Interstellar abundances in the neutral and ionized gas of NGC 604

Lebouteiller, V.; Kunth, D.; Lequeux, J.; Aloisi, Alessandra; Désert, Jean-Michel; Hébrard, G.; Étangs, A. Lecavelier des; Vidal‐Madjar, A.

doi:10.1051/0004-6361:20053161

Cited by 22 publications

(44 citation statements)

References 47 publications

(57 reference statements)

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“…The [Si/H] value we derive for the disk-halo interface of M33 is similar to that found by Lebouteiller et al (2006) for the H II region NGC 604 (i.e., S5) using Si II λ1020.7. Their value is [Si/X]=[-1.2, -0.2].…”

Section: CMsupporting

confidence: 84%

HST/Cos Observations of Ionized Gas Accretion at the Disk–halo Interface of M33

Zheng

Peek

Werk

et al. 2017

ApJ

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We report the detection of accreting ionized gas at the disk-halo interface of the nearby galaxy M33. We analyze HST/COS absorption-line spectra of seven ultraviolet-bright stars evenly distributed across the disk of M33. We find Si IV absorption components consistently redshifted relative to the bulk M33's ISM absorption along all the sightlines. The Si IV detection indicates an enriched, diskwide, ionized gas inflow toward the disk. This inflow is most likely multi-phase as the redshifted components can also be observed in ions with lower ionization states (e.g., S II, P II, Fe II, Si II). Kinematic modeling of the inflow is consistent with an accreting layer at the disk-halo interface of M33, which has an accretion velocity of 110 +15 −20 km s −1 at a distance of 1.5+1.0 −1.0 kiloparsec above the disk. The modeling indicates a total mass of ∼ 3.9 × 10 7 M for the accreting material at the diskhalo interface on the near side of the M33 disk , with an accretion rate of ∼ 2.9 M yr −1 . The high accretion rate and the level of metal-enrichment suggest the inflow is likely to be the fall back of M33 gas from a galactic fountain and/or the gas pulled loosed during a close interaction between M31 and M33. Our study of M33 is the first to unambiguously reveal the existence of a disk-wide, ionized gas inflow beyond the Milky Way, providing a better understanding of gas accretion in the vicinity of a galaxy disk.

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Section: CMsupporting

confidence: 84%

HST/Cos Observations of Ionized Gas Accretion at the Disk–halo Interface of M33

Zheng

Peek

Werk

et al. 2017

ApJ

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“…In fact, even though Ar i has an IP of 15.76 eV, i.e., above that of H i, Sofia & Jenkins (1998) proposed that the PICS of Ar i is such that it can be ionized into Ar ii when hydrogen is still in H i. The calculations of chemical abundances in the neutral gas of star-forming regions seem to agree with this proposal (see e.g., Lecavelier et al 2004;Lebouteiller et al 2004Lebouteiller et al , 2006. In addition, the study of the spatial variations of MIR features across NGC 3603 shows that the [Ar ii] line intensity correlates with that of the PDR tracers such as the PAHs, and not with the usual ionized gas tracers such as Lebouteiller et al 2007).…”

Section: Argon Ionization Structurementioning

confidence: 92%

Chemical Composition and Mixing in Giant HiiRegions: NGC 3603, 30 Doradus, and N66

Lebouteiller¹,

Bernard─Salas²,

Brandl³

et al. 2008

ApJ

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We investigate the chemical abundances of NGC 3603 in the Milky Way, of 30 Doradus in the Large Magellanic Cloud, and of N66 in the Small Magellanic Cloud. Mid-infrared observations with the Infrared Spectrograph on board the Spitzer Space Telescope allow us to probe the properties of distinct physical regions within each object, the central ionizing cluster, the surrounding ionized gas, photodissociation regions, and buried stellar clusters. We detect, and [Fe iii] lines and derive the ionic abundances. Based on the ionic abundance ratio ( Ne iii/H )/(S iii/H ), we find that the gas observed in the MIR is characterized by a lower degree of ionization than the gas observed in the optical spectra. We compute the elemental abundances of Ne, S, Ar, and Fe. We find that the -elements Ne, S, and Ar scale with each other. Our determinations agree well with the abundances derived from the optical. The Ne/S ratio is higher than the solar value in the three giant H ii regions and points toward a moderate depletion of sulfur on dust grains. We find that the neon and sulfur abundances display a remarkably small dispersion (0.11 dex in 15 positions in 30 Doradus), suggesting a relatively homogeneous ISM, even though smallscale mixing cannot be ruled out. Subject headingg s: H ii regions -infrared: ISM -ISM: atoms -ISM: individual ( NGC 3603, 30 Doradus, N66)

