Excitation Mechanism of Near‐Infrared [Fe<scp>ii</scp>] Emission in Seyfert and Starburst Galaxies

Mouri, Hideaki; Kawara, Kimiaki; Taniguchi, Yoshiaki

doi:10.1086/308142

Cited by 77 publications

(107 citation statements)

References 84 publications

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“…The [FeII] emission is usually associated with regions where the gas is partially ionised by X-rays or shocks (Mouri et al 2000). Shocks from supernovae cause efficient grain destruction that releases the iron atoms contained in the dust.…”

Section: Emission Lines and Star Formationmentioning

confidence: 99%

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

López

Colina

Arribas

et al. 2012

A&A

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We present an atlas of a sample of local (z < 0.1) LIRGs (10) and ULIRGs (7) covering the luminosity range log(L IR /L ) = 11.1−12.4. The atlas is based on near-infrared H (1.45−1.85 μm) and K-band (1.95−2.45 μm) VLT-SINFONI integral field spectroscopy (IFS). The atlas presents the ionised, partially ionised, and warm molecular gas two-dimensional flux distributions and kinematics over an FoV of ∼3 × 3 kpc (LIRGs) and ∼12 × 12 kpc (ULIRGs) and with average linear resolutions of ∼0.2 kpc and ∼0.9 kpc, respectively. The different phases of the gas show a wide morphological variety with the nucleus as the brightest Brγ source for ∼33% of the LIRGs and ∼71% of the ULIRGs, whereas all the LIRGs and ULIRGs have their maximum H 2 emission in their nuclear regions. In LIRGs, the ionised gas distribution is dominated by the emission from the star-forming rings or giant HII regions in the spiral arms. The Brγ and [FeII] line at 1.644 μm trace the same structures, although the emission peaks at different locations in some of the objects, and the [FeII] seems to be more extended and diffuse. The ULIRG subsample is at larger distances and contains mainly pre-coalescence interacting systems. Although the peaks of the molecular gas emission and the continuum coincide in ∼71% of the ULIRGs, regions with intense Paα (Brγ) emission tracing luminous star-forming regions located at distances of 2−4 kpc away from the nucleus are also detected, usually associated with secondary nuclei or tidal tails. LIRGs have mean observed (i.e. uncorrected for internal extinction) SFR surface densities of about 0.4 to 0.9 M yr −1 kpc −2 over large areas (4−9 kpc 2 ) with peaks of about 2−2.5 M yr −1 kpc −2 in the smaller regions (0.16 kpc 2 ) associated with the nucleus of the galaxy or the brightest Brγ region. ULIRGs do have similar average SFR surface densities for the integrated emitting regions of ∼0.4 M yr −1 kpc −2 in somewhat larger areas (100−200 kpc 2 ) and for the Paα peak (∼2 M yr −1 kpc −2 in 4 kpc 2 ). The observed gas kinematics in LIRGs is primarily due to rotational motions around the centre of the galaxy, although local deviations associated with radial flows and/or regions of higher velocity dispersions are present. The ionised and molecular gas share the same kinematics (velocity field and velocity dispersion) to first order, showing slight differences in the velocity amplitudes (peak-to-peak) in some cases, whereas the average velocity dispersions are compatible within uncertainties. As expected, the kinematics of the ULIRG subsample is more complex, owing to the interacting nature of the objects of the sample.

