Outflows of Very Ionized Gas in the Centers of Seyfert Galaxies: Kinematics and Physical Conditions

Rodríguez-Ardila, A.; Prieto, M. A.; Viegas, S. M.; Gruenwald, R.

doi:10.1086/508864

Cited by 94 publications

(158 citation statements)

References 33 publications

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“…Given previous reports of spectroscopic binary AGN candidates (with double-peaked [O iii], and perhaps Hβ), SDSS J1316+1753 suggests itself as another candidate which, in particular, has all of its emission lines double-peaked. However, line splitting of individual or all emission lines has also occasionally been observed before in single AGNs (e.g., Heckman et al 1981;Veilleux 1991aVeilleux , 1991bRodriguez-Ardila et al 2006), and in a few compact radio sources (e.g., Holt et al 2008). It has been suggested to be linked to the geometry of, or local physics in, the NLR, or the influence of radio jets.…”

Section: Discussionmentioning

confidence: 72%

Narrow Double-Peaked Emission Lines of SDSS J131642.90+175332.5: Signature of a Single or a Binary Agn in a Merger, Jet-Cloud Interaction, or Unusual Narrow-Line Region Geometry

Komossa

2009

ApJ

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We present an analysis of the active galaxy SDSS J131642.90+175332.5, which is remarkable because all of its narrow emission lines are double-peaked, and because it additionally shows an extra broad component (FHWM ∼ 1400 km s −1 ) in most of its forbidden lines, peaking in between the two narrow systems. The peaks of the two narrow systems are separated by 400-500 km s −1 in velocity space. The spectral characteristics of double-peaked [O iii] emission have previously been interpreted as a signature of dual or binary active galactic nuclei (AGNs), among other models. In the context of the binary scenario, SDSS J131642.90+175332.5 is a particularly good candidate because not just one line but all of its emission lines are double-peaked. However, we also discuss a number of other scenarios which can potentially account for double-peaked narrow emission lines, including projection effects, a two-sided outflow, jet-cloud interactions, special narrow-line region (NLR) geometries (disks, bars, or inner spirals), and a galaxy merger with only one AGN illuminating two NLRs. We argue that the similarity of the emission-line ratios in both systems, and the presence of the very unusual broad component at intermediate velocity, makes a close pair of unrelated AGNs unlikely, and rather argues for processes in a single galaxy or merger. We describe future observations that can distinguish between these remaining possibilities.

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Section: Discussionmentioning

confidence: 72%

Narrow Double-Peaked Emission Lines of SDSS J131642.90+175332.5: Signature of a Single or a Binary Agn in a Merger, Jet-Cloud Interaction, or Unusual Narrow-Line Region Geometry

Komossa

2009

ApJ

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“…Shock velocities greater than 200 km s −1 produce strong free-free X-ray emission and thus can be the cause of the observed extended X-rays and, in turn, additionally contribute to the H2 excitation. (Rossa et al 2000;Bennert et al 2006;Rodríguez-Ardila et al 2006). Moreover, evidence of an extended coronal emission was reported by Rossa et al (2000) and Rodríguez-Ardila et al (2006), who found that [Fe vii] λ6087Å is emitted in a region of ∼ 100 pc in radius from the the centre.…”

Section: Excitation Of the Molecular Gasmentioning

confidence: 83%

“…The use of the high ionization coronal line emitting spectrum as a signature of energetic AGN-driven outflows at scales of few pc from the centre allowed Rodríguez-Ardila et al (2006) to open a new window to explore this subject. Because of their high-ionization potential ( 100 eV), these lines are genuine tracers of the presence of an AGN (Penston 1984;Marconi et al 1994).…”

Section: Introductionmentioning

confidence: 99%

“…Among the closest AGNs displaying a remarkable coronal line spectrum is NGC 1386 (Reunanen et al 2002;Rodríguez-Ardila et al 2006). This source is, instead of a powerful AGN, in the borderline between the high luminous Seyfert type and the low luminosity AGN (LLAGN) class, as inferred from its low nuclear bolometric luminosity, ∼ 3 × 10 42 erg s −1 (Fernández-Ontiveros et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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Powerful outflows in the central parsecs of the low-luminosity active galactic nucleus NGC 1386

Rodríguez-Ardila

Prieto

Mazzalay

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Low-luminosity Active Galactic Nuclei, i.e. L bol /L edd ∼ 10 −6 − 10 −3 constitute the bulk population of Active Galactic Nuclei (AGNs). Powerful jets, common in these objects, are a crucial source of feedback energy driving mass outflows into the host galaxy and the intergalactic medium. This paper reports the first direct measurement of powerful mass outflows traced by the forbidden high ionization gas in the low luminosity AGN NGC 1386 at scales of a few parsecs from the central engine. The high angular resolution of the data allows us to directly measure the location, morphology and kinematic of the outflow. This has the form of two symmetrical expanding hot gas shells moving in opposite directions along the line of sight. The co-spatiality of the gas shells with radio emission seen at the same parsec scales and with X-rays indicates that this is a shock-driven outflow presumably induced by an incipient corejet. With a minimum number of assumptions, we derive a mass outflow rate of 11 M ⊙ yr −1 , comparable to those of powerful AGN. The result has strong implications in the global accounting of feedback mass and energy driven by a low-luminosity AGN into the medium and the corresponding galaxy evolution.