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“…Since we use the information from all available lines in the wavelength range, the error bar can be significantly smaller than when considering a single line. We refer to L04 and Lebouteiller et al (2006Lebouteiller et al ( , 2009) for more details. The comparison between the column densities we derive and the FUSE results asks for caution.…”

Section: Heavy Elementsmentioning

confidence: 99%

“…Uncertainties also remain in deriving column densities from absorption-lines in complex systems. Most FUSE studies of BCDs assumed a single absorption component arising from a single homogeneous line of sight with the exception of Mark 59 (Thuan et al 2002; see also Lebouteiller et al 2006 for the giant H  region NGC 604 in M 33). A more realistic approach would be to consider multiple lines of sight toward massive stars, each line of sight intersecting clouds with possibly different physical conditions (such as turbulent and radial velocity) and chemical properties.…”

Section: Introductionmentioning

confidence: 99%

“…A more realistic approach would be to consider multiple lines of sight toward massive stars, each line of sight intersecting clouds with possibly different physical conditions (such as turbulent and radial velocity) and chemical properties. Whenever individual absorption components are unresolved, it is almost impossible to tell whether they are saturated, in which case the column density inferred from the global absorption line can be severely underestimated (see e.g., Lebouteiller et al 2006). Following the suggestion of Kunth & Sargent (1986), Bowen et al (2005) got around the problem by deriving the abundances in the neutral gas of the dwarf spiral galaxy SBS 1543+593 along a quasar line of sight.…”

Section: Introductionmentioning

confidence: 99%

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Chemical enrichment and physical conditions in I Zw 18

Lebouteiller

Heap

Hubený

et al. 2013

A&A

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Context. Low-metallicity star-forming dwarf galaxies are prime targets to understand the chemical enrichment of the interstellar medium. The H  region contains the bulk of the mass in blue compact dwarfs, and it provides important constraints on the dispersal and mixing of heavy elements released by successive star-formation episodes. The metallicity of the H  region is also a critical parameter to investigate the future star-formation history, as metals provide most of the gas cooling that will facilitate and sustain star formation. Aims. Our primary objective is to study the enrichment of the H  region and the interplay between star-formation history and metallicity evolution. Our secondary objective is to constrain the spatial-and time-scales over which the H  and H  regions are enriched, and the mass range of stars responsible for the heavy element production. Finally, we aim to examine the gas heating and cooling mechanisms in the H  region. Methods. We observed the most metal-poor star-forming galaxy in the Local Universe, I Zw 18, with the Cosmic Origin Spectrograph onboard Hubble. The abundances in the neutral gas are derived from far-ultraviolet absorption-lines (H , C , C *, N , O , ...) and are compared to the abundances in the H  region. Models are constructed to calculate the ionization structure and the thermal processes. We investigate the gas cooling in the H  region through physical diagnostics drawn from the fine-structure level of C + . Results. We find that H  region abundances are lower by a factor of ∼2 as compared to the H  region. There is no differential depletion on dust between the H  and H  region. Using sulfur as a metallicity tracer, we calculate a metallicity of 1/46 Z (vs. 1/31 Z in the H  region). From the study of the C/O, [O/Fe], and N/O abundance ratios, we propose that C, N, O, and Fe are mainly produced in massive stars. We argue that the H  envelope may contain pockets of pristine gas with a metallicity essentially null. Finally, we derive the physical conditions in the H  region by investigating the C * absorption line. The cooling rate derived from C * is consistent with collisions with H 0 atoms in the diffuse neutral gas. We calculate the star-formation rate from the C * cooling rate assuming that photoelectric effect on dust is the dominant gas heating mechanism. Our determination is in good agreement with the values in the literature if we assume a low dust-to-gas ratio (∼2000 times lower than the Milky Way value).

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Interstellar abundances in the neutral and ionized gas of NGC 604

Cited by 22 publications

References 47 publications

HST/Cos Observations of Ionized Gas Accretion at the Disk–halo Interface of M33

HST/Cos Observations of Ionized Gas Accretion at the Disk–halo Interface of M33

Chemical Composition and Mixing in Giant HiiRegions: NGC 3603, 30 Doradus, and N66

Chemical enrichment and physical conditions in I Zw 18

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