Freshly Formed Dust in the Cassiopeia A Supernova Remnant as Revealed by the<i>Spitzer Space Telescope</i>

Rho, Jeonghee; Kozasa, Takashi; Reach, W. T.; Smith, John David; Rudnick, Lawrence; DeLaney, Tracey; Ennis, J.; Gomez, Haley Louise; Tappe, Achim

doi:10.1086/523835

Cited by 239 publications

(414 citation statements)

References 46 publications

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“…Using the data from Rho et al (2008), it is straightforward to estimate the dust mass in each pixel of the Spitzer map of the Cas A. Its comparison with the optical image of this supernova remnant allows us to determine the dust-to-gas mass ratio in If the emitting dust with temperature T d ≈ 100 K (Rho et al 2008) is distributed over the entire volume of the knot, then the dust-to-gas mass ratio is of the order of 2-5%.…”

Section: Effects Of the Dust On The Post-shock Pir Structurementioning

confidence: 99%

“…Its comparison with the optical image of this supernova remnant allows us to determine the dust-to-gas mass ratio in If the emitting dust with temperature T d ≈ 100 K (Rho et al 2008) is distributed over the entire volume of the knot, then the dust-to-gas mass ratio is of the order of 2-5%. If, on the other hand, the dust emits only in the line-emitting regions, then the dust-to-gas mass ratio is of the order of unity.…”

Section: Effects Of the Dust On The Post-shock Pir Structurementioning

confidence: 99%

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Fine-structure infrared lines from the Cassiopeia A knots

Docenko

Sunyaev

2010

A&A

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Aims. Archival observations of infrared fine-structure lines of the young Galactic supernova remnant Cassiopeia A allow us to test existing models and determine the physical parameters of various regions of the fast-moving knots, which are metal-dominated clouds of material ejected by the supernova explosion. Spitzer data are used to determine the fluxes of the O, Ne, Si, S, Ar, and Fe ion fine-structure lines originating in the fast-moving knots. The ratios of these line fluxes are used as plasma diagnostics. We also determine the infrared line flux ratios with respect to the optical [O iii] 5007 Å line in the knots with previously measured reddening. Additionally, we analyze several optical and near-infrared observations of the fast-moving knots to obtain clearer insight into the post-shock photoionized region structure. Results. We show that the infrared oxygen line flux predictions of all existing theoretical models are correct only to within a factor of a several. Comparison of the model predictions shows that to reproduce the observations it is essential to include the effects of the electron conductivity and dust. Detailed analysis of the diagnostic line flux ratios of various ions allows us to qualitatively confirm the general model of fast-moving knot emission and determine observationally for the first time the physical conditions in the photoionized region after the shock. We infer from the [O iii] line flux ratios that the pre-shock cloud densities are higher than assumed in existing theoretical models and most probably correspond to several hundred particles per cm 3 . We also determine the Cas A luminosity in the infrared continuum and lines. We show that accounting for the charge exchange processes in the post-shock photoionized region allows us to reproduce most of the relevant spectral line ratios even in the frame of a single-temperature model of this region. We also estimate its plasma parameters, thickness, and carbon abundance.

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Section: Effects Of the Dust On The Post-shock Pir Structurementioning

confidence: 99%

Section: Effects Of the Dust On The Post-shock Pir Structurementioning

confidence: 99%

Fine-structure infrared lines from the Cassiopeia A knots

Docenko

Sunyaev

2010

A&A

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“…These silicate dust particles are thought to be mainly produced in oxygen-rich asymptotic giant branch (AGB) stars (e.g., Gail et al 2009). Besides AGB stars, other sources such as novae, supernovae type II (Wooden et al 1993;Rho et al 2008Rho et al , 2009), young stellar objects (Dwek & Scalo 1980), and red giant stars (Nittler et al 1997) can produce silicate dust. Even dust formation in the ISM may occur in interstellar clouds (Jones & Nuth 2011).…”

