Near-infrared spectroscopy of nearby Seyfert galaxies - I. First results

Reunanen, J.; Kotilainen, Jari; Prieto, M. A.

doi:10.1046/j.1365-8711.2002.05181.x

Cited by 101 publications

(164 citation statements)

References 50 publications

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“…This is consistent with the near-infrared rotational-vibrational spectra taken across the nucleus by Reunanen et al (2002).…”

supporting

confidence: 89%

“…There is also gas inflow inside the ring possibly fueling the central supermassive black hole (Prieto et al 2005;Fathi et al 2006;Davies et al 2009), triggering the formation of a compact star cluster seen near the nucleus. The star-forming ring and the nucleus of NGC 1097 are prominent in CO 1-0 (Kohno et al 2003) as well as rovibrational H 2 and hydrogen recombination lines (Reunanen et al 2002;Kotilainen et al 2000). Tracers of denser molecular gas such as CO 2-1 and HCN (Kohno et al 2003) peak at the nucleus and where the dust lanes and the ring intersect.…”

Section: Introductionmentioning

confidence: 99%

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A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITHHERSCHEL-PACS ANDSPITZER-IRS

Beirão

Armus

Hélou

et al. 2012

ApJ

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NGC 1097 is a nearby Seyfert 1 galaxy with a bright circumnuclear starburst ring, a strong large-scale bar, and an active nucleus. We present a detailed study of the spatial variation of the far-infrared (FIR) [C ii]158 μm and [O i]63 μm lines and mid-infrared H 2 emission lines as tracers of gas cooling, and of the polycyclic aromatic hydrocarbon (PAH) bands as tracers of the photoelectric heating, using Herschel-PACS and Spitzer-IRS infrared spectral maps. We focus on the nucleus and the ring, and two star-forming regions (Enuc N and Enuc S). We estimated a photoelectric gas heating efficiency ([C ii]158 μm+[O i]63 μm)/PAH in the ring about 50% lower than in Enuc N and S. The average 11.3/7.7 μm PAH ratio is also lower in the ring, which may suggest a larger fraction of ionized PAHs, but no clear correlation with [C ii]158 μm/PAH(5.5-14 μm) is found. PAHs in the ring are responsible for a factor of two more [C ii]158 μm and [O i]63 μm emission per unit mass than PAHs in the Enuc S. spectral energy distribution (SED) modeling indicates that at most 25% of the FIR power in the ring and Enuc S can come from high-intensity photodissociation regions (PDRs), in which case G 0 ∼ 10 2.3 and n H ∼ 10 3.5 cm −3 in the ring. For these values of G 0 and n H , PDR models cannot reproduce the observed H 2 emission. Much of the H 2 emission in the starburst ring could come from warm regions in the diffuse interstellar medium that are heated by turbulent dissipation or shocks.

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“…This is consistent with the near-infrared rotational-vibrational spectra taken across the nucleus by Reunanen et al (2002).…”

supporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITHHERSCHEL-PACS ANDSPITZER-IRS

Beirão

Armus

Hélou

et al. 2012

ApJ

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“…taken from Reunanen et al (2002) and assuming T = 2000 K, a transition probability A S (1) = 3.47 × 10 −7 s −1 (Turner et al 1977), and the population fraction in the ν = 1, J = 3 level f ν=1,J=3 = 0.0122 (Scoville et al 1982). I 1−0S (1) is the flux of H 2 2.121 µm corrected for intrinsic E(B − V).…”

Section: Molecular and Absorption Linesmentioning

confidence: 99%

Optical and NIR spectroscopy of Mrk 1210: constraints and physical conditions of the active nucleus

Mazzalay

Rodríguez-Ardila

2006

A&A

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Aims. Mrk 1210 is an outstanding Seyfert 2 galaxy because it displays signatures of recent circumnuclear star formation and a high level of X-ray activity, in addition to the classical spectral characteristics typical of an AGN. Here we investigate the extinction affecting the nuclear and extended emitting gas, the kinematics of the narrow-line region, and the physical properties and conditions of that gas. Methods. Near-infrared and optical spectra of the nuclear and extended emission region of Mrk 1210 are presented, covering the interval 0.4−2.4 µm. Emission and absorption lines were used to infer, respectively, the geometrical extension of the ionized gas and the contribution of the underlying stellar population to the observed integrated continuum. The emission line profiles were employed to study the kinematics in the NLR. The reddening and physical condition of the gas were investigated by means of flux ratios among permitted and forbidden lines. 12 CO(6−3) 1.618 µm overtone bandhead helped to estimate the contribution of the stellar population to the continuum. It was found that 83 ± 8% of the H-band continuum has a stellar origin. It improves previous estimates, which claimed that at least 50% of the observed continuum was attributed to the AGN. Analysis of the emission line profiles, both allowed and forbidden, shows a narrower (FWHM ∼ 500 km s −1 ) line on top of a broad (FWHM > 1000 km s −1 ) blue-shifted component. This seems to be associated to a nuclear outflow. This hypothesis is supported by 6 cm VLBI observations, which show a radio ejecta extending up to ∼30 pc from the nucleus. This result does not require the presence of the hidden BLR claimed to be present in previous NIR observations of this object. Internal extinction, calculated by means of several indicators including [Fe ii] flux ratios not previously used before in AGNs, reveals a dusty AGN, while the extended regions are barely affected by dust, if at all. The density and temperature are calculated for the NLR using optical and NIR lines as diagnostic ratios. The results show electronic temperatures from 10 000 K up to 40 000 K and densities between 10 3 −10 5 cm −3 . The higher temperatures show that shocks, most probably related to the radio outflow, must contribute to the line emission.

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“…Near-infrared spectroscopy (Reunanen et al 2002;Kotilainen et al 2000) reveals emission from both ro-vibrational H 2 and H-recombination lines at the nucleus, the star-forming ring, and the region in between. Optical long-slit spectroscopy (Storchi-Bergmann et al 1996) shows strong ionized gas emission from both the nucleus and the ring, along with faint line emission from the inner region, exhibiting a LINER-type spectrum.…”

Section: Introductionmentioning

confidence: 99%

Far-infrared line imaging of the starburst ring in NGC 1097 with theHerschel/PACS spectrometer

Beirão¹,

Armus²,

Appleton

et al. 2010

A&A

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NGC 1097 is a nearby SBb galaxy with a Seyfert nucleus and a bright starburst ring. We study the physical properties of the interstellar medium (ISM) in the ring using spatially resolved far-infrared spectral maps of the circumnuclear starburst ring of NGC 1097, obtained with the PACS spectrometer on board the Herschel Space Observatory. In particular, we map the important ISM cooling and diagnostic emission lines of [

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Near-infrared spectroscopy of nearby Seyfert galaxies - I. First results

Cited by 101 publications

References 50 publications

A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITHHERSCHEL-PACS ANDSPITZER-IRS

A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITHHERSCHEL-PACS ANDSPITZER-IRS

Optical and NIR spectroscopy of Mrk 1210: constraints and physical conditions of the active nucleus

Far-infrared line imaging of the starburst ring in NGC 1097 with theHerschel/PACS spectrometer

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