Spatially Resolved 3 Micron Spectroscopy of IRAS 22272+5435: Formation and Evolution of Aliphatic Hydrocarbon Dust in Proto–Planetary Nebulae

Goto, Miwa; Gäessler, Wolfgang; Hayano, Yutaka; Iye, Masanori; Kamata, Yukiko; Kanzawa, Tomio; Kobayashi, Naoto; Minowa, Yosuke; Saint-Jacques, David; Takami, Hideki; Takato, Naruhisa; Terada, Hiroshi

doi:10.1086/368018

Cited by 62 publications

(64 citation statements)

References 63 publications

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“…Class A and B PAHs have been processed by the hard radiation of the central stars, suppressing the aliphatic component (e.g. Goto et al 2002Goto et al , 2003Goto et al , 2007. This agrees with the results of Pino et al (2008), who show that Class C sources, with a redshifted 6.2 μm feature, have a strong a strong aliphatic emission feature at 3.4 μm.…”

Section: Extending the Correlation Towards Cooler Starssupporting

confidence: 88%

When an old star smolders

Smolders¹,

Acke²,

Verhoelst³

et al. 2010

A&A

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Polycyclic aromatic hydrocarbons (PAHs) produce characteristic infrared emission bands that have been observed in a wide range of astrophysical environments, where carbonaceous material is subjected to ultraviolet (UV) radiation. Although PAHs are expected to form in carbon-rich AGB stars, they have up to now only been observed in binary systems where a hot companion provides a hard radiation field. In this letter, we present low-resolution infrared spectra of four S-type AGB stars, selected from a sample of 90 S-type AGB stars observed with the infrared spectrograph aboard the Spitzer satellite. The spectra of these four stars show the typical infrared features of PAH molecules. We confirm the correlation between the temperature of the central star and the centroid wavelength of the 7.9 μm feature, present in a wide variety of stars spanning a temperature range from 3000 to 12 000 K. Three of four sources presented in this paper extend this relation towards lower temperatures. We argue that the mixture of hydrocarbons we see in these S-stars has a rich aliphatic component. The fourth star, BZ CMa, deviates from this correlation. Based on the similarity with the evolved binary TU Tau, we predict that BZ CMa has a hot companion as well.

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Section: Extending the Correlation Towards Cooler Starssupporting

confidence: 88%

When an old star smolders

Smolders¹,

Acke²,

Verhoelst³

et al. 2010

A&A

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“…In fact, observational evidence strongly suggests that carbon dust consists of hydrogenated amorphous carbon (HAC or a-C:H) materials that form around evolved stars, metamorphose there (e.g., Goto et al 2003) and further evolve in the ISM (e.g., Jones et al 1990;Pino et al 2008;Jones 2009). HAC material could also form directly into the ISM from the UV processing of ice mantles after leaving the dense medium as suggested by Greenberg et al (1995) or via direct accretion of carbon and hydrogen (e.g.…”

Section: The Nature Of Interstellar Carbon Grainsmentioning

confidence: 99%

The global dust SED: tracing the nature and evolution of dust with DustEM

Compiègne

Verstraete

Jones

et al. 2010

A&A

394

724

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The Planck and Herschel missions are currently measuring the far-infrared to millimeter emission of dust, which combined with existing IR data, will for the first time provide the full spectral energy distribution (SED) of the galactic interstellar medium dust emission, from the mid-IR to the mm range, with an unprecedented sensitivity and down to spatial scales ∼30 . Such a global SED will allow a systematic study of the dust evolution processes (e.g. grain growth or fragmentation) that directly affect the SED because they redistribute the dust mass among the observed grain sizes. The dust SED is also affected by variations of the radiation field intensity. Here we present a versatile numerical tool, DustEM, that predicts the emission and extinction of dust grains given their size distribution and their optical and thermal properties. In order to model dust evolution, DustEM has been designed to deal with a variety of grain types, structures and size distributions and to be able to easily include new dust physics. We use DustEM to model the dust SED and extinction in the diffuse interstellar medium at high-galactic latitude (DHGL), a natural reference SED that will allow us to study dust evolution. We present a coherent set of observations for the DHGL SED, which has been obtained by correlating the IR and HI-21 cm data. The dust components in our DHGL model are (i) polycyclic aromatic hydrocarbons; (ii) amorphous carbon and (iii) amorphous silicates. We use amorphous carbon dust, rather than graphite, because it better explains the observed high abundances of gas-phase carbon in shocked regions of the interstellar medium. Using the DustEM model, we illustrate how, in the optically thin limit, the IRAS/Planck HFI (and likewise Spitzer/Herschel for smaller spatial scales) photometric band ratios of the dust SED can disentangle the influence of the exciting radiation field intensity and constrain the abundance of small grains (a < ∼ 10 nm) relative to the larger grains. We also discuss the contributions of the different grain populations to the IRAS, Planck (and similarly to Herschel) channels. Such information is required to enable a study of the evolution of dust as well as to systematically extract the dust thermal emission from CMB data and to analyze the emission in the Planck polarized channels. The DustEM code described in this paper is publically available.

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“…and with the likely irradiation effects and the associated aliphatic to aromatic transformation in the ISM (e.g., Jones 1990; Dartois et al 2004a,b;Pino et al 2008;Mennella 2008;Godard et al 2011), in circumstellar regions (e.g., Goto et al 2003Goto et al , 2007Sloan et al 2007;Pino et al 2008), in interplanetary dust particles (IDPs, Muñoz Caro et al 2006) and solar system organics (Dalle Ore et al 2011). Thus, the most physically-realistic carbonaceous grain materials, albeit inherently rather complex, would appear to be the extensive family of (hydrogenated) amorphous carbons, a-C(:H) 4 .…”

Section: Hydrogenated Amorphous Carbons A-c(:h)mentioning

confidence: 99%

The global dust modelling framework THEMIS

Jones

Koehler

Ysard

et al. 2017

A&A

248

345

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Here we introduce the interstellar dust modelling framework THEMIS (The Heterogeneous dust Evolution Model for Interstellar Solids), which takes a global view of dust and its evolution in response to the local conditions in interstellar media. This approach is built upon a core model that was developed to explain the dust extinction and emission in the diffuse interstellar medium. The model was then further developed to self-consistently include the effects of dust evolution in the transition to denser regions. The THEMIS approach is under continuous development and we are currently extending the framework to explore the implications of dust evolution in HII regions and the photon-dominated regions associated with star formation. We provide links to the THEMIS, DustEM and DustPedia websites where more information about the model, its input data and applications can be found.

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Spatially Resolved 3 Micron Spectroscopy of IRAS 22272+5435: Formation and Evolution of Aliphatic Hydrocarbon Dust in Proto–Planetary Nebulae

Cited by 62 publications

References 63 publications

When an old star smolders

When an old star smolders

The global dust SED: tracing the nature and evolution of dust with DustEM

The global dust modelling framework THEMIS

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