2002A&A...381..606M


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.25CET21:01:58

2002A&A...381..606M - Astronomy and Astrophysics, volume 381, 606-627 (2002/1-2)

ISO spectroscopy of compact HII regions in the Galaxy. II. Ionization and elemental abundances.

MARTIN-HERNANDEZ N.L., PEETERS E., MORISSET C., TIELENS A.G.G.M., COX P., ROELFSEMA P.R., BALUTEAU J.-P., SCHAERER D., MATHIS J.S., DAMOUR F., CHURCHWELL E. and KESSLER M.F.

Abstract (from CDS):

Based on the ISO spectral catalogue of compact HII regions by Peeters et al. (2002A&A...381..571P) we present a first analysis of the hydrogen recombination and atomic fine-structure lines originated in the ionized gas. The sample consists of 34 HII regions located at galactocentric distances between RGal=0 and 15kpc. The SWS HI recombination lines between 2 and 8µm are used to estimate the extinction law at these wavelengths for 14 HII regions. An extinction in the K band between 0 and ∼3mag has been derived. The fine-structure lines of N, O, Ne, S and Ar are detected in most of the sources. Most of these elements are observed in two different ionization stages probing a range in ionization potential up to 41eV. The ISO data, by itself or combined with radio data taken from the literature, is used to derive the elemental abundances relative to hydrogen. The present data thus allow us to describe for each source its elemental abundance, its state of ionization and to constrain the properties of the ionizing star(s). The main results of this study are as follows. The ionization ratios Ar++/Ar+, N++/N+, S+3/S++ and Ne++/Ne+, which measure the degree of ionization and to first order, the hardness of the stellar radiation, seem to increase with RGal. These ionization ratios correlate well with each other, implying that the spectral hardening affects equally the full range of ionizing energies. A Galactocentric gradient of N/O (ΔlogN/O=-0.056±0.009dex/kpc) is observed in the sense of a decreasing abundance ratio with RGal in agreement with previous studies. Abundance gradients for neon and argon are derived of the form Δlog Ne/H=-0.039±0.007dex/kpc and Δlog(Ar/H)=-0.045±0.011dex/kpc. These elemental gradients could be enlarged by the existing Galactic Te gradient. Adopting a Te gradient of approximately 330K/kpc, the slopes in the Ne/H and Ar/H gradients become -0.06 and -0.07dex/kpc, respectively. Lower limits for the sulphur and oxygen abundances are derived. Nitrogen abundances are derived for 16 sources.

Abstract Copyright:

Journal keyword(s): ISM: abundances - ISM: dust, extinction - ISM: HII regions - galaxy: abundances - infrared: ISM: lines - atomic data

Simbad objects: 35

goto Full paper

goto View the reference in ADS

Number of rows : 35

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 GAL 124.64+02.54 HII 01 07 50.70 +65 21 21.4           ~ 42 0
2 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 330 0
3 [BNM96] 289.880-0.799 HII 11 00 59.4870059429 -60 50 22.774209522           ~ 35 0
4 GRS G291.86 -00.68 HII 11 16 33.8 -61 29 59           ~ 20 0
5 ESO 95-1 HII 12 09 01.260 -63 15 59.63     16.00     ~ 92 2
6 IRAS 12073-6233 mul 12 10 00.4 -62 49 57           ~ 48 0
7 [GS70] 298.2-00.3 HII 12 10 01.886 -62 50 00.46           ~ 65 1
8 IRAS 12331-6134 HII 12 36 01.9 -61 51 04           ~ 22 0
9 IRAS 15384-5348 HII 15 42 17.787 -53 58 30.88           ~ 37 1
10 IRAS 15502-5302 HII 15 54 07.2 -53 11 20           ~ 44 0
11 MSX6C G332.1544-00.4487 HII 16 16 40.776 -51 17 06.36           ~ 35 1
12 GAL 350.10+00.09 HII 17 19 26.1 -37 10 54           ~ 30 0
13 GAL 351.46-00.44 HII 17 25 31.7 -36 21 54           ~ 23 0
14 IRAS 17279-3350 HII 17 31 18.0 -33 52 50           ~ 23 0
15 NAME Sgr C MoC 17 44 36.3 -29 28 13           ~ 318 0
16 NAME Sgr D HII HII 17 48 41.79 -28 01 41.3           ~ 63 1
17 GAL 007.47+00.06 HII 18 02 13.0 -22 27 52           ~ 37 0
18 GAL 009.62+00.19 HII 18 06 13.9 -20 31 44           ~ 188 0
19 GAL 013.88+00.28 HII 18 14 35.2 -16 45 21           ~ 54 0
20 NAME HH 80-81 IRS HII 18 19 11.8 -20 47 35           ~ 135 0
21 [WAM82] 023.955+0.152 HII 18 34 24.9 -07 54 50           ~ 70 1
22 GAL 029.96-00.02 Y*O 18 46 03.7 -02 39 21           ~ 336 1
23 GAL 031.40-00.26 HII 18 49 32.1 -01 29 04           ~ 43 0
24 RAFGL 5536 HII 18 50 30.8 -00 01 59           ~ 40 0
25 [WWB83] G033.91+0.11 HII 18 52 50.4 +00 55 29           ~ 90 1
26 GAL 049.20-00.35 Cl* 19 23 02.1 +14 16 40           ~ 64 0
27 SH 2-87 HII 19 46 20.7 +24 35 15           ~ 152 2
28 W 58a HII 20 01 45.8 +33 32 43           ~ 278 4
29 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 959 0
30 IRAS 21190+5140 HII 21 20 44.8 +51 53 28           ~ 128 2
31 IRAS 21270+5423 IR 21 28 42.0 +54 36 51           ~ 18 1
32 SH 2-128 HII 21 32 10.393 +55 52 42.36   10.8       ~ 164 3
33 SH 2-138 HII 22 32 45.7 +58 28 20           ~ 108 2
34 IC 1470 HII 23 05 09.9 +60 14 31   11.5       ~ 168 1
35 SH 2-159 Y*O 23 15 31.27440 +61 07 10.4450           ~ 176 2

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2002A&A...381..606M and select 'bookmark this link' or equivalent in the popup menu


2021.02.25-21:01:58

© Université de Strasbourg/CNRS

    • Contact