Tracing the extreme interplay between radio jets and the ISM in IC 5063

Morganti, Raffaella; Frieswijk, W.; Oonk, Raymond; Oosterloo, Tom; Tadhunter, C. N.

doi:10.1051/0004-6361/201220734

Cited by 90 publications

(101 citation statements)

References 35 publications

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“…H i emission (8.4 × 10 9 M ) is traced in a regularly rotating warped disk with radius ∼2 arcmin (about 28 kpc), which is associated with the system of dust lanes. The likely counterpart of the H i disk is also detected in CO as originally observed with SEST in CO(1−0) by Wiklind et al (1995) and, more recently, with APEX in CO(2−1) by Morganti et al (2013b).…”

Section: A Case Study: Ic 5063supporting

confidence: 66%

“…The single pointing ALMA observation detects molecular gas up to a radius of ∼10 , therefore covering only the very inner part (r < 2 kpc) of the H i disk observed with ATCA (Morganti et al 1998). The bulk of the emission covers the same range of velocities (between 3140 to 3630 km s −1 ) as traced by the APEX observations (Morganti et al 2013b). However, the wider band of ALMA allows us to trace a much broader component of blueshifted gas, going down to velocities of ∼2750 km s −1 , i.e.…”

Section: The Alma Datamentioning

confidence: 85%

“…This hypothesis has been further strengthened by observations (using ISAAC on the VLT) of warm molecular gas (H 2 at 2.2 μm) which have, for the first time, shown the presence of outflowing molecular gas co-spatial with the bright radio hot spot (Tadhunter et al 2014). A signature of outflow of cold molecular gas has been found using CO(2−1) observations with APEX (Morganti et al 2013b). The limited spatial resolution of these observations did not allow us to determine where the outflow is occurring in relation to the radio structure and the main goal of the ALMA data presented in this paper is to remedy this situation.…”

Section: A Case Study: Ic 5063mentioning

confidence: 86%

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

Morganti

Oosterloo

Oonk

et al. 2015

A&A

223

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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Section: A Case Study: Ic 5063supporting

confidence: 66%

Section: The Alma Datamentioning

confidence: 85%

Section: A Case Study: Ic 5063mentioning

confidence: 86%

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

Morganti

Oosterloo

Oonk

et al. 2015

A&A

223

269

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“…Possibly, this power is drained into mechanical energy of the wind that interacts with the jets, and is eventually transformed into mechanical energy of the W 50 shell (Dubner et al, 1998). Similarly, the high efficiency of the mechanical energy transfer from jets to atomic and molecular outflows in the surroundings is observed in AGNs (Morganti et al, 2013).…”

Section: Discussionmentioning

confidence: 99%

Simulation of kinematics of SS 433 radio jets that interact with the ambient medium

Panferov

2014

A&A

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Context. The mildly relativistic jets of SS 433 are believed to inflate the surrounding supernova remnant W 50, possibly depositing more than 99% of their kinetic energy in the remnant expansion. Where and how this transformation of the energy occurs is as yet unknown. We can learn from this that the jets decelerate and that this deceleration is non-dissipative. Aims. We uncover the deviation of the arcsecond-scale precessing radio jets of SS 433 from the ballistic locus described by the kinematic model as a signature of the dynamics issuing from the interaction of the jets with the ambient medium. Methods. To do this, we simulated the kinematics of these jets, taking into account the ram pressure on the jets, which we estimated from the profile of brightness of synchrotron radiation along the radio jets, assuming pressure balance in the jets. Results. We found that to fit an observable locus in all scales the radio jets need to be decelerated and twisted in addition to the precession torsion, mostly within the first one-fifth of the precession period, and subsequently they extend in a way that imitates ballistic jets. This jet kinematics implies a smaller distance to SS 433 than the currently accepted 5.5 kpc. The physical parameters of the jet model, which links jets dynamics with radiation, are physically reliable and characteristic for the SS 433 jets. The model proposes that beyond the radio-brightening zone, the jet clouds expand because they are in pressure balance with the intercloud medium, and heat up with distance according to the law T = 2 × 10 4 (r/10 15 cm) 1.5 K. Conclusions. This model naturally explains and agrees with, the observed properties of the radio jets: a) the shock-pressed morphology; b) the brightness profile; c) the ∼10% deflections of the jet kinematics from the standard kinematic model -a magnitude of the jet speed decrement in our simulation; d) the precession-phase deviations from the standard kinematic model predictions; e) the dichotomy of the distances to the object, 4.8 kpc vs. 5.5 kpc, which are determined on the basis of the jet kinematics on scales of sub-arcsecond and several arcseconds, respectively; and f) the reheating on arcsecond scales.

