Optical Classification of Southern Warm Infrared Galaxies

Kewley, Lisa J.; Heisler, Charlene A.; Dopita, Michael A.; Lumsden, S. L.

doi:10.1086/318944

Cited by 442 publications

(643 citation statements)

References 90 publications

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“…Firstly, in Kewley et al (2001), we have shown that the optical diagnostic diagrams are extremely sensitive to the presence of an AGN. An AGN that contributes only 20% to the optical emission increases the line ratios sufficiently that it would be classiÐed as an AGN.…”

Section: The Observational Comparison Samplementioning

confidence: 98%

“…Spectra were obtained in the red and blue wavelength ranges using the Double Beam Spectrograph on the Mount Stromlo and Siding Springs 2.3 m telescope. Full details of our observations are discussed in Kewley et al (2000Kewley et al ( , 2001. All 225 objects were classiÐed into AGN, starburst, and LINER types using new theoretical classiÐcation lines on the VO87 diagnostic diagrams.…”

Section: The Observational Comparison Samplementioning

confidence: 99%

“…These models are used in conjunction with our large observational data set described in Kewley et al ( , 2001 to place new observational constraints on the shape of the EUV ionizing radiation Ðeld. Since the two stellar population spectral synthesis codes provide a wide choice of stellar mass loss formulations, evolutionary tracks, and stellar atmospheric transfer models, they provide strikingly di †erent predictions about the shape and intensity of the EUV Ðeld as a function of stellar age.…”

Section: Introductionmentioning

confidence: 99%

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Theoretical Modeling of Starburst Galaxies

Kewley

Dopita

Sutherland

et al. 2001

ApJ

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2,539

110

3,967

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We have modeled a large sample of infrared starburst galaxies using both the PEGASE v2.0 and STARBURST99 codes to generate the spectral energy distribution (SED) of the young star clusters. PEGASE utilizes the Padova group tracks, while STARBURST99 uses the Geneva group tracks, allowing comparison between the two. We used our MAPPINGS III code to compute photoionization models that include a self-consistent treatment of dust physics and chemical depletion. We use the standard optical diagnostic diagrams as indicators of the hardness of the EUV radiation Ðeld in these galaxies. These diagnostic diagrams are most sensitive to the spectral index of the ionizing radiation Ðeld in the 1È4 ryd region. We Ðnd that warm infrared starburst galaxies contain a relatively hard EUV Ðeld in this region. The PEGASE ionizing stellar continuum is harder in the 1È4 ryd range than that of STARBURST99. As the spectrum in this regime is dominated by emission from Wolf-Rayet (W-R) stars, this discrepancy is most likely due to the di †erences in stellar atmosphere models used for the W-R stars. The PEGASE models use the Clegg & Middlemass planetary nebula nuclei (PNN) atmosphere models for the W-R stars, whereas the STARBURST99 models use the Schmutz, Leitherer, & Gruenwald W-R atmosphere models. We believe that the Schmutz et al. atmospheres are more applicable to the starburst galaxies in our sample ; however, they do not produce the hard EUV Ðeld in the 1È4 ryd region required by our observations. The inclusion of continuum metal blanketing in the models may be one solution. Supernova remnant (SNR) shock modeling shows that the contribution by mechanical energy from SNRs to the photoionization models is >20%. The models presented here are used to derive a new theoretical classiÐcation scheme for starbursts and active galactic nucleus (AGN) galaxies based on the optical diagnostic diagrams.

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Section: The Observational Comparison Samplementioning

confidence: 98%

Section: The Observational Comparison Samplementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Theoretical Modeling of Starburst Galaxies

Kewley

Dopita

Sutherland

et al. 2001

ApJ

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2,539

110

3,967

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“…A classification scheme using optical emission line ratios was first put forward by Heckman (1980) and subsequently amendments have been proposed by, inter alia, Baldwin et al (1981), Kewley et al (2001Kewley et al ( , 2006 and Kauffmann et al (2003a). In this research, a two-pronged approach was adopted to identify LINERs.…”

Section: Diagnostic Tests To Select Linersmentioning

confidence: 99%

The mass fraction of AGN and the Fundamental Plane of black hole activity from a large X-ray-selected sample of LINERs

Nisbet

Best

2015

Mon. Not. R. Astron. Soc.

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A sample of 576 X-ray selected LINERs was constructed by combining data from the 3XMM-DR4 and SDSS-DR7 catalogues. The sample was used to investigate the fraction of galaxies hosting a LINER, finding that the fraction is a strong function of both stellar mass and black hole mass (increasing as f LINER ∝ M 1.6±0.2 * and f LINER ∝ M 0.6±0.1 BH respectively) and that it rises close to unity at the highest black hole masses and lowest X-ray luminosities. After obtaining radio flux densities from the FIRST survey, the sample was also used to investigate the Fundamental Plane of black hole activity -a scale-invariant relationship between black hole mass, X-ray luminosity and radio luminosity that is believed to hold across at least nine orders of magnitude of mass. There are key advantages in using only LINERs for the derivation as these are the counterparts of the "low-hard" X-ray binaries for which the relationship is tightest. The Fundamental Plane was found to be log LR erg/s = 0.65 +0.07 −0.07 log LX 10 42 erg/s +0.69 +0.10 −0.10 log MBH 10 8 M +38.35 +0.10 −0.10 . The scatter around the plane was 0.73 ± 0.03 dex, too large to suggest that the Fundamental Plane can be used as a tool to estimate black hole mass from the observables of X-ray and radio luminosity. The black hole mass scaling is sensitive to the slope of the mass -velocity dispersion relation and, in order to achieve consistency with X-ray binaries, the analysis favours a steep gradient for this relationship, as found in recent research.

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“…Arp 161 is a compact HII galaxy (Kewley et al (2001)) with a faint optical fan to the southwest with a length of ∼ 45 " (16.2 kpc) (Fig. 22).…”

Section: Arp 161mentioning

confidence: 99%

The Structure and Interaction History of Moderate Luminosity Mergers

Hüttemeister¹,

Manthey²

2006

Proc. IAU

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Interaction and merging are the two most important driving forces of galaxy evolution. In contrast to the well studied major mergers of two large gas-rich disk galaxies, which may lead to Ultraluminous Infrared Galaxies (ULIRGs, LFIR>1012 L⊙), mergers between galaxies of unequal mass or a spiral and an elliptical (S+E mergers) are still poorly understood. These moderate luminosity mergers typically have LFIR > 1011 L⊙. Here, we present the results of our multiwavelength study of a sample of such kind of mergers, including interferometric HI and single-dish CO observations, optical and near-infrared imaging as well as optical spectroscopy.

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Optical Classification of Southern Warm Infrared Galaxies

Cited by 442 publications

References 90 publications

Theoretical Modeling of Starburst Galaxies

Theoretical Modeling of Starburst Galaxies

The mass fraction of AGN and the Fundamental Plane of black hole activity from a large X-ray-selected sample of LINERs

The Structure and Interaction History of Moderate Luminosity Mergers

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