Abstract
Quasar feedback may regulate the growth of supermassive black holes, quench coeval star formation, and impact galaxy morphology and the circumgalactic medium. However, direct evidence for ...quasar feedback in action at the epoch of peak black hole accretion at
z
≈ 2 remains elusive. A good case in point is the
z
= 1.6 quasar WISEA J100211.29+013706.7 (XID 2028), where past analyses of the same ground-based data have come to different conclusions. Here, we revisit this object with the integral-field unit of the Near Infrared Spectrograph on board the JWST as part of Early Release Science program Q3D. The excellent angular resolution and sensitivity of the JWST data reveal new morphological and kinematic substructures in the outflowing gas plume. An analysis of the emission-line ratios indicates that photoionization by the central quasar dominates the ionization state of the gas with no obvious sign for a major contribution from hot young stars anywhere in the host galaxy. The rest-frame near-UV emission aligned along the wide-angle cone of outflowing gas is interpreted as a scattering cone. The outflow has cleared a channel in the dusty host galaxy, through which some of the quasar ionizing radiation is able to escape and heat the surrounding interstellar and circumgalactic media. Although the warm ionized outflow is not powerful enough to impact the host galaxy via mechanical feedback, radiative feedback by the active galactic nucleus, aided by the outflow, may help to explain the unusually small molecular gas mass fraction in the galaxy host.
Abstract
Massive galaxies formed most actively at redshifts
z
= 1–3 during the period known as “cosmic noon.” Here we present an emission-line study of the extremely red quasar ...SDSSJ165202.64+172852.3’s host galaxy at
z
= 2.94, based on observations with the Near Infrared Spectrograph integral field unit on board JWST. We use standard emission-line diagnostic ratios to map the sources of gas ionization across the host and a swarm of companion galaxies. The quasar dominates the photoionization, but we also discover shock-excited regions orthogonal to the ionization cone and the quasar-driven outflow. These shocks could be merger-induced or—more likely, given the presence of a powerful galactic-scale quasar outflow—these are signatures of wide-angle outflows that can reach parts of the galaxy that are not directly illuminated by the quasar. Finally, the kinematically narrow emission associated with the host galaxy presents as a collection of 1 kpc–scale clumps forming stars at a rate of at least 200
M
⊙
yr
−1
. The interstellar medium within these clumps shows high electron densities, reaching up to 3000 cm
−3
, with metallicities ranging from half to a third solar with a positive metallicity gradient, and
V
-band extinctions up to 3 mag. The star formation conditions are far more extreme in these regions than in local star-forming galaxies but consistent with those of massive galaxies at cosmic noon. The JWST observations simultaneously reveal an archetypal rapidly forming massive galaxy undergoing a merger, a clumpy starburst, an episode of obscured near-Eddington quasar activity, and an extremely powerful quasar outflow.
Abstract
Quasar-driven galactic outflows are a major driver of the evolution of massive galaxies. We report observations of a powerful galactic-scale outflow in a
z
= 3 extremely red and ...intrinsically luminous (
L
bol
≃ 5 × 10
47
erg s
−1
) quasar SDSSJ1652 + 1728 with the Near-infrared Spectrograph on board JWST. We analyze the kinematics of rest-frame optical emission lines and identify the quasar-driven outflow extending out to ∼10 kpc from the quasar with a velocity offset of (
v
r
= ± 500 km s
−1
) and high velocity dispersion (FWHM = 700–2400 km s
−1
). Due to JWST’s unprecedented surface brightness sensitivity in the near-infrared, we unambiguously show that the powerful high velocity outflow in an extremely red quasar encompasses a large swath of the host galaxy’s interstellar medium. Using the kinematics and dynamics of optical emission lines, we estimate the mass outflow rate—in the warm ionized phase alone—to be at least 2300 ± 1400
M
⊙
yr
−1
. We measure a momentum flux ratio between the outflow and the quasar accretion disk of ∼1 on a kpc scale, indicating that the outflow was likely driven in a relatively high (>10
23
cm
−2
) column density environment through radiation pressure on dust grains. We find a coupling efficiency between the bolometric luminosity of the quasar and the outflow of 0.1%, matching the theoretical prediction of the minimum coupling efficiency necessary for negative quasar feedback. The outflow has sufficient energetics to drive the observed turbulence seen in shocked regions of the quasar host galaxy, which are likely directly responsible for prolonging the time that it takes for gas to cool efficiently.
