Shock Processing of Interstellar Dust and Polycyclic Aromatic Hydrocarbons in the Supernova Remnant N132D

Tappe, Achim; Rho, Jeonghee; Reach, W. T.

doi:10.1086/508741

Cited by 69 publications

(101 citation statements)

References 54 publications

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“…In fact the IRS spectroscopy indicates the presence of a broad feature around 18 μm at the ejecta position of G292.0+1.8 (Ghavamian et al, 2009). A similar broad feature in 18-24 μm has also been reported for other SNRs (Tappe et al, 2006;Rho et al, 2008Rho et al, , 2009b A broad feature around 22 μm has been reported in the Carina nebula and other massive star-forming regions, suggesting a possible connection of the broad feature to dust grains formed in SNe (Chan & Onaka, 2000;. Figure 3 shows a comparison of the spectrum of the Carina nebula with those of Cas A and Sharpless 171 star-forming region .…”

Section: Observations Of Supernova Remnantssupporting

confidence: 79%

Evolving Gas and Dust in the Galaxy and Galaxies to be seen by SPICA

Onaka

Sakon

Kaneda

et al. 2009

SPICA Joint European/Japanese Workshop

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Supernovae (SNe) and low-mass evolved stars eject elements synthesized in stellar interior to the interstellar space as solid particles, whereas dust grains are destroyed efficiently in SN shocks. A large fraction of interstellar dust must in fact be formed in dense clouds rather than being supplied by stellar sources. All of these processes in our Galaxy and nearby galaxies can be studied most effectively by imaging spectroscopy in the mid-to far-infrared instruments on board SPICA, only which allow us to investigate in detail the nature of dust grains as well as the abundance and physical conditions of gas species in the various regions in galaxies. This report summarizes the discussions of the science working group in Japan with the emphasis on investigations of the dust formation in stellar sources and dense clouds, and the material evolution in nearby galaxies that only SPICA can carry out.

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Section: Observations Of Supernova Remnantssupporting

confidence: 79%

Evolving Gas and Dust in the Galaxy and Galaxies to be seen by SPICA

Onaka

Sakon

Kaneda

et al. 2009

SPICA Joint European/Japanese Workshop

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“…The ratio of the emission from the 15-20 μm plateau to the 6.2 μm PAH feature is ∼0.4 for Kes 17 and other H 2 emitting SNRs, similar to NGC 7331 but larger than for the PDR. This ratio is smaller than that of the young SNR N132D (Tappe et al 2006). The difference in PAH features between molecular SNRs and N132D is due to the environments of SNRs.…”

Section: Pah From Slow Shocks: Molecular Supernova Remnantsmentioning

confidence: 63%

“…We found evidence for spatial variations of the PAH features, both in intensity and wavelength, when comparing spectra extracted along the IRS long-low slit from the shell of the remnant and the adