The dense molecular gas in the <i>z</i>  ∼  6 QSO SDSS J231038.88+185519.7 resolved by ALMA

Feruglio, C.; Fiore, F.; Carniani, Stefano; Maiolino, R.; D’Odorico, V.; Luminari, A.; Barai, Paramita; Bischetti, M.; Bongiorno, A.; Cristiani, S.; Ferrara, Andrea; Gallerani, S.; Marconi, A.; Pallottini, Andrea; Piconcelli, E.; Zappacosta, L.

doi:10.1051/0004-6361/201833174

Cited by 44 publications

(82 citation statements)

References 72 publications

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“…This may imply that CO (9 − 8), (8 − 7) and H 2 O lines trace similar dense molecular regions that are closer to the central SMBH compared to CO (2 − 1) and [C II] 158µm. The redshift measured with the CO (9 − 8), (8 − 7), and H 2 O lines are within the uncertainties consistent with that from previous [C II], CO (2 − 1) and (6 − 5) observations (Wang et al 2013;Feruglio et al 2018;Shao et al 2019). The OH + line is not as strong as the other detections, so we fix the center frequency to the [C II] 158µm redshift, and fit a Gaussian profile to the spectra extracted from the peak pixel.…”

Section: Resultssupporting

confidence: 90%

“…4 ± 0. 1) at similar spatial resolution (Wang et al 2013;Feruglio et al 2018;Shao et al 2019). This may imply that CO (9 − 8), (8 − 7) and H 2 O lines trace similar dense molecular regions that are closer to the central SMBH compared to CO (2 − 1) and [C II] 158µm.…”

Section: Resultsmentioning

confidence: 96%

“…J2310+1855 hosts a SMBH of ≈ 4 × 10 9 M (Jiang et al 2016). It was detected in bright dust continuum, CO (2 − 1) and (6 − 5), [C II] 158µm and [O III] 88µm lines (Wang et al 2013;D'Odorico et al 2018;Feruglio et al 2018;Hashimoto et al 2018;Carniani et al 2019;Shao et al 2019). This quasar is also detected in bright CO (10 − 9) emission with a line flux of 1.04 ± 0.17 Jy km s −1 (Riechers et al in prep).…”

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confidence: 99%

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Probing the Full CO Spectral Line Energy Distribution (SLED) in the Nuclear Region of a Quasar-starburst System at z = 6.003

Wang

Riechers

et al. 2020

ApJ

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We report Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO (8 − 7), (9 − 8), H 2 O(2 0,2 − 1 1,1 ) and OH + (1 1 − 0 1 ) and NOrthern Extended Millimeter Array (NOEMA) observations of CO (5 − 4), (6 − 5), (12 − 11) and (13 − 12) towards the z = 6.003 quasar SDSS J231038.88+185519.7, aiming to probe the physical conditions of the molecular gas content of this source. We present the best sampled CO spectral line energy distribution (SLED) at z = 6.003, and analyzed it with the radiative transfer code MOLPOP-CEP. Fitting the CO SLED to a one-component model indicates a kinetic temperature T kin = 228 K, molecular gas density log(n(H 2 )/cm −3 )=4.75, and CO column density log(N (CO)/cm −2 ) = 17.5, although a two-component model better fits the data. In either case, the CO SLED is dominated by a "warm" and "dense" component. Compared to samples of local (Ultra) Luminous Infrared Galaxies ((U)LIRGs), starburst galaxies and high redshift Submillimeter Galaxies (SMGs), J2310+1855 exhibits higher CO excitation at (J ≥ 8), like other high redshift quasars. The high CO excitation, together with the enhanced L H2O /L IR , L H2O /L CO and L OH + /L H2O ratios, suggests that besides the UV radiation from young massive stars, other mechanisms such as shocks, cosmic rays and X-rays might also be responsible for the heating and ionization of the molecular gas. In the nuclear region probed by the molecular emissions lines, any of these mechanisms might be present due to the powerful quasar and the starburst activity.

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Section: Resultssupporting

confidence: 90%

Section: Resultsmentioning

confidence: 96%

mentioning

confidence: 99%

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Probing the Full CO Spectral Line Energy Distribution (SLED) in the Nuclear Region of a Quasar-starburst System at z = 6.003

Wang

Riechers

et al. 2020

ApJ

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“…No BLR emission lines have been detected in all quasars but J2310+1855, for which we derived a CIV-based M BH estimate of 6 × 10 9 M (see Appendix D for full details of the observations). Our estimation is consistent, within the error, with that reported by Feruglio et al (2018) and Shen et al (2019). We note that Shen et al (2019), who published NIR spectra of a large sample of z ∼ 5.7 QSOs, also provide a M BH measurement for J2310+1855 through virial relation based on MgII as well.…”

Section: Black Hole Mass From Lbt Datasupporting

confidence: 91%

The ALMA view of the high-redshift relation between supermassive black holes and their host galaxies

