Black hole and host galaxy growth in an isolated <i>z</i> ∼ 6 QSO observed with ALMA

Tripodi, R.; Feruglio, C.; Fiore, F.; Bischetti, M.; D’Odorico, V.; Carniani, Stefano; Cristiani, S.; Gallerani, S.; Maiolino, R.; Marconi, A.; Pallottini, Andrea; Piconcelli, E.; Vallini, L.; Zana, Tommaso

doi:10.1051/0004-6361/202243920

Cited by 12 publications

(43 citation statements)

References 106 publications

(167 reference statements)

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“…With the best-fitting UV/optical power law (red lines) and NIR to mid-infrared (MIR) CAT3D AGN torus model (brown lines; Hönig & Kishimoto 2017) in Shao et al (2019), and the source size of twice the effective radius of the dust continuum underlying CO (9-8) listed in Table 2, we derived an average dust temperature T dust of 53 +4 −4 K, a total dust mass M dust, app of 1.27 +0.62 −0.35 × 10 9 M and an overall emissivity index β of 1.90 +0.33 −0.27 . Our dust temperature is smaller than the value of 71 ± 4 K derived by Tripodi et al (2022), and our dust mass is ∼3 times higher. This is due to the differences in the AGN dust torus model used, which has a significant contribution in the rest frame wavelength range 100 µm in our case, whereas the impact of the AGN dust torus on the total dust continuum emission in Tripodi et al (2022) is limited 50 µm.…”

Section: Dust Diagnosticcontrasting

confidence: 79%

“…16 × 0 . 13, which is similar to the one of Tripodi et al (2022), and a sensitivity of 0.15 mJy/beam per 17 km/s. The residual spectrum between the observed one and the best-fit double-Gaussian model is only noise-like, with an rms of 0.70 mJy.…”

Section: Outflow Traced By Oh +supporting

confidence: 72%

“…This may indicate that the central SMBH grows the bulk of its mass before the formation of most of the stellar mass in this quasar host galaxy in the early Universe. Wang et al (2013) and Tripodi et al (2022) also found the same result for quasar J2310+1855. This is consistent with what has been found for other high-luminosity z ∼ 6 quasars (e.g., Wang et al 2019).…”

Section: The Coevolution Of the Quasar And Its Host Galaxysupporting

confidence: 70%

“…The ∼4 kpc resolution [C ii] data reveal a dynamical mass of 9.6 × 10 10 M with an approximate estimate of the inclination angle (46 • , determined from the ratio between the minor and major axis), suggesting a M BH /M bulge value that is higher than the local value (Wang et al 2013). Tripodi et al (2022) used ∼1 kpc resolution [C ii] data to find a dynamical mass of 5.2 × 10 10 M within a 1.7 kpc region, based on a kinematic modeling on the data cube with a rotating disk inclination angle of 25 • . However, the limited spatial resolution introduces large uncertainties in the determination of the gas kinematics, making it difficult to perform a dynamical decomposition of the quasar-host system.…”

Section: Introductionmentioning

confidence: 98%

“…A detailed CO spectral line energy distribution analysis reveals that, in addition to the far-UV radiation from young and massive stars, another gas heating mechanism (e.g., X-ray radiation and/or shocks) may be needed to explain the observed CO luminosities (Carniani et al 2019;Li et al 2020b). The low excitation water para-H 2 O (2 02 -1 11 ) and para-H 2 O (3 22 -3 13 ), OH + (1 1 -0 1 ) lines, and lines from ionized gas such as [O i] 146 µm, [O iii] 88 µm, and [N ii] 122 µm have been detected with ALMA toward J2310+1855, and a solar-level metallicity is proposed based on the [O iii]/[N ii] ratio (Hashimoto et al 2019b;Li et al 2020a;Tripodi et al 2022). We should note that [N ii] 122 µm is an upper [N ii] line (i.e., the transition of 3 P 2 -3 P 1 ), so there are potential excitation effects.…”

