Infrared imaging and spectroscopy of NGC 7469

Genzel, R.; Weitzel, L.; Tacconi-Garman, L. E.; Blietz, M.; Cameron, M.; Krabbe, Â. C.; Lutz, D.; Sternberg, A.

doi:10.1086/175588

Cited by 165 publications

(202 citation statements)

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“…For NGC 7469 several tracers (e.g. 5 GHz radio continuum, J, H, K imaging, PAHs, CO (2−1)) were found to be located in a circumnuclear ring/spiral arm system (Wilson et al 1991;Mazzarella et al 1994;Miles et al 1994;Genzel et al 1995;Davies et al 2004). A comparison with the starburst and molecular rings in NGC 1614 shows some prominent similarities.…”

Section: Comparing Ngc 1614 With Galaxies With Nuclear Molecular Ringsmentioning

confidence: 91%

The NGC 1614 interacting galaxy

König

Aalto

Müller

et al. 2013

A&A

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Minor mergers frequently occur between giant and gas-rich low-mass galaxies and can provide significant amounts of interstellar matter to refuel star formation and power active galactic nuclei (AGN) in the giant systems. Major starbursts and/or AGN result when fresh gas is transported and compressed in the central regions of the giant galaxy. This is the situation in the starburst minor merger NGC 1614, whose molecular medium we explore at half-arcsecond angular resolution through our observations of 12 CO (2−1) emission using the Submillimeter Array (SMA). We compare our 12 CO (2−1) maps with optical and Paα, Hubble Space Telescope and high angular resolution radio continuum images to study the relationships between dense molecular gas and the NGC 1614 starburst region. The most intense 12 CO emission occurs in a partial ring with ∼230 pc radius around the center of NGC 1614, with an extension to the northwest into the dust lane that contains diffuse molecular gas. We resolve ten giant molecular associations (GMAs) in the ring, which has an integrated molecular mass of ∼8 × 10 8 M . Our interferometric observations filter out a large part of the 12 CO (1−0) emission mapped at shorter spacings, indicating that most of the molecular gas is diffuse and that GMAs only exist near and within the circumnuclear ring. The molecular ring is uneven with most of the mass on the western side, which also contains GMAs extending into a pronounced tidal dust lane. The spatial and kinematic patterns in our data suggest that the northwest extension of the ring is a cosmic umbilical cord that is feeding molecular gas associated with the dust lane and tidal debris into the nuclear ring, which contains the bulk of the starburst activity. The astrophysical process for producing a ring structure for the final resting place of accreted gas in NGC 1614 is not fully understood, but the presence of numerous GMAs suggests an orbit-crowding or resonance phenomenon. There is some evidence that star formation is progressing radially outward within the ring, indicating that a self-triggering mechanism may also affect star formation processes. The net result of this merger therefore very likely increases the central concentration of stellar mass in the NGC 1614 remnant giant system.

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Section: Comparing Ngc 1614 With Galaxies With Nuclear Molecular Ringsmentioning

confidence: 91%

The NGC 1614 interacting galaxy

König

Aalto

Müller

et al. 2013

A&A

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“…Three of the galaxies (NGC 34, IRASF 05189-2524, and UGC 05101) are advanced major mergers. The other three galaxies (NGC 5135,NGC 7130,and NGC 7469) are spirals, although NGC 7130 and NGC 7469 have peculiar morphologies suggesting recent minor interactions (Genzel et al 1995;Bellocchi et al 2012). …”

Section: Samplementioning

confidence: 95%

Warm molecular gas temperature distribution in six local infrared bright Seyfert galaxies

Pereira-Santaella

Spinoglio

Werf

et al. 2014

A&A

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We simultaneously analyze the spectral line energy distributions (SLEDs) of CO and H 2 of six local luminous infrared (IR) Seyfert galaxies. For the CO SLEDs, we used new Herschel/SPIRE FTS data (from J = 4-3 to J = 13-12) and ground-based observations for the lower-J CO transitions. The H 2 SLEDs were constructed using archival mid-IR Spitzer/IRS and near-IR VLT/SINFONI data for the rotational and ro-vibrational H 2 transitions, respectively. In total, the SLEDs contain 26 transitions with upper level energies between 5 and 15 000 K. A single, constant density, model (n H 2 ∼ 10 4.5−6 cm −3 ) with a broken power-law temperature distribution reproduces well both the CO and H 2 SLEDs. The power-law indices are β 1 ∼ 1-3 for warm molecular gas (20 K< T < 100 K) and β 2 ∼ 4-5 for hot molecular gas (T > 100 K). We show that the steeper temperature distribution (higher β) for hot molecular gas can be explained by shocks and photodissociation region (PDR) models; however, the exact β values are not reproduced by PDR or shock models alone and a combination of both is needed. We find that the three major mergers among our targets have shallower temperature distributions for warm molecular gas than the other three spiral galaxies. This can be explained by a higher relative contribution of shock excitation, with respect to PDR excitation, for the warm molecular gas in these mergers. For only one of the mergers, IRASF 05189-2524, the shallower H 2 temperature distribution differs from that of the spiral galaxies. The presence of a bright active galactic nucleus in this source might explain the warmer molecular gas observed.