Pensabene

Carniani

Perna

et al. 2020

A&A

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Context. The existence of tight correlations between supermassive black holes (BHs) and their host galaxies properties in the local Universe suggests a closely linked evolution. Investigating these relations up to the high redshifts (z 6) is crucial to understand the interplay between star-formation and BH growth across the cosmic time and to set constraints on galaxy formation and evolution models. In this work we focus on the relation between BH mass (M BH ) and the dynamical mass (M dyn ) of the host galaxy. Aims. Previous works suggest an evolution of the M BH − M dyn relation with redshift indicating that BH growth precedes the galaxy mass assembly during their co-evolution at z > 3. However, dynamical galaxy masses at high redshift are often estimated through the virial theorem thus introducing significant uncertainties. This work aims at studying the M BH − M dyn relation of a sample of 2 < z < 7 quasars by constraining their galaxy masses through a full kinematical modelling of the cold gas kinematics thus avoiding all possible biases and effects introduced by the rough estimates usually adopted so far. Methods. For this purpose we retrieved public observations of 72 quasar host galaxies observed in [CII] 158µm or CO transitions with the Atacama Large Millimeter Array (ALMA). We then selected those quasars whose line emission is spatially resolved and performed a kinematic analysis on ALMA observations. We estimated the dynamical mass of the systems by modelling the gas kinematics with a rotating disc taking into account geometrical and instrumental effects. Our dynamical mass estimates, combined with M BH obtained from literature and our own new CIVλ1550 observations have allowed us to investigate the M BH /M dyn in the early Universe. Results. Overall we obtained a sample of 10 quasars at z ∼ 2 − 7 in which line emission is detected with high SNR ( 5 − 10) and the gas kinematics is spatially resolved and dominated by ordered rotation. The estimated dynamical masses place 6 out of 10 quasars above the local relation yielding to a M BH /M dyn ratios ∼ 10× higher than those estimated in low-z galaxies. On the other hand we found that 4 quasars at z ∼ 4 − 6 have dynamical-to-BH mass ratios consistent with what is observed in early type galaxies in the local Universe.

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“…The size (major axes) of CO(6-5) emission is 1.8 ± 0.4 times smaller than that of [C ii] emission, indicating that the molecular gas is more centrally concentrated than [C ii]. Similar result is also reported in the host galaxy of a bright z = 6 quasar (Feruglio et al 2018).…”

Section: Co Molecular Lines Observationssupporting

confidence: 79%

Spatially Resolved Interstellar Medium and Highly Excited Dense Molecular Gas in the Most Luminous Quasar at z = 6.327

Wang

Fan

et al. 2019

ApJ

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Among more than 200 quasars known at z 6, only one object, J0100+2802 (z=6.327), was found hosting a > 10 10 M super-massive black hole (SMBH). In order to investigate the host galaxy properties of J0100+2802, we performed multi-band ALMA observations, aiming at mapping the dust continuum, [C ii] and CO(6-5) emission lines with sub-kiloparsec scale resolution, as well as detecting high-J CO lines in CO(11-10), CO(10-9), and CO(7-6). The galaxy size is measured to be R major = 3.6 ± 0.2 kpc from the high resolution continuum observations. No ordered motion on kilo-parsec scales was found in both [C ii] and CO(6-5) emissions. The velocity dispersion is measured to be 161±7 km s −1 , ∼3 times smaller than that estimated from the local M-σ relation. In addition, we found that the CO emission is more concentrate (a factor of 1.8±0.4) than the [C ii] emission. Together with CO(2-1) detected by VLA, we measured the CO Spectral Line Energy Distribution (SLED), which is best fit by a two-components model, including a cool component at ∼ 24 K with a density of n (H 2 ) =10 4.5 cm −3 , and a warm component at ∼ 224 K with a density of n (H 2 ) =10 3.6 cm −3 . We also fitted the dust continuum with a graybody model, which indicates that it has either a high dust emissivity β 2 or a hot dust temperature T dust 60 K, or a combination of both factors. The highly excited CO emission and hot dust temperature suggest that the powerful AGN in J0100+2802 could contribute to the gas and dust heating although future observations are needed to confirm this.

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The dense molecular gas in the z ∼ 6 QSO SDSS J231038.88+185519.7 resolved by ALMA

Cited by 44 publications

References 72 publications

Probing the Full CO Spectral Line Energy Distribution (SLED) in the Nuclear Region of a Quasar-starburst System at z = 6.003

Probing the Full CO Spectral Line Energy Distribution (SLED) in the Nuclear Region of a Quasar-starburst System at z = 6.003

The ALMA view of the high-redshift relation between supermassive black holes and their host galaxies

Spatially Resolved Interstellar Medium and Highly Excited Dense Molecular Gas in the Most Luminous Quasar at z = 6.327

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