The Compact, ∼1 kpc Host Galaxy of a Quasar at a Redshift of 7.1

Venemans, Bram; Walter, Fabian; Decarli, Roberto; Bañados, Eduardo; Hodge, J. A.; Hewett, Paul C.; McMahon, R. G.; Mortlock, D.; Simpson, Chris

doi:10.3847/1538-4357/aa62ac

Cited by 98 publications

(145 citation statements)

References 57 publications

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“…A remarkable example is given by the famous QSO SDSSJ1148+5251 (Fan et al 2003), one of the first z > 6 QSOs discovered by the SDSS survey, where observations of the [CII]158µm line with the PdBI interferometer have revealed the presence of large-scale gas outflows extending out to 30 kpc from the QSO and moving with velocities of > 1000 km s −1 (Cicone et al 2015). This largescale outflow extends well beyond the characteristic size of the host galaxies of z ∼ 6 QSOs (∼ 1 − 3 kpc Wang et al 2013;Venemans et al 2017), and then expands on scales comparable with that of the hosting dark matter halo, possibly affecting the QSO local environment.…”

Section: Introductionmentioning

confidence: 99%

Exponentially growing bubbles around early supermassive black holes

Gilli¹,

Calura²,

D’Ercole³

et al. 2017

A&A

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We address the as yet unexplored issue of outflows induced by exponentially growing power sources, focusing on early supermassive black holes (BHs). We assumed that these objects grow to 10 9 M by z=6 by Eddington-limited accretion and convert 5% of their bolometric output into a wind. We first considered the case of energy-driven and momentum-driven outflows expanding in a region where the gas and total mass densities are uniform and equal to the average values in the Universe at z > 6. We derived analytic solutions for the evolution of the outflow: for an exponentially growing power with e-folding time t S al , we find that the late time expansion of the outflow radius is also exponential, with e-folding time of 5t S al and 4t S al in the energy-driven and momentum-driven limit, respectively. We then considered energy-driven outflows produced by quasi-stellar objects (QSOs) at the centre of early dark matter halos of different masses and powered by BHs growing from different seeds. We followed the evolution of the source power and of the gas and dark matter density profiles in the halos from the beginning of the accretion until z = 6. The final bubble radius and velocity do not depend on the seed BH mass, but are instead smaller for larger halo masses. At z=6, bubble radii in the range 50-180 kpc and velocities in the range 400-1000 km s −1 are expected for QSOs hosted by halos in the mass range 3 × 10 11 − 10 13 M . These radius and velocity scales compare well with those measured for the outflowing gas in the z=6.4 QSO SDSS J1148+5251. By the time the QSO is observed, we found that the total thermal energy injected within the bubble in the case of an energy-driven outflow is E th ∼ 5 × 10 60 erg. This is in excellent agreement with the value of E th = (6.2 ± 1.7) × 10 60 erg measured through the detection of the thermal Sunyaev-Zeldovich effect around a large population of luminous QSOs at lower redshifts. This suggests that QSO outflows are closer to the energy-driven limit than to the momentum-driven limit. We investigated the stability of the expanding gas shell in the case of an energy-driven supersonic outflow propagating within a dark matter halo with M h = 3 × 10 11 M at z=6. We found that the shell is Rayleigh-Taylor unstable already at early times and, by means of a simple model, we investigated the fate of the fragments detaching from the shell. We found that these fragments should rapidly evaporate because of the extremely high temperature of the hot gas bubble if this does not cool. Since the only effective cooling mechanism for such a gas is inverse Compton by the cosmic microwave background (CMB) photons (IC-CMB), which is important only at z ≥ 6, we speculate that such shell fragments may be observed only around high-z QSOs, where IC-CMB cooling of the bubble gas can prevent their evaporation.

