NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

Cazzoli, S.; Paz, A. Gil de; Márquez, I.; Masegosa, J.; Iglesias, Jorge Mario Ortega; Gallego, J.; Carrasco, E.; Cedazo, R.; García-Vargas, M. L.; Castillo-Morales, Á.; Pascual, S.; Cardiel, N.; Pérez-Calpena, A.; Gómez-Álvarez, P.; Martínez-Delgado, I.; Hermosa-Muñoz, L.

doi:10.1093/mnras/staa409

Cited by 22 publications

(23 citation statements)

References 99 publications

(140 reference statements)

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“…In ESO 320-G030, a nuclear disk with projected radius of ≈ 40 pc attains these conditions, though still with moderately warm dust (T dust ≈ 55 K). The disk is distorted, elongated in the direction of the bar, and highly turbulent (∆V/V rot ≈ 1); it is thus expected to be geometrically thick (e.g., Cazzoli et al 2020).…”

Section: Discussionmentioning

confidence: 99%

A proto-pseudobulge in ESO 320-G030 fed by a massive molecular inflow driven by a nuclear bar

González-Alfonso

Pereira-Santaella

Fischer

et al. 2021

A&A

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Galaxies with nuclear bars are believed to efficiently drive gas inward, generating a nuclear starburst and possibly an active galactic nucleus (AGN). We confirm this scenario for the isolated, double-barred, luminous infrared galaxy ESO 320-G030 based on an analysis of Herschel and ALMA spectroscopic observations. Herschel/PACS and SPIRE observations of ESO 320-G030 show absorption or emission in 18 lines of H 2 O, which we combine with the ALMA H 2 O 4 23 − 3 30 448 GHz line (E upper ∼ 400 K) and continuum images to study the physical properties of the nuclear region. Radiative transfer models indicate that three nuclear components are required to account for the multi-transition H 2 O and continuum data. An envelope, with radius R ∼ 130 − 150 pc, dust temperature T dust ≈ 50 K, and N H2 ∼ 2 × 10 23 cm −2 , surrounds a nuclear disk with R ∼ 40 pc that is optically thick in the far-infrared (τ 100 µm ∼ 1.5 − 3, N H2 ∼ 2 × 10 24 cm −2). In addition, an extremely compact (R ∼ 12 pc), warm (≈ 100 K), and buried (τ 100 µm > 5, N H2 5 × 10 24 cm −2) core component is required to account for the very high-lying H 2 O absorption lines. The three nuclear components account for 70% of the galaxy luminosity (SFR ∼ 16−18 M yr −1). The nucleus is fed by a molecular inflow observed in CO 2-1 with ALMA, which is associated with the nuclear bar. With decreasing radius (r = 450 − 225 pc), the mass inflow rate increases up tȯ M inf ∼ 20 M yr −1 , which is similar to the nuclear star formation rate (SFR), indicating that the starburst is sustained by the inflow. At lower r, ∼ 100 − 150 pc, the inflow is best probed by the far-infrared OH ground-state doublets, with an estimatedṀ inf ∼ 30 M yr −1. The inferred short timescale of ∼ 20 Myr for nuclear gas replenishment indicates quick secular evolution, and indicates that we are witnessing an intermediate stage (< 100 Myr) proto-pseudobulge fed by a massive inflow that is driven by a strong nuclear bar. We also apply the H 2 O model to the Herschel far-infrared spectroscopic observations of H 18 2

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Section: Discussionmentioning

confidence: 99%

A proto-pseudobulge in ESO 320-G030 fed by a massive molecular inflow driven by a nuclear bar

González-Alfonso

Pereira-Santaella

Fischer

et al. 2021

A&A

Self Cite

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“…Rupke & Veilleux 2013;Cazzoli et al 2014Cazzoli et al , 2016Pereira-Santaella et al 2016Fluetsch et al 2021) and luminous AGNs (e.g. quasars or Seyferts galaxies; Feruglio et al 2010;Müller-Sánchez et al 2011;Fiore et al 2017;Brusa et al 2018;Venturi et al 2018;Cazzoli et al 2020). These works demonstrated the power of the 3D IFS in studies of this kind.…”

Section: Introductionmentioning

confidence: 76%

Unexplored outflows in nearby low luminosity AGNs: the case of NGC 1052

Cazzoli,

Muñoz,

Márquez

et al. 2022

Preprint

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Context. Multi-phase outflows play a central role in galaxy evolution shaping the properties of galaxies. Understanding outflows and their effects in low luminosity AGNs, such as LINERs, is essential. Indeed these latter bridge the gap between normal and active galaxies, being the most numerous AGN population in the local Universe. Aims. Our goal is to analyse the kinematics and ionisation mechanisms of the multi-phase gas of NGC 1052, the prototypical LINER, in order to detect and map ionised and neutral phases of the putative outflow. Methods. We obtained Very Large Telescope MUSE and Gran Telescopio Canarias MEGARA optical integral field spectroscopy data for NGC 1052. Besides stellar kinematics maps, by modelling spectral lines with multiple Gaussian components, we obtained flux, kinematic, and excitation maps of both ionised and neutral gas.Results. The stars are distributed in a dynamically hot disc (V/σ ∼ 1.2), with a centrally peaked velocity dispersion map (σ c = 201 ± 10 km s −1 ) and large observed velocity amplitudes (∆V = 167 ± 19 km s −1 ). The ionised gas, probed by the primary component is detected up to ∼ 30 (∼ 3.3 kpc) mostly in the polar direction with blue and red velocities (|V| < 250 km s −1 ). The velocity dispersion map shows a notable enhancement (σ > 90 km s −1 ) crossing the galaxy along the major axis of rotation in the central 10 .The secondary component has a bipolar morphology, velocity dispersion larger than 150 km s −1 and velocities up to 660 km s −1 . A third component is detected with MUSE (barely with MEGARA) but not spatially resolved. The BLR-component (used to model the broad Hα emission only) has a full width half maximum of 2427 ± 332 and 2350 ± 470 km s −1 for MUSE and MEGARA data, respectively. The maps of the NaD absorption indicate optically thick neutral gas with complex kinematics. The velocity field is consistent with a slow rotating disc (∆V = 77 ± 12 km s −1 ) but the velocity dispersion map is off-centred without any counterpart in the (centrally peaked) flux map. Conclusions. We found evidence of an ionised gas outflow (secondary component) with mass of 1.6 ± 0.6 × 10 5 M , and mass rate of 0.4 ± 0.2 M yr −1 . The outflow is propagating in a cocoon of gas with enhanced turbulence and might be triggering the onset of kpc-scale buoyant bubbles (polar emission), both probed by the primary component. Taking into account the energy and kinetic power of the outflow (1.3 ± 0.9 × 10 53 erg and 8.8 ± 3.5 × 10 40 erg s −1 , respectively) as well as its alignment with both the jet and the cocoon, and that the gas is collisionally ionised (due to gas compression), we consider that the most likely power source of the outflow is the jet, although some contribution from the AGN is possible. The hints of the presence of a neutral gas outflow are weak.

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“…Language 3 (IDL) environment for the [N ii] λ6584 Å and [S ii] emission lines separately (e.g., Cazzoli et al 2020). We found that constraints to the line widths of FWHM < 1 Å (≈ 45 km s −1 at the rest-frame wavelengths of these lines) and absolute radial velocities with respect to the systemic velocity 4 (|v r |) between 130 and 250 km s −1 produced optimal results.…”

Section: Data Analysis: Mapping the Jetmentioning

confidence: 85%

Tomography of the unique on-going jet in the planetary nebula NGC 2392

Guerrero,

Cazzoli,

Rechy-Garcia

et al. 2021

Preprint

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Jets (fast collimated outflows) are claimed to be the main shaping agent of the most asymmetric planetary nebula (PNe) as they impinge on the circumstellar material at late stages of the asymptotic giant branch (AGB) phase. The first jet detected in a PN was that of NGC 2392, yet there is no available image because its low surface brightness contrast with the bright nebular emission. Here we take advantage from the tomographic capabilities of GTC MEGARA high-dispersion integral field spectroscopic observations of the jet in NGC 2392 to gain unprecedented details of its morphology and kinematics. The jet of NGC 2392 is found to emanate from the central star, break through the walls of the inner shell of this iconic PN and extend outside the nebula's outermost regions with an Sshaped morphology suggestive of precession. At odds with the fossil jets found in mature PNe, the jet in NGC 2392 is currently being collimated and launched. The high nebular excitation of NGC 2392, which implies a He ++ /He ionization fraction too high to be attributed to the known effective temperature of the star, has been proposed in the past to hint at the presence of a hot white dwarf companion. In conjunction with the hard X-ray emission from the central star, the present-day jet collimation would support the presence of such a double-degenerate system where one component undergoes accretion from a remnant circumbinary disk of the common envelope phase.

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NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

Cited by 22 publications

References 99 publications

A proto-pseudobulge in ESO 320-G030 fed by a massive molecular inflow driven by a nuclear bar

A proto-pseudobulge in ESO 320-G030 fed by a massive molecular inflow driven by a nuclear bar

Unexplored outflows in nearby low luminosity AGNs: the case of NGC 1052

Tomography of the unique on-going jet in the planetary nebula NGC 2392

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