STORM IN A “TEACUP”: A RADIO-QUIET QUASAR WITH ≈10 kpc RADIO-EMITTING BUBBLES AND EXTREME GAS KINEMATICS

Harrison, C. M.; Thomson, A. P.; Alexander, D. M.; Bauer, F. E.; Edge, A. C.; Hogan, M. T.; Mullaney, James; Swinbank, A. M.

doi:10.1088/0004-637x/800/1/45

Cited by 89 publications

(155 citation statements)

References 130 publications

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“…Although the QSOs are considered radio-quiet, these radio luminosities are consistent with those of low-redshift Seyferts and QSOs where broad emission lines on 100−1000 pc scales could be directly associated with the hotspots of radio jets (e.g. Fu & Stockton 2009;Müller-Sánchez et al 2011;Husemann et al 2013b;Harrison et al 2015). This matches with our findings that the very broad lines must be emitted on scales <1 kpc that cannot be resolved with the seeing-limited optical observations at z ∼ 0.6.…”

Section: Given the Enhanced Asymmetry In The [O Iii] Light Distributionsupporting

confidence: 89%

Large-scale outflows in luminous QSOs revisited

Husemann

Scharwächter

Bennert

et al. 2016

A&A

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Context. Feedback from active galactic nuclei (AGN) is thought to play an important role in quenching star formation in galaxies. However, the efficiency with which AGN dissipate their radiative energy into the ambient medium remains strongly debated. Aims. Enormous observational efforts have been made to constrain the energetics of AGN feedback by mapping the kinematics of the ionized gas on kpc scale. We study how the observed kinematics and inferred energetics are affected by beam smearing of a bright unresolved narrow-line region (NLR) due to seeing. Methods. We re-analyse optical integral-field spectroscopy of a sample of twelve luminous unobscured quasi-stellar objects (QSOs) (0.4 < z < 0.7) previously presented in the literature. The point-spread function (PSF) for the observations is directly obtained from the light distribution of the broad Hβ line component. Therefore, we are able to compare the ionized gas kinematics and derived energetics of the total, truly spatially extended, and unresolved [O iii] emission. Results. We find that the spatially resolved [O iii] line width on kpc scales is significantly narrower than the one before PSF deblending. The extended NLRs (ENLRs) appear intrinsically offset from the QSO position or more elongated which can be interpreted in favour of a conical outflow on large scales while a spherical geometry cannot be ruled out for the unresolved NLR. We find that the kinetic power at 5 kpc distance based on a spherical model is reduced by two orders of magnitude for a conical outflow and one order of magnitude for the unresolved NLR after PSF deblending. This reduced kinetic power corresponds to only 0.01−0.1 per cent of the bolometric AGN luminosity. This is smaller than the 5−10% feedback efficiency required by some cosmological simulations to reproduce the massive galaxy population. The injected momentum fluxes are close or below the simple radiation-pressure limit L bol /c for the conical outflow model for the NLR and ENLR when beam smearing is considered. Conclusions. Integral-field spectroscopy is a powerful tool to investigate the energetics of AGN outflows, but the impact of beam smearing has to be taken into account in the high contrast regime of QSOs. For the majority of observations in the literature, this has not been addressed carefully so that the incidence and energetics of presumed kpc-scale AGN-driven outflows still remain an unsolved issue, from an observational perspective.

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Section: Given the Enhanced Asymmetry In The [O Iii] Light Distributionsupporting

confidence: 89%

Large-scale outflows in luminous QSOs revisited

Husemann

Scharwächter

Bennert

et al. 2016

A&A

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“…For the Teacup AGN, three offset fields cover virtually all the emission-line regions seen in the HST ACS images (Keel et al 2015). Similar data for this galaxy taken with the ESO VIMOS system have been shown by Harrison et al (2015); they describe results only for the [O III] emission lines, and the spatial scale of 0.67 per pixel limits their spatial resolution compared to these GMOS For straightforward comparison of emission-line properties over wide ranges in signal-to-noise ratio (SNR), we fit Gaussian profiles to the lines, constraining Hα and the adjacent [N II] lines to have the same full width at half-maximum (FWHM), with the same constraint on the [S II] doublet. In some regions, each line is double or triple, so we fit blended sets of Gaussians; we used the IRAF task splot interactively on the data cubes sampled in 0.2 spatial increments.…”

Section: Spectroscopic Mappingsupporting

confidence: 72%

“…The Teacup AGN was shown to have resolved outflow signatures by Harrison et al (2015). We find double or asymmetric profiles extending 2 north, 4 west, > 1.5 south, and 2 east in a roughly circular zone.…”

