A two-stage outflow in NGC 1068

May, D.; Steiner, J. E.

doi:10.1093/mnras/stx886

Cited by 31 publications

(36 citation statements)

References 59 publications

(146 reference statements)

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“…Lopez-Rodriguez et al (2016) argue that this interaction can explain the increase of the polarization degree of the MIR emission in this region. Furthermore, gas streamers connecting the CND and the torus with an extent and morphology similar to the ones imaged by ALMA were previously detected in the 2.12 µm H 2 line, a tracer of hot molecular gas (T k ≥ 10 3 K) (Müller Sánchez et al 2009;Barbosa et al 2014;May & Steiner 2017). Our interpretation of the kinematics of the gas detected by ALMA in these structures favors the outflow scenario, also invoked by Barbosa et al (2014) and May & Steiner (2017), rather than the inflow scenario, first proposed by Müller Sánchez et al (2009).…”

Section: The Gas Streamers Seen At Other Wavelengths: Evidence Of Outmentioning

confidence: 66%

“…Furthermore, gas streamers connecting the CND and the torus with an extent and morphology similar to the ones imaged by ALMA were previously detected in the 2.12 µm H 2 line, a tracer of hot molecular gas (T k ≥ 10 3 K) (Müller Sánchez et al 2009;Barbosa et al 2014;May & Steiner 2017). Our interpretation of the kinematics of the gas detected by ALMA in these structures favors the outflow scenario, also invoked by Barbosa et al (2014) and May & Steiner (2017), rather than the inflow scenario, first proposed by Müller Sánchez et al (2009). We note that the inflow interpretation of Müller Sánchez et al (2009) was based on an analysis of the mean-velocity field of the gas streamers.…”

Section: The Gas Streamers Seen At Other Wavelengths: Evidence Of Outmentioning

confidence: 66%

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ALMA images the many faces of the NGC 1068 torus and its surroundings

García‐Burillo

Combes

Almeida

et al. 2019

A&A

138

103

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Aims. We investigate the fueling and the feedback of nuclear activity in the nearby (D = 14 Mpc) Seyfert 2 barred galaxy NGC 1068, by studying the distribution and kinematics of molecular gas in the torus and its connections to the host galaxy disk. Methods. We use the Atacama Large Millimeter Array (ALMA ) to image the emission of a set of molecular gas tracers in the circumnuclear disk (CND) and the torus of the galaxy using the CO(2-1), CO(3-2) and HCO + (4-3) lines and their underlying continuum emission with high spatial resolutions (0.03 −0.09 2−6 pc). These transitions, which span a wide range of physical conditions of molecular gas (n(H 2 ) ⊂ 10 3 −10 7 cm −3 ), are instrumental in revealing the density radial stratification and the complex kinematics of the gas in the torus and its surroundings. Results. The ALMA images resolve the CND as an asymmetric ringed disk of D 400 pc-size and mass of 1.4 × 10 8 M sun . The CND shows a marked deficit of molecular gas in its central 130 pc-region. The inner edge of the ring is associated with the presence of edge-brightened arcs of NIR polarized emission, which are identified with the current working surface of the ionized wind of the active galactic nucleus (AGN). ALMA proves the existence of an elongated molecular disk/torus in NGC 1068 of M gas torus 3 × 10 5 M , which extends over a large range of spatial scales D 10 − 30 pc around the central engine. The new observations evidence the density radial stratification of the torus: the HCO + (4-3) torus, with a full size D HCO + (4−3) = 11 ± 0.6 pc, is a factor of 2-3 smaller than its CO(2-1) and CO(3-2) counterparts, which have full-sizes D CO(3−2) = 26 ± 0.6 pc and D CO(2−1) = 28 ± 0.6 pc, respectively. This result brings into light the many faces of the molecular torus. The torus is connected to the CND through a network of molecular gas streamers detected inside the CND ring. The kinematics of molecular gas show strong departures from circular motions in the torus, the gas streamers, and the CND ring. These velocity field distortions are interconnected and are part of a 3D outflow that reflects the effects of AGN feedback on the kinematics of molecular gas across a wide range of spatial scales around the central engine. In particular, we estimate through modeling that a significant fraction of the gas inside the torus ( 0.4 − 0.6 × M gas torus ) and a comparable amount of mass along the gas streamers are outflowing. However, the bulk of the mass, momentum and energy of the molecular outflow of NGC 1068 is contained at larger radii in the CND region, where the AGN wind and the radio jet are currently pushing the gas assembled at the Inner Lindblad Resonance (ILR) ring of the nuclear stellar bar. Conclusions. In our favored scenario a wide-angle AGN wind launched from the accretion disk of NGC1068 is currently impacting a sizable fraction of the gas inside the torus. However, a large gas reservoir ( 1.2 − 1.8 × 10 5 M ), which lies close to the equatorial plane of the torus, remains unaffected by the feedback of...

