Disk, merger, or outflow? Molecular gas kinematics in two powerful obscured QSOs at<i>z</i> ≥ 3.4

Polletta, M.; Nesvadba, N. P. H.; Neri, R.; Omont, A.; Berta, S.; Bergeron, J.

doi:10.1051/0004-6361/201116446

Cited by 36 publications

(63 citation statements)

References 130 publications

(254 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…By measuring λL λ (7.8 μm) of all quasars with CO detections, we find that only three of these sources at z < 5 have extreme intrinsic luminosities (λL λ (7.8 μm) > ∼ 10 47 erg/s). Other six quasars with CO detection have 10 46 < λL λ (7.8 μm) < 10 46.5 erg/s, including the two highly obscured SWIRE quasars of Polletta et al (2011). To characterise quantitatively the unique population of hyperluminous quasars we need to substantially increase the sample with gas mass, dynamical mass, and SFR detections.…”

Section: Discussionmentioning

confidence: 99%

“…We note that the scatter in the correlation is higher for the lensed objects, probably because both luminosities have been corrected for the same amplification factor, but the source of the 7.8 μm luminosity is most likely very compact (pc scale), while the source of the CO luminosity could be more extended (a few kpc), implying an amplification pattern more complex than the assumed one. The 7.8 μm luminosities of highly obscured (Compton thick, N H > 10 24 cm −2 , two are from Polletta et al 2011, and Mrk 231) have been computed using the 6.5-22 μm fluxes, not corrected for extinction, which however may be relevant in highly obscured objects even at such long wavelengths. AGNs at z > 5.8 are found at the lower part of the correlation.…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Gas reservoir of a hyper-luminous quasar atz= 2.6

Feruglio

Bongiorno²,

Fiore³

et al. 2014

A&A

View full text Add to dashboard Cite

Context. Understanding the relationship between the formation and evolution of galaxies and their central super-massive black holes (SMBH) is one of the main topics in extragalactic astrophysics. Links and feedback may reciprocally affect both black hole and galaxy growth. Aims. Observations of the CO line at the main epoch of galaxy and SMBH assembly (z = 2−4) are crucial to investigating the gas mass, star formation, and accretion onto SMBHs, and the effect of AGN feedback. Potential correlations between AGN and host galaxy properties can be highlighted by observing extreme objects. Methods. We targeted CO(3-2) in ULAS J1539+0557, a hyper-luminous quasar (L bol > 10 48 erg/s) at z = 2.658, selected through its unusual red colour in the UKIDSS Large Area Survey (ULAS). Results. We find a molecular gas mass of 4.1 ± 0.8 × 10 10 M , by adopting a conversion factor α = 0.8 M K −1 km s −1 pc 2 , and a gas fraction of ∼0.4−0.1, depending mostly on the assumed source inclination. We also find a robust lower limit to the star-formation rate (SFR = 250−1600 M /yr) and star-formation efficiency (SFE = 25−350 L /(K km s −1 pc 2 ) by comparing the observed opticalnear-infrared spectral energy distribution with AGN and galaxy templates. The black hole gas consumption timescale, M(H 2 )/Ṁ acc , is ∼160 Myr, similar to or higher than the gas consumption timescale. Conclusions. The gas content and the star formation efficiency are similar to those of other high-luminosity, highly obscured quasars, and at the lower end of the star-formation efficiency of unobscured quasars, in line with predictions from AGN-galaxy co-evolutionary scenarios. Further measurements of the (sub)mm continuum in this and similar sources are mandatory to obtain a robust observational picture of the AGN evolutionary sequence.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Gas reservoir of a hyper-luminous quasar atz= 2.6

Feruglio

Bongiorno²,

Fiore³

et al. 2014

A&A

View full text Add to dashboard Cite

show abstract

“…None of our sources is close to the [OIII]λ5007Å/Hβ ∼ 10 value characteristic of the majority of type 2 quasars at low redshifts (Zakamska & Greene 2014), which would indicate an additional contribution to Balmer lines and thus a type 1 classification. Unfortunately, this method is also ambiguous, as the ionization conditions may be strongly modified by partial obscuration of the continuum and by the ram (2014) shown with grey and black crosses (black for peak signal-to-noise of [OIII] 20, grey otherwise; median w 90 = 1060 km s −1 ); X-ray selected obscured quasars at z ∼ 1.0 − 1.5 from Brusa et al (2015) shown with green circles (median w 90 = 1300 km s −1 ; infrared-selected red quasars at z < 1 from Urrutia et al (2012) shown with blue circles (fitting parameters for [OIII] emission for these objects are published by Brusa et al 2015; median w 90 = 1580 km s −1 ); submm-selected z ∼ 2 active galaxies from Harrison et al (2012) shown with magenta circles (median w 90 = 1330 km s −1 ); and z = 3.4 type 2 quasar SW022513 shown in orange from Polletta et al (2008); Nesvadba et al (2011);Polletta et al (2011). We also show a handful of type 1 quasars in cyan from Cano-Díaz et al (2012); Komossa et al (2015); Carniani et al (2015) wherever the data are available, with w 80 from Carniani et al (2015) estimated from their kinematic maps and scaled up to w 90 using the median value from .…”

