Stellar and ionized gas kinematics of the interacting Seyfert 1.9 galaxy NGC 2992

García-Lorenzo, B.; Arribas, S.; Mediavilla, E.

doi:10.1051/0004-6361:20011243

Cited by 22 publications

(38 citation statements)

References 23 publications

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“…One can identify this plane with the plane of the accretion disk, which itself is not modeled. The resulting position angle is −27 • with the SE part of it pointing away from us, consistent with the redshifted emission there seen by García-Lorenzo et al (2001).…”

Section: A Geometric Model For the Inner 3 ×supporting

confidence: 84%

“…It is generally assumed that the NW edge of the disk of NGC 2992 is closest to us with trailing spiral arms, and that the SE cone is closer and directed at us. However, an arc-shaped emission found by García-Lorenzo et al (2001), which might be associated with the radio loop, is red shifted in the SE, and can therefore only be consistent with an outflow if it is pointing away from us.…”

Section: Measured [O Iii] and Hα Lines Atmentioning

confidence: 87%

“…The velocity field of H 2 1-0S(1) and also that of Brγ, albeit not as clearly, show redshifted emission also to the southeast. García-Lorenzo et al (2001) investigated the velocity field of [O iii] and found an arc of redshifted velocities to the southeast and one of blueshifted velocities to the northwest with velocities of (64 ± 18) km s −1 , and (−79 ± 28) km s −1 , respectively. These arcs are just outside our field of view.…”

Section: -Dimensional Flux Distributions Velocities and Velocity Dmentioning

confidence: 99%

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Adaptive optics near infrared integral field spectroscopy of NGC 2992

Friedrich¹,

Davies²,

Hicks³

et al. 2010

A&A

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Aims. NGC 2992 is an intermediate Seyfert 1 galaxy showing outflows on kilo parsec scales which might be due either to AGN or starburst activity. We therefore aim at investigating its central region for a putative starburst in the past and its connection to the AGN and the outflows. Methods. Observations were performed with the adaptive optics near infrared integral field spectrograph SINFONI on the VLT, complemented by longslit observations with ISAAC on the VLT, as well as N-and Q-band data from the Spitzer archive. The spatial and spectral resolutions of the SINFONI data are 50 pc and 83 km s −1 , respectively. The field of view of 3 × 3 corresponds to 450 pc × 450 pc. Brγ equivalent width and line fluxes from PAHs were compared to stellar population models to constrain the age of the putative recent star formation. A simple geometric model of two mutually inclined disks and an additional cone to describe an outflow was developed to explain the observed complex velocity field in H 2 1-0S(1). Results. The morphologies of the Brγ and the stellar continuum are different suggesting that at least part of the Brγ emission comes from the AGN. This is confirmed by PAH emission lines at 6.2 μm and 11.2 μm and the strength of the silicon absorption feature at 9.7 μm, which point to dominant AGN activity with a relatively minor starburst contribution. We find a starburst age of 40-50 Myr from Brγ line diagnostics and the radio continuum; ongoing star formation can be excluded. Both the energetics and the timescales indicate that the outflows are driven by the AGN rather than the starburst. The complex velocity field observed in H 2 1-0S(1) in the central 450 pc can be explained by the superposition of the galaxy rotation and an outflow.

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Section: A Geometric Model For the Inner 3 ×supporting

confidence: 84%

Section: Measured [O Iii] and Hα Lines Atmentioning

confidence: 87%

Section: -Dimensional Flux Distributions Velocities and Velocity Dmentioning

confidence: 99%

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Adaptive optics near infrared integral field spectroscopy of NGC 2992

Friedrich¹,

Davies²,

Hicks³

et al. 2010

A&A

View full text Add to dashboard Cite

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“…This component would be related to the AGN, and not to the interaction (García-Lorenzo, Arribas, & Mediavilla 2001). The hidden Seyfert nucleus is probably located at the apex outflow origin and at the center of the bulge, but it does not seem to coincide with the kinematic center of the disk (García-Lorenzo, Arribas, & Mediavilla 2001).…”

Section: Introductionmentioning

confidence: 91%

“…• , as measured from the [O III] image reported by García-Lorenzo, Arribas, & Mediavilla (2001). This would correspond to a torus width of 25…”

Section: Nuclear Sed Modelling With Clumpy Torus Modelsmentioning

confidence: 99%

The nuclear and extended infrared emission of the Seyfert galaxy NGC 2992 and the interacting system Arp 245

