Optical Classification of Southern Warm Infrared Galaxies

By Lisa J. Kewley, C. Heisler, M. Dopita, S. Lumsden. 2001

376 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/55d42edeb8093f113a2a6ce4e164054d8ba26438

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Citations in the corpus

The physical properties of star-forming galaxies in the low-redshift universe (2003, methodology): “The line has been taken from equation (5) in Kewley et al. (2001b), but our models have an identical upper limit.”
Metallicities and Physical Conditions in Star-forming Galaxies at z ~ 1.0-1.5 (2008, methodology): “Groves et al. (2006) suggest that the offset on the BPT diagram seen in some high-redshift galaxies is mostly caused by contribution from AGNs, as they found properties of their candidate low-metallicity H II/AGN composites similar to those of the host galaxies of AGNs (Kauffmann et al. 2003a; Heckm”
The 2-10 keV luminosity as a Star Formation Rate indicator (2002, background): “…the number of points in the fit), Lpred is the luminosity expected from the best fit relation and Lobs the observed 2 References: NGC55 - Webster & Smith (1983); NGC253, 1672 & 1808 - Kewley et al. (2001); NGC3256 - Moran et al. (1999); Antennae - Rubin et al. (1970), Dobrodiy & Pronik (1979). one.”
New insights into the stellar content and physical conditions of star-forming galaxies at z = 2-3 from spectral modelling (2008, methodology): “Theoretical modelling of nebular emission from star-forming galaxies (e.g. Charlot & Longhetti 2001; Kewley et al. 2001a) shows that a shift upwards in the BPT diagram can be achieved by increasing either the ionization parameter U (which in the usual definition is the ratio of the volume densities…”
Aperture Effects on Star Formation Rate, Metallicity, and Reddening (2005, methodology): “Because ambiguous galaxies are likely to contain both starburst and AGN activity (see e.g., Kewley et al. 2001b; Hill et al. 1999), we do not include them in the following analysis.”
Optical Star Formation Rate Indicators (2005, positive): “Both the integrated and SDSS samples map out similar sequences, which agree well with the theoretical models by Kewley et al. (2001a).”
REST-FRAME OPTICAL SPECTRA OF THREE STRONGLY LENSED GALAXIES AT z ∼ 2 (2009, background): “…line ratio allowed us to measure the density of the star forming regions in the Cosmic Horseshoe and the Clone, and the low resulting ratios indicated high densities of about ∼ 103 cm−3, which is an order of magnitude higher than the values encountered in local starbursts (Kewley et al. 2001b).”
SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements (2016, methodology): “On the classical BPT diagram (Baldwin et al. 1981; Veilleux & Osterbrock 1987; Kewley et al. 2001, 2006; Kauffmann et al. 2003), the location of an H ii region is mainly determined by its metallicity and ionization parameter (e.g., Kewley et al. 2002; Dopita et al. 2013).”
GALAXY-WIDE SHOCKS IN LATE-MERGER STAGE LUMINOUS INFRARED GALAXIES (2011, background): “The primary factors influencing emission line strengths are the shape of the extreme ultraviolet (EUV) spectrum and the abundance of the emission line gas (Kewley et al. 2001; Dopita et al. 2000).”
[O II] as a Star Formation Rate Indicator (2004, methodology): “Because these galaxies are likely to contain both starburst and AGN activity (see e.g., Kewley et al. 2001a; Hill et al. 1999), we do not include them in the following analysis.”
Data Release 1 of the Dark Energy Spectroscopic Instrument (2025, positive): “…( 1981 ) classification, assuming the more recent dividing lines of D. R. Law et al. ( 2021, implemented by default ) compared with the traditional dividing lines of L. J. Kewley et al. ( 2001 ) , which were reported to potentially overestimate the presence of AGN ( e.g., R. Pucha et al. 2025 ) .”
The impact of gas inflows on star formation rates and metallicities in barred galaxies (2011, background): “Galaxies whose emission line ratios indicate a significant photoionization contribution from an active galactic nucleus (AGN) are excluded (Kewley et al. 2001).”
A High Spatial Resolution X-Ray and Hα Study of Hot Gas in the Halos of Star-forming Disk Galaxies. I. Spatial and Spectral Properties of the Diffuse X-Ray Emission (2003, background): “There is no sign of any AGN activity, its optical spectroscopic classification being that of a standard H ii galaxy (Kewley et al. 2001).”
THEORETICAL EVOLUTION OF OPTICAL STRONG LINES ACROSS COSMIC TIME (2013, methodology): “…at High Redshift In local galaxies, semi-empirical and theoretical classification lines are used to successfully separate star-forming galaxies from those containing an AGN or shock excitation (e.g., Veilleux & Osterbrock 1987; Kewley et al. 2001b; Kauffmann et al. 2003; Kewley et al. 2006b).”
Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. I. The Role of ISM Pressure and the Molecular Cloud Dissipation Timescale (2004, neutral): “For these,the [S II] 6717=6731 A ratio indicates ne 1000 cm 3 (Kewley et al.2001,b).”
BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics (2017, methodology): “Baldwin et al. (1981) first proposed the use of line diagnostic diagrams, which have subsequently been developed and refined in numerous studies (e.g. Veilleux & Osterbrock 1987; Kewley et al. 2001; Shirazi & Brinchmann 2012).”
Galaxy pairs in the Sloan Digital Sky Survey – IX. Merger-induced AGN activity as traced by the Wide-field Infrared Survey Explorer (2014, methodology): “Using the classification scheme from Kewley et al. (2001), there are 200 optically identified AGNs in the pairs sample, of which 175 are not identified as AGN using theW1−W2 > 0.8 colour cut.”