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Circosta, C.; Mainieri, V.; Lamperti, Isabella; Padovani, P.; Bischetti, M.; Harrison, C. M.; Kakkad, D.; Zanella, Anita; Vietri, G.; Lanzuisi, G.; Salvato, M.; Brusa, M.; Carniani, Stefano; Cicone, C.; Cresci, G.; Feruglio, C.; Mannucci, F.; Marconi, A.; Perna, M.; Piconcelli, E.; Puglisi, A.; Saintonge, A.; Schramm, Malte; Vignali, C.; Zappacosta, L.

doi:10.1051/0004-6361/202039270

Cited by 38 publications

(66 citation statements)

References 148 publications

(208 reference statements)

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“…To avoid systematics related to the assumption of CO-to-H 2 conversion factor, we compare directly the CO line luminosity instead of the H 2 mass. This compilation also includes the sample by Circosta et al (2021), who recently performed an X-ray selection of both type I and type II AGNs with a range of bolometric luminosities, independently of their millimetre or infra-red emission. This more homogeneous sample also presents the advantage of being observed entirely in the CO(3-2) line, so that a direct comparison can be made with J0015+1842 regardless of the assumption of the excitation correction.…”

Section: Discussionmentioning

confidence: 99%

“…However, with its likely lower cold dust emission, J0015+1842 is located closer to the region populated by MS galaxies and SMGs, and with molecular content well above that of most X-ray selected AGNs. The only AGN in the sample of Circosta et al (2021) with similar CO luminosity is cid_1253 (COSMOS J100130.56+021842.6) with log(L CO(3−2) /(K km s −1 pc −2 )) = 10.80±0.04 and FWHM(CO) = 810±93 km s −1 . This object is a merger, hosting a narrow-line (type II) AGN, while J0015+1842 is a regular quasar with broad emission lines (type I).…”

Section: Discussionmentioning

confidence: 99%

“…4. Full width at half maximum vs. luminosity of the CO emission line in J0015+1842 (red star) compared to that in z > 1 AGNs (compiled by Bischetti et al (2021), with X-ray selected broad-line (BL) and narrow-line (NL) AGNs from Circosta et al (2021) shown by orange triangles). Measurements using CO(3-2) are shown with darker symbols than those from other CO lines.…”

Section: Continuum 3 MM Emission and Fir Luminositymentioning

confidence: 99%

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Remarkably high mass and velocity dispersion of molecular gas associated with a regular, absorption-selected type I quasar

Noterdaeme

Balashev

Combes

et al. 2021

A&A

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We present 3 mm observations of the quasar J0015+1842 at z = 2.63 with the NOrthern Extended Millimeter Array (NOEMA). Our data reveal molecular gas, traced with a Gaussian CO(3–2) line, with a remarkably high velocity dispersion (FWHM = 1010 ± 120 km s−1) that corresponds to a total molecular mass MH2 ≈ (3.4 − 17) × 1010 M⊙, depending on the adopted CO-to-H2 conversion factor αCO = (0.8 − 4.0) M⊙ (km s−1 pc2)−1. Assuming the 3 mm continuum emission is thermal, we derive a dust mass of about Mdust ∼ 5 × 108 M⊙. J0015+1842 is located in the molecular gas-rich region in the IR versus CO line luminosity diagram, in between the main locus of main-sequence and sub-millimetre galaxies and that of most other active galactic nuclei targeted so far for CO measurements. While the high velocity dispersion of the CO line suggests a merging system, J0015+1842 is observed to be a regular, only very moderately dust-reddened (AV ∼ 0.3 − 0.4) type I quasar from its UV-optical spectrum, from which we infer a mass of the super-massive black hole of about MBH ≈ 6 × 108 M⊙. We suggest that J0015+1842 is observed at a galaxy evolutionary stage where a massive merger has brought significant amounts of gas towards an actively accreting super-massive black hole (quasar). While the host still contains a large amount of dust and molecular gas with a high velocity dispersion, the quasar has already cleared the way towards the observer, likely through powerful outflows, as has recently been revealed by optical observations of the same object. High angular resolution observations of this and similar systems are expected to help us better determine the respective importance of evolution and orientation in the appearance of quasars and their host galaxies. These observations have the potential to investigate early feedback and star-formation processes in galaxies in their quasar phases.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Continuum 3 MM Emission and Fir Luminositymentioning

confidence: 99%

See 1 more Smart Citation

Remarkably high mass and velocity dispersion of molecular gas associated with a regular, absorption-selected type I quasar

Noterdaeme

Balashev

Combes

et al. 2021

A&A

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“…All spectra were extracted from the primary-beam corrected cubes. The ALMA CO(3-2) data are the same as in Circosta et al (2021). We reduced them using the CASA pipeline (v.5.1) and subtracted the continuum in the uv plane using uvcontsub with a linear polynomial fit, estimating the continuum from the ν obs < 107.2 GHz and ν obs > 107.6 GHz channels, corresponding to |v| > 560 km s −1 .…”