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Section: Emission Lines and Star Formationmentioning

confidence: 99%

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

López

Colina

Arribas

et al. 2012

A&A

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“…This is in apparent contradiction to the higher values one would expect near the nucleus, given the power-law radiation and the more massive jet/outflow winds from the AGN, compared to excitation from stars in the disk (e.g. Black & van Dishoeck 1987;Forbes & Ward 1993;Maloney et al 1996;Simpson et al 1996;Mouri et al 2000).…”

Section: Nuclear Vs Off-nuclear Aperturesmentioning

confidence: 58%

Near-infrared long-slit spectra of Seyfert galaxies: gas excitation across the central kiloparsec

Laan

Schinnerer

Armus

2013

A&A

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Context. The excitation of the gas phase of the interstellar medium can be driven by various mechanisms. In galaxies with an active nucleus, such as Seyfert galaxies, both radiative and mechanical energy from the central black hole, or the stars in the disk surrounding it may play a role. Aims. We investigate the relative importance and range of influence of the active galactic nucleus for the excitation of ionized and molecular gas in the central kiloparsec of its host galaxy. Methods. We present H-and K-band long-slit spectra for a sample of 21 nearby (D < 70 Mpc) Seyfert galaxies obtained with the NIRSPEC instrument on the Keck telescope. For each galaxy, we fit the nebular line emission, stellar continua, and warm molecular gas as a function of distance from the nucleus. Results. Our analysis does not reveal a clear difference between the nucleus proper and off-nuclear environment in terms of excitation mechanisms, suggesting that the influence of an AGN reaches far into the disk of the host galaxy. The radial variations in emission line ratios indicate that, while local mechanisms do affect the gas excitation, they are often averaged out when measuring over extended regions.

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“…1 (Oliva et al 1989;Mouri et al 2000). Such a large difference arises because Fe atoms in photoionized gas are in higher ionization stages and also probably because the Fe abundance in shocked gas is enhanced by dust destruction.…”

Section: Nir [Fe Ii] Emission Lines and J Shocksmentioning

confidence: 99%

“…Such a large difference arises because Fe atoms in photoionized gas are in higher ionization stages and also probably because the Fe abundance in shocked gas is enhanced by dust destruction. Therefore, [Fe II] emission can be used as a tracer of fast radiative atomic shocks, although strong [Fe II] lines may be observable in sources ionized by X-rays, e.g., in active galactic nuclei (Mouri et al 2000). The Fe + ion has four ground terms, each of which has 3-5 closely-spaced levels to form a 16 level system (Pradhan & Nahar 2011).…”

Section: Nir [Fe Ii] Emission Lines and J Shocksmentioning

confidence: 99%

“…Most of the [Fe II] emission, however, originates from the temperature plateau region where the ionization fraction is not too low, as shown in Figure 2. Numerical shock models covering some parameter 216 B.-C. Koo spaces are available in Hollenbach et al (1989), Mouri et al (2000), and Allen et al (2008). A grid of shock models with updated atomic parameters is in preparation by the author of this paper.…”

Section: Nir [Fe Ii] Emission Lines and J Shocksmentioning

confidence: 99%

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Infrared [Fe II] and Dust Emissions from Supernova Remnants

Koo

2013

Proc. IAU

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The SNRs belonging to the former group are also bright in near-infrared H2 emission, indicating that both atomic and molecular shocks are pervasive in these SNRs. The SNRs belonging to the latter group have relatively small radii in general, implying that most of them are likely the remnants of SN IIL/b or SN IIn that had strong mass loss before the explosion. I also comment on the "[Fe II]-H 2 reversal" in SNRs and on using the [Fe II]-line luminosity as an indicator of the supernova (SN) rate in galaxies. In the mid-and far-infrared regimes, thermal dust emission is dominant. The dust in SNRs can be heated either by collisions with gas species in a hot plasma or by radiation from a shock front. I discuss the characteristics of the infrared morphology of the SNRs interacting with molecular clouds and their dust heating processes. Finally, I give a brief summary of the detection of SN dust and crystalline silicate dust in SNRs.

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Excitation Mechanism of Near‐Infrared [Feii] Emission in Seyfert and Starburst Galaxies

Cited by 77 publications

References 84 publications

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

Near-infrared long-slit spectra of Seyfert galaxies: gas excitation across the central kiloparsec

Infrared [Fe II] and Dust Emissions from Supernova Remnants

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