ALMA multiline observations toward the central region of NGC 613

Miyamoto, Yusuke; Nakai, Naomasa; Seta, Masumichi; Salak, Dragan; Nagai, Makoto; Kaneko, Hiroyuki

doi:10.1093/pasj/psx076

Cited by 16 publications

(39 citation statements)

References 65 publications

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“…Besides that, the molecular gas kinematics, observed with the Atacama Large Millimeter/Submillimeter Array (ALMA), indicates a rotation of gas in the ring. The portion of the ring to the west presents redshifted emission and that to the east, presents blueshifted emission (Miyamoto et al 2017(Miyamoto et al , 2018Audibert et al 2019;Combes et al 2019). Such a kinematic behaviour is compatible with the one observed from the images of Br γ by Böker et al (2008).…”

Section: Introductionsupporting

confidence: 87%

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The nuclear region of NGC 613 -- II. Kinematics and stellar archaeology

da Silva,

Menezes,

Steiner

2020

Preprint

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In this work, we continue the study of the central region of NGC 613 by da Silva et al. (2020), by analysing the stellar and gas kinematics and the stellar archaeology in optical and near-infrared data cubes. The high spatial resolution of the Gemini Multi-Object Spectrograph (GMOS) data cube allowed the detection, using spectral synthesis methods, of an inner circumnuclear ring, with a radius of ∼ 1 arcsec, composed of ∼ 10 9 -yr stellar populations. Such a ring is located between the nucleus and the circumnuclear ring composed by H ii regions detected in previous works. Besides that, there is a stellar rotation around the nucleus and the rings follow the same direction of rotation with different velocities. The intensity-weighted average stellar velocity dispersion at the centre is 92 ± 3 km s −1 . Three distinct gas outflow components were detected. The direction of the outflow observed with the H α emission line is compatible with the direction of the previously observed radio jet. The direction of one of the outflows detected in the [O iii]λ5007 emission coincides with the axis of the ionization cone. There is no difference regarding the stellar populations and the stellar kinematics along the double stellar emission, probably separated by a dust lane as mentioned in Paper I, confirming that they are part of the same structure.

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Section: Introductionsupporting

confidence: 87%

“…On the other hand, Mazzuca et al (2008) did not find any age gradient between the H ii regions, whose stars are older than 10 Myr, and they affirm that those regions where formed by gravitation instabilities in the Lindblad resonance region. The star-forming rate seems to be higher to the east portion of the ring (Miyamoto et al 2017).…”

Section: Introductionmentioning

confidence: 87%

The nuclear region of NGC 613 -- II. Kinematics and stellar archaeology

da Silva,

Menezes,

Steiner

2020

Preprint

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“…At 4.86 and 14.94 GHz, three blobs were detected in the central kpc, forming a linear structure whose PA is 12 • (Hummel & Jorsater 1992). Miyamoto et al (2017) also detected an elongated structure in 95 GHz with PA= 20 • ± 8 • . All these data show the presence of a nuclear radio jet.…”

Section: Introductionmentioning

confidence: 83%

“…NGC 613 has a rich nuclear region. The presence of an AGN (Veron-Cetty & Veron 1986), of a star-forming ring ( Hummel & Jorsater 1992, Böker et al 2007, 2008, Miyamoto et al 2017, of a radio jet (Hummel et al 1987, Hummel & Jorsater 1992, Miyamoto et al 2017, of a nuclear spiral (Audibert et al 2019), of an outflow (detected from the study of the [O iii]λ5007 emission by Hummel et al 1987) and of shock waves (Davies et al 2017) has already been reported in the literature, making this environment interesting to be studied and challenging to be understood.…”

Section: Discussionmentioning

confidence: 99%

“…According to Böker et al (2007Böker et al ( , 2008 and Falcón-Barroso et al (2008, the circumnuclear ring of NGC 613 is formed by seven H ii regions. This ring can also be observed in radio wavelengths (Hummel & Jorsater 1992;Miyamoto et al 2017Miyamoto et al , 2018Audibert et al 2019) and, if its structure is circular, the inclination should be 55 • ± 5 • (Hummel & Jorsater 1992). Combes et al (2019) and Audibert et al (2019) found that this ring is connected to the bar in two points, at NW and SE, as Böker et al (2008) previously estimated by using the Hubble Space Telescope (HST) images, and that the ring is indeed clumpy as it is shown in the image of Brγ (Falcón-Barroso et al 2014).…”

