2002
DOI: 10.1086/344104
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Optical Recombination Lines of Heavy Elements in Giant Extragalactic HiiRegions

Abstract: We present high resolution observations of the giant extragalactic H II regions NGC 604, NGC 2363, NGC 5461 and NGC 5471, based on observations taken with the ISIS spectrograph on the William Herschel Telescope. We have detected -by the first time-C II and O II recombination lines in these objects. We find that recombination lines give larger C ++ and O ++ abundances than collisionallly excited lines, suggesting that temperature variations can be present in the objects. We detect [Fe IV] lines in NGC 2363 and … Show more

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Cited by 112 publications
(178 citation statements)
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“…The peculiar position of NGC 2363 is indicated in Figure 6 because it will be discussed later. The figure shows the wellknown C/O vs. O/H correlation found in previous works by, for example, Garnett et al (1995Garnett et al ( , 1999) from observations of CELs or Esteban et al (2002Esteban et al ( , 2009) from observations of RLs. Figure 6 includes the time evolution of the abundances predicted by the chemical evolution models of the Milky Way disc presented by Esteban et al (2013).…”
Section: The C/o Vs O/h Relationsupporting
confidence: 59%
“…The peculiar position of NGC 2363 is indicated in Figure 6 because it will be discussed later. The figure shows the wellknown C/O vs. O/H correlation found in previous works by, for example, Garnett et al (1995Garnett et al ( , 1999) from observations of CELs or Esteban et al (2002Esteban et al ( , 2009) from observations of RLs. Figure 6 includes the time evolution of the abundances predicted by the chemical evolution models of the Milky Way disc presented by Esteban et al (2013).…”
Section: The C/o Vs O/h Relationsupporting
confidence: 59%
“…1b smaller symbols correspond to models for which [N ] λ5755/Hβ is smaller than 10 −4 . This is the flux limit attained by Esteban et al (2002) with 3 hours of integration on a 4 m telscope for the brightest H  region in M 33.…”
Section: The Biasesmentioning
confidence: 74%
“…Recombination lines have also been detected in a few H  regions (e.g. Peimbert et al 1993;Esteban et al 1998Esteban et al , 1999Esteban et al , 2002Tsamis et al 2003b;Garcia-Rojas et al 2004). Here again they lead to higher abundances than collisionally excited lines, although not to the same extreme as in planetary nebulae.…”
Section: Derive Abundances From Pure Recombination Linesmentioning
confidence: 99%
“…To obtain a consistent and, possibly, more correct set of data for the hydrogen distributions, the conversion from CO flux to H 2 surface density has been redone using the oxygen-dependent calibration by Wilson (1995), assuming the O/H-gradient derived by Esteban et al (2002Esteban et al ( , 2005.…”
Section: Abundance Datamentioning
confidence: 99%