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J/MNRAS/460/1739    Giant HII regions BOND abundances        (Vale Asari+, 2016)

BOND: Bayesian Oxygen and Nitrogen abundance Determinations in giant H II regions using strong and semistrong lines. Vale Asari N., Stasinska G., Morisset C., Cid Fernandes R. <Mon. Not. R. Astron. Soc., 460, 1739-1757 (2016)> =2016MNRAS.460.1739V (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; H II regions ; Abundances Keywords: methods: data analysis - ISM: abundances - H II regions - galaxies: abundances Abstract: We present the Bayesian oxygen and nitrogen abundance determinations (bond) method. bond is a Bayesian code (available at: to simultaneously derive oxygen and nitrogen abundances in giant HII regions. It compares observed emission lines to a grid of photoionization models without assuming any relation between O/H and N/O. Our grid spans a wide range in O/H, N/O and ionization parameter U, and covers different starburst ages and nebular geometries. Varying starburst ages accounts for variations in the ionizing radiation field hardness, which arise due to the ageing of HII regions or the stochastic sampling of the initial mass function. All previous approaches assume a strict relation between the ionizing field and metallicity. The other novelty is extracting information on the nebular physics from semistrong emission lines. While strong lines ratios alone ([OIII]/Hβ, [OII]/Hβ and [NII]/Hβ) lead to multiple O/H solutions, the simultaneous use of [ArIII]/[NeIII] allows one to decide whether an HII region is of high or low metallicity. Adding HeI/Hβ pins down the hardness of the radiation field. We apply our method to HII regions and blue compact dwarf galaxies, and find that the resulting N/O versus O/H relation is as scattered as the one obtained from the temperature-based method. As in previous strong-line methods calibrated on photoionization models, the bond O/H values are generally higher than temperature-based ones, which might indicate the presence of temperature fluctuations or kappa distributions in real nebulae, or a too soft ionizing radiation field in the models. Description: BOND determines nitrogen and oxygen gas-phase abundances by using strong and semistrong lines and comparing them to a grid of photoionization models in a Bayesian framework. The code is written in python and its source is publicly available at The grid of models presented here is included in the 3MdB data base (Morisset, Delgado-Inglada & Flores-Fajardo 2015RMxAA..51..103M, see under the reference 'BOND'. The Bayesian posterior probability calculated by bond stands on two pillars: our grid of models and our choice of observational constraints (from which we calculate our likelihoods). We discuss each of these in turn. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 221 708 Giant HII regions and blue compact dwarves emission lines table2.dat 168 156 BOND results for sample B of Giant HII regions and blue compact dwarves
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Id [1/708] Sequnetial number 5 A1 --- r_Id Reference for Id (1) 7- 23 A17 --- Name HII region name (NGCNNNNNNNN) 25- 34 E10.5 --- F3727 Line flux of [OII] 3737Å relative to Hβ 36- 45 E10.5 --- e_F3727 rms uncertainty on F3727 47- 56 E10.5 --- F3869 ?=0 Line flux of [NeII] 3869Å relative to Hβ 58- 67 E10.5 --- e_F3869 ?=0 rms uncertainty on F3869 69- 78 E10.5 --- F4363 ?=0 Line flux of [OIII] 4363Å relative to Hβ 80- 89 E10.5 --- e_F4363 ?=0 rms uncertainty on F4363 91-100 E10.5 --- F5007 Line flux of [OIII] 5007Å relative to Hβ 102-111 E10.5 --- e_F5007 rms uncertainty on F5007 113-122 E10.5 --- F5755 ?=0 Line flux of [NII] 5755Å relative to Hβ 124-133 E10.5 --- e_F5755 ?=0 rms uncertainty on F5755 135-144 E10.5 --- F5876 ?=0 Line flux of [HeI] 5876Å relative to Hβ 146-155 E10.5 --- e_F5876 ?=0 rms uncertainty on F5876 157-166 E10.5 --- F6584 Line flux of [NII] 6584Å relative to Hβ 168-177 E10.5 --- e_F6584 rms uncertainty on F6584 179-188 E10.5 --- F7135 ?=0 Line flux of [ArIII] 7153Å relative to Hβ 190-199 E10.5 --- e_F7135 ?=0 rms uncertainty on F7135 201-210 E10.5 --- limF4363 ?=0 Upper limit of [OIII] 4363Å line flux relative to Hβ 212-221 E10.5 --- limF5755 ?=0 Upper limit of [NII] 5755Å line flux relative to Hβ
Note (1): References as follows: a = Bolin et al. (2005, Cat. J/A+A/441/981) b = Bresolin et al. (2004ApJ...615..228B) c = Kennicutt et al. (2003ApJ...591..801K) d = van Zee et al. (1998, Cat. J/AJ/116/2805) g = Bresolin et al. (2009ApJ...700..309B) i = Bresolin (2007ApJ...656..186B) j = Bresolin et al. (2010MNRAS.404.1679B) k = Li et al. (2013ApJ...766...17L) l = Zurita & Bresolin (2012MNRAS.427.1463Z) m = Bresolin et al. (2012ApJ...750..122B) n = Goddard et al. (2011MNRAS.412.1246G) p = Bresolin et al. (2009, Cat. J/ApJ/695/580) z = Izotov et al. (2007, Cat. J/ApJ/662/15)
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Id [1/708] Sequnetial number 5- 15 E11.5 [-] logO/H(jmod) Maximun a posteriori logO/H 17- 27 E11.5 [-] logN/O(jmod) Maximun a posteriori logN/O 29- 39 E11.5 [-] logO/H(jc68cen) Centre term for logO/H 41- 50 E10.5 [-] logO/H(jc68sig) 68% credibility ellipse error for logO/H 52- 62 E11.5 [-] logN/O(jc68cen) Centre term for logN/O 64- 73 E10.5 [-] logN/O(jc68sig) 68% credibility ellipse error for logN/O 75- 85 E11.5 [-] jc68(cov) Covariance term used to construct the 68 per cent credibility ellipse 87- 96 E10.5 [-] jc68(scale) Scaling used to construct the 68 per cent credibility ellipse 98-108 E11.5 [-] logO/H(mmed) Marginalized median value of logO/H 110-120 E11.5 [-] logN/O(mmed) Marginalized median value of logN/O 122-132 E11.5 [-] logO/H(mp68l) Lower value of 68% equal-tailed interval for logO/H 134-144 E11.5 [-] logO/H(mp68u) Upper value of 68% equal-tailed interval for logO/H 146-156 E11.5 [-] logN/O(mp68l) Lower value of 68% equal-tailed interval for logN/O 158-168 E11.5 [-] logN/O(mp68u) Upper value of 68% equal-tailed interval for logN/O
History: Copied at
(End) Patricia Vannier [CDS] 06-Oct-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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