Section: Observationsmentioning

confidence: 99%

“…[OIII] = 1700 km s −1 , Kakkad et al 2020). Using snapshot 1 -resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations, Circosta et al (2021) resolved the CO(3-2) stemming from the interstellar medium (ISM), and found no evidence for depletion of H 2 gas with respect to inactive galaxies at matched z, M * , and broadly covering the same star formation rate (SFR) range. In this Letter we present new Atacama Compact Array (ACA) CO(3-2) observations of cid_346 tracing significant additional CO emission beyond the ISM, which led to the first image of a molecular halo out to r ∼ 200 kpc.…”

Section: Introductionmentioning

confidence: 99%

Super

Cicone

Mainieri

Circosta

et al. 2021

A&A

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We present the discovery of copious molecular gas in the halo of cid_346, a z = 2.2 quasar studied as part of the SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER). New Atacama Compact Array (ACA) CO(3−2) observations detect a much higher flux (by a factor of 14 ± 5) than measured on kiloparsec scales (r ≲ 8 kpc) using previous snapshot Atacama Large Millimeter/submillimeter Array data. Such additional CO(3−2) emission traces a structure that extends out to r ∼ 200 kpc in projected size, as inferred through direct imaging and confirmed by an analysis of the uv visibilities. This is the most extended molecular circumgalactic medium (CGM) reservoir that has ever been mapped. It shows complex kinematics, with an overall broad line profile (FWHM = 1000 km s−1) that is skewed towards redshifted velocities up to at least v ∼ 1000 km s−1. Using the optically thin assumption, we estimate a strict lower limit for the total molecular CGM mass observed by ACA of MmolCGM > 1010 M⊙. There is however room for up to MmolCGM ∼ 1.7 × 1012 M⊙, once optically thick CO emission with αCO = 3.6 M⊙ (K km s−1 pc2)−1 and L′CO(3−2)/L′CO(1−0) = 0.5 are assumed. Since cid_346 hosts quasar-driven ionised outflows and since there is no evidence of merging companions or an overdensity, we suggest that outflows may have played a crucial rule in seeding metal-enriched, dense gas on halo scales. However, the origin of such an extended molecular CGM remains unclear.

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The Close AGN Reference Survey (CARS)

Singha

Scharwächter

McElroy

et al. 2022

A&A

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Context. Active galactic nuclei (AGN) are thought to be intimately connected with their host galaxies through feeding and feedback processes. A strong coupling is predicted and supported by cosmological simulations of galaxy formation, but the details of the physical mechanisms are still observationally unconstrained. Aims. Galaxies are complex systems of stars and a multiphase interstellar medium (ISM). A spatially resolved multiwavelength survey is required to map the interaction of AGN with their host galaxies on different spatial scales and different phases of the ISM. The goal of the Close AGN Reference Survey (CARS) is to obtain the necessary spatially resolved multiwavelength observations for an unbiased sample of local unobscured luminous AGN. Methods. We present the overall CARS survey design and the associated wide-field optical integral-field unit (IFU) spectroscopy for all 41 CARS targets at z < 0.06 randomly selected from the Hamburg/ESO survey of luminous unobscured AGN. This data set provides the backbone of the CARS survey and allows us to characterize host galaxy morphologies, AGN parameters, precise systemic redshifts, and ionized gas distributions including excitation conditions, kinematics, and metallicities in unprecedented detail. Results. We focus our study on the size of the extended narrow-line region (ENLR) which has been traditionally connected to AGN luminosity. Given the large scatter in the ENLR size–luminosity relation, we performed a large parameter search to identify potentially more fundamental relations. Remarkably, we identified the strongest correlation between the maximum projected ENLR size and the black hole mass, consistent with an RENLR,max ∼ MBH0.5 relationship. We interpret the maximum ENLR size as a timescale indicator of a single black hole (BH) radiative-efficient accretion episode for which we inferred 〈log(tAGN/[yr])〉 = (0.45 ± 0.08)log(MBH/[M⊙]) + 1.78−0.67+0.54 using forward modeling. The extrapolation of our inferred relation toward higher BH masses is consistent with an independent lifetime estimate from the He II proximity zones around luminous AGN at z ∼ 3. Conclusions. While our proposed link between the BH mass and AGN lifetime might be a secondary correlation itself or impacted by unknown biases, it has a few relevant implications if confirmed. For example, the famous AGN Eigenvector 1 parameter space may be partially explained by the range in AGN lifetimes. Also, the lack of observational evidence for negative AGN feedback on star formation can be explained by such timescale effects. Further observational tests are required to confirm or rule out our BH mass dependent AGN lifetime hypothesis.

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Super

Cited by 38 publications

References 148 publications

Remarkably high mass and velocity dispersion of molecular gas associated with a regular, absorption-selected type I quasar

Remarkably high mass and velocity dispersion of molecular gas associated with a regular, absorption-selected type I quasar

Super

The Close AGN Reference Survey (CARS)

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