García-Bernete

Almeida

Acosta–Pulido

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present subarcsecond resolution infrared (IR) imaging and mid-IR spectroscopic observations of the Seyfert 1.9 galaxy NGC 2992, obtained with the Gemini North Telescope and the Gran Telescopio CANARIAS (GTC). The N-band image reveals faint extended emission out to ∼3 kpc, and the PAH features detected in the GTC/CanariCam 7.5-13 µm spectrum indicate that the bulk of this extended emission is dust heated by star formation. We also report arcsecond resolution MIR and far-IR imaging of the interacting system Arp 245, taken with the Spitzer Space Telescope and the Herschel Space Observatory. Using these data, we obtain nuclear fluxes using different methods and find that we can only recover the nuclear fluxes obtained from the subarcsecond data at 20-25 µm, where the AGN emission dominates. We fitted the nuclear IR spectral energy distribution of NGC 2992, including the GTC/CanariCam nuclear spectrum (∼50 pc), with clumpy torus models. We then used the best-fitting torus model to decompose the Spitzer/IRS 5-30 µm spectrum (∼630 pc) in AGN and starburst components, using different starburst templates. We find that, whereas at shorter mid-IR wavelengths the starburst component dominates (64% at 6 µm), the AGN component reaches 90% at 20 µm. We finally obtained dust masses, temperatures and star formation rates for the different components of the Arp 245 system and find similar values for NGC 2992 and NGC 2993. These measurements are within those reported for other interacting systems in the first stages of the interaction.

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NGC 2992: Interplay between the multiphase disc, wind, and radio bubbles

Zanchettin,

Feruglio,

Massardi

et al. 2023

A&A

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We present an analysis of the gas kinematics in NGC 2992 based on VLT/MUSE, ALMA, and VLA data. Our aim is to characterise the disc, the wind, and their interplay in the cold molecular and warm ionised phases. NGC 2992 is a changing-look Seyfert known to host both a nuclear ultrafast outflow (UFO), and an AGN-driven kiloparsec-scale ionised wind. CO(2−1) and Hα arise from a multiphase disc with an inclination of 80 deg and radii of 1.5 and 1.8 kpc, respectively. By modelling the gas kinematics, we find that the velocity dispersion of the cold molecular phase, σgas, is consistent with that of star forming galaxies at the same redshift, except in the inner 600 pc region, and in the region between the cone walls and the disc, where σgas is a factor of 3−4 larger than in star forming galaxies for both the cold molecular and the warm ionised phases. This suggests that a disc–wind interaction locally boosts the gas turbulence. We detect a clumpy ionised wind in Hβ, [O III], Hα, and [N II] distributed in two wide-opening-angle ionisation cones reaching scales of 7 kpc (40 arcsec). The [O III] wind expands with a velocity exceeding −1000 km s−1 in the inner 600 pc, which is a factor of approximately five greater than the previously reported wind velocity. Based on spatially resolved electron density and ionisation parameter maps, we infer an ionised outflow mass of Mof, ion = (3.2 ± 0.3)×107 M⊙, and a total ionised outflow rate of Ṁof,ion = 13.5 ± 1 M⊙ yr−1. We detected ten clumps of cold molecular gas located above and below the disc in the ionisation cones, reaching maximum projected distances of 1.7 kpc and showing projected bulk velocities of up to 200 km s−1. On these scales, the wind is multiphase, with a fast ionised component and a slower molecular one, and a total mass of Mof, ion + mol = 5.8 × 107 M⊙, of which the molecular component carries the bulk of the mass, namely Mof, mol = 4.3 × 107 M⊙. The dusty molecular outflowing clumps and the turbulent ionised gas are located at the edges of the radio bubbles, suggesting that the bubbles interact with the surrounding medium through shocks, as also supported by the [O I]/Hα ratio. Conversely, both the large opening angle and the dynamical timescale of the ionised wind detected in the ionisation cones on 7 kpc scales indicate that this is not related to the radio bubbles but instead likely associated with a previous AGN episode. Finally, we detect a dust reservoir that is co-spatial with the molecular disc, with a cold dust mass of Mdust = (4.04 ± 0.03)×106 M⊙, which is likely responsible for the extended Fe Kα emission seen on 200 pc scales in hard X-rays and interpreted as reflection by cold dust.

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Stellar and ionized gas kinematics of the interacting Seyfert 1.9 galaxy NGC 2992

Cited by 22 publications

References 23 publications

Adaptive optics near infrared integral field spectroscopy of NGC 2992

Adaptive optics near infrared integral field spectroscopy of NGC 2992

The nuclear and extended infrared emission of the Seyfert galaxy NGC 2992 and the interacting system Arp 245

NGC 2992: Interplay between the multiphase disc, wind, and radio bubbles

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