Testing the blast-wave AGN feedback scenario in MCG-03-58-007

Sirressi, Mattia; Cicone, C.; Severgnini, P.; Braito, V.; Dotti, Massimo; Ceca, R. Della; Reeves, J. N.; Matzeu, G. A.; Vignali, C.; Ballo, L.

doi:10.1093/mnras/stz2249

Cited by 24 publications

(35 citation statements)

References 64 publications

(111 reference statements)

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“…MCG-03-58-007 was also observed with ALMA, revealing a component that likely corresponds to a low velocity (v CO ∼ 170 km s −1 ) molecular outflow in the central 4 kpc. However, as for PDS 456 and I Zw 1 , the kinetic power of the putative molecular outflow is at least two orders of magnitude below the expected value for an energy conserving wind ( E Mol / E X ∼ 4 × 10 −3 ; Sirressi et al 2019).…”

Section: Introductionmentioning

confidence: 81%

“…Thus on average the derived kinetic output of this zone is of the order of L KIN ∼ 1.7 × 10 44 erg s −1 , which is ∼ 5%L bol , where the bolometric luminosity of MCG-03-58-007 is L bol ∼ 3 × 10 45 erg s −1 (B18). Regardless of the N H variability, all the estimates of the kinetic energy of the X-ray wind are at least two orders of magnitude above the kinetic energy carried by the molecular gas phase (with E CO / E X ranging from ∼ 3 × 10 −3 to ∼ 10 −2 ; Sirressi et al 2019). Note that, despite the large errors on the N H and the uncertainties on the black hole mass, we cannot reconcile the different measurements of the X-ray wind energetics versus the large scale CO wind.…”

Section: The Slower Outflow Componentmentioning

confidence: 99%

“…c : Outflow kinetic power ( E) in Eddington units d : The kinetic power unit is erg s −1 and is derived for M BH = 10 8 M ⊙. e : The outflow energetics for the molecular gas depends on the CO-to-H 2 conversion factor, here a factor of 2.1M ⊙ (K km s−1 pc2) −1 was adopted (Sirressi et al 2019). in line with the typical estimates for powerful winds in other AGN (e.g.…”

Section: The Slower Outflow Componentmentioning

confidence: 99%

“…In order to compare the disk wind kinematics with the ones reported for the possible kpc-scale molecular outflow (Sirressi et al 2019), we considered the values obtained for the persistent component (zone 1) and converted the E to the absolute values of the kinetic output by adopting the estimated black hole mass of MCG-03-58-007 of M BH ∼ 10 8 M ⊙ (see B18 and Sirressi et al 2019). The kinetic power of this zone ranges from L KIN ∼ 10 44 erg s −1 , as measured during the first part of the XMM-Newton observations, to ∼ 3 × 10 44 erg s −1 for the Suzaku observation (see Table 3).…”

Section: The Slower Outflow Componentmentioning

confidence: 99%

“…This indicates the importance of the incident radiation upon the wind: as the luminosity and thus the radiation pressure increases, a faster wind is driven. MCG-03-58-007 is a bright and nearby Seyfert 2 galaxy (F 2−10 keV ∼ 2 × 10 −12 erg cm −2 s −1 , z = 0.03233; Sirressi et al 2019). The first deep Suzaku (Mitsuda et al 2007) observation performed in 2010 showed a spectrum of an obscured AGN (N H ∼ 2 × 10 23 cm −2 ) and, surprisingly, two deep (EW ∼ 300 eV) blue-shifted absorption troughs at E = 7.4 ± 0.1 keV and E = 8.5 ± 0.2 keV (Braito et al 2018, hereafter B18).…”

Section: Introductionmentioning

confidence: 99%

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The stratified disc wind of MCG-03-58-007

Braito

Reeves

Severgnini

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Past Suzaku, XMM-Newton and NuSTAR observations of the nearby (z = 0.03233) bright Seyfert 2 galaxy MCG-03-58-007 revealed the presence of two deep and blue-shifted iron K-shell absorption line profiles. These could be explained with the presence of two phases of a highly ionized, high column density accretion disk wind outflowing with vout1 ∼ −0.1c and vout2 ∼ −0.2c. Here we present two new observations of MCG-03-58-007: one was carried out in 2016 with Chandra and one in 2018 with Swift. Both caught MCG-03-58-007 in a brighter state (F2 − 10 keV ∼ 4 × 10−12 erg cm−2 s−1) confirming the presence of the fast disk wind. The multi-epoch observations of MCG-03-58-007 covering the period from 2010 to 2018 were then analysed. These data show that the lower velocity component outflowing with vout1 ∼ −0.072 ± 0.002c is persistent and detected in all the observations, although it is variable in column density in the range NH ∼ 3 − 8 × 1023 cm−2. In the 2016 Swift observation we detected again the second faster component outflowing with vout2 ∼ −0.2c, with a column density ($N_{\mbox{H}}=7.0^{+5.6}_{-4.1}\times 10^{23}$ cm−2), similar to that seen during the Suzaku observation. However during the Chandra observation two years earlier, this zone was not present (NH < 1.5 × 1023 cm−2), suggesting that this faster zone is intermittent. Overall the multi-epochs observations show that the disk wind in MCG-03-58-007 is not only powerful, but also extremely variable, hence placing MCG-03-58-007 among unique disk winds such as the one seen in the famous QSO PDS456. One of the main results of this investigation is the consideration that these winds could be extremely variable, sometime appearing and sometime disappearing; thus to reach solid and firm conclusions about their energetics multiple observations are mandatory.