Abstract
The O
iii
5007 Å emission line is the most common tracer of warm, ionized outflows in active galactic nuclei across cosmic time. JWST newly allows us to use mid-IR spectral features at both ...high spatial and spectral resolution to probe these same winds. Here we present a comparison of ground-based, seeing-limited O
iii
and space-based, diffraction-limited S
iv
10.51
μ
m maps of the powerful, kiloparsec-scale outflow in the Type 1 red quasar SDSS J110648.32+480712.3. The JWST data are from the Mid-InfraRed Instrument. There is a close match in resolution between the data sets (∼0.″6), in ionization potential of the O
+2
and S
+3
ions (35 eV) and in line sensitivity (1–2 × 10
−17
erg s
−1
cm
−2
arcsec
−2
). The O
iii
and S
iv
line shapes match in velocity and line width over much of the 20 kpc outflowing nebula, and S
iv
is the brightest line in the rest-frame 3.5–19.5
μ
m range, demonstrating its usefulness as a mid-IR probe of quasar outflows. O
iii
is nevertheless intrinsically brighter and provides better contrast with the point-source continuum, which is strong in the mid-IR. There is a strong anticorrelation of O
iii
/S
iv
with average velocity, which is consistent with a scenario of differential obscuration between the approaching (blueshifted) and receding (redshifted) sides of the flow. The dust in the wind may also obscure the central quasar, consistent with models that attribute red quasar extinction to dusty winds.
Quasar-driven galactic outflows are a major driver of the evolution of
massive galaxies. We report observations of a powerful galactic-scale outflow
in a $z=3$ extremely red, intrinsically luminous ...($L_{\rm bol}\simeq 5\times
10^{47}$erg s$^{-1}$) quasar SDSSJ1652+1728 with the Near Infrared Spectrograph
(NIRSpec) on board JWST. We analyze the kinematics of rest-frame optical
emission lines and identify the quasar-driven outflow extending out to $\sim
10$ kpc from the quasar with a velocity offset of ($v_{r}=\pm 500$ km s$^{-1}$)
and high velocity dispersion (FWHM$=700-2400$ km s$^{-1}$). Due to JWST's
unprecedented surface brightness sensitivity in the near-infrared -- we
unambiguously show that the powerful high velocity outflow in an extremely red
quasar (ERQ) encompasses a large swath of the host galaxy's interstellar medium
(ISM). Using the kinematics and dynamics of optical emission lines, we estimate
the mass outflow rate -- in the warm ionized phase alone -- to be at least
$2300\pm1400$ $M_{\odot}$ yr$^{-1}$. We measure a momentum flux ratio between
the outflow and the quasar accretion disk of $\sim$1 on kpc scale, indicating
that the outflow was likely driven in a relatively high ($>10^{23}$cm$^{-2}$)
column density environment through radiation pressure on dust grains. We find a
coupling efficiency between the bolometric luminosity of the quasar and the
outflow of 0.1$\%$, matching the theoretical prediction of the minimum coupling
efficiency necessary for negative quasar feedback. The outflow has sufficient
energetics to drive the observed turbulence seen in shocked regions of the
quasar host galaxy, likely directly responsible for prolonging the time it
takes for gas to cool efficiently.
Massive galaxies formed most actively at redshifts $z=1-3$ during the period
known as `cosmic noon.' Here we present an emission-line study of an extremely
red quasar SDSSJ165202.64+172852.3 host ...galaxy at $z=2.94$, based on
observations with the Near Infrared Spectrograph (NIRSpec) integral field unit
(IFU) on board JWST. We use standard emission-line diagnostic ratios to map the
sources of gas ionization across the host and a swarm of companion galaxies.
The quasar dominates the photoionization, but we also discover shock-excited
regions orthogonal to the ionization cone and the quasar-driven outflow. These
shocks could be merger-induced or -- more likely, given the presence of a
powerful galactic-scale quasar outflow -- these are signatures of wide-angle
outflows that can reach parts of the galaxy that are not directly illuminated
by the quasar. Finally, the kinematically narrow emission associated with the
host galaxy presents as a collection of 1 kpc-scale clumps forming stars at a
rate of at least 200 $M_{\odot}$ yr$^{-1}$. The ISM within these clumps shows
high electron densities, reaching up to 3,000 cm$^{-3}$ with metallicities
ranging from half to a third solar with a positive metallicity gradient and V
band extinctions up to 3 magnitudes. The star formation conditions are far more
extreme in these regions than in local star-forming galaxies but consistent
with that of massive galaxies at cosmic noon. JWST observations reveal an
archetypical rapidly forming massive galaxy undergoing a merger, a clumpy
starburst, an episode of obscured near-Eddington quasar activity, and an
extremely powerful quasar outflow simultaneously.
Quasar feedback may regulate the growth of supermassive black holes, quench coeval star formation, and impact galaxy morphology and the circumgalactic medium. However, direct evidence for quasar ...feedback in action at the epoch of peak black hole accretion at z ~ 2 remains elusive. A good case in point is the z = 1.6 quasar WISEA J100211.29+013706.7 (XID 2028) where past analyses of the same ground-based data have come to different conclusions. Here we revisit this object with the integral field unit of the Near Infrared Spectrograph (NIRSpec) on board the James Webb Space Telescope (JWST) as part of Early Release Science program Q3D. The excellent angular resolution and sensitivity of the JWST data reveal new morphological and kinematic sub-structures in the outflowing gas plume. An analysis of the emission line ratios indicates that photoionization by the central quasar dominates the ionization state of the gas with no obvious sign for a major contribution from hot young stars anywhere in the host galaxy. Rest-frame near-ultraviolet emission aligned along the wide-angle cone of outflowing gas is interpreted as a scattering cone. The outflow has cleared a channel in the dusty host galaxy through which some of the quasar ionizing radiation is able to escape and heat the surrounding interstellar and circumgalactic media. The warm ionized outflow is not powerful enough to impact the host galaxy via mechanical feedback, but radiative feedback by the AGN, aided by the outflow, may help explain the unusually small molecular gas mass fraction in the galaxy host.
