2006A&A...459..161L


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.12CEST17:20:54

2006A&A...459..161L - Astronomy and Astrophysics, volume 459, 161-174 (2006/11-3)

Interstellar abundances in the neutral and ionized gas of NGC604.

LEBOUTEILLER V., KUNTH D., LEQUEUX J., ALOISI A., DESERT J.-M., HEBRARD G., LECAVELIER DES ETANGS A. and VIDAL-MADJAR A.

Abstract (from CDS):

We present FUSE spectra of the giant H region NGC604 in the spiral galaxy M33. Chemical abundances are tentatively derived from far-UV absorption lines and compared to those derived from optical emission lines. Absorption lines from neutral hydrogen and heavy elements were observed against the continuum provided by the young massive stars embedded in the H region. We derived the column densities of H, N, O, Si, P, Ar, and Fe, fitting the line profiles with either a single component or several components. We used CLOUDY to correct for contamination from the ionized gas. Archival HST/STIS spectra across NGC604 allowed us to investigate how inhomogeneities affect the final H column density. Kinematics show that the neutral gas is physically related to the H region. The STIS spectra reveal H column density fluctuations up to 1dex across NCG604. Nevertheless, we find that the H column density determined from the global STIS spectrum does not differ significantly from the average over the individual sightlines. Our net results using the column densities derived with FUSE, assuming a single component, show that N, O, Si, and Ar are apparently underabundant in the neutral phase by a factor of ∼ 10 or more with respect to the ionized phase, while Fe is the same. However, we discuss the possibility that the absorption lines are made of individual unresolved components, and find that only P, Ar, and Fe lines should not be affected by the presence of hidden saturated components, while N, O, and Si might be much more affected. If N, O, and Si are actually underabundant in the neutral gas of NGC604 with respect to the ionized gas, this would confirm earlier results obtained for the blue compact dwarfs, and their interpretations. However, a deeper analysis focused on P, Ar, and Fe mitigates the above conclusion and indicates that the neutral gas and ionized gas could have similar abundances.

Abstract Copyright:

Journal keyword(s): galaxies: abundances - galaxies: starburst - ultraviolet: ISM - ISM: abundances - ISM: HII regions - ISM: individual objects: NGC604

CDS comments: Table 4: stars NNNa are not in Miskey et al. (2003AJ....125.3071M) except the star 578b not identified. These stars are not in SIMBAD.

Simbad objects: 13

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Number of rows : 13

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 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5149 1
2 NGC 604 HII 01 34 32.1 +30 47 01           ~ 545 0
3 NGC 625 AGN 01 35 04.632 -41 26 10.32 12.37 11.78 11.25 11.03 11.5 ~ 249 2
4 SBSG 0335-052 bCG 03 37 44.04 -05 02 38.5     16.65     ~ 435 1
5 NGC 1705 SBG 04 54 13.500 -53 21 39.82 12.32 12.96 12.56 12.58 12.9 ~ 597 1
6 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1742 1
7 * mu. Col V* 05 45 59.8953630749 -32 18 23.164726112 3.84 4.90 5.18 5.30 5.57 O9.5V 457 0
8 Mrk 116 PaG 09 34 02.1 +55 14 25           ~ 999 1
9 Mrk 209 bCG 12 26 16.02 +48 29 36.6   15.3       ~ 303 0
10 Mrk 59 AGN 12 59 00.288 +34 50 42.45           ~ 309 2
11 NGC 4861 H2G 12 59 02.340 +34 51 33.98   12.90 12.32     ~ 355 2
12 SBSG 1543+593 LSB 15 44 20.30 +59 12 24.2   17.5 16.9     ~ 51 2
13 * zet Oph Be* 16 37 09.5390545 -10 34 01.529471 1.73 2.58 2.56 2.46 2.50 O9.2IVnn 1729 2

    Equat.    Gal    SGal    Ecl

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2020.08.12-17:20:54

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