A photoionization model of the spatial distribution of the optical and mid-infrared properties in NGC 595

Montero, E. Pérez; Relaño, M.; Vı́lchez, J. M.; Monreal-Ibero, A.

doi:10.1111/j.1365-2966.2010.17941.x

Cited by 9 publications

(18 citation statements)

References 51 publications

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“…However, the general picture is far from this simple one-to-one association. For example, Pérez-Montero et al (2011) studied a sample of BCD galaxies that are N-overabundant over large areas supporting the idea of enrichment caused by accretion of less chemically processed gas (see also Kehrig et al 2008). A similar result was found by Amorín et al (2012) for a set of BCD galaxies at higher redshift.…”

Section: On the Relationship Between Extra N And Wr Starssupporting

confidence: 56%

“…At present, the astronomical community is still in the process of understanding under which conditions these can be applied to small portions of them (e.g. Pérez-Montero et al 2011;Ercolano et al 2012). The areas analyzed in this section will be closer to this notion of complete H ii region than individual spaxels.…”

Section: Gaseous Emission In Selected Aperturesmentioning

confidence: 99%

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The ionized gas in the central region of NGC 5253

Monreal-Ibero

Walsh

Vı́lchez

2012

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Context. Blue compact dwarf (BCD) galaxies constitute the ideal laboratories to test the interplay between massive star formation and the surrounding gas. As one of the nearest BCD galaxies, NGC 5253 was previously studied with the aim to elucidate in detail the starburst interaction processes. Some open issues regarding the properties of its ionized gas still remain to be addressed. Aims. The 2D structure of the main physical and chemical properties of the ionized gas in the core of NGC 5253 has been studied. Methods. Optical integral field spectroscopy (IFS) data has been obtained with FLAMES Argus and lower resolution gratings of the Giraffe spectrograph. Results. We derived 2D maps for different tracers of electron density (n e ), electron temperature (T e ) and ionization degree.

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Section: On the Relationship Between Extra N And Wr Starssupporting

confidence: 56%

Section: Gaseous Emission In Selected Aperturesmentioning

confidence: 99%

The ionized gas in the central region of NGC 5253

Monreal-Ibero

Walsh

Vı́lchez

2012

A&A

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“…We used the same methodology and geometrical approach assumed for the modelling of NGC 595 that was carried out by Pérez-Montero et al (2011a). This consists of the direct comparison between the transmitted spectra predicted by the models in each annulus, as defined over the shell, and the IFS observed spectra in the same regions.…”

Section: Mb Thin-shell Geometry Modelsmentioning

confidence: 99%

“…This is done to derive physical properties and chemical abundances by means of photoionisation models of the well-studied GH iiR NGC 588. To do so, we took two different assumptions: i) an improved version of the approach employed by Pérez-Montero et al (2011a) for NGC 595, based on different models for the individual observed spatial elements which are used to explain the observations that are caused by azimuthal variations of its properties throughout the field of view and ii) a single model projected onto the sky which is used to explain the variations as a consequence of the perspective. In the next section, we describe the 2D structure of NGC 588 and the data sampling of the spatial distribution for both optical and mid-IR data studied in MI11 and the derivation of the integrated dust-to-gas ratio from dust temperature and total H i mass.…”

Section: Introductionmentioning

confidence: 99%

“…This is the case of the codes, NEBU_3D (Morisset et al 2005) or Cloudy 3D (Morisset 2006). In a novel approach to reproduce IFS data, Pérez-Montero et al (2011a) use 1D photoionisation models to fit the optical IFS ) and 8 μm and 24 μm mid-IR Spitzer bands properties of the giant H ii region (GH iiR) NGC 595 in the disc of M33. In that work, different annuli around the ionising source are defined in the area covered by a mosaic of several integral field unit (IFU) pointings, and their measured integrated properties are later fitted by the models.…”

Section: Introductionmentioning

confidence: 99%

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The giant H ii region NGC 588 as a benchmark for 2D photoionisation models