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“…The nuclear infrared 3-4 µm flux of NGC 7469 is one of the highest among observed Seyfert 1 galaxies with no detectable 3.3 µm PAH emission features (Imanishi & Wada 2004). Recent sensitive ground-based 8-13 µm spectroscopy has shown some signatures of an 11.3 µm PAH emission feature from the NGC 7469 nucleus (Honig et al 2010;Esquej et al 2014), but the estimated nuclear starburst luminosity is only ∼20% of the AGN luminosity (Esquej et al 2014;Genzel et al 1995). Interferometric CO J=2-1 and HCN/HCO + J=4-3 observations of the NGC 7469 nucleus revealed that molecular emission lines at the nuclear position are narrow with a full width at 10% intensity <400 km s −1 (Davies et al 2004;Izumi et al 2015).…”

Section: Targetsmentioning

confidence: 97%

ALMA HCN AND HCO⁺ J = 3 − 2 OBSERVATIONS OF OPTICAL SEYFERT AND LUMINOUS INFRARED GALAXIES: CONFIRMATION OF ELEVATED HCN-TO-HCO⁺ FLUX RATIOS IN AGNS

2016

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We present the results of our ALMA observations of three AGN-dominated nuclei in optical Seyfert 1 galaxies (NGC 7469, I Zw 1, and IC 4329 A) and eleven luminous infrared galaxies (LIRGs) with various levels of infrared estimated energetic contributions by AGNs at the HCN and HCO + J=3-2 emission lines. The HCN and HCO + J=3-2 emission lines are clearly detected at the main nuclei of all sources, except for IC 4329 A. The vibrationally excited (v 2 =1f) HCN J=3-2 and HCO + J=3-2 emission lines are simultaneously covered, and HCN v 2 =1f J=3-2 emission line signatures are seen in the main nuclei of two LIRGs, IRAS 12112+0305 and IRAS 22491−1808, neither of which show clear buried AGN signatures in the infrared. If the vibrational excitation is dominated by infrared radiative pumping, through the absorption of infrared 14 µm photons, primarily originating from AGN-heated hot dust emission, then these two LIRGs may contain infrared-elusive, but (sub)millimeter-detectable, extremely deeply buried AGNs. These vibrationally excited emission lines are not detected in the three AGN-dominated optical Seyfert 1 nuclei. However, the observed HCN v 2 =1f to v=0 flux ratios in these optical Seyferts are still consistent with the intrinsic flux ratios in LIRGs with detectable HCN v 2 =1f emission lines. The observed HCN-to-HCO + J=3-2 flux ratios tend to be higher in galactic nuclei with luminous AGN signatures compared with starburst-dominated regions, as previously seen at J=1-0 and J=4-3.

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Infrared imaging and spectroscopy of NGC 7469

Cited by 165 publications

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The NGC 1614 interacting galaxy

The NGC 1614 interacting galaxy

Warm molecular gas temperature distribution in six local infrared bright Seyfert galaxies

ALMA HCN AND HCO⁺ J = 3 − 2 OBSERVATIONS OF OPTICAL SEYFERT AND LUMINOUS INFRARED GALAXIES: CONFIRMATION OF ELEVATED HCN-TO-HCO⁺ FLUX RATIOS IN AGNS

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Infrared imaging and spectroscopy of NGC 7469

Cited by 165 publications

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The NGC 1614 interacting galaxy

The NGC 1614 interacting galaxy

Warm molecular gas temperature distribution in six local infrared bright Seyfert galaxies

ALMA HCN AND HCO+ J = 3 − 2 OBSERVATIONS OF OPTICAL SEYFERT AND LUMINOUS INFRARED GALAXIES: CONFIRMATION OF ELEVATED HCN-TO-HCO+ FLUX RATIOS IN AGNS

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ALMA HCN AND HCO⁺ J = 3 − 2 OBSERVATIONS OF OPTICAL SEYFERT AND LUMINOUS INFRARED GALAXIES: CONFIRMATION OF ELEVATED HCN-TO-HCO⁺ FLUX RATIOS IN AGNS