Dust properties in H II regions in M 33

Relaño, M.; Kennicutt, Robert C.; Lisenfeld, U.; Verley, S.; Hermelo, I.; Boquien, M.; Albrecht, M.; Krämer, C.; Braine, J.; Pérez-Montero, E.; Xilouris, E. M.; Kovács, A.; Staguhn, Johannes

doi:10.1051/0004-6361/201628139

Cited by 16 publications

(24 citation statements)

References 73 publications

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“…Such a trend may reflect a tendency for PAH destruction to occur in star-forming regions, where O stars supply high energy photons that photodestroy PAHs, and a significant fraction of the dust is exposed to starlight intensities high enough to elevate the L(70)/L dust ratio. Many studies have previously noted suppression of PAH emission in H II regions (e.g., Giard et al 1994;Helou et al 2004;Povich et al 2007;Relaño et al 2016). In a detailed study of PAH abundances in the Magellanic Clouds, Chastenet et al (2019) show that q PAH is reduced in regions close to sources of H-ionizing radiation.…”

Section: Resolved Trends Of Dl07 Parametersmentioning

confidence: 92%

Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample

Aniano

Draine

Hunt

et al. 2020

ApJ

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Dust and starlight are modeled for the KINGFISH project galaxies. With data from 3.6µm to 500µm, models are strongly constrained. For each pixel in each galaxy we estimate (1) dust surface density; (2) q PAH , the dust mass fraction in PAHs; (3) distribution of starlight intensities heating the dust; (4) luminosity emitted by the dust; and (5) dust luminosity from regions with high starlight intensity. The models successfully reproduce both global and resolved spectral energy distributions. We provide well-resolved maps for the dust properties. As in previous studies, we find q PAH to be an increasing function of metallicity, above a threshold Z/Z ≈ 0.15. Dust masses are obtained by summing the dust mass over the map pixels; these "resolved" dust masses are consistent with the masses inferred from model fits to the global photometry. The global dust-to-gas ratios obtained from

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Section: Resolved Trends Of Dl07 Parametersmentioning

confidence: 92%

Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample

Aniano

Draine

Hunt

et al. 2020

ApJ

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“…Draine & Li 2007;Compiègne et al 2011;Jones et al 2013). In Relaño et al (2016) we compared both Desert et al (1990) and Compiègne et al (2011) dust models and found that they both agree in reproducing the relative abundance of VSG and BG grains. Aoyama et al (2017) and Hou et al (2017) performed GADGET-3 SPH simulations (originally explained by Springel (2005)) of an isolated galaxy incorporating dust evolution mechanisms.…”

Section: Integrated Seds Of a Galaxy Samplementioning

confidence: 90%

Evolution of grain size distribution in galactic discs

Relaño

Lisenfeld

Hou

et al. 2020

A&A

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Context. Dust is formed out of stellar material and is constantly affected by different mechanisms occurring in the ISM. Dust grains behave differently under these mechanisms depending on their sizes, and therefore the dust grain size distribution also evolves as part of the dust evolution itself. Following how the grain size distribution evolves is a difficult computing task that is just recently being overtaking. Smoothed particle hydrodynamic (SPH) simulations of a single galaxy as well as cosmological simulations are producing the first predictions of the evolution of the dust grain size distribution. Aims. We compare for the first time the evolution of the dust grain size distribution predicted by the SPH simulations with the results provided by the observations. We are able to validate not only the predictions of the evolution of the small to large grain mass ratio (D S /D L ) within a galaxy, but also to give observational constraints for the recent cosmological simulations that include the grain size distribution in the dust evolution framework. Methods. We select a sample of three spiral galaxies with different masses: M 101, NGC 628 and M 33. We fit the dust spectral energy distribution (SED) across the disc of each object and derive the abundance of the different grain types included in the dust model. We analyse how the radial distribution of the relative abundance of the different grain size populations changes over the whole disc within each galaxy. The D S /D L ratio as a function of the galactocentric distance and metallicity is directly compared to what is predicted by the SPH simulations. Results. We find good agreement between the observed radial distribution of D S /D L and what is obtained from the SPH simulations of a single galaxy. The comparison agrees with the expected evolutionary stage of each galaxy. We show that the central parts of NGC 628, at high metallicity and with a high molecular gas fraction, are mainly affected not only by accretion but also by coagulation of dust grains. The centre of M 33, having lower metallicity and lower molecular gas fraction, presents an increase of the D S /D L ratio, showing that shattering is very effective in creating a large fraction of small grains. Finally, the observational results provided by our galaxies confirm the general relations predicted by the cosmological simulations based on the two grain size approximation. However, we present evidence that the simulations could be overestimating the amount of large grains in high massive galaxies.