Montero

Monreal-Ibero

Relaño

et al. 2014

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Aims. We use optical integral field spectroscopy and 8 μm and 24 μm mid-IR observations of the giant H ii region NGC 588 in the disc of M33 as input and constraints for two-dimensional tailor-made photoionisation models under different geometrical approaches. We do this to explore the spatial distribution of gas and dust in the interstellar, ionised medium surrounding multiple massive stars. Methods. Two different geometrical approaches are followed for the modelling structure: i) Each spatial element of the emitting gas is studied individually using models, which assume that the ionisation structure is complete in each element, to look for azimuthal variations across gas and dust. ii) A single model is considered, and the two-dimensional structure of the gas and the dust are assumed to be due to the projection of an emitting sphere onto the sky.Results. The models in both assumptions reproduce the radial profiles of Hβ surface brightness, the observed number of ionising photons, and the strong optical emission-line relative intensities. The first approach produces a constant-density, matter-bounded thin shell of variable thickness and dust-to-gas ratio, while the second gives place to a radiation-bounded, thick shell sphere of decreasing particle density. However, the radial profile of the 8 μm/24 μm IR ratio, depending on the gas and dust geometry, only fits well when the thick-shell model is used. The resulting dust-to-gas mass ratio, which was obtained empirically from the derived dust mass using data from Spitzer, also has a better fit using the thick-shell solution. In both approaches, models support the importance of the low surface-brightness positions on the integrated spectrum of the nebula, the chemical homogeneity, the ionisation-parameter radial decrease, and the robustness of strong-line methods to derive the equivalent effective temperature in extended regions. These results must be taken with care in view of the very low extinction values that are derived from the IR, as compared to that derived from the Balmer decrement. Besides, the IR can be possibly contaminated with the emission from a cloud of diffuse gas and dust above the plane of the galaxy detected at 250 μm Herschel image.

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Dust properties in H II regions in M 33

Relaño

Kennicutt

Lisenfeld

et al. 2016

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Context. The infrared emission (IR) of the interstellar dust has been claimed to be a tracer of the star formation rate. However, the conversion of the IR emission into star formation rate can be strongly dependent on the physical properties of the dust, which are affected by the environmental conditions where the dust is embedded. Aims. We study here the dust properties of a set of H ii regions in the Local Group Galaxy M 33 presenting different spatial configurations between the stars, gas and dust to understand the dust evolution under different environments. Methods. We model the SED of each region using the DustEM tool and obtain the mass relative to hydrogen for Very Small Grains (Y VSG ), Polycyclic Aromatic Hydrocarbons (Y PAH ) and Big Grains (Y BG ). We furthermore perform a pixel-by-pixel SED modelling and derive maps of relative mass of each grain type for the whole surface of the two most luminous H ii regions in M 33, NGC 604 and NGC 595. Results. The relative mass of the VSGs (Y VSG /Y TOTAL ) changes with the morphology of the region: Y VSG /Y TOTAL is a factor of ∼1.7 higher for H ii regions classified as filled and mixed than for regions presenting a shell structure. The enhancement of VSGs within NGC 604 and NGC 595 is correlated to expansive gas structures with velocities ≥50 km s −1 . The gas-to-dust ratio derived for the H ii regions in our sample exhibits two regimes related to the H i−H 2 transition of the ISM. Regions corresponding to the H i diffuse regime present a gas-to-dust ratio compatible with the expected value if we assume that the gas-to-dust ratio scales linearly with metallicity, while regions corresponding to a H 2 molecular phase present a flatter dust-gas surface density distribution. Conclusions. The fraction of VSGs can be affected by the conditions of the interstellar environment: strong shocks of ∼ 50-90 km s −1 existing in the interior of the most luminous H ii regions can lead to fragmentation of BGs into smaller ones, while the more evolved shell and clear shell objects provide a more quiescent environment where reformation of dust BG grains might occur. The gas-to-dust variations found in this analysis might imply that grain coagulation and/or gas-phase metals incorporation to the dust mass is occurring in the interior of the H ii regions in M 33.

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A photoionization model of the spatial distribution of the optical and mid-infrared properties in NGC 595

Cited by 9 publications

References 51 publications

The ionized gas in the central region of NGC 5253

The ionized gas in the central region of NGC 5253

The giant H ii region NGC 588 as a benchmark for 2D photoionisation models

Dust properties in H II regions in M 33

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