An Empirical Test and Calibration of H<scp>ii</scp>Region Diagnostics

Kennicutt, Robert C.; Bresolin, Fabio; French, H. B.; Martin, Pierre

doi:10.1086/309075

Cited by 79 publications

(132 citation statements)

References 74 publications

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“…The position of an object in the BPT diagram is a function of metallicity and the ionization state of the emitting gas (e.g, Kennicutt et al 2000) and can be roughly divided into three regions (following Kauffmann et al 2003a). The lower left region contains emission line galaxies dominated by star-formation.…”

Section: Optical Spectroscopic Measurementsmentioning

confidence: 99%

Physical Properties and Environments of Nearby Galaxies

Blanton

Moustakas

2009

Annu. Rev. Astron. Astrophys.

511

442

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We review the physical properties of nearby, relatively luminous galaxies, using results from newly available massive data sets together with more detailed observations. First, we present the global distribution of properties, including the optical and ultraviolet luminosity, stellar mass, and atomic gas mass functions. Second, we describe the shift of the galaxy population from "late" galaxy types in underdense regions to "early" galaxy types in overdense regions. We emphasize that the scaling relations followed by each galaxy type change very little with environment, with the exception of some minor but detectable effects. The shift in the population is apparent even at the densities of small groups and therefore cannot be exclusively due to physical processes operating in rich clusters. Third, we divide galaxies into four crude types -spiral, lenticular, elliptical, and merging systems -and describe some of their more detailed properties. We attempt to put these detailed properties into the global context provided by large surveys. Contents

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Section: Optical Spectroscopic Measurementsmentioning

confidence: 99%

Physical Properties and Environments of Nearby Galaxies

Blanton

Moustakas

2009

Annu. Rev. Astron. Astrophys.

511

442

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“…In general, diagnostic diagrams using a range of emission-line intensities are useful for differentiating resolved emission sources such as PN from Hii regions, SNRs and other objects (e.g. Sabbadin, Minello & Bianchini 1977;Cantó 1981;Fesen, Blair & Kirshner 1985;Riera, Phillips & Mampaso 1990;Phillips & Guzman 1998;Kennicutt et al 2000;Riesgo-Tirado & López 2002;Riesgo & López 2006;Kniazev, Pustilnik & Zucker 2008;Raga et al 2008). However, the situation becomes more complex when compact or pseudo-stellar PN are considered.…”

Section: Diagnostic Toolsmentioning

confidence: 99%

Planetary Nebulae: Observational Properties, Mimics and Diagnostics

Frew

Parker

2010

Publ. – Astron. Soc. Aust

185

262

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Abstract:The total number of true, likely and possible planetary nebulae (PN) now known in the Milky Way is nearly 3000, double the number known a decade ago. The new discoveries are a legacy of the recent availability of wide field, narrowband imaging surveys, primarily in the light of H-alpha. In this paper, we summarise the various PN discovery techniques, and give an overview of the many types of objects which mimic PN and which appear as contaminants in both Galactic and extragalactic samples. Much improved discrimination of classical PN from their mimics is now possible based on the wide variety of high-quality multiwavelength data sets that are now available. We offer improved taxonomic and observational definitions for the PN phenomenon based on evaluation of these better diagnostic capabilities. However, we note that evidence is increasing that the PN phenomenon is heterogeneous, and PN are likely to be formed from multiple evolutionary scenarios. In particular, the relationships between some collimated symbiotic outflows and bipolar PN remain uncertain.

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“…The emission line ratios considered have different sensitivities to the input parameters. (Pagel et al 1979;Kennicutt et al 2000;Dors & Copetti 2003;Morisset et al 2004 (Henry & Howard 1995).…”

Section: The Modeling Proceduresmentioning

confidence: 99%

Abundance gradients in a sample of barred spiral galaxies

Dors¹,

Copetti²

2005

A&A

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Abstract.We used photoionization models in order to reproduce the observed gradients of emission-line ratios for H  regions located in the normal spiral galaxy M 101 and in three barred spiral galaxies, namely NGC 1365, NGC 925, and NGC 1073. The behavior of the following nebular parameters across the disk of these galaxies was determined: temperature of the ionizing star (T eff ), ionization parameter (U), and the abundance ratios O/H, N/O, and S/O. Our O/H predictions were found to be consistent with some empirical abundance determinations, but are overestimated by a factor of 0.1−0.4 dex when compared to the direct abundance determinations. NGC 1073 seems to be overabundant in nitrogen compared to other spiral galaxies. No gradient of S/O was found in the studied galaxies, and we derived a positive T eff gradient of T eff / R = (400 ± 112) K kpcand U ranging from −3.0 to −2.3. The N/O vs. O/H diagram in general is consistent with chemical evolution models that assume that the nitrogen synthesis has both a primary and a secondary component compared to oxygen. However, a very strong N/O dependence on the O/H at high abundance was found.

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An Empirical Test and Calibration of HiiRegion Diagnostics

Cited by 79 publications

References 74 publications

Physical Properties and Environments of Nearby Galaxies

Physical Properties and Environments of Nearby Galaxies

Planetary Nebulae: Observational Properties, Mimics and Diagnostics

Abundance gradients in a sample of barred spiral galaxies

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