The gentle monster PDS 456

Bischetti, M.; Piconcelli, E.; Feruglio, C.; Fiore, F.; Carniani, Stefano; Brusa, M.; Cicone, C.; Vignali, C.; Bongiorno, A.; Cresci, G.; Mainieri, V.; Maiolino, R.; Marconi, A.; Nardini, E.; Zappacosta, L.

doi:10.1051/0004-6361/201935524

Cited by 83 publications

(102 citation statements)

References 72 publications

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“…Actually, with the more recent IRAM and ALMA data, only Mrk 231 and IRAS 17020+4544 (Longinotti et al 2018) are consistent with the above scenario. An energy conserving wind can be clearly ruled out for both the prototype of the fast disk winds PDS 456 (Bischetti et al 2019) and the powerful wind of I Zw 1 . This hints for a range of efficiencies in transferring the kinetic energy of the inner wind out to the large-scale molecular component (Mizumoto et al 2019), which suggest that the role of the powerful disk winds in the galaxy evolution may be more complex that what we thought.…”

Section: Introductionmentioning

confidence: 99%

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: 99%

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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“…Recent results on other sources support such picture, but the coupling between the inner UFO and the neutral/molecular outflow is found between the two extreme regimes of momentum-and energy-driving, indicating either a low efficiency of the coupling and/or in-situ formation of molecular gas depending on the particular environment in each galaxy (Feruglio et al 2015(Feruglio et al , 2017Mizumoto et al 2019;Bischetti et al 2019. In Fig.…”

Section: From Nuclear To Galaxy Scale Feedbackmentioning

confidence: 73%

Tracing AGN feedback, from the SMBH horizon up to cluster scales

Tombesi

2019

Proc. IAU

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Observations performed in the last decades have shown that supermassive black holes (SMBHs) and cosmic structures are not separate elements of the Universe. While galaxies extend on spatial scales about ten orders of magnitude larger than the horizon of SMBHs, black holes would not exist without matter feeding them, and cosmic structures would not be the same without feedback from SMBHs. Powerful winds/jets in active galactic nuclei (AGN) may be the basis of this co-evolution. Synergistic observations in the X-rays and other wavebands have been proven to be fundamental to map AGN winds from the event horizon up to galaxy scales, providing a promising avenue to study the multi-phase SMBH feeding and feedback processes. Moreover, a spatially resolved, spectroscopic analysis of AGN in clusters will allow us to probe the multiphase medium ranging from galactic up to cluster scales. Revolutionary advances are expected in the upcoming decade with new multi-wavelength observatories, ranging from radio to X-rays.

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“…For a majority of our sample, it is possible to see a relation between the maximum outflow rate and (left panel) and the position where the peak outflow rate occurs and the maximum outflow rate for each target (right panel). relativistic outflows (UFOs) observed in the X-ray spectra of some AGN (Bischetti et al 2019).…”

Section: Discussionmentioning

confidence: 99%

“…We are currently exploring this possibility (Trindade Falcão et al in preparation). Also, neutral and molecular gas could be contributing to the outflow (see section 2.5) and, altogether, could provide a much higher mass outflow rate (Tombesi et al 2015;Bischetti et al 2019).…”

Section: Discussionmentioning

confidence: 99%

Hubble Space Telescope observations of [O iii] emission in nearby QSO2s: physical properties of the ionized outflows

Falcão

Kraemer

Fischer

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use Hubble Space Telescope (HST)/ Space Telescope Imaging Spectrograph (STIS) long-slit G430M and G750M spectra to analyse the extended [O III] λ5007 emission in a sample of twelve nearby (z >0.12) luminous (Lbol > 1.6 × 1045 erg s−1) QSO2s. The purpose of the study is to determine the properties of the mass outflows of ionised gas and their role in AGN feedback. We measure fluxes and velocities as functions of radial distances. Using Cloudy models and ionising luminosities derived from [O III] λ5007, we are able to estimate the densities for the emission-line gas. From these results, we derive masses of [O III]-emitting gas, mass outflow rates, kinetic energies, kinetic luminosities, momenta and momentum flow rates as a function of radial distance for each of the targets. For the sample, masses are several times 103M⊙ − 107M⊙ and peak outflow rates are 9.3 × 10−3M⊙ yr−1 to 10.3 M⊙ yr−1. The peak kinetic luminosities are 3.4 × 10−8 to 4.9 × 10−4 of the bolometric luminosity, which does not approach the 5.0 × 10−3 - 5.0 × 10−2 range required by some models for efficient feedback. For Mrk 34, which has the largest kinetic luminosity of our sample, in order to produce efficient feedback there would have to be 10 times more [O III]-emitting gas than we detected at its position of maximum kinetic luminosity. Three targets show extended [O III] emission, but compact outflow regions. This may be due to different mass profiles or different evolutionary histories.

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The gentle monster PDS 456

Cited by 83 publications

References 72 publications

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

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

Tracing AGN feedback, from the SMBH horizon up to cluster scales

Hubble Space Telescope observations of [O iii] emission in nearby QSO2s: physical properties of the ionized outflows

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