Section: 1mentioning

confidence: 99%

Discovery of extreme [O iii] λ5007 Å outflows in high-redshift red quasars

Zakamska

Hamann

Pâris

et al. 2016

Mon. Not. R. Astron. Soc.

203

271

View full text Add to dashboard Cite

Black hole feedback is now a standard component of galaxy formation models. These models predict that the impact of black hole activity on its host galaxy likely peaked at z = 2−3, the epoch of strongest star formation activity and black hole accretion activity in the Universe. We used XShooter on the Very Large Telescope to measure rest-frame optical spectra of four z ∼ 2.5 extremely red quasars with infrared luminosities ∼ 10 47 erg s −1 . We present the discovery of very broad (full width at half max= 2600 − 5000 km s −1 ), strongly blue-shifted (by up to 1500 km s −1 ) [OIII]λ5007Å emission lines in these objects. In a large sample of type 2 and red quasars, [OIII] kinematics are positively correlated with infrared luminosity, and the four objects in our sample are on the extreme end both in [OIII] kinematics and infrared luminosity. We estimate that at least 3% of the bolometric luminosity in these objects is being converted into the kinetic power of the observed wind. Photo-ionization estimates suggest that the [OIII] emission might be extended on a few kpc scales, which would suggest that the extreme outflow is affecting the entire host galaxy of the quasar. These sources may be the signposts of the most extreme form of quasar feedback at the peak epoch of galaxy formation, and may represent an active "blow-out" phase of quasar evolution.

show abstract

“…(A color version of this figure is available in the online journal.) high-redshift quasars (Nesvadba et al 2011b;Polletta et al 2011) and high-redshift radio galaxies (Humphrey et al 2006).…”

Section: Efficiency Of the Transfer From The Jet Kineticmentioning

confidence: 99%

Strong Molecular Hydrogen Emission and Kinematics of the Multiphase Gas in Radio Galaxies With Fast Jet-Driven Outflows

Guillard

Ogle

Emonts

et al. 2012

ApJ

113

157

View full text Add to dashboard Cite

Observations of ionized and neutral gas outflows in radio galaxies (RGs) suggest that active galactic nucleus (AGN) radio jet feedback has a galaxy-scale impact on the host interstellar medium, but it is still unclear how the molecular gas is affected. Thus, it is crucial to determine the physical conditions of the molecular gas in powerful RGs to understand how radio sources may regulate the star formation in their host galaxies. We present deep Spitzer Infrared Spectrograph (IRS) high-resolution spectroscopy of eight nearby RGs that show fast H i outflows. Strikingly, all of these H i-outflow RGs have bright H 2 mid-IR lines that cannot be accounted for by UV or X-ray heating. This strongly suggests that the radio jet, which drives the H i outflow, is also responsible for the shock excitation of the warm H 2 gas. In addition, the warm H 2 gas does not share the kinematics of the ionized/neutral gas. 4C 12.50, 3C 459, and PKS 1549-79. This shows that, contrary to the H i gas, the H 2 gas is inefficiently coupled to the AGN jet-driven outflow of ionized gas. While the dissipation of a small fraction (<10%) of the jet kinetic power can explain the turbulent heating of the molecular gas, our data show that the bulk of the warm molecular gas is not expelled from these galaxies.

show abstract

Disk, merger, or outflow? Molecular gas kinematics in two powerful obscured QSOs atz ≥ 3.4

Cited by 36 publications

References 130 publications

Gas reservoir of a hyper-luminous quasar atz= 2.6

Gas reservoir of a hyper-luminous quasar atz= 2.6

Discovery of extreme [O iii] λ5007 Å outflows in high-redshift red quasars

Strong Molecular Hydrogen Emission and Kinematics of the Multiphase Gas in Radio Galaxies With Fast Jet-Driven Outflows

Contact Info

Product

Resources

About