QSO2 outflow characterization using data obtained with OSIRIS at the Gran Telescopio Canarias

Bellocchi, E.; Martín, Montserrat Villar; Cabrera-Lavers, A.; Emonts, Bjorn

doi:10.1051/0004-6361/201935270

Cited by 7 publications

(11 citation statements)

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“…The extent of the compact ionized outflow (R) is, R = 0.8 ± 0.3 kpc. In only 1 QSO (SDSS 0741+3020), Bellocchi et al (2019) detected a large outflow extending to at least ∼ 4 kpc from the central engine. Baron & Netzer (2019) investigated 2377 type 2 AGN showing visible [O III] wing emission from the parent sample of 24,264 AGN following Mullaney et al (2013).…”

Section: Discussionmentioning

confidence: 95%

“…They reported that only 2 of QSOs have outflow radius beyond 1 kpc, while 10 other QSOs have radii < 600 pc. Bellocchi et al (2019) investigated the ionized gas outflows in 6 type 2 QSOs with observations from the optical imager and long-slit spectrograph (OSIRIS) mounted on the 10.4m Gran Telescopio Canarias Spanish telescope (GTC). They identified ionized outflows in 4 out of 6 type 2 QSOs and reported that the ionized outflows are spatially unresolved in 2 QSOs and compact in 1 QSO.…”

Section: Discussionmentioning

confidence: 99%

“…This is known as beam smearing. Recent studies have reported sub-kpc scale outflows (e.g., Villar-Martin et al 2016;Tadhunter et al 2018;Kawaguchi et al 2018;Bellocchi et al 2019;Baron & Netzer 2019). Therefore, the spatial extensions of these outflows still remains as an open question.…”

Section: Introductionmentioning

confidence: 99%

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The Close AGN Reference Survey (CARS): Locating the [O III] wing component in luminous local Type 1 AGN

Singha,

Husemann,

Urrutia

et al. 2021

Preprint

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Context. The strong asymmetry in the optical [O III] λ5007 emission line is one of the best signatures of AGN-driven warm (∼ 10 4 K) ionized gas outflows on host galaxy scales. While large spectroscopic surveys like SDSS have characterized the kinematics of [O III] for large samples of AGN, estimating the associated energetics requires spatially resolving these outflows with, for example, IFU studies. Aims. As part of the Close AGN Reference Survey (CARS) we obtained spatially-resolved IFU spectroscopy for a representative sample of 39 luminous type 1 AGN at 0.01 < z < 0.06 with MUSE and VIMOS IFUs at the VLT to infer the spatial location of the ionized gas outflows. Methods. We compare the light distributions of the [O III] wing to that of the Hβ broad emission line region, a classical point source (PSF). We then use the PSF to distinguish between the unresolved and resolved [O III] wing emission. We further determine its location using spectro-astrometry for the point-like sources. Results. The [O III] wing is spatially unresolved in 23 out of the 36 AGN with >80% of the flux associated with a point-like source. We measure <100 pc offsets in the spatial location of the outflow from the AGN nucleus using the spectro-astrometry technique for these sources. For the other 13 AGN, the [O III] wing emission is resolved and possibly extended on kpc scale. Conclusions. We conclude that [O III] wing emission can be compact or extended in an unbiased luminous AGN sample, where both cases are likely to appear. Electron density in the compact [O III] wing regions (median n e ∼ 1900 cm −3 ) is nearly a magnitude higher than in the extended ones (median n e ∼ 500 cm −3 ). The presence of spatially extended and compact [O III] wing emission is unrelated to the AGN bolometric luminosity and to inclination effects, which means other features such as time delays, or mechanical feedback/radio jets may shape the ionized gas outflow properties.

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Section: Discussionmentioning

confidence: 95%

Section: Discussionmentioning

confidence: 99%

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The Close AGN Reference Survey (CARS): Locating the [O III] wing component in luminous local Type 1 AGN

Singha,

Husemann,

Urrutia

et al. 2021

Preprint

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“…Each of the five sources we selected (Table 1) showed symmetric double radio structure on arcsec angular scales in the 8.4-GHz VLA images, and their overall radio spectra were reported to be inverted [11]. Two of our targets, J0741+3020 and J0956+5735, were included in the sample of Bellocchi et al [24], who looked for ionized gas outflows in obscured quasars. According to their optical spectroscopic observations, outflows are detected in both objects.…”