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“…The high values of Y VSG /Y TOTAL and the corresponding low values of Y BG /Y TOTAL at location where the Hα luminosity is high, could be explained by the reprocessing of the BGs fragmenting into VSGs. Relaño et al (2016) shows that for a sample of H ii regions in M 33 catalogued in terms of morphology, the most intense regions tend to have a higher fraction of VSGs than the more diffuse shell-type H ii regions. The high velocity shocks occurring inside the most luminous H ii regions can destroy the BGs giving as consequence an increase of the VSG fraction.…”

Section: Grain Abundancesmentioning

confidence: 97%

“…Paradis et al 2011;Stephens et al 2014) and very small grains (VSGs) can coagulate on the surfaces of big grains (BGs) (Stepnik et al 2003;Paradis et al 2009;Köhler et al 2012). In an observational study Relaño et al (2016) (hereafter Paper I) found that the abundance of VSGs is higher in intense star-forming regions, where shocks might be present, than in more quiescent diffusetype H ii regions. Besides, it is also well known that the amount of polycyclic aromatic hydrocarbons (PAHs) are reduced in regions of intense ISRF (e.g.…”

Section: Introductionmentioning

confidence: 99%

Spatially resolving the dust properties and submillimetre excess in M 33

Relaño

Looze

Kennicutt

et al. 2018

A&A

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Context. The relative abundance of the dust grain types in the interstellar medium is directly linked to physical quantities that trace the evolution of galaxies. Because of the poor spatial resolution of the infrared/submillimetre data, we are able to study the dependence of the resolved infrared Spectral Energy Distribution (SED) across regions of the interstellar medium (ISM) with different physical properties in just a few objects. Aims. We study the dust properties of the whole disc of M 33 at spatial scales of ∼170 pc. This analysis allows us to infer how the relative dust grain abundance changes with the conditions of the ISM, study the existence of a submillimetre excess and look for trends of the gas-to-dust mass ratio (GDR) with other physical properties of the galaxy. Methods. For each pixel in the disc of M 33 we fit the infrared SED using a physically motivated dust model that assumes an emissivity index β close to 2. We apply a Bayesian statistical method to fit the individual SEDs and derive the best output values from the study of the probability density function of each parameter. We derive the relative amount of the different dust grains in the model, the total dust mass, and the strength of the interstellar radiation field (ISRF) heating the dust at each spatial location. Results. The relative abundance of very small grains (VSGs) tends to increase, and for big grains (BGs) to decrease, at high values of Hα luminosity. This shows that the dust grains are modified inside the star-forming regions, in agreement with a theoretical framework of dust evolution under different physical conditions. The radial dependence of the GDR is consistent with the shallow metallicity gradient observed in this galaxy. The strength of the ISRF derived in our model correlates with the star formation rate (SFR) in the galaxy in a pixel by pixel basis. Although this is expected it is the first time that a correlation between both quantities is reported. We produce a map of submillimetre excess in the 500 µm SPIRE band for the disc of M 33. The excess can be as high as 50% and increases at large galactocentric distances. We further study the relation of the excess with other physical properties of the galaxy and find that the excess is prominent in zones of diffuse ISM outside the main star-forming regions, where the molecular gas and dust surface density are low.

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Dust properties in H II regions in M 33

Cited by 16 publications

References 73 publications

Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample

Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample

Evolution of grain size distribution in galactic discs

Spatially resolving the dust properties and submillimetre excess in M 33

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