Section: Introductionmentioning

confidence: 99%

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The interstellar medium distribution, gas kinematics, and system dynamics of the far-infrared luminous quasar SDSS J2310+1855 at z = 6.0

Shao

Wang

Weiß

et al. 2022

A&A

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We present Atacama Large Millimeter/submillimeter Array (ALMA) sub-kiloparsec-to kiloparsec-scale resolution observations of the [C ii], CO (9-8), and OH + (1 1 -0 1 ) lines along with their dust continuum emission toward the far-infrared (FIR) luminous quasar SDSS J231038.88+185519.7 at z = 6.0031, to study the interstellar medium distribution, the gas kinematics, and the quasar-host system dynamics. We decompose the intensity maps of the [C ii] and CO (9-8) lines and the dust continuum with two-dimensional elliptical Sérsic models. The [C ii] brightness follows a flat distribution with a Sérsic index of 0.59. The CO (9-8) line and the dust continuum can be fit with an unresolved nuclear component and an extended Sérsic component with a Sérsic index of ∼1, which may correspond to the emission from an active galactic nucleus dusty molecular torus and a quasar host galaxy, respectively. The different [C ii] spatial distribution may be due to the effect of the high dust opacity, which increases the FIR background radiation on the [C ii] line, especially in the galaxy center, significantly suppressing the [C ii] emission profile. The dust temperature drops with distance from the center. The effective radius of the dust continuum is smaller than that of the line emission and the dust mass surface density, but is consistent with that of the star formation rate surface density. This may indicate that the dust emission is a less robust tracer of the dust and gas distribution but is a decent tracer of the obscured star formation activity. The OH + (1 1 -0 1 ) line shows a P-Cygni profile with an absorption at ∼-400 km/s, which may indicate an outflow with a neutral gas mass of (6.2 ± 1.2) × 10 8 M along the line of sight. We employed a three-dimensional tilted ring model to fit the [C ii] and CO (9-8) data cubes. The two lines are both rotation dominated and trace identical disk geometries and gas motions. This suggest that the [C ii] and CO (9-8) gas are coplanar and corotating in this quasar host galaxy. The consistent circular velocities measured with [C ii] and CO (9-8) lines indicate that these two lines trace a similar gravitational potential. We decompose the circular rotation curve measured from the kinematic model fit to the [C ii] line into four matter components (black hole, stars, gas, and dark matter). The quasar-starburst system is dominated by baryonic matter inside the central few kiloparsecs. We constrain the black hole mass to be 2.97 +0.51 −0.77 × 10 9 M ; this is the first time that the dynamical mass of a black hole has been measured at z ∼ 6. This mass is consistent with that determined using the scaling relations from quasar emission lines. A massive stellar component (on the order of 10 9 M ) may have already existed when the Universe was only ∼0.93 Gyr old. The relations between the black hole mass and the baryonic mass of this quasar indicate that the central supermassive black hole may have formed before its host galaxy.

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Section: Dust Diagnosticcontrasting

confidence: 79%

Section: Outflow Traced By Oh +supporting

confidence: 72%

Section: The Coevolution Of the Quasar And Its Host Galaxysupporting

confidence: 70%

Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

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The interstellar medium distribution, gas kinematics, and system dynamics of the far-infrared luminous quasar SDSS J2310+1855 at z = 6.0

Shao

Wang

Weiß

et al. 2022

A&A

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Unveiling the warm and dense ISM in z > 6 quasar host galaxies via water vapor emission

Pensabene

Werf

Decarli³

et al. 2022

A&A

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Water vapor (H 2 O) is one of the brightest molecular emitters after carbon monoxide (CO) in galaxies with high infrared (IR) luminosity, and allows us to investigate the warm dense phase of the interstellar medium (ISM) where star formation occurs. However, due to the complexity of its radiative spectrum, H 2 O is not frequently exploited as an ISM tracer in distant galaxies. Therefore, H 2 O studies of the warm and dense gas at high-z remains largely unexplored. In this work we present observations conducted with the Northern Extended Millimeter Array (NOEMA) toward three z > 6 IR-bright quasars J2310+1855, J1148+5251, and J0439+1634 targeted in their multiple para-/ortho-H 2 O transitions (3 12 − 3 03 , 1 11 − 0 00 , 2 20 − 2 11 , and 4 22 − 4 13 ), as well as their far-IR (FIR) dust continuum. By combining our data with previous measurements from the literature we estimate dust masses and temperatures, continuum optical depths, IR luminosities, and the star-formation rates from the FIR continuum. We model the H 2 O lines using the MOLPOP-CEP radiative transfer code and find that water vapor lines in our quasar host galaxies are primarily excited in warm dense (gas kinetic temperature and density of T kin = 50 K, n H 2 ∼ 10 4.5 − 10 5 cm −3 ) molecular medium with water vapor column density of N H 2 O ∼ 2 × 10 17 − 3 × 10 18 cm −3 . High-J H 2 O lines are mainly radiatively pumped by the intense optically-thin far-IR radiation field associated with a warm dust component with temperatures of T dust ∼ 80 − 190 K that account for < 5 − 10% of the total dust mass. In the case of J2310+1855, our analysis points to a relatively high value of the continuum optical depth at 100 µm (τ 100 ∼ 1). Our results are in agreement with expectations based on the H 2 O spectral line energy distribution of local and high-z ultra-luminous IR galaxies and active galactic nuclei (AGN). The analysis of the Boltzmann diagrams highlights the interplay between collisions and IR pumping in populating the high H 2 O energy levels and allows us to directly compare the excitation conditions in the targeted quasar host galaxies. In addition, the observations enable us to sample the high-luminosity part of the H 2 O-total-IR (TIR) luminosity relations (L H 2 O − L TIR ). Overall, our results point to supralinear trends suggesting that H 2 O-TIR relations are likely driven by IR pumping rather than the mere co-spatiality between the FIR-continuum-and the line-emitting regions. The observed L H 2 O /L TIR ratios in our z > 6 quasars do not show any strong deviations with respect to those measured in star-forming galaxies and AGN at lower redshift. This supports the idea that H 2 O can be likely used to trace the star-formation buried deep within the dense molecular clouds.

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Dynamical signature of a stellar bulge in a quasar-host galaxy at z ≃ 6

Tripodi

Lelli

Feruglio

et al. 2023

A&A

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We present a dynamical analysis of a quasar-host galaxy at z 6 (SDSS J2310+1855) using a high-resolution ALMA observation of the [CII] emission line. The observed rotation curve was fitted with mass models that considered the gravitational contribution of a thick gas disc, a thick star-forming stellar disc, and a central mass concentration, which is likely due to a combination of a spheroidal component (i.e. a stellar bulge) and a supermassive black hole (SMBH). The SMBH mass of 5 × 10 9 M , previously measured using the CIV and MgII emission lines, is not sufficient to explain the high velocities in the central regions. Our dynamical model suggests the presence of a stellar bulge with a mass of M bulge ∼ 10 10 M in this object, when the Universe was younger than 1 Gyr. To finally be located on the local M SMBH − M bulge relation, the bulge mass should increase by a factor of ∼40 from z = 6 to 0, while the SMBH mass should grow by a factor of 4 at most. This points towards asynchronous galaxy-BH co-evolution. Imaging with the JWST will allow us to validate this scenario.

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Black hole and host galaxy growth in an isolated z ∼ 6 QSO observed with ALMA

Cited by 12 publications

References 106 publications

The interstellar medium distribution, gas kinematics, and system dynamics of the far-infrared luminous quasar SDSS J2310+1855 at z = 6.0

The interstellar medium distribution, gas kinematics, and system dynamics of the far-infrared luminous quasar SDSS J2310+1855 at z = 6.0

Unveiling the warm and dense ISM in z > 6 quasar host galaxies via water vapor emission

Dynamical signature of a stellar bulge in a quasar-host galaxy at z ≃ 6

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