Dust evolution across the Horsehead nebula

Schirmer, T.; Abergel, A.; Verstraete, L.; Ysard, N.; Juvela, M.; Jones, A. P.; Habart, E.

doi:10.1051/0004-6361/202037937

Cited by 22 publications

(24 citation statements)

References 96 publications

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“…Based on Herschel and Spitzer observations of the Horsehead together with the THEMIS 3 dust model (Jones et al 2013(Jones et al , 2017, Schirmer et al (2020) show a strong depletion of nano-grains in the irradiated outer part of this PDR. The nano-grain dust-to-gas ratio is 6-10 times lower and the minimum size of these grains is 2-2.25 times larger than in the diffuse ISM.…”

Section: Parametrisation Of Nano-grain Depletion In Thementioning

confidence: 96%

“…Flagey et al 2009;Ysard et al 2013Ysard et al , 2016Juvela et al 2020;Saajasto et al 2021) and most specifically in PDRs (e.g. Berné et al 2007;Abergel et al 2010;Pilleri et al 2012;Arab et al 2012;Van De Putte et al 2019;Schirmer et al 2020). Based on the Spitzer and Herschel observation together with the THEMIS dust model (Jones et al 2013(Jones et al , 2017 and the radiative transfer code SOC (Juvela 2019), Schirmer et al (2020) constrained the dust properties in the Horsehead nebula.…”

Section: Introductionmentioning

confidence: 99%

“…Berné et al 2007;Abergel et al 2010;Pilleri et al 2012;Arab et al 2012;Van De Putte et al 2019;Schirmer et al 2020). Based on the Spitzer and Herschel observation together with the THEMIS dust model (Jones et al 2013(Jones et al , 2017 and the radiative transfer code SOC (Juvela 2019), Schirmer et al (2020) constrained the dust properties in the Horsehead nebula. They found that in the outer irradiated part of the Horsehead (i.e.…”

Section: Introductionmentioning

confidence: 99%

“…We show the influence of the nano-grain depletion in the outer irradiated part of the Horsehead (Schirmer et al 2020) on the physics and chemistry of this region using the Meudon PDR code (Le Petit et al 2006). The paper is organised as follows.…”

Section: Introductionmentioning

confidence: 99%

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Influence of the nano-grain depletion in photon-dominated regions: Application to the gas physics and chemistry in the Horsehead

Schirmer,

Habart,

Ysard

et al. 2021

Preprint

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Context. The large disparity in physical conditions from the diffuse interstellar medium (ISM) to denser clouds such as photondominated regions (PDRs) triggers an evolution of the dust properties (i.e. composition, size, and shape). The gas physics and chemistry are tightly connected to these dust properties and are therefore affected by dust evolution and especially the nano-grain depletion in the outer irradiated part of PDRs. Aims. We highlight the influence of nano-grain depletion on the gas physics and chemistry in the Horsehead nebula, a prototypical PDR. Methods. We used a model for atomic and molecular gas in PDRs, the Meudon PDR code, using diffuse ISM-like dust and Horseheadlike dust to study the influence of nano-grain depletion on the gas physics and chemistry, focusing on the impact on photoelectric heating and H2 formation and, therefore, on the H 2 gas lines. Results. We find that nano-grain depletion in the Horsehead strongly affects gas heating through the photoelectric effect and thus the gas temperature and the H 2 formation, hence the H → H 2 position. Consequently, the first four pure rotational lines of H 2 (e.g. 0-0 S(0), S(1), S(2), and S(3)) vary by a factor of 2 to 14. The 0-0 S(3) line that is often underestimated in models is underestimated even more when taking nano-grain depletion into account due to the decrease in gas heating through the photoelectric effect. This strongly suggests that our understanding of the excitation of H 2 and/or of heating processes in the Horsehead, and more generally in PDRs, is still incomplete. Conclusions. Nano-grain depletion in the outer part of the Horsehead has a strong influence on several gas tracers that will be prominent in JWST observations of irradiated clouds. We therefore need to take this depletion into account in order to improve our understanding of the Horsehead, and more generally PDRs, and to contribute to the optimal scientific return of the mission.

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Section: Parametrisation Of Nano-grain Depletion In Thementioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Influence of the nano-grain depletion in photon-dominated regions: Application to the gas physics and chemistry in the Horsehead

Schirmer,

Habart,

Ysard

et al. 2021

Preprint

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“…Such continuous replenishment of dust from disk accretion is likely combined with other local processes like the regeneration of nm-sized grains by the partial photo-fragmentation of larger aggregates (Schirmer et al 2020). Photo-fragmentation is expected to liberate, from one larger grain (e.g., mm-sized), billions of hot nano-particles that will thus dominate the IR emission.…”

