The NGC 1614 interacting galaxy

König, S.; Aalto, S.; Müller, S.; Beswick, R.; Gallagher, John S.

doi:10.1051/0004-6361/201220453

Cited by 28 publications

(71 citation statements)

References 63 publications

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“…König et al (2016) The red cross indicates the nucleus thatis detected in Pa α and radio continuum emission (Olsson et al 2010;Herrero-Illana et al 2014). The red circle indicates the approximate outer edge of the starburst ring (König et al 2013;Herrero-Illana et al 2014;Xu et al 2015;S16a). observation has a quasar as the flux calibrator, so we estimate the absolute systematic error on the flux calibration for our Band3 data by using the ALMA Calibrator Source Catalog.…”

Section: Band3 Data: Atacama Compact Array and 12m Arraymentioning

confidence: 99%

“…The CO(1-0) outflow shows an extended blueshifted . The white circle indicates the approximate outer edge of the starburst ring (König et al 2013;Herrero-Illana et al 2014;Xu et al 2015;Saito 2016a). …”

Section: Aca+12m Combined Co(1-0) Datamentioning

confidence: 99%

“…The global CO spectral line energy distribution (SLED) is characterized by a steep decline toward higher-J transitions (Rosenberg et al 2015). High-resolution (∼0 25∼83 pc) ALMA Band9 observations revealed that the CO(6-5) distribution coincides with a starburst ring (r<350 pc) detected in Pa α ( Figure 1(c); Alonso-Herrero et al 2001) and 8.4GHz radio continuum emission (Xu et al 2015), while the CO(2-1) and CO(3-2) emission are more extended (Wilson et al 2008;König et al 2013;Sliwa et al 2014). Recent high-sensitivity CO(2-1) observations revealed the presence of a high-velocity wing, which might be associated with a nuclear molecular outflow (García-Burillo et al 2015), whereas deep CO(1-0) imaging found that extended molecular gas components associated with the southern tidal tail and a dust lane (König et al 2016).…”

Section: Introductionmentioning

confidence: 96%

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Spatially Resolved CO SLED of the Luminous Merger Remnant NGC 1614 with ALMA

Saito

Iono

et al. 2017

ApJ

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We present high-resolution (1 0) Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO(1-0) and CO(2-1) rotational transitions toward the nearby IR-luminous merger NGC1614 supplemented with ALMA archival data of CO(3-2)and CO(6-5) transitions. The CO(6-5) emission arises from the starburst ring (central 590 pc in radius), while the lower-J CO lines are distributed over the outer disk (∼3.3 kpc in radius). Radiative transfer and photon-dominated region (PDR) modeling reveals that the starburst ring has a single warmer gas component with more a intense far-ultraviolet radiation field (ñ 10 A two-phase molecular interstellar medium with a warm and cold (>70 and ∼19 K) component is also an applicable model for the starburst ring. A possible source for heating the warm gas component is mechanical heating due to stellar feedback rather than PDR. Furthermore, we find evidence for non-circular motions along the north-south optical bar in the lower-J CO images, suggesting a cold gas inflow. We suggest that star formation in the starburst ring is sustained by the bardriven cold gas inflowand that starburst activities radiatively and mechanically power the CO excitation. The absence of a bright active galactic nucleus can be explained by a scenario wherecold gas accumulating on the starburst ring is exhausted as the fuel for star formationor is launched as an outflow before being able to feed to the nucleus.

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Section: Band3 Data: Atacama Compact Array and 12m Arraymentioning

confidence: 99%

Section: Aca+12m Combined Co(1-0) Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

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Spatially Resolved CO SLED of the Luminous Merger Remnant NGC 1614 with ALMA

Saito

Iono

et al. 2017

ApJ

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“…The molecular gas in this source, imaged by the OVRO, SMA, CARMA, and ALMA interferometers, is distributed in a nuclear disk and a fainter extension (Wilson et al 2008;Olsson et al 2010;König et al 2013;Sliwa et al 2014;Xu et al 2015;Usero et al, in prep.). The recent 0.…”

Section: Ngc 1614mentioning

confidence: 99%

High-resolution imaging of the molecular outflows in two mergers: IRAS 17208-0014 and NGC 1614

