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Title

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

AuthorsPereira-Santaella, Miguel ; Colina, Luis ; Alonso-Herrero, A. ; Usero, Antonio; Díaz-Santos, T. ; García-Burillo, S.; Alberdi, Antxón ; González-Martín, Omaira ; Herrero-Illana, Rubén ; Imanishi, Masatoshi; Levenson, N.; Pérez-Torres, Miguel A. ; Ramos-Almeida, Cristina
KeywordsGalaxies: starburst
Galaxies: nuclei
Galaxies: individual: NGC 1614
Galaxies: active
Infrared: galaxies
Issue Date2015
PublisherOxford University Press
CitationMonthly Notices of the Royal Astronomical Society 454(4): 3679-3687 (2015)
AbstractWe present new mid-infrared (mid-IR) N-band spectroscopy and Q-band photometry of the local luminous IR galaxy NGC 1614, one of the most extreme nearby starbursts. We analyse 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 (LIR < 6 × 1043 erg s−1) is only <5 per cent 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 (Pa α, 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 Pa α SFR. The former can be explained because we do not include diffuse polycyclic aromatic hydrocarbon (PAH) emission in our measurements, while the latter might indicate that the dust temperature is particularly warmer in the central regions of NGC 1614.
Publisher version (URL)https://doi.org/10.1093/mnras/stv2242
URIhttp://hdl.handle.net/10261/140234
DOI10.1093/mnras/stv2242
Identifiersdoi: 10.1093/mnras/stv2242
issn: 0035-8711
e-issn: 1365-2966
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