Section: Sample Selection and Observing Goalsmentioning

confidence: 99%

High-Resolution Radio Observations of Five Optically Selected Type 2 Quasars

et al. 2020

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Many low-luminosity active galactic nuclei (AGNs) contain a compact radio core which can be observed with high angular resolution using very long baseline interferometry (VLBI).Combining arcsec-scale structural information with milliarcsec-resolution VLBI imaging is a useful way to characterise the objects and to find compact cores on parsec scales. VLBI imaging could also be employed to look for dual AGNs when the sources show kpc-scale double symmetric structure with flat or inverted radio spectra. We observed five such sources at redshifts 0.36 < z < 0.58 taken from an optically selected sample of Type 2 quasars with the European VLBI Network (EVN) at 1.7 and 5 GHz. Out of the five sources, only one (SDSS J1026-0042) shows a confidently detected compact VLBI core at both frequencies. The other four sources are marginally detected at 1.7 GHz only, indicating resolved-out radio structure and steep spectra. Using first-epoch data from the ongoing Karl G. Jansky Very Large Array Sky Survey, we confirm that indeed all four of these sources have steep radio spectra on arcsec scale, contrary to the inverted spectra reported earlier in the literature. However, the VLBI-detected source, SDSS J1026−0042, has a flat integrated spectrum. Radio AGNs that show kpc-scale symmetric structures with truly flat or inverted spectra could still be promising candidates of dual AGNs, to be targeted with VLBI observations in the future.Symmetry 2020, xx, 1 2 of 14 low accretion rates (< 10 −2 − 10 −3 times the Eddington rate [3]). LLAGNs also have radio emission that seems originating from compact jets on parsec (pc) scales [3][4][5].Using the technique of very long baseline interferometry (VLBI), we can directly observe compact pc or even sub-pc scale radio emission. The baselines of the globally distributed radio telescope arrays, such as the European VLBI Network (EVN), are up to a few thousand kilometers long, providing milliarcsec (mas) or sub-mas resolution, depending on the observing frequency. Because of the high resolution, a VLBI detection of a radio source at GHz frequencies typically implies high brightness temperatures (T b > 10 6−7 K) that can be produced by the non-thermal (synchrotron) emission of AGNs [6,7]. A radio power exceeding 10 21 W Hz −1 in a source unresolved by the Karl G. Jansky Very Large Array (VLA) on arcsec scales is already indicative of accretion-powered nuclear activity [7] or maybe circumnuclear starburst. Detection of a compact core with VLBI in a high-luminosity source is a very strong AGN indicator.In LLAGNs, compact radio emission with flat (i.e., with spectral index −0.5 ≤ α ≤ 0, where the flux density is S ∝ ν α , and ν is the frequency) or inverted (α > 0) radio continuum spectrum can indicate radio emission that is fueled by a synchrotron self-absorbed jet base coupled to an underluminous accretion disk (e.g., [4]) or an accretion inflow onto the black hole [8]. When observed at high frequencies, magnetized plasma in the accretion disc corona can also produce compact sub-pc scale optically ...

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“…During the last ten years it has become clear that ionised outflows are ubiquitous in QSO2 at different redshift (z) (e.g. Villar-Martín et al 2011;2016;Greene et al 2011;Mullaney et al 2013;Zakamska & Greene 2014;Bellocchi et al 2019). They appear to be triggered in general by processes related to the nuclear activity (e.g.…”

Section: Introductionmentioning

confidence: 99%

Interactions between the large-scale radio structures and the gas in a sample of optically selected type 2 quasars

Villar-Martin,

Emonts,

Lavers

et al. 2021

Preprint

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Context. The role of radio mode feedback in non radio-loud quasars needs to be explored in depth to determine its true importance. Its effects can be identified based on the evidence of interactions between the radio structures and the ambient ionised gas. Aims. We investigate this in a sample of 13 optically selected type-2 quasars (QSO2) at z <0.2 with Very Large Array (VLA) FIRST Survey radio detections. None are radio loud. The ranges of [OIII]λ5007 and monochromatic radio luminosities are log(L [OIII] /erg s −1 )∼42.08-42.79 and log(P1.4 GHz/erg s −1 Hz −1 ) ∼30.08-31.76. All show complex optical morphologies, with signs of distortion across tens of kpc due to mergers/interactions. Methods. We have searched for evidence of interactions between the radio structures and the ionised gas by characterising and comparing their morphologies. The first is traced by narrow band Hα images obtained with the GTC 10.4m Spanish telescope and the Osiris instrument. The second is traced by VLA radio maps obtained with A and B configurations to achieve both high resolution and brightness sensitivity.Results. The radio luminosity has an active galatic nucleus (AGN) component in 11/13 QSO2, which is spatially extended in our radio data in 9 of them (jets/lobes/other). The relative contribution of the extended radio emission to the total P1.4 GHz is in most cases in the range 30% to 90%. The maximum sizes are in the range d R max ∼few-500 kpc. QSO2 undergoing interaction/merger events appear to be invariably associated with ionised gas spread over large spatial scales with maximum distances from the AGN in the range rmax ∼12-90 kpc. The morphology of the ionised gas at <30 kpc is strongly influenced by AGN related processes. Evidence for radio-gas interactions exist in 10/13 QSO2; that is, all but one with confirmed AGN radio components. The interactions are identified across different spatial scales, from the nuclear narrow line region up to tens of kpc. Conclusions. Although this sample cannot be considered representative of the general population of QSO2, it supports the idea that large scale low/modest power radio sources can exist in radio-quiet QSO2, which can provide a source of feedback on scales of the spheroidal component of galaxies and well into the circumgalactic medium, in systems where radiative mode feedback is expected to dominate.

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QSO2 outflow characterization using data obtained with OSIRIS at the Gran Telescopio Canarias

Cited by 7 publications

References 72 publications

The Close AGN Reference Survey (CARS): Locating the [O III] wing component in luminous local Type 1 AGN

The Close AGN Reference Survey (CARS): Locating the [O III] wing component in luminous local Type 1 AGN

High-Resolution Radio Observations of Five Optically Selected Type 2 Quasars

Interactions between the large-scale radio structures and the gas in a sample of optically selected type 2 quasars

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