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Section: Introductionmentioning

confidence: 81%

Section: The Slower Outflow Componentmentioning

confidence: 99%

Section: The Slower Outflow Componentmentioning

confidence: 99%

Section: The Slower Outflow Componentmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The stratified disc wind of MCG-03-58-007

Braito

Reeves

Severgnini

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Galaxy-scale ionised winds driven by ultra-fast outflows in two nearby quasars

Marasco

Cresci

Nardini

et al. 2020

A&A

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We used MUSE adaptive optics data in narrow field mode to study the properties of the ionised gas in MR 2251−178 and PG 1126−041, two nearby (z ≃ 0.06) bright quasars (QSOs) hosting sub-pc scale ultra-fast outflows (UFOs) detected in the X-ray band. We decomposed the optical emission from diffuse gas into a low- and a high-velocity components. The former is characterised by a clean, regular velocity field and a low (∼80 km s−1) velocity dispersion. It traces regularly rotating gas in PG 1126−041, while in MR 2251−178 it is possibly associated with tidal debris from a recent merger or flyby. The other component is found to be extended up to a few kpc from the nuclei, and shows a high (∼800 km s−1) velocity dispersion and a blue-shifted mean velocity, as is expected from outflows driven by active galactic nuclei (AGN). We estimate mass outflow rates up to a few M⊙ yr−1 and kinetic efficiencies LKIN/LBOL between 1−4 × 10−4, in line with those of galaxies hosting AGN of similar luminosities. The momentum rates of these ionised outflows are comparable to those measured for the UFOs at sub-pc scales, which is consistent with a momentum-driven wind propagation. Pure energy-driven winds are excluded unless about 100× additional momentum is locked in massive molecular winds. In comparing the outflow properties of our sources with those of a small sample of well-studied QSOs hosting UFOs from the literature, we find that winds seem to systematically lie either in a momentum-driven or an energy-driven regime, indicating that these two theoretical models bracket the physics of AGN-driven winds very well.

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Molecular gas kinematics in the nuclear region of nearby Seyfert galaxies with ALMA

Belete

Andreani

Fernández-Ontiveros

et al. 2021

A&A

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Context. The study of the distribution, morphology, and kinematics of cold molecular gas in the nuclear and circumnuclear regions of active galactic nuclei (AGNs) helps to characterise and hence to quantify the impact of the AGNs on the host galaxy over its lifetime. Aims. We present the analysis of the molecular gas in the nuclear regions of three Seyfert galaxies, NGC 4968, NGC 4845, and MCG-06-30-15, using Atacama Large sub-Millimetre Array (ALMA) observations of the CO(2−1) emission line. The aim is to determine the kinematics of the gas in the central (∼1 kpc) region and thereby to probe nuclear fueling and feedback of AGNs. Methods. We used two different softwares, namely the 3D-Based Analysis of Rotating Object via Line Observations and DiskFit, to model the kinematics of the gas in the molecular disc, and thereby to determine the gas rotation and any kinematical perturbations. Results. Circular motions dominate the kinematics of the molecular gas in the central discs, mainly in NGC 4845 and MCG-06-30-15; however there is clear evidence of non-circular motions in the central (∼1 kpc) region of NGC 4845 and NGC 4968. The strongest non-circular motion is detected in the inner disc of NGC 4968, mainly along the minor kinematic axis, with a velocity ∼115 km s−1. Of all DiskFit models, the bisymmetric model is found to give the best fit for NGC 4968 and NGC 4845, indicating that the observed non-circular motions in the inner disc of these galaxies could result from the nuclear barred structure, where the gas streams in elliptical orbits aligned along the bar. If the dynamics of NGC 4968 is modelled as a corotation pattern just outside of the bar, the bar pattern speed becomes Ωb = 52 km s−1 kpc−1; the corotation is set at 3.5 kpc; and the inner Lindblad resonance (ILR) ring is R = 300 pc, corresponding to the CO emission ring. In the NGC 4968 galaxy, the torques exerted on the gas by the bar are positive in the centre, within the gas nuclear ring, and negative outside. This shows that the gas is transiently trapped in the ILR. The comparison of the CO intensity maps with the map of the cold dust emission shows an absence of CO in the centre of NGC 4968; also the dust distribution and CO emission in and around the centre of NGC 4845 have similar extensions. The 1.2 mm ALMA continuum is peaked and compact in NGC 4968 and MCG-06-30-15, but their CO(2−1) emissions have extended distributions. Allowing the CO-to-H2 conversion factor αCO between 0.8 and 3.2, which is typical of nearby galaxies of the same type, the molecular mass M(H2) is estimated to be ∼3 − 12 × 107 M⊙ (NGC 4968), ∼9 − 36 × 107 M⊙ (NGC 4845), and ∼1 − 4 × 107 M⊙ (MCG-06-30-15). Conclusions. We conclude that the observed non-circular motions in the molecular disc of NGC 4968 and likely those seen in NGC 4845 are due to the presence of the bar in the nuclear region. We discuss the possibility that the observed pattern in the kinematics might be a consequence of the presence of AGNs, and this might be the case for NGC 4845. At the current spectral and spatial resolution and sensitivity, we cannot claim any strong evidence in these sources of the long sought feedback or feeding effect resulting from the presence of AGNs.

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Testing the blast-wave AGN feedback scenario in MCG-03-58-007

Cited by 24 publications

References 64 publications

The stratified disc wind of MCG-03-58-007

The stratified disc wind of MCG-03-58-007

Galaxy-scale ionised winds driven by ultra-fast outflows in two nearby quasars

Molecular gas kinematics in the nuclear region of nearby Seyfert galaxies with ALMA

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