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“…The [SiVI] line has a high ionisation potential (167 eV) and it is associated with Seyfert activity where the gas is ionised outside the broad line region of the AGN (Bedregal et al 2009). The [SiVI] emission is usually rather compact, concentrated around the unresolved nucleus and extending up to a few tens or a few hundred parsecs in some Seyferts (Prieto et al 2005;Rodríguez-Ardila et al 2006). While in galaxies like IRASF 12115-4656 and IRAS 23128-5919 the emission is unresolved (i.e.…”

Section: Coronal Line Emissionmentioning

confidence: 99%

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

López

Colina

Arribas

et al. 2012

A&A

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We present an atlas of a sample of local (z < 0.1) LIRGs (10) and ULIRGs (7) covering the luminosity range log(L IR /L ) = 11.1−12.4. The atlas is based on near-infrared H (1.45−1.85 μm) and K-band (1.95−2.45 μm) VLT-SINFONI integral field spectroscopy (IFS). The atlas presents the ionised, partially ionised, and warm molecular gas two-dimensional flux distributions and kinematics over an FoV of ∼3 × 3 kpc (LIRGs) and ∼12 × 12 kpc (ULIRGs) and with average linear resolutions of ∼0.2 kpc and ∼0.9 kpc, respectively. The different phases of the gas show a wide morphological variety with the nucleus as the brightest Brγ source for ∼33% of the LIRGs and ∼71% of the ULIRGs, whereas all the LIRGs and ULIRGs have their maximum H 2 emission in their nuclear regions. In LIRGs, the ionised gas distribution is dominated by the emission from the star-forming rings or giant HII regions in the spiral arms. The Brγ and [FeII] line at 1.644 μm trace the same structures, although the emission peaks at different locations in some of the objects, and the [FeII] seems to be more extended and diffuse. The ULIRG subsample is at larger distances and contains mainly pre-coalescence interacting systems. Although the peaks of the molecular gas emission and the continuum coincide in ∼71% of the ULIRGs, regions with intense Paα (Brγ) emission tracing luminous star-forming regions located at distances of 2−4 kpc away from the nucleus are also detected, usually associated with secondary nuclei or tidal tails. LIRGs have mean observed (i.e. uncorrected for internal extinction) SFR surface densities of about 0.4 to 0.9 M yr −1 kpc −2 over large areas (4−9 kpc 2 ) with peaks of about 2−2.5 M yr −1 kpc −2 in the smaller regions (0.16 kpc 2 ) associated with the nucleus of the galaxy or the brightest Brγ region. ULIRGs do have similar average SFR surface densities for the integrated emitting regions of ∼0.4 M yr −1 kpc −2 in somewhat larger areas (100−200 kpc 2 ) and for the Paα peak (∼2 M yr −1 kpc −2 in 4 kpc 2 ). The observed gas kinematics in LIRGs is primarily due to rotational motions around the centre of the galaxy, although local deviations associated with radial flows and/or regions of higher velocity dispersions are present. The ionised and molecular gas share the same kinematics (velocity field and velocity dispersion) to first order, showing slight differences in the velocity amplitudes (peak-to-peak) in some cases, whereas the average velocity dispersions are compatible within uncertainties. As expected, the kinematics of the ULIRG subsample is more complex, owing to the interacting nature of the objects of the sample.

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Outflows of Very Ionized Gas in the Centers of Seyfert Galaxies: Kinematics and Physical Conditions

Cited by 94 publications

References 33 publications

Narrow Double-Peaked Emission Lines of SDSS J131642.90+175332.5: Signature of a Single or a Binary Agn in a Merger, Jet-Cloud Interaction, or Unusual Narrow-Line Region Geometry

Narrow Double-Peaked Emission Lines of SDSS J131642.90+175332.5: Signature of a Single or a Binary Agn in a Merger, Jet-Cloud Interaction, or Unusual Narrow-Line Region Geometry

Powerful outflows in the central parsecs of the low-luminosity active galactic nucleus NGC 1386

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

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