2001A&A...369..594P


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.29CET21:12:21

2001A&A...369..594P - Astronomy and Astrophysics, volume 369, 594-604 (2001/4-2)

On the oxygen abundance determination in HII regions. High-metallicity regions.

PILYUGIN L.S.

Abstract (from CDS):

This is our second paper devoted to the problem of line intensity - oxygen abundance calibration starting from the idea of McGaugh (1991ApJ...380..140M) that the strong oxygen lines ([OII] λλ3727, 3729 and [OIII] λλ4959, 5007) contain the necessary information to determine accurate abundances in HII regions. In the previous study (Pilyugin, 2000) the corresponding relations were obtained for the low-metallicity HII regions (12+logO/H≤7.95, the lower branch of the O/H-R23 diagram). The high-metallicity HII regions (12+logO/H≥8.2, the upper branch of the O/H-R23 diagram) are considered in the present study. A relation of the type O/H=f(P, R23) between oxygen abundance and the value of abundance index R23, introduced by Pagel et al. (1979MNRAS.189...95P), and the excitation parameter P (which is defined here as the contribution of the radiation in [OIII] λλ4959, 5007 lines to the ``total" oxygen radiation) has been derived empirically using the available oxygen abundances determined via measurement of a temperature-sensitive line ratio [OIII]4959,5007/[OIII]4363 (Te-method). By comparing oxygen abundances in high-metallicity HII regions derived with the Te-method and those derived with the suggested relations (P-method), it was found that the precision of oxygen abundance determination with the P-method is around 0.1dex (the mean difference for the 38 HII regions considered is ∼0.08 dex) and is comparable to that of the Te-method. A relation of the type Te=f(P, R23) between electron temperature and the values of abundance index R23 and the excitation parameter P was derived empirically using the available electron temperatures determined via measurement of temperature-sensitive line ratios. The maximum value of differences between electron temperatures determined via measurement of temperature-sensitive line ratios and those derived with the suggested relation is around 1000K for HII regions considered here, the mean value of differences for 38 HII regions is ∼500K, which is the same order of magnitude as the uncertainties of electron temperature determinations in high-metallicity HII regions via measured temperature-sensitive line ratios.

Abstract Copyright:

Journal keyword(s): ISM: HII regions - galaxies: abundances - galaxies: ISM - galaxies: spiral

CDS comments: Table 1: C6w aperture not HII region

Simbad objects: 47

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Number of rows : 47

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 55 GiG 00 14 53.602 -39 11 47.86 8.54 8.58 7.87 7.84   ~ 712 2
2 NGC 281 HII 00 52 25.1 +56 33 54           ~ 229 1
3 NGC 300 GiG 00 54 53.4460065856 -37 41 03.182962667 8.83 8.69 8.13 7.46   ~ 1329 2
4 NGC 450 H2G 01 15 30.470 -00 51 38.98   13.4   13.3 13.2 ~ 205 0
5 NGC 588 HII 01 32 45.2 +30 38 54 14.59 14.40 14.44 14.89 15.16 ~ 117 1
6 NGC 604 HII 01 34 32.1 +30 47 01           ~ 551 0
7 [VSH98] NGC 925 -022+227 HII 02 27 15.0383 +33 38 33.000           ~ 3 0
8 NGC 925 H2G 02 27 16.913 +33 34 43.97   10.69 10.12 9.55   ~ 701 1
9 [WR97] 25 HII 03 18 03.50 -66 33 32.3           ~ 5 0
10 [WR97] 20 HII 03 18 05.30 -66 30 27.1           ~ 5 0
11 NGC 1313 G 03 18 16.046 -66 29 53.74   10.06 10.0 9.40 10.4 ~ 614 2
12 NGC 1491 HII 04 03 15.9 +51 18 54           ~ 107 1
13 [VHS97] UGC 2984-2 HII 04 13 12.0 +13 25 08           ~ 2 0
14 UGC 2984 LSB 04 13 12.403 +13 25 19.10   17       ~ 47 0
15 NGC 1569 IG 04 30 49.186 +64 50 52.52 11.72 11.86 11.03     ~ 1158 3
16 SH 2-212 HII 04 40 36.50 +50 27 44.3           ~ 92 2
17 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14998 1
18 M 42 HII 05 35 17.3 -05 23 28           ~ 3752 0
19 NAME Ori A MoC 05 38 -07.1           ~ 2698 0
20 NGC 2122 As* 05 48 55 -70 04.1     10.43     ~ 90 0
21 NGC 2359 HII 07 18 30.000 -13 13 36.00           ~ 158 0
22 HK NGC 2403 542 HII 07 36 19.9 +65 37 07           ~ 14 0
23 HK NGC 2403 313 HII 07 36 50.3 +65 36 45           ~ 8 0
24 NGC 2403 AGN 07 36 51.396 +65 36 09.17 9.31 8.84 8.38 8.19   ~ 1627 1
25 HK NGC 2403 270 Cl* 07 36 52.13 +65 36 48.5           ~ 22 0
26 [S75b] NGC 2403 2 HII 07 37 06.82 +65 36 38.7           ~ 37 0
27 HK NGC 2403 65 HII 07 37 19.5 +65 33 57           ~ 9 0
28 NGC 2467 HII 07 52 18 -26 25.7           ~ 175 1
29 [VSH98] NGC 2805 -068-079 HII 09 20 09.9286 +64 04 52.000           ~ 4 0
30 NGC 2805 GiP 09 20 20.3890361599 +64 06 10.699751669   11.9       ~ 192 1
31 [VSH98] NGC 2805 +037-115 HII 09 20 25.9413 +64 04 16.000           ~ 3 0
32 [VSH98] NGC 2805 +116-098 HII 09 20 37.9891 +64 04 33.000           ~ 4 0
33 UGC 5716 G 10 31 43.267 +25 18 27.40   17       ~ 64 0
34 [VHS97] UGC 5716-1 HII 10 31 44.4 +25 18 25           ~ 2 0
35 NGC 4228 SBG 12 15 39.174 +36 19 36.80 10.63 10.30 9.93 9.74   ~ 870 1
36 [H82] NGC 4214 11 Cl* 12 15 40.539 +36 19 30.25           ~ 10 0
37 HK NGC 4214 55 Cl* 12 15 40.7700 +36 19 11.060           ~ 12 0
38 NGC 4395 Sy2 12 25 48.8639154223 +33 32 48.694684028 10.84 10.54 10.11 9.98   ~ 1007 1
39 [VSH98] NGC 5457 -459-053 HII 14 02 20.0183 +54 20 02.000           ~ 5 0
40 [VSH98] NGC 5457 -347+276 HII 14 02 32.7359 +54 25 31.000           ~ 4 0
41 M 101 GiP 14 03 12.583 +54 20 55.50   8.46 7.86 7.76   ~ 2577 2
42 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 944 2
43 SH 2-49 HII 18 19.0 -13 52           ~ 31 1
44 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1491 0
45 NGC 7000 HII 20 58 47 +44 19.8           ~ 365 1
46 [WS83] NGC 55 7 HII ~ ~           ~ 2 0
47 [WS83] NGC 55 2 HII ~ ~           ~ 2 0

    Equat.    Gal    SGal    Ecl

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2020.10.29-21:12:21

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