Spatially resolving the dust properties and submillimetre excess in M 33

Relaño, M.; Looze, I. De; Kennicutt, Robert C.; Lisenfeld, U.; Dariush, Aliakbar; Verley, S.; Braine, J.; Tabatabaei, F. S.; Krämer, C.; Boquien, M.; Xilouris, E. M.; Gratier, P.

doi:10.1051/0004-6361/201732347

Cited by 29 publications

(43 citation statements)

References 87 publications

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“…The dust-to-molecular gas mass ratio instead follows two different trends based on the assumption on X CO : it increases with increasing T, from T = 1 to T = 10, when adopting a constant X CO (Left panel), while it increases from T = 1 to T = 4 but starts to decrease for T > 4 when assuming a metallicity-dependent X CO (Right panel). The assumption of a metallicity-dependent X CO better reproduces the expected decrease of the dust-to-total gas mass ratio (e.g., Draine et al 2007;Rémy-Ruyer et al 2014;Hunt et al 2015b;Relaño et al 2018;De Vis et al 2019), as the metal content decreases with T (as is also discussed below). However, the trend of dust-to-H 2 mass ratio versus T shown in the Right panel of Fig.…”

Section: Molecular-to-atomic Gas Mass Ratiomentioning

confidence: 83%

The ISM scaling relations in DustPedia late-type galaxies: A benchmark study for the Local Universe

Casasola

Bianchi

Vis

et al. 2020

A&A

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Aims. The purpose of this work is the characterization of the main scaling relations between all of the interstellar medium (ISM) components, namely dust, atomic, molecular, and total gas, and gas-phase metallicity, as well as other galaxy properties, such as stellar mass (M star ) and galaxy morphology, for late-type galaxies in the Local Universe. Methods. This study was performed by extracting late-type galaxies from the entire DustPedia sample and by exploiting the large and homogeneous dataset available thanks to the DustPedia project. The sample consists of 436 galaxies with morphological stage spanning from T = 1 to 10, M star from 6 × 10 7 to 3 × 10 11 M , star formation rate from 6 × 10 −4 to 60 M yr −1 , and oxygen abundance from 12 + log(O/H) = 8 to 9.5. Molecular and atomic gas data were collected from the literature and properly homogenized. All the masses involved in our analysis refer to the values within the optical disks of galaxies. The scaling relations involving the molecular gas are studied by assuming both a constant and a metallicity-dependent CO-to-H 2 conversion factor (X CO ). The analysis was performed by means of the survival analysis technique, in order to properly take into account the presence of both detection and nondetection in the data. Results. We confirm that the dust mass correlates very well with the total gas mass, and find -for the first time-that the dust mass correlates better with the atomic gas mass than with the molecular one. We characterize important mass ratios such as the gas fraction, the molecular-to-atomic gas mass ratio, the dust-to-total gas mass ratio (DGR), and the dust-to-stellar mass ratio, and study how they relate to each other, to galaxy morphology, and to gas-phase metallicity. Only the assumption of a metallicity-dependent X CO reproduces the expected decrease of the DGR with increasing morphological stage and decreasing gas-phase metallicity, with a slope of about 1. The DGR, the gas-phase metallicity, and the dust-to-stellar mass ratio are, for our galaxy sample, directly linked to galaxy morphology. The molecular-to-atomic gas mass ratio and the DGR show a positive correlation for low molecular gas fractions, but for galaxies rich in molecular gas this trend breaks down. To our knowledge, this trend has never been found before, and provides new constraints for theoretical models of galaxy evolution and a reference for high-redshift studies. We discuss several scenarios related to this finding. Conclusions. The DustPedia database of late-type galaxies is an extraordinary tool for the study of the ISM scaling relations, thanks to its homogeneous collection of data for the different ISM components. The database is made publicly available to the whole community.