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Section: Introductionmentioning

confidence: 99%

Exponentially growing bubbles around early supermassive black holes

Gilli¹,

Calura²,

D’Ercole³

et al. 2017

A&A

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“…Even subtracting the quasar emission with a well-understood point-spread function (PSF) in the ultraviolet (UV) and optical can leave residual noise from the wings of the quasar emission that overwhelms the host galaxy. Recent ALMA observations at millimeter wavelengths-where the central AGN emission is less of an issue-can resolve the cold molecular gas content of distant quasar host galaxies on ∼1-2 kpc scales (Wang et al 2013;Paraficz et al 2017;Venemans et al 2017). More local, low-redshift studies (  z 0.4) using adaptive optics and HST can recover host galaxy morphologies in the optical and near-infrared and find that quasar hosts can be early-or late-type galaxies (Dunlop et al 2003;Guyon et al 2006) and can exhibit significant star formation (e.g., Young et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Spatially Resolved Patchy Lyα Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8

Bayliss¹,

Sharon²,

Acharyya³

et al. 2017

ApJL

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We report the detection of extended Lyα emission from the host galaxy of SDSSJ2222+2745, a strongly lensed quasar at z=2.8. Spectroscopic follow-up clearly reveals extended Lyα in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging and resolve spatial scales as small as ∼200 pc. In the source plane, we recover the host galaxy morphology to within a few hundred parsecs of the central AGN and map the extended Lyα emission to its physical origin on one side of the host galaxy at radii ∼0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyα and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyα, host galaxy Lyα, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong-lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.

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“…Thus, it directly traces the distribution of star formation activity and the kinematic properties of the atomic/ionized gas in quasar host galaxies (Kimball et al 2015;Díaz-Santos et al 2016;Venemans et al 2017). Sixteen quasars at z 5.7 7.1 < < are detected in [C II] line emission, with modern submillimeter/ millimeter interferometer arrays such as the NOrthern Extended Millimeter Array (NOEMA) and Atacama Large Millimeter/ submillimeter Array (ALMA; Walter et al 2009;Venemans et al 2012Venemans et al , 2016Venemans et al , 2017Wang et al 2013Wang et al , 2016Willott et al 2013Willott et al , 2015Bañados et al 2015). These objects have [C II] to far-infrared (FIR) luminosity ratios over a wide range of (0.19−4.8)×10…”

Section: Introductionmentioning

confidence: 99%

Gas Dynamics of a Luminous z = 6.13 Quasar ULAS J1319+0950 Revealed by ALMA High-resolution Observations

Shao

Wang

Jones

et al. 2017

ApJ

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We present new Atacama Large Millimeter/submillimeter Array (ALMA) observations of the dust continuum and [C II] 158 μm fine structure line emission toward a far-infrared-luminous quasar, ULAS J131911.29+095051.4 at z=6.13, and combine the new Cycle 1 data with ALMA Cycle 0 data. The combined data have an angular resolution of ∼0 3, and resolve both the dust continuum and the [C II] line emission on a few kiloparsec scales. The [C II] line emission is more irregular than that of the dust continuum emission, which suggests different distributions between the dust and the [C II]-emitting gas. The combined data confirm the [C II] velocity gradient that we had previously detected in a lower-resolution ALMA image from the Cycle 0 data alone. We apply a tilted ring model to the [C II] velocity map to obtain a rotation curve, and constrain the circular velocity to be 427±55 km s −1 at a radius of 3.2 kpc with an inclination angle of 34°. We measure the dynamical mass within the 3.2 kpc region to be 13.4 5.3 7.8 -+ M 10 . This yields a black-hole and host galaxy mass ratio of 0.020 0.007 0.013 -+ , which is about 4 2 3 -+ times higher than that of the present-day M BH /M bulge ratio. This suggests that the supermassive black hole grows the bulk of its mass before the formation of most of the stellar mass in this quasar host galaxy in the early universe.

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The Compact, ∼1 kpc Host Galaxy of a Quasar at a Redshift of 7.1

Cited by 98 publications

References 57 publications

Exponentially growing bubbles around early supermassive black holes

Exponentially growing bubbles around early supermassive black holes

Spatially Resolved Patchy Lyα Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8

Gas Dynamics of a Luminous z = 6.13 Quasar ULAS J1319+0950 Revealed by ALMA High-resolution Observations

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