Section: Introductionmentioning

confidence: 99%

Absorption and scattering by interstellar dust in the silicon K-edge of GX 5-1

Zeegers

Costantini

Vries

et al. 2017

A&A

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Context. We study the absorption and scattering of X-ray radiation by interstellar dust particles, which allows us to access the physical and chemical properties of dust. The interstellar dust composition is not well understood, especially on the densest sight lines of the Galactic Plane. X-rays provide a powerful tool in this study. Aims. We present newly acquired laboratory measurements of silicate compounds taken at the Soleil synchrotron facility in Paris using the Lucia beamline. The dust absorption profiles resulting from this campaign were used in this pilot study to model the absorption by interstellar dust along the line of sight of the low-mass X-ray binary (LMXB) GX 5-1. Methods. The measured laboratory cross-sections were adapted for astrophysical data analysis and the resulting extinction profiles of the Si K-edge were implemented in the SPEX spectral fitting program. We derive the properties of the interstellar dust along the line of sight by fitting the Si K-edge seen in absorption in the spectrum of GX 5-1. Results. We measured the hydrogen column density towards GX 5-1 to be 3.40 ± 0.1 × 10 22 cm −2 . The best fit of the silicon edge in the spectrum of GX 5-1 is obtained by a mixture of olivine and pyroxene. In this study, our modeling is limited to Si absorption by silicates with different Mg:Fe ratios. We obtained an abundance of silicon in dust of 4.0 ± 0.3 × 10 −5 per H atom and a lower limit for total abundance, considering both gas and dust, of > 4.4 × 10 −5 per H atom, which leads to a gas to dust ratio of > 0.22. Furthermore, an enhanced scattering feature in the Si K-edge may suggest the presence of large particles along the line of sight.

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“…Recently, supernova remnant (SNR) is focused as the candidate to fill the missing budget in the supply of the interstellar dust (e.g. Rho et al 2008;Lee et al 2009;Ishihara et al 2010b). In particular, many discussions have focused on the supply of dust from the remnants of core-collapse (type II) supernovae since the discovery of dust in the early universe (Bertoldi et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Galactic distributions of carbon- and oxygen-rich AGB stars revealed by the AKARI mid-infrared all-sky survey

Ishihara

Kaneda

Onaka

et al. 2011

A&A

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Context. The environmental conditions for asympotic giant branch (AGB) stars to reach the carbon-rich (C-rich) phase are important to understand the evolutionary process of AGB stars. The difference between the spatial distributions of C-rich and oxygen-rich (O-rich) AGB stars is essential for the study of the Galactic structure and the chemical evolution of the interstellar medium. Aims. We quantitatively investigate the spatial distributions of C-rich and O-rich AGB stars in our Galaxy. We discuss the difference between them and its origin. Methods. We classify a large number of AGB stars newly detected by the AKARI mid-infrared all-sky survey. In the color-color diagrams, we define their occupation zones based on the locations of known objects. We then obtain the spatial distributions of C-rich and O-rich AGB stars, assuming that they have the same luminosity for a given mass-loss rate. Results. We find that O-rich AGB stars are concentrated toward the Galactic center and that the density decreases with Galactocentric distance, whereas C-rich AGB stars show a relatively uniform distribution within about 8 kpc of Sun. Conclusions. Our result confirms the trends reported in previous studies and extends them to a Galactic scale. We discuss the relations between our result, the Galactic metallicity gradient, and the chemical evolution of the ISM in our Galaxy.

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Freshly Formed Dust in the Cassiopeia A Supernova Remnant as Revealed by theSpitzer Space Telescope

Cited by 239 publications

References 46 publications

Fine-structure infrared lines from the Cassiopeia A knots

Fine-structure infrared lines from the Cassiopeia A knots

Absorption and scattering by interstellar dust in the silicon K-edge of GX 5-1

Galactic distributions of carbon- and oxygen-rich AGB stars revealed by the AKARI mid-infrared all-sky survey

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