The WISSH quasars project

Bischetti, M.; Feruglio, C.; Piconcelli, E.; Duras, F.; Pérez-Torres, M. Á.; Herrero, Raúl Gómez; Venturi, G.; Carniani, Stefano; Bruni, G.; Gavignaud, I.; Testa, V.; Bongiorno, A.; Brusa, M.; Circosta, C.; Cresci, G.; D’Odorico, V.; Maiolino, R.; Marconi, A.; Mingozzi, Matilde; Pappalardo, C.; Perna, M.; Traianou, Efthalia; Travascio, A.; Vietri, G.; Zappacosta, L.; Fiore, F.

doi:10.1051/0004-6361/202039057

Cited by 57 publications

(98 citation statements)

References 196 publications

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“…4 we compare the width and luminosity of the detected CO line with those seen in other z > 1 AGNs from the literature. We used the compilation of unlensed AGNs by Bischetti et al (2021) and retrieved the line widths from the original detection publications. In a few cases where several spectrally resolved components were reported, we ))…”

Section: Discussionmentioning

confidence: 99%

“…We compared the CO content of J0015+1842 with that of other AGNs as a function of the infra-red luminosity in Fig. 5 using the same compilation as previously, but restricted to systems for which Bischetti et al (2021) considered the infra-red measurement to be reasonably reliable (their Sect. 6.2).…”

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%

“…assume T d in the range 40-80 K, this results in an uncertainty of about one order of magnitude of log L IR /L = 12.2−13.1. We also note that if a merging or companion galaxy contributes to this infra-red luminosity (Bischetti et al 2021), then the value could be considered as an upper limit to the infra-red luminosity of the quasar host alone.…”

Section: Continuum 3 MM Emission and Fir Luminositymentioning

confidence: 99%

“…Weiß et al 2012;Nesvadba et al 2020). The studies have mostly focused on the bright end of the infra-red luminosity distribution and showed that luminous quasars generally have a low ratio of molecular gas masses to star formation rates (SFR) (e.g., Bischetti et al 2021), while starburst galaxies have much higher ratios of molecular masses to SFR, supporting the evolutionary paradigm. Several studies have also searched for CO emission in obscured quasars, that is, possibly at the short-lived intermediate stage between the SB and optically bright quasar phase (e.g., Polletta et al 2011;Brusa et al 2015), but differences with luminous quasars are apparently found only for Compton-thick cases, which are more likely associated with the initial steps of the blow-out phase (Perna et al 2018).…”

Section: Introductionmentioning

confidence: 98%

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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%

Section: Continuum 3 MM Emission and Fir Luminositymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

See 3 more Smart Citations

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

View full text Add to dashboard Cite

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The accretion of a solar mass per day by a 17-billion solar mass black hole

Wolf,

Lai,

Onken

et al. 2024

Nat Astron

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A dynamical measure of the black hole mass in a quasar 11 billion years ago

Abuter,

Allouche,

Amorim

et al. 2024

Nature

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Tight relationships exist in the local Universe between the central stellar properties of galaxies and the mass of their supermassive black hole (SMBH)1–3. These suggest that galaxies and black holes co-evolve, with the main regulation mechanism being energetic feedback from accretion onto the black hole during its quasar phase4–6. A crucial question is how the relationship between black holes and galaxies evolves with time; a key epoch to examine this relationship is at the peaks of star formation and black hole growth 8–12 billion years ago (redshifts 1–3)7. Here we report a dynamical measurement of the mass of the black hole in a luminous quasar at a redshift of 2, with a look back in time of 11 billion years, by spatially resolving the broad-line region (BLR). We detect a 40-μas (0.31-pc) spatial offset between the red and blue photocentres of the Hα line that traces the velocity gradient of a rotating BLR. The flux and differential phase spectra are well reproduced by a thick, moderately inclined disk of gas clouds within the sphere of influence of a central black hole with a mass of 3.2 × 108 solar masses. Molecular gas data reveal a dynamical mass for the host galaxy of 6 × 1011 solar masses, which indicates an undermassive black hole accreting at a super-Eddington rate. This suggests a host galaxy that grew faster than the SMBH, indicating a delay between galaxy and black hole formation for some systems.

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The WISSH quasars project

Cited by 57 publications

References 196 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

The accretion of a solar mass per day by a 17-billion solar mass black hole

A dynamical measure of the black hole mass in a quasar 11 billion years ago

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