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Section: The Gas Streamers Seen At Other Wavelengths: Evidence Of Outmentioning

confidence: 66%

Section: The Gas Streamers Seen At Other Wavelengths: Evidence Of Outmentioning

confidence: 66%

ALMA images the many faces of the NGC 1068 torus and its surroundings

García‐Burillo

Combes

Almeida

et al. 2019

A&A

138

103

View full text Add to dashboard Cite

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“…Both Brγ and [FeII] show in general the same velocity structure albeit with slightly lower absolute velocities. This is in contrast to the H 2 (1-0) S(1)kinematics which show much lower velocities and dispersions and suggests there is a lack of molecular gas in the outflow due to the AGN inflating a bubble in the disk such as the one seen in NGC 1068 (May & Steiner 2017).…”

Section: Ionized Gas Kinematicsmentioning

confidence: 69%

The multiphase gas structure and kinematics in the circumnuclear region of NGC 5728

Shimizu

Davies

Lutz

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report on our combined analysis of HST, VLT/MUSE, VLT/SINFONI, and ALMA observations of the local Seyfert 2 galaxy, NGC 5728 to investigate in detail the feeding and feedback of the AGN. The datasets simultaneously probe the morphology, excitation, and kinematics of the stars, ionized gas, and molecular gas over a large range of spatial scales (10 pc-10 kpc). NGC 5728 contains a large stellar bar which is driving gas along prominent dust lanes to the inner 1 kpc where the gas settles into a circumnuclear ring. The ring is strongly star forming and contains a substantial population of young stars as indicated by the lowered stellar velocity dispersion and gas excitation consistent with HII regions. We model the kinematics of the ring using the velocity field of the CO (2-1) emission and stars and find it is consistent with a rotating disk. The outer regions of the disk, where the dust lanes meet the ring, show signatures of inflow at a rate of 1 M yr −1 . Inside the ring, we observe three molecular gas components corresponding to the circular rotation of the outer ring, a warped disk, and the nuclear stellar bar. The AGN is driving an ionized gas outflow that reaches a radius of 250 pc with a mass outflow rate of 0.08 M yr −1 consistent with its luminosity and scaling relations from previous studies. While we observe distinct holes in CO emission which could be signs of molecular gas removal, we find that largely the AGN is not disrupting the structure of the circumnuclear region.

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“…Everett & Murray (2007) explored Parker wind models to explain the ∼ 100 pc outflows in AGN, but found no self-consistent temperature profile that could explain all of the kinematics. They did note that the generic hydromagnetic winds explored by Matzner & McKee (1999) could explain the acceleration, and there are morphological similarities between that model and the observations of May & Steiner (2017), but it was not clear how to explain the deceleration without interaction with the surrounding medium.…”

Section: Biconical Frustummentioning

confidence: 98%

H i Kinematics along the Minor Axis of M82

Martini

Leroy

Mangum

et al. 2018

ApJ

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M82 is one of the best studied starburst galaxies in the local universe, and is consequently a benchmark for studying star formation feedback at both low and high redshift. We present new VLA H I observations that reveal the cold gas kinematics along the minor axis in unprecedented detail. This includes the detection of H I up to 10 kpc along the minor axis toward the South and beyond 5 kpc to the North. A surprising aspect of these observations is that the line-of-sight H I velocity decreases substantially from about 120 km s −1 to 50 km s −1 from 1.5 to 10 kpc off the midplane. The velocity profile is not consistent with the H I gas cooling from the hot wind. We demonstrate that the velocity decrease is substantially greater than the deceleration expected from gravitational forces alone. If the H I consists of a continuous population of cold clouds, some additional drag force must be present, and the magnitude of the drag force places a joint constraint on the ratio of the ambient medium to the typical cloud size and density. We also show that the H I kinematics are inconsistent with a simple conical outflow centered on the nucleus, but instead require the more widespread launch of the H I over the ∼ 1 kpc extent of the starburst region. Regardless of the launch mechanism for the H I gas, the observed velocity decrease along the minor axis is sufficiently great that the H I may not escape the halo of M82. We estimate the H I outflow rate is much less than 1 M ⊙ yr −1 at 10 kpc off the midplane.

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A two-stage outflow in NGC 1068

Cited by 31 publications

References 59 publications

ALMA images the many faces of the NGC 1068 torus and its surroundings

ALMA images the many faces of the NGC 1068 torus and its surroundings

The multiphase gas structure and kinematics in the circumnuclear region of NGC 5728

H i Kinematics along the Minor Axis of M82

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