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“…The outflow phenomenon concerns virtually all the phases of the interstellar medium (ISM), including the ionized gas (e.g., Heckman et al 1990;Colina et al 1991;Martin 1998;Holt et al 2008;Crenshaw et al 2010;Rupke & Veilleux 2013;Arribas et al 2014), the neutral A&A 580, A35 (2015) atomic medium (e.g., Heckman et al 2000;Rupke et al 2002Rupke et al , 2005aRupke et al , 2005bRupke et al , 2005cMorganti et al 2005;Martin 2005Martin , 2006Chen et al 2010), as well as the molecular gas phase (e.g., Feruglio et al 2010;Fischer et al 2010;Sturm et al 2011;Alatalo et al 2011Alatalo et al , 2015Chung et al 2011;Aalto et al 2012;Dasyra & Combes 2012;Maiolino et al 2012;Combes et al 2013;Morganti et al 2013;Veilleux et al 2013;Cicone et al 2012Cicone et al , 2014Cicone et al , 2015García-Burillo et al 2014;González-Alfonso et al 2014;Davies et al 2014;Emonts et al 2014;Sakamoto et al 2014). This multiwavelength evidence underlines that the overall impact of outflows can only be quantified if all of their ISM phases are studied in different populations of galaxies.…”

Section: Introductionmentioning

confidence: 99%

High-resolution imaging of the molecular outflows in two mergers: IRAS 17208-0014 and NGC 1614

García‐Burillo

Combes

Usero

et al. 2015

A&A

107

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Context. Galaxy evolution scenarios predict that the feedback of star formation and nuclear activity (AGN) can drive the transformation of gas-rich spiral mergers into (ultra) luminous infrared galaxies and, eventually, lead to the build-up of QSO/elliptical hosts. Aims. We study the role that star formation and AGN feedback have in launching and maintaining the molecular outflows in two starburst-dominated advanced mergers, NGC 1614 (D L = 66 Mpc) and IRAS 17208-0014 (D L = 181 Mpc), by analyzing the distribution and kinematics of their molecular gas reservoirs. Both galaxies present evidence of outflows in other phases of their ISM. Methods. We used the Plateau de Bure interferometer (PdBI) to image the CO(1-0) and CO(2-1) line emissions in NGC 1614 and IRAS 17208-0014, respectively, with high spatial resolution (0. 5-1. 2). The velocity fields of the gas were analyzed and modeled to find the evidence of molecular outflows in these sources and characterize the mass, momentum, and energy of these components. Results. While most (≥95%) of the CO emission stems from spatially resolved (∼2−3 kpc-diameter) rotating disks, we also detect in both mergers the emission from high-velocity line wings that extend up to ±500-700 km s −1 , well beyond the estimated virial range associated with rotation and turbulence. The kinematic major axis of the line-wing emission is tilted by ∼90 • in NGC 1614 and by ∼180 • in IRAS 17208-0014 relative to the major axes of their respective rotating disks. These results can be explained by the existence of non-coplanar molecular outflows in both systems: the outflow axis is nearly perpendicular to the rotating disk in NGC 1614, but it is tilted relative to the angular momentum axis of the rotating disk in IRAS 17208-0014. Conclusions. In stark contrast to NGC 1614, where star formation alone can drive its molecular outflow, the mass, energy, and momentum budget requirements of the molecular outflow in IRAS 17208-0014 can be best accounted for by the existence of a so far undetected (hidden) AGN of L AGN ∼ 7 × 10 11 L . The geometry of the molecular outflow in IRAS 17208-0014 suggests that the outflow is launched by a non-coplanar disk that may be associated with a buried AGN in the western nucleus.

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Tracing the extreme interplay between radio jets and the ISM in IC 5063

Cited by 90 publications

References 35 publications

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

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

Simulation of kinematics of SS 433 radio jets that interact with the ambient medium

High-resolution imaging of the molecular outflows in two mergers: IRAS 17208-0014 and NGC 1614

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