Strong Emission Line H II Galaxies in the Sloan Digital Sky Survey. I. Catalog of DR1 Objects with Oxygen Abundances from Te Measurements

By A. Kniazev, S. Pustilnik, E. Grebel, Henry Lee, A. Pramskij. 2004

139 citations recorded by the source corpus.

We present the first edition of the SDSS H II galaxies with Oxygen abundances Catalog (SHOC), which is a listing of strong emission-line galaxies (ELGs) from the Sloan Digital Sky Survey (SDSS). Oxygen abundances have been obtained with the classic Te method. We describe the method exploiting the SDSS database to construct this sample. The selection procedures are described and discussed in detail, as well as some problems encountered in the process of deriving reliable emission line parameters. The method was applied to the SDSS Data Release 1 (DR1). We present 612 SDSS emission-line galaxies (624 separate SDSS targets in total), for which the oxygen abundances 12 + log(O/H) have rms uncertainties ≤0.20 dex. The subsample of 263 ELGs (272 separate SDSS targets) have an uncertainty ≤0.10 dex, while 459 ELGs (470 separate SDSS targets) have an uncertainty ≤0.15 dex. The catalog includes the main parameters of all selected ELGs, the intensities and equivalent widths of hydrogen and oxygen emission lines, as well as oxygen abundances with their uncertainties. The information on the presence of Wolf-Rayet blue and/or red bumps in 109 galaxies is also included. With the use of combined g, r, i SDSS images we performed visual morphological classification of all SHOC galaxies. Four hundred sixty-one galaxies (∼75%) are classified as confident or probable blue compact galaxies (BCG/BCG?), 78 as irregular ones, 20 as low surface brightness galaxies (LSBG), 10 as obviously interacting, and 43 as spiral galaxies. In creating the catalog, 30 narrow-line active galactic nuclei and 69 LINERs were also identified; these are also presented apart of the main catalog. We outline briefly the content of the catalog, and the prospects of its use for statistical studies of the star formation and chemical evolution issues. Some of these studies will be presented in the forthcoming paper. Finally, we show that the method presented by Kniazev et al. for calculating O+/H+ using intensities of the [O II] λλ7320, 7330 lines for SDSS emission-line spectra in the absence of [O II] λ3727 line appears to yield reliable results over a wide range of studied oxygen abundances: 7.10 < 12 + log(O/H) < 8.5.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/23c76959104654df4d745c93d6b4cdf385cedb64

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Citations in the corpus

Mid-Infrared Properties of Low-Metallicity Blue Compact Dwarf Galaxies from the Spitzer Infrared Spectrograph (2005, background): “The metallicity of UM 461 is 0.087 Z (Kniazev et al. 2004).”
Virgo Cluster Early-Type Dwarf Galaxies with the Sloan Digital Sky Survey. II. Early-Type Dwarfs with Central Star Formation (2006, background): “Note that the problem of apparent truncation of strong emission lines in SDSS spectra reported by Kniazev et al. (2004) does not occur in any of our spectra.”
OPTICAL SPECTROSCOPY AND NEBULAR OXYGEN ABUNDANCES OF THE SPITZER/SINGS GALAXIES (2010, background): “…SDSS and a representative sample of metal-rich H ii regions with well-measured electron temperatures (red squares; Garnett et al. 1997; van Zee et al. 1998; Kennicutt et al. 2003a; Kniazev et al. 2004; Bresolin et al. 2004, 2005; Izotov & Thuan 2004; Izotov et al. 2006; Rosolowsky & Simon 2008).”
Galaxies with Wolf-Rayet signatures in the low-redshift Universe. A survey using the Sloan Digital Sky Survey (2008, methodology): “As pointed out by Kniazev et al. (2004) this can to some extent be remedied by using the [O ii] 7320, 7330 quadruplet instead, but this is a much weaker line.”
Strongly star forming galaxies in the local Universe with nebular He iiλ4686 emission (2012, methodology): “When possible, we use the [O II] λλ7318–7330 quadruplet instead (Kniazev et al. 2004), but as this is a fairly weak line and falls in a region with significant sky emission, we cannot always make use of this line.”
EXTRAGALACTIC CHEMICAL ABUNDANCES: DO H ii REGIONS AND YOUNG STARS TELL THE SAME STORY? THE CASE OF THE SPIRAL GALAXY NGC 300 (2009, result): “This supports the result obtained by Kniazev et al. (2004) from the spectra of more than 200 H II galaxies from the Sloan Digital Sky Survey [log(O/H)7325 − log(O/H)3727 = −0.002±0.002], and the conclusion that [O II]λ7325 can be used to measure O+/H+ ionic abundances, albeit with larger…”
Metallicity Calibrations and the Mass-Metallicity Relation for Star-forming Galaxies (2008, background): “The SDSS catalog contains very few metal-poor galaxies (Izotov et al. 2004; Kniazev et al. 2003, 2004; Papaderos et al. 2006; Izotov et al. 2006a).”
The chemical composition of metal-poor emission-line galaxies in the Data Release 3 of the Sloan Digital Sky Survey (2005, methodology): “The oxygen abundances for some galaxies from Table 3 are also in agreement with independent abundance determinations from the same SDSS spectra by Kniazev et al. (2003, 2004).”