Quasar-driven galactic outflows are a major driver of the evolution of massive galaxies. We report observations of a powerful galactic-scale outflow in a \(z=3\) extremely red, intrinsically luminous ...(\(L_{\rm bol}\simeq 5\times 10^{47}\)erg s\(^{-1}\)) quasar SDSSJ1652+1728 with the Near Infrared Spectrograph (NIRSpec) on board JWST. We analyze the kinematics of rest-frame optical emission lines and identify the quasar-driven outflow extending out to \(\sim 10\) kpc from the quasar with a velocity offset of (\(v_{r}=\pm 500\) km s\(^{-1}\)) and high velocity dispersion (FWHM\(=700-2400\) km s\(^{-1}\)). Due to JWST's unprecedented surface brightness sensitivity in the near-infrared -- we unambiguously show that the powerful high velocity outflow in an extremely red quasar (ERQ) encompasses a large swath of the host galaxy's interstellar medium (ISM). Using the kinematics and dynamics of optical emission lines, we estimate the mass outflow rate -- in the warm ionized phase alone -- to be at least \(2300\pm1400\) \(M_{\odot}\) yr\(^{-1}\). We measure a momentum flux ratio between the outflow and the quasar accretion disk of \(\sim\)1 on kpc scale, indicating that the outflow was likely driven in a relatively high (\(>10^{23}\)cm\(^{-2}\)) column density environment through radiation pressure on dust grains. We find a coupling efficiency between the bolometric luminosity of the quasar and the outflow of 0.1\(\%\), matching the theoretical prediction of the minimum coupling efficiency necessary for negative quasar feedback. The outflow has sufficient energetics to drive the observed turbulence seen in shocked regions of the quasar host galaxy, likely directly responsible for prolonging the time it takes for gas to cool efficiently.
Massive galaxies formed most actively at redshifts \(z=1-3\) during the period known as `cosmic noon.' Here we present an emission-line study of an extremely red quasar SDSSJ165202.64+172852.3 host ...galaxy at \(z=2.94\), based on observations with the Near Infrared Spectrograph (NIRSpec) integral field unit (IFU) on board JWST. We use standard emission-line diagnostic ratios to map the sources of gas ionization across the host and a swarm of companion galaxies. The quasar dominates the photoionization, but we also discover shock-excited regions orthogonal to the ionization cone and the quasar-driven outflow. These shocks could be merger-induced or -- more likely, given the presence of a powerful galactic-scale quasar outflow -- these are signatures of wide-angle outflows that can reach parts of the galaxy that are not directly illuminated by the quasar. Finally, the kinematically narrow emission associated with the host galaxy presents as a collection of 1 kpc-scale clumps forming stars at a rate of at least 200 \(M_{\odot}\) yr\(^{-1}\). The ISM within these clumps shows high electron densities, reaching up to 3,000 cm\(^{-3}\) with metallicities ranging from half to a third solar with a positive metallicity gradient and V band extinctions up to 3 magnitudes. The star formation conditions are far more extreme in these regions than in local star-forming galaxies but consistent with that of massive galaxies at cosmic noon. JWST observations reveal an archetypical rapidly forming massive galaxy undergoing a merger, a clumpy starburst, an episode of obscured near-Eddington quasar activity, and an extremely powerful quasar outflow simultaneously.
Rotating disk electrodes (RDEs) are widely used in electrochemical characterization to analyze the mechanisms of various electrocatalytic reactions. RDE experiments often make use of or require ...collection and quantification of gaseous products. The combination of rotating parts and gaseous analytes makes the design of RDE cells that allow for headspace analysis challenging due to gas leaks at the interface of the cell body and the rotator. In this manuscript we describe a new, hermetically sealed electrochemical cell that allows for electrode rotation while simultaneously providing a gastight environment. Electrode rotation in this new cell design is controlled by magnetically coupling the working electrode to a rotating magnetic driver. Calibration of the RDE using a tachometer shows that the rotation speed of the electrode is the same as that of the magnetic driver. To validate the performance of this cell for hydrodynamic measurements, limiting currents from the reduction of a potassium ferrocyanide (K4Fe(CN)6·3H2O) were measured and shown to compare favorably with calculated values from the Levich equation and with data obtained using more typical, nongastight RDE cells. Faradaic efficiencies of ∼95% were measured in the gas phase for oxygen evolution in alkaline media at an Inconel 625 alloy electrocatalyst during rotation at 1600 rpm. These data verify that a gastight environment is maintained even during rotation.
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