Section: Two Separated Grain Populationsmentioning

confidence: 99%

First MATISSE L-band observations of HD 179218

Кокоулина

Matter

López

et al. 2021

A&A

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Context. Carbon is one of the most abundant components in the Universe. While silicates have been the main focus of solid phase studies in protoplanetary discs (PPDs), little is known about the solid carbon content especially in the planet-forming regions (~0.1–10 au). Fortunately, several refractory carbonaceous species present C-H bonds (such as hydrogenated nano-diamond and amorphous carbon as well as polycyclic aromatic hydrocarbons), which generate infrared (IR) features that can be used to trace the solid carbon reservoirs. The new mid-IR instrument MATISSE, installed at the Very Large Telescope Interferometer (VLTI), can spatially resolve the inner regions (~1–10 au) of PPDs and locate, down to the au-scale, the emission coming from carbon grains. Aims. Our aim is to provide a consistent view on the radial structure, down to the au-scale, as well as basic physical properties and the nature of the material responsible for the IR continuum emission in the inner disk region around HD 179218. Methods. We implemented a temperature-gradient model to interpret the disk IR continuum emission, based on a multiwavelength dataset comprising a broadband spectral energy distribution and VLTI H-, L-, and N-bands interferometric data obtained in low spectral resolution. Then, we added a ring-like component, representing the carbonaceous L-band features-emitting region, to assess its detectability in future higher spectral resolution observations employing mid-IR interferometry. Results. Our temperature-gradient model can consistently reproduce our dataset. We confirmed a spatially extended inner 10 au emission in H- and L-bands, with a homogeneously high temperature (~1700 K), which we associate with the presence of stochastically heated nano-grains. On the other hand, the N-band emitting region presents a ring-like geometry that starts at about 10 au with a temperature of 400 K. Moreover, the existing low resolution MATISSE data exclude the presence of aromatic carbon grains (i.e., producing the 3.3 μm feature) in close proximity tothe star (≲1 au). Future medium spectral resolution MATISSE data will confirm their presence at larger distances. Conclusions. Our best-fit model demonstrates the presence of two separated dust populations: nano-grains that dominate the near- to mid-IR emission in the inner 10 au region and larger grains that dominate the emission outward. The presence of such nano-grains in the highly irradiated inner 10 au region of HD 179218 requires a replenishment process. Considering the expected lifetime of carbon nano-grains from The Heterogeneous dust Evolution Model for Interstellar Solids (THEMIS model), the estimated disk accretion inflow of HD 179218 could significantly contribute to feed the inner 10 au region in nano-grains.Moreover, we also expect a local regeneration of those nano-grains by the photo-fragmentation of larger aggregates.

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A nearby galaxy perspective on dust evolution

Galliano

Nersesian

Bianchi

et al. 2021

A&A

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Context. The efficiency of the different processes responsible for the evolution of interstellar dust on the scale of a galaxy are, to date, very uncertain, spanning several orders of magnitude in the literature. Yet, precise knowledge of the grain properties is key to addressing numerous open questions about the physics of the interstellar medium and galaxy evolution. Aims. This article presents an empirical statistical study, aimed at quantifying the timescales of the main cosmic dust evolution processes as a function of the global properties of a galaxy. Methods. We modeled a sample of ≃800 nearby galaxies, spanning a wide range of metallicities, gas fractions, specific star formation rates, and Hubble stages. We derived the dust properties of each object from its spectral energy distribution. Through an additional level of analysis, we inferred the timescales of dust condensation in core-collapse supernova ejecta, grain growth in cold clouds, and dust destruction by shock waves. Throughout this paper, we have adopted a hierarchical Bayesian approach, resulting in a single large probability distribution of all the parameters of all the galaxies, to ensure the most rigorous interpretation of our data. Results. We confirm the drastic evolution with metallicity of the dust-to-metal mass ratio (by two orders of magnitude), found by previous studies. We show that dust production by core-collapse supernovae is efficient only at very low metallicity, a single supernova producing on average less than ≃0.03 M⊙/SN of dust. Our data indicate that grain growth is the dominant formation mechanism at metallicity above ≃1/5 solar, with a grain growth timescale shorter than ≃50 Myr at solar metallicity. Shock destruction is relatively efficient, a single supernova clearing dust on average in at least ≃1200 M⊙/SN of gas. These results are robust when assuming different stellar initial mass functions. In addition, we show that early-type galaxies are outliers in several scaling relations. This feature could result from grain thermal sputtering in hot X-ray emitting gas, which is a hypothesis supported by a negative correlation between the dust-to-stellar mass ratio and the X-ray photon rate per grain. Finally, we confirm the well-known evolution of the aromatic-feature-emitting grain mass fraction as a function of metallicity and interstellar radiation field intensity. Our data indicate that the relation with metallicity is significantly stronger. Conclusions. Our results provide valuable constraints for simulations of galaxies. They imply that grain growth is the likely dust production mechanism in dusty high-redshift objects. We also emphasize the determinant role of local, low metallicity systems in order to address these questions.

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Dust evolution across the Horsehead nebula

Cited by 22 publications

References 96 publications

Influence of the nano-grain depletion in photon-dominated regions: Application to the gas physics and chemistry in the Horsehead

Influence of the nano-grain depletion in photon-dominated regions: Application to the gas physics and chemistry in the Horsehead

First MATISSE L-band observations of HD 179218

A nearby galaxy perspective on dust evolution

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