Section: Introductionmentioning

confidence: 99%

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The nuclear region of NGC 613 – I. Multiwavelength analysis

Silva

Menezes

Steiner

2020

Monthly Notices of the Royal Astronomical Society

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In this paper, we report a detailed study with a variety of data from optical, nearinfrared, X-ray, and radio telescopes of the nuclear region of the galaxy NGC 613 with the aim of understanding its complexity. We detected an extended stellar emission in the nucleus that, at first, appears to be, in the optical band, two stellar nuclei separated by a stream of dust. The active galactic nucleus (AGN) is identified as a variable point-like source between these two stellar components. There is a central hard X-ray emission and an extended soft X-ray emission that closely coincides with the ionization cone, as seen in the [O iii]λ5007 emission. The centroid of the [O i]λ6300 emission does not coincide with the AGN, being shifted by 0.24 arcsec towards the ionization cone; this shift is probably caused by a combination of differential dust extinction together with emission and reflection in the ionization cone. The optical spectra extracted from the central region are typical of low-ionization nuclear emission-line regions. We also identify 10 H ii regions, eight of them in a star forming ring that is visible in Brγ, [Fe ii]λ16436 and molecular CO(3-2) images observed in previous studies. Such a ring also presents weak hard X-ray emission, probably associated with supernova remnants, not detected in other studies. The position of the AGN coincides with the centre of a nuclear spiral (detected in previous works) that brings gas and dust from the bar to the nucleus, causing the high extinction in this area.

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ALMA observations of molecular tori around massive black holes

Combes

García‐Burillo

Audibert

et al. 2019

A&A

208

243

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We report Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO(3-2) emission in a sample of seven Seyfert/LINER galaxies at the unprecedented spatial resolution of 0 . 1 = 4-9 pc. Our aim is to explore the close environment of active galactic nuclei (AGN), and the dynamical structures leading to their fueling, through the morphology and kinematics of the gas inside the sphere of influence of the black hole. The selected galaxies host low-luminosity AGN and have a wide range of activity types (Seyferts 1 to 2, LINERs), and barred or ringed morphologies. The observed maps reveal the existence of circumnuclear disk structures, defined by their morphology and decoupled kinematics, in most of the sample. We call these structures molecular tori, even though they often appear as disks without holes in the center. They have varying orientations along the line of sight, unaligned with the host galaxy orientation. The radius of the tori ranges from 6 to 27 pc, and their mass from 0.7 × 10 7 to 3.9 × 10 7 M . The most edge-on orientations of the torus correspond to obscured Seyferts. In only one case (NGC 1365), the AGN is centered on the central gas hole of the torus. On a larger scale, the gas is always piled up in a few resonant rings 100 pc in scale that play the role of a reservoir to fuel the nucleus. In some cases, a trailing spiral is observed inside the ring, providing evidence for feeding processes. More frequently, the torus and the AGN are slightly off-centered with respect to the bar-resonant ring position, implying that the black hole is wandering by a few 10 pc amplitude around the center of mass of the galaxy. Our spatial resolution allows us to measure gas velocities inside the sphere of influence of the central black holes. By fitting the observations with different simulated cubes, varying the torus inclination and the black hole mass, it is possible to estimate the mass of the central black hole, which is in general difficult for such late-type galaxies, with only a pseudo-bulge. In some cases, AGN feedback is revealed through a molecular outflow, which will be studied in detail in a subsequent article.

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ALMA multiline observations toward the central region of NGC 613

Cited by 16 publications

References 65 publications

The nuclear region of NGC 613 -- II. Kinematics and stellar archaeology

The nuclear region of NGC 613 -- II. Kinematics and stellar archaeology

The nuclear region of NGC 613 – I. Multiwavelength analysis

ALMA observations of molecular tori around massive black holes

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