Section: Agn Outflows and Feedbackmentioning

confidence: 63%

Fading AGN Candidates: AGN Histories and Outflow Signatures^∗

Keel

Lintott

Maksym

et al. 2017

ApJ

101

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We consider the energy budgets and radiative history of eight fading AGN, identified from an energy shortfall between the requirements to ionize very extended (radius > 10 kpc) ionized clouds and the luminosity of the nucleus as we view it directly. All show evidence of significant fading on ≈ 50, 000-year timescales. We explore the use of minimum ionizing luminosity Q ion derived from photoionization balance in the brightest pixels in Hα at each projected radius. Tests using presumably constant Palomar-Green (PG) QSOs, and one of our targets with detailed photoionization modeling, suggest that we can derive useful histories of individual AGN, with the caveat that the minimum ionizing luminosity is always an underestimate and subject to uncertainties about fine structure in the ionized material. These consistency tests suggest that the degree of underestimation from the upper envelope of reconstructed Q ion values is roughly constant for a given object and therefore does not prevent such derivation. The AGN in our sample show a range of behaviors, with rapid drops and standstills; the common feature is a rapid drop in the last ≈ 2 × 10 4 years before the direct view of the nucleus. The e-folding timescales for ionizing luminosity are mostly in the thousands of years, with a few episodes as short as 400 years. In the limit of largely obscured AGN, we find additional evidence for fading from the shortfall between even the lower limits from recombination balance and the maximum luminosities derived from from infrared fluxes. We compare these long-term light curves, and the occurrence of these fading objects among all optically identified AGN, to simulations of AGN accretion; the strongest variations on these timespans are seen in models with strong and local (parsec-scale) feedback. We present Gemini integral-field optical spectroscopy, which shows a very limited role for outflows in these ionized structures. While rings and loops of emission, morphologically suggestive of outflow, are common, their kinematic structure shows some to be in regular rotation. UGC 7342 exhibits local signatures of outflows < 300 km s −1 , largely associated with very diffuse emission, and possibly entraining gas in one of the clouds seen in HST images. Only in the Teacup AGN do we see outflow signatures of order 1000 km s −1 . In contrast to the extended emission regions around many radio-loud AGN, the clouds around these fading AGN consist largely of tidal debris being externally illuminated but not displaced by AGN outflows.

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“…A number of cases in which this situation may occur have recently been identified; e.g. NGC 1266 (Alatalo et al 2011;Nyland et al 2013); NGC 1433 (Combes et al 2013); J1430+1339, nicknamed the "Teacup AG" (Harrison et al 2015). However, direct evidence that the radio plasma is at the origin of these outflows of cold gas is, so far, not available in all these cases.…”

Section: Resultsmentioning

confidence: 99%

The fast molecular outflow in the Seyfert galaxy IC 5063 as seen by ALMA

Morganti

Oosterloo

Oonk

et al. 2015

A&A

216

269

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We use high-resolution (0.5 arcsec) CO(2−1) observations performed with the Atacama Large Millimetre/submillimetre Array to trace the kinematics of the molecular gas in the Seyfert 2 galaxy IC 5063. The data reveal that the kinematics of the gas is very complex. A fast outflow of molecular gas extends along the entire radio jet (∼1 kpc), with the highest outflow velocities about 0.5 kpc from the nucleus, at the location of the brighter hot spot in the western lobe. The ALMA data show that a massive, fast outflow with velocities up to 650 km s −1 of cold molecular gas is present, in addition to the outflow detected earlier in warm H 2 , H i and ionized gas. All phases of the gas outflow show similar kinematics. IC 5063 appears to be one of the best examples of the multi-phase nature of AGN-driven outflows. Both the central AGN and the radio jet could energetically drive the outflow, however, the characteristics of the outflowing gas point to the radio jet being the main driver. This is an important result because IC 5063, although one of the most powerful Seyfert galaxies, is a relatively weak radio source (P 1.4 GHz = 3 × 10 23 W Hz −1 ). All the observed characteristics can be described by a scenario of a radio plasma jet expanding into a clumpy medium, interacting directly with the clouds and inflating a cocoon that drives a lateral outflow into the interstellar medium. This model is consistent with results obtained by recent simulations. A stronger, direct interaction between the jet and a gas cloud is present at the location of the brighter western lobe. This interaction may also be responsible for the asymmetry in the radio brightness of the two lobes. Even assuming the most conservative values for the conversion factor CO-to-H 2 , we find that the mass of the outflowing gas is between 1.9 and 4.8 × 10 7 M , of which between 0.5 and 1.3 × 10 7 M is associated with the fast outflow at the location of the western lobe. These amounts are much larger than those of the outflow of warm gas (molecular and ionized) and somewhat larger than of the H i outflow. This suggests that most of the observed cold molecular outflow is due to fast cooling after being shocked. This gas is the end product of the cooling process, although some of it could be the result of only partly dissociated clouds. Our CO observations demonstrate that fast outflows of substantial masses of molecular gas can be driven by relativistic jets, although in the case of IC 5063 the outflows are not fast enough to remove significant amounts of gas from the galaxy and the effects are limited to the central ∼0.5 kpc from the centre.

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STORM IN A “TEACUP”: A RADIO-QUIET QUASAR WITH ≈10 kpc RADIO-EMITTING BUBBLES AND EXTREME GAS KINEMATICS

Cited by 89 publications

References 130 publications

Large-scale outflows in luminous QSOs revisited

Large-scale outflows in luminous QSOs revisited

Fading AGN Candidates: AGN Histories and Outflow Signatures^∗

The fast molecular outflow in the Seyfert galaxy IC 5063 as seen by ALMA

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STORM IN A “TEACUP”: A RADIO-QUIET QUASAR WITH ≈10 kpc RADIO-EMITTING BUBBLES AND EXTREME GAS KINEMATICS

Cited by 89 publications

References 130 publications

Large-scale outflows in luminous QSOs revisited

Large-scale outflows in luminous QSOs revisited

Fading AGN Candidates: AGN Histories and Outflow Signatures∗

The fast molecular outflow in the Seyfert galaxy IC 5063 as seen by ALMA

Contact Info

Product

Resources

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Fading AGN Candidates: AGN Histories and Outflow Signatures^∗