrasting integrated star formation rates (SFRs), we find that the slope and normalization of the star-forming main sequence in TNG50 are quantitatively consistent with values derived by fitting observations from 3D-HST with the Prospector Bayesian inference framework. The previous offsets of 0.2â1 dex between observed and simulated main-sequence normalizations are resolved when using the updated masses and SFRs from Prospector. The scatter is generically smaller in TNG50 than in 3D-HST for more massive galaxies with M*&gt; 1010âMâ, by âŒ10â40 per cent, after accounting for observational uncertainties. When comparing resolved star formation, we also find good agreement between TNG50 and 3D-HST: average specific star formation rate (sSFR) radial profiles of galaxies at all masses and radii below, on, and above the SFMS are similar in both normalization and shape. Most noteworthy, massive galaxies with M*&gt; 1010.5âMâ, which have fallen below the SFMS due to ongoing quenching, exhibit a clear central SFR suppression, in both TNG50 and 3D-HST. In contrast, the original Illustris simulation and a variant TNG run without black hole kinetic wind feedback, do not reproduce the central SFR profile suppression seen in data. In TNG, inside-out quenching is due to the supermassive black hole (SMBH) feedback model operating at low accretion rates
âBeads-on-a-stringâ star formation tied to one of the most powerful active galactic nucleus outbursts observed in a cool-core galaxy cluster
With two central galaxies engaged in a major merger and a remarkable chain of 19 young stellar superclusters wound around them in projection, the galaxy cluster SDSS J1531+3414 (z = 0.335) offers an excellent laboratory to study the interplay between mergers, active galactic nucleus (AGN) feedback, and star formation. New Chandra X-ray imaging reveals rapidly cooling hot (T ⌠106 K) intracluster gas, with two âwingsâ forming a concave density discontinuity near the edge of the cool core. LOFAR 144 MHz observations uncover diffuse radio emission strikingly aligned with the âwings,â suggesting that the âwingsâ are actually the opening to a giant X-ray supercavity. The steep radio emission is likely an ancient relic of one of the most energetic AGN outbursts observed, with 4pV > 1061 erg. To the north of the supercavity, GMOS detects warm (T ⌠104 K) ionized gas that enshrouds the stellar superclusters but is redshifted up to +800 km sâ1 with respect to the southern central galaxy. The Atacama Large Millimeter/submillimeter Array detects a similarly redshifted âŒ1010 M â reservoir of cold (T ⌠102 K) molecular gas, but it is offset from the young stars by âŒ1â3 kpc. We propose that the multiphase gas originated from low-entropy gas entrained by the X-ray supercavity, attribute the offset between the young stars and the molecular gas to turbulent intracluster gas motions, and suggest that tidal interactions stimulated the âbeads-on-a-stringâ star formation morphology
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