New Improved Calibration Relations for the Determination of Electron Temperatures and Oxygen and Nitrogen Abundances in H Ii Regions

Pilyugin, L. S.; Vı́lchez, J. M.; Thuan, T. X.

doi:10.1088/0004-637x/720/2/1738

Cited by 163 publications

(266 citation statements)

References 63 publications

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“…Pilyugin et al (2010) find that the method shows very good agreement with the abundances they derive using the direct method, with root mean square differences of 0.075 dex for the oxygen abundance and 0.05 dex for the nitrogen abundance. Li, Bresolin & Kennicutt (2013) find similar differences with the direct method for their sample H ii regions, around 0.09 dex in the oxygen abundance.…”

Section: The Ons Methodsmentioning

confidence: 62%

“…We used different strong-line methods to derive oxygen and nitrogen abundances for the full sample. We have chosen strong-line methods calibrated with large samples of H ii regions with temperature-based abundance determinations: the P method of Pilyugin & Thuan (2005), the ONS method of Pilyugin et al (2010), the C method of Pilyugin et al (2012), and the O3N2 and N2 methods calibrated by Marino et al (2013).…”

Section: Discussionmentioning

confidence: 99%

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The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

Arellano-Córdova

Rodríguez

Mayya

et al. 2015

Mon. Not. R. Astron. Soc.

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We study the sensitivity of the methods available for abundance determinations in H ii regions to potential observational problems. We compare the dispersions they introduce around the oxygen and nitrogen abundance gradients when applied to five different sets of spectra of H ii regions in the galaxy M81. Our sample contains 116 H ii regions with galactocentric distances of 3 to 33 kpc, including 48 regions observed by us with the OSIRIS long-slit spectrograph at the 10.4-m Gran Telescopio Canarias telescope. The direct method can be applied to 31 regions, where we can get estimates of the electron temperature. The different methods imply oxygen abundance gradients with slopes of −0.010 to −0.002 dex kpc −1 , and dispersions in the range 0.06-0.25 dex. The direct method produces the shallowest slope and the largest dispersion, illustrating the difficulty of obtaining good estimates of the electron temperature. Three of the strong-line methods, C, ONS, and N2, are remarkably robust, with dispersions of ∼ 0.06 dex, and slopes in the range −0.008 to −0.006 dex kpc −1 . The robustness of each method can be directly related to its sensitivity to the line intensity ratios that are more difficult to measure properly. Since the results of the N2 method depend strongly on the N/O abundance ratio and on the ionization parameter, we recommend the use of the C and ONS methods when no temperature estimates are available or when they have poor quality, although the behaviour of these methods when confronted with regions that have different properties and different values of N/O should be explored.

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Section: The Ons Methodsmentioning

confidence: 62%

Section: Discussionmentioning

confidence: 99%

The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

Arellano-Córdova

Rodríguez

Mayya

et al. 2015

Mon. Not. R. Astron. Soc.

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“…The second approach uses the empirical relations between certain combinations of strong-line intensities and metallicity, which is derived by the Te-method (e.g. Alloin et al 1979;Pagel et al 1979;Pilyugin 2001;Pettini & Pagel 2004;Pilyugin & Thuan 2005;Stasińska 2006;Pilyugin et al 2010).…”

Section: Oxygen Abundancesmentioning

confidence: 99%

On the universality of luminosity–metallicity and mass–metallicity relations for compact star-forming galaxies at redshifts 0 < z < 3

Izotov

Гусева

Fricke

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We study relations between global characteristics of low-redshift (0 < z < 1) compact star-forming galaxies, including absolute optical magnitudes, Hβ emission-line luminosities (or equivalently star-formation rates), stellar masses, and oxygen abundances. The sample consists of 5182 galaxies with high-excitation H ii regions selected from the SDSS DR7 and SDSS/BOSS DR10 surveys adopting a criterion [O iii]λ4959/Hβ 1. These data were combined with the corresponding data for high-redshift (2 z 3) star-forming galaxies. We find that in all diagrams low-z and high-z star-forming galaxies are closely related indicating a very weak dependence of metallicity on stellar mass, redshift, and star-formation rate. This finding argues in favour of the universal character of the global relations for compact star-forming galaxies with high-excitation H ii regions over redshifts 0 < z < 3.

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“…It is believed that the most direct way to estimate metallicity is through the use of electron temperature Te (Stasińska 2004 (Pilyugin, Vílchez & Thuan 2010). In Holmberg II data on the [O ii]λλ3727, 3729 lines are not available except for a couple of complexes, so we rely on the 'NS' calibration (Pilyugin & Mattsson 2011) to estimate metallicities in this galaxy.…”

Section: Metallicitiesmentioning

confidence: 99%

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

Khramtsova¹,

Wiebe²,

Lozinskaya³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of optical spectroscopy and infrared aperture photometry of more than 100 H ii complexes in nine galaxies. Spectra obtained with the 6-m telescope of SAO RAS are used along with archival data from Spitzer and several ground-based telescopes to infer a strength of polycyclic aromatic hydrocarbon (PAH) emission, age, properties of the UV radiation field, and metallicity of studied H ii complexes. Physical properties (age, radiation field parameters, metallicity) are related to the F 8 /F 24 ratio used as a proxy for the PAH abundance in order to reveal factors that may influence the PAH evolution in H ii complexes. The well-known correlation between the F 8 /F 24 ratio and metallicity is confirmed in the studied complexes. The infrared flux ratio also correlates with the [O iii]λ5007/Hβ ratio which is often considered as an indicator of the radiation field hardness, but this correlation seems to be a mere reflection of a correlation between [O iii]λ5007/Hβ and metallicity. In separate metallicity bins, the F 8 /F 24 ratio is found to correlate with an age of an H ii complex, which is estimated from the equivalent width of Hβ line. The correlation is positive for low metallicity complexes and negative for high metallicity complexes. Analysing various mechanisms of PAH formation and destruction in the context of found correlations, we suggest that PAH abundance is likely altered by the UV radiation within H ii complexes, but this is not necessarily due to their destruction. If PAHs can also form in H ii complexes due to some processes like aromatisation, photodestruction, shattering and sputtering of very small grains, the net F 8 /F 24 ratio is determined by a balance between all these processes that can be different at different metallicities.

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New Improved Calibration Relations for the Determination of Electron Temperatures and Oxygen and Nitrogen Abundances in H Ii Regions

Cited by 163 publications

References 63 publications

The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

On the universality of luminosity–metallicity and mass–metallicity relations for compact star-forming galaxies at redshifts 0 < z < 3

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

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