Abundance Gradients in the Galaxy

By A. Rudolph, M. Fich, G. R. Bell, Travis Norsen, J. Simpson, M. Haas, E. Erickson. 2006

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View Paper: https://www.semanticscholar.org/paper/6eb955a3910317acf8773f95a84eb3aadfc77f54

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In Astronomy and Astrophysics

Citations in the corpus

EXTRAGALACTIC CHEMICAL ABUNDANCES: DO H ii REGIONS AND YOUNG STARS TELL THE SAME STORY? THE CASE OF THE SPIRAL GALAXY NGC 300 (2009, methodology): “This method has been pursued with success in the Milky Way (Martín-Hernández et al. 2002; Rudolph et al. 2006), but has been rarely applied to derive abundance gradients for external spiral galaxies.”
The Hα surface brightness–radius relation: a robust statistical distance indicator for planetary nebulae (2015, unknown): “V ) D (pc) Type References EGB 4 82 −6.35 0.05 830 ± 160 CV bowshock RN98, GT01 Fr 2-11 208 −5.40 0.05 163+231−37 CV bowshock FM06, F08, vL07 Abell 35 419 −5.12 0.04 220 ± 100 Ionized ISM F08, Z12 DeHt 5 297 −5.25 0.10 345+19−17 Ionized ISM F08, B09 EGB 1 277 −5.37 0.23 470 ± 140 Ionized ISM F08, U ”
Physical Processes in the Interstellar Medium (2014, background): “The metallicity of the gas in the CMZ is therefore around twice the solar value (Ferrière, Gillard & Jean, 2007), while in the outer Galaxy, metallicities are typically somewhat sub-solar (Rudolph et al., 2006).”
The Initial Mass Function of the Massive Star-forming Region NGC 3603 from Near-Infrared Adaptive Optics Observations (2007, methodology): “This is based on the fact that the Galactocentric distance of NGC 3603 is similar to that of the Sun, so that the radial gradient of the metallicity in the Milky Way does not need to be taken into account (e.g. Rudolph et al. 2006).”
SDSS IV MaNGA – metallicity and nitrogen abundance gradients in local galaxies (2017, background): “…lines, radio recombination lines and collisionally excited lines, leading to somewhat discrepant results, see for example Henry & Worthey 1999; Rudolph et al. 2006; Blanc et al. 2015), O/B-type stars (Smartt & Rolleston 1997; Rolleston et al. 2000), Cepheids (Luck et al. 2003; Pedicelli et…”
OPTICAL SPECTROSCOPY AND NEBULAR OXYGEN ABUNDANCES OF THE SPITZER/SINGS GALAXIES (2010, background): “…μm, [O iii] λ52 μm, [N iii] λ57 μm, [O iii] λ88 μm, [N ii] λ122 μm), which are insensitive to variations in electron temperature, will be crucial in establishing the abundances of metal-rich H ii regions (Martı́nHernández et al. 2002; Garnett et al. 2004a; Rudolph et al. 2006; Rubin et al. 2008).”