Metal Abundances of KISS Galaxies. II. Nebular Abundances of 12 Low-Luminosity Emission-Line Galaxies

Melbourne, Jason; Phillips, Andrew C.; Salzer, John J.; Grönwall, C.; Sarajedini, Vicki L.

doi:10.1086/381067

Cited by 44 publications

(50 citation statements)

References 38 publications

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“…The oxygen abundances derived via the P-method are in agreement with the abundances determined using the T e -method over the full range of abundances (see Fig. 1, and Melbourne et al 2004). This allows us to conclude that the P-method provides reliable abundance determinations in H  regions.…”

Section: Introductionsupporting

confidence: 73%

Chemical abundances in spiral and irregular galaxies

Pilyugin¹,

Contini²,

Vı́lchez³

2004

A&A

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Abstract. The validity of oxygen and nitrogen abundances derived from the global emission-line spectra of galaxies via the P-method has been investigated using a collection of published spectra of individual H  regions in irregular and spiral galaxies. The conclusion of Kobulnicky et al. (1999, ApJ, 514, 544) that global emission-line spectra can reliably indicate the chemical properties of galaxies has been confirmed. It has been shown that the comparison of the global spectrum of a galaxy with a collection of spectra of individual H  regions can be used to distinguish high and low metallicity objects and to estimate accurate chemical abundances in a galaxy. The oxygen and nitrogen abundances in samples of UV-selected and normal nearby galaxies have been determined. It has been found that the UV-selected galaxies occupy the same area in the N/O−O/H diagram as individual H  regions in nearby galaxies. Finally, we show that intermediate-redshift galaxies systematically deviate from the metallicity-luminosity trend of local galaxies.

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Section: Introductionsupporting

confidence: 73%

Chemical abundances in spiral and irregular galaxies

Pilyugin¹,

Contini²,

Vı́lchez³

2004

A&A

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“…The spectra acquired exhibited broad and nebular He ii emission lines, and SBS 1415+437 was therefore included in the latest WR galaxy catalogue . Subsequent spectroscopic analyses were published by Melbourne & Salzer (2002), Melbourne et al (2004), Guseva et al (2003), Izotov & Thuan (2004), and Lee et al (2004). Figure 26 shows the spectra of regions A and C obtained using the instrument ISIS at the 4.2 m WHT and a slit places at a PA 20…”

Section: Sbs 1415+437mentioning

confidence: 99%

Massive star formation in Wolf-Rayet galaxies

López-Sánchez

Esteban

2009

A&A

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Aims. We have performed a comprehensive multiwavelength analysis of a sample of 20 starburst galaxies that show the presence of a substantial population of very young massive stars, most of them classified as Wolf-Rayet (WR) galaxies. In this paper, the second of the series, we present the results of the analysis of long-slit intermediate-resolution spectroscopy of star-formation bursts for 16 galaxies of our sample. Methods. We study the spatial localization of the WR stars in each galaxy. We analyze the excitation mechanism and derive the reddening coefficient, physical conditions, and chemical abundances of the ionized gas. We study the kinematics of the ionized gas to check the rotation/turbulence pattern of each system. When possible, tentative estimates of the Keplerian mass of the galaxies are calculated. Results. Aperture effects and the exact positioning of the slit onto the WR-rich bursts seem to play a fundamental role in their detection. We check that the ages of the last star-forming burst estimated using optical spectra agree with those derived from Hα imagery. Our analysis shows that a substantial fraction of the galaxies exhibit evidence of perturbed kinematics. With respect to the results found in individual galaxies, we remark the detection of objects with different metallicity and decoupled kinematics in Haro 15 and Mkn 1199, the detection of tidal streams in IRAS 08208+2816, Tol 9, and perhaps in SBS 1319+579, and the development of a merging process in both SBS 0926+606 A and Tol 1457-262. Conclusions. All of these results -in combination with those obtained in Paper I -reinforce the hypothesis that interactions with or between dwarf objects is a very important mechanism in triggering massive-star formation in starburst galaxies, especially in dwarf ones. It must be highlighted that only deep and very detailed observations -as presented in this paper -can provide clear evidences that these subtle interaction processes are taking place.

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“…For the KISS galaxy sample, Melbourne et al (2004) find a metallicity vs. B-band luminosity relation expressed by…”

Section: Metallicitymentioning

confidence: 99%

“…Metallicities have been estimated by Melbourne et al (2004) using the T e method. Where not possible, the authors used the standard R 23 method improved by the introduction of the p 3 factor (Pilyugin 2000).…”

Section: Metallicitymentioning

confidence: 99%

The host galaxy of GRB 031203: a new spectroscopic study

Margutti

Chincarini

Covino

et al. 2007

A&A

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Aims. The host galaxy of the long-duration gamma-ray burst (GRB) 031203 (HG 031203) offers a precious opportunity to study in detail the environment of a nearby GRB. The aim is to better characterize this galaxy and analyse the possible evolution with time of the spectroscopic quantities we derive. Methods. We analyse HG 031203 using a set of optical spectra acquired with the ESO-VLT and Keck telescope. We compare the metallicity, luminosity and star formation properties of this galaxy and of the other supernova-long gamma-ray burst hosts in the local universe (z < 0.2) against the KPNO International Spectroscopic Survey. Results. HG 031203 is a metal poor, actively star forming galaxy (star formation rate of 12.9 ± 2.2 M yr −1 ) at z = 0.1054. From the emission-line analysis we derive an intrinsic reddening E HG (B − V) ≈ 0.4. This parameter doesn't show a compelling evidence of evolution at a month time-scale. We find an interstellar medium temperature of ≈12 500 K and an electronic density of N e = 160 cm −3 . After investigating for possible Wolf-Rayet emission features in our spectra, we consider dubious the classification of HG 031203 as a Wolf-Rayet galaxy. Long gamma-ray burst (LGRB) and supernova hosts in the local universe (z < 0.2) show, on average, specific star formation rates higher than ordinary star forming galaxy at the same redshift. On the other hand, we find that half of the hosts follows the metallicity-luminosity relation found for star-burst galaxies; HG 031203 is a clear outlier, with its really low metallicity (12 + log (O/H) = 8.12 ± 0.04).

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Metal Abundances of KISS Galaxies. II. Nebular Abundances of 12 Low-Luminosity Emission-Line Galaxies

Cited by 44 publications

References 38 publications

Chemical abundances in spiral and irregular galaxies

Chemical abundances in spiral and irregular galaxies

Massive star formation in Wolf-Rayet galaxies

The host galaxy of GRB 031203: a new spectroscopic study

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