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Section: Molecular-to-atomic Gas Mass Ratiomentioning

confidence: 83%

The ISM scaling relations in DustPedia late-type galaxies: A benchmark study for the Local Universe

Casasola

Bianchi

Vis

et al. 2020

A&A

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“…F mod (band), and F obs (band) are the corresponding modelled and observed fluxes in each band. the derivation of the gas-to-dust ratio mass maps is presented in Vílchez et al (2019) for M 101 and NGC 628 and Relaño et al (2018) for M 33.…”

Section: Spatially Resolved Studiesmentioning

confidence: 99%

“…In the right panels we show the radial variation of D tot (normalised to R 25 ), and in the left panels we show the variation of D tot as a function of metallicity. The observed data points have been derived using the gas-to-dust mass maps obtained previously in Vílchez et al (2019) for M 101 and NGC 628, and Relaño et al (2018) for M 33. We integrate these maps in elliptical rings of 0.1 R 25 width and take the mean value as the representative value for the gas-to-dust mass ratio in each ring.…”

Section: Dust To Gas Mass Ratio Versus Metallicity and Radiusmentioning

confidence: 99%

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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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“…These two effects may orig- All log q = 6. 75, 7, 7.25, 7.5, 7.75, 8, 8.25, 8.5 Z/Z = 0.3, 0.5, 1, 2, 3, 5 Σ Hα -selected HII regions Σ Hα -selected DIG regions inate from different aspects of dust attenuation, where the former reflects the different stars/dust geometry for H ii-and DIG-dominated populations (Kreckel et al 2013), and the latter implies the difference in dust properties (e.g., the size distribution of dust grains; Relaño et al 2018) Although most of the previous works attributed the integrated A V,star /A V,gas to the geometry effect (e.g., Price et al 2014;Reddy et al 2015;Koyama et al 2019), the conclusions drawn from Figure 5 imply that the local physical conditions of ionized gas may also have a significant effect on the A V,star /A V,gas ratio. The dust attenuation at wavelength λ (A λ ) along the line of sight s can be written as…”

Section: Dust Attenuations On the N2o2 Vs O32 Diagrammentioning

confidence: 99%

A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

Lin

Kong

2020

ApJ

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The state-of-the-art geometry models of stars/dust suggest that dust attenuation toward nebular regions (A V,gas ) is always larger than that of stellar regions (A V,star ). Utilizing the newly released integral field spectroscopic data from the Mapping Nearby Galaxies at Apache Point Observatory survey, we investigate whether and how the A V,star /A V,gas ratio varies from subgalactic to galactic scales. On a subgalactic scale, we report a stronger correlation between A V,star and A V,gas for more active H ii regions. The local A V,star /A V,gas is found to have moderate nonlinear correlations with three tracers of diffuse ionized gas (DIG), as well as indicators of gas-phase metallicity and ionization. The DIG regions tend to have larger A V,star /A V,gas compared to classic H ii regions excited by young OB stars. Metal-poor regions with a higher ionized level suffer much less nebular attenuation and thus have larger A V,star /A V,gas ratios. A low-A V,gas and high-A V,star /A V,gas sequence, which can be resolved into DIG-dominated and metal-poor regions, on the three BPT diagrams is found. Based on these observations, we suggest that besides the geometry of stars/dust, local physical conditions such as metallicity and ionized level also play an important role in determining the A V,star /A V,gas . On a galactic scale, the global A V,star /A V,gas ratio has strong correlations with stellar mass (M * ), moderate correlations with star formation rate (SFR) and metallicity, and weak correlations with inclination and specific SFR. Galaxies with larger M * and higher SFR that are more metal-rich tend to have smaller A V,star /A V,gas ratios. Such correlations form a decreasing trend of A V,star /A V,gas along the star-forming main sequence and mass-metallicity relation. The dust growth process accompanied by galaxy growth might be one plausible explanation for our observations.

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Spatially resolving the dust properties and submillimetre excess in M 33

Cited by 29 publications

References 87 publications

The ISM scaling relations in DustPedia late-type galaxies: A benchmark study for the Local Universe

The ISM scaling relations in DustPedia late-type galaxies: A benchmark study for the Local Universe

Evolution of grain size distribution in galactic discs

A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

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