García‐Burillo

Combes

Usero

et al. 2015

A&A

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107

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Context. Galaxy evolution scenarios predict that the feedback of star formation and nuclear activity (AGN) can drive the transformation of gas-rich spiral mergers into (ultra) luminous infrared galaxies and, eventually, lead to the build-up of QSO/elliptical hosts. Aims. We study the role that star formation and AGN feedback have in launching and maintaining the molecular outflows in two starburst-dominated advanced mergers, NGC 1614 (D L = 66 Mpc) and IRAS 17208-0014 (D L = 181 Mpc), by analyzing the distribution and kinematics of their molecular gas reservoirs. Both galaxies present evidence of outflows in other phases of their ISM. Methods. We used the Plateau de Bure interferometer (PdBI) to image the CO(1-0) and CO(2-1) line emissions in NGC 1614 and IRAS 17208-0014, respectively, with high spatial resolution (0. 5-1. 2). The velocity fields of the gas were analyzed and modeled to find the evidence of molecular outflows in these sources and characterize the mass, momentum, and energy of these components. Results. While most (≥95%) of the CO emission stems from spatially resolved (∼2−3 kpc-diameter) rotating disks, we also detect in both mergers the emission from high-velocity line wings that extend up to ±500-700 km s −1 , well beyond the estimated virial range associated with rotation and turbulence. The kinematic major axis of the line-wing emission is tilted by ∼90 • in NGC 1614 and by ∼180 • in IRAS 17208-0014 relative to the major axes of their respective rotating disks. These results can be explained by the existence of non-coplanar molecular outflows in both systems: the outflow axis is nearly perpendicular to the rotating disk in NGC 1614, but it is tilted relative to the angular momentum axis of the rotating disk in IRAS 17208-0014. Conclusions. In stark contrast to NGC 1614, where star formation alone can drive its molecular outflow, the mass, energy, and momentum budget requirements of the molecular outflow in IRAS 17208-0014 can be best accounted for by the existence of a so far undetected (hidden) AGN of L AGN ∼ 7 × 10 11 L . The geometry of the molecular outflow in IRAS 17208-0014 suggests that the outflow is launched by a non-coplanar disk that may be associated with a buried AGN in the western nucleus.

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“…The central kpc of NGC 1614 contains a compact nucleus (45-80 pc), which dominates the near-IR continuum emission, and a bright circumnuclear SF ring (diameter∼ 600 pc), which is predominant in Paα (Alonso-Herrero et al 2001) and other SF indicators like the polycyclic aromatic hydrocarbon (PAH) emission (Díaz-Santos et al 2008;Väisänen et al 2012), cold molecular gas (König et al 2013;Sliwa et al 2014;Xu et al 2015), and radio continuum (Olsson et al 2010;Herrero-Illana et al 2014). In addition, García-Burillo et al (2015) found a massive cold molecular gas outflow (3×10 7 M ;Ṁout ∼40 M yr −1 ) which can be powered by the SF in the ring.…”

Section: Introductionmentioning

confidence: 99%

Sub-arcsec mid-IR observations of NGC 1614: Nuclear star formation or an intrinsically X-ray weak AGN?

Pereira-Santaella¹,

Colina²,

Alonso‐Herrero³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present new mid-infrared N -band spectroscopy and Q-band photometry of the local luminous infrared galaxy NGC 1614, one of the most extreme nearby starbursts. We analyze the mid-IR properties of the nucleus (central 150 pc) and four regions of the bright circumnuclear (diameter∼ 600 pc) star-forming (SF) ring of this object. The nucleus differs from the circumnuclear SF ring by having a strong 8-12 µm continuum (low 11.3 µm PAH equivalent width). These characteristics, together with the nuclear X-ray and sub-mm properties, can be explained by an X-ray weak active galactic nucleus (AGN), or by peculiar SF with a short molecular gas depletion time and producing an enhanced radiation field density. In either case, the nuclear luminosity (L IR <6×10 43 erg s −1 ) is only <5 % of the total bolometric luminosity of NGC 1614. So this possible AGN does not dominate the energy output in this object. We also compare three star-formation rate (SFR) tracers (Paα, 11.3 µm PAH, and 24 µm emissions) at 150 pc scales in the circumnuclear ring. In general, we find that the SFR is underestimated (overestimated) by a factor of 2-4 (2-3) using the 11.3 µm PAH (24 µm) emission with respect to the extinction corrected Paα SFR. The former can be explained because we do not include diffuse PAH emission in our measurements, while the latter might indicate that the dust temperature is particularly warmer in the central regions of NGC 1614.

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The NGC 1614 interacting galaxy

Cited by 28 publications

References 63 publications

Spatially Resolved CO SLED of the Luminous Merger Remnant NGC 1614 with ALMA

Spatially Resolved CO SLED of the Luminous Merger Remnant NGC 1614 with ALMA

High-resolution imaging of the molecular outflows in two mergers: IRAS 17208-0014 and NGC 1614

Sub-arcsec mid-IR observations of NGC 1614: Nuclear star formation or an intrinsically X-ray weak AGN?

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