2005ApJ...631..231P


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.25CET07:10:08

2005ApJ...631..231P - Astrophys. J., 631, 231-243 (2005/September-3)

Oxygen abundance determination in H II regions: the strong line intensities-abundance calibration revisited.

PILYUGIN L.S. and THUAN T.X.

Abstract (from CDS):

The problem of oxygen abundance determination in H II regions based on the ``strong oxygen line intensities-oxygen abundance'' empirical calibration is revisited. A compilation of spectroscopic data of H II regions in spiral and irregular galaxies with a measured [O III] λ4363 line intensity has been carried out, resulting in a sample containing more than 700 individual measurements.
Method. are devised to select out only high-precision measurements from that original sample. Te-based oxygen abundances have been recomputed in the same way for all H II regions with high-precision measurements. That sample of Teabundances is used to recalibrate the empirical relations between the oxygen abundance and the strong oxygen line intensities for both high (the upper branch of the O/H-R23diagram) and low (the lower branch) metallicities, within the framework of the P method, where P is the excitation parameter. Concerning high-metallicity H II regions, an alternative way for deriving oxygen abundances using only measurements of the strong nebular oxygen lines is proposed. The method is based on a tight correlation between the flux in the auroral [O III] λ4363 line and the fluxes in the nebular [O II] λλ3727, 3729 and [O III] λλ4959, 5007 lines, called the ff relation. This relation is also used to select out high-metallicity H II regions with high-precision O/HTemeasurements. In contrast to previous work, the new upper branch P calibration is based only on O/HTeabundances. It is found that O/HPabundances usually agree well with the O/Hffabundances, although faint (logR23≲-0.5) low-excitation (P≲0.25) H II regions may show systematic differences that can be as large as ∼0.1 dex. As for the newly derived low-metallicity P calibration, it is shown to be robust. The calibrations derived from the sample containing all O/HTeabundance determinations and from that containing only recent (since 1995) measurements are found to be in very good agreement. For both low- and high-metallicity H II regions, the new calibration gives O/HPabundances that agree with O/HTeabundances to within 0.1 dex.

Abstract Copyright:

Journal keyword(s): Galaxies: Abundances - ISM: H II Regions - ISM: Abundances

Simbad objects: 20

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Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 1232 EmG 03 09 45.514 -20 34 45.48   10.67 9.87 9.53 10.2 ~ 266 0
2 CDT NGC 1232 1 HII 03 09 49.5010 -20 33 43.000           ~ 14 0
3 CCM 71A HII 13 29 39.555 +47 08 42.12           ~ 15 0
4 CCM 84A HII 13 29 43.766 +47 13 07.74           ~ 8 0
5 CCM 72 HII 13 29 44.242 +47 10 23.81           ~ 25 0
6 [TA91] 1 HII 13 29 52.074 +47 12 44.86           ~ 8 0
7 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3848 4
8 CCM 107 HII 13 29 53.1 +47 12 40           ~ 6 0
9 CCM 6A HII 13 29 53.369 +47 12 10.80           ~ 4 0
10 CCM 37A HII 13 29 55.981 +47 11 55.98           ~ 8 0
11 [TA91] 18 HII 13 29 56.644 +47 10 45.90           ~ 8 0
12 CCM 10 HII 13 29 59.521 +47 13 57.76           ~ 27 0
13 [TA91] 7 HII 13 30 00.823 +47 11 38.81           ~ 6 0
14 CCM 55 HII 13 30 02.336 +47 09 50.42           ~ 14 0
15 CCM 53 HII 13 30 02.716 +47 09 58.25           ~ 13 0
16 CCM 54 HII 13 30 03.436 +47 09 42.78           ~ 10 0
17 CCM 57A HII 13 30 04.335 +47 12 56.49           ~ 7 0
18 [HBS84] 29 HII 14 02 54.200 +54 22 25.56           ~ 35 0
19 M 101 GiP 14 03 12.583 +54 20 55.50   8.46 7.86 7.76   ~ 2579 2
20 [H69] NGC 5457 40 PoG 14 03 31.300 +54 21 05.81           ~ 39 0

    Equat.    Gal    SGal    Ecl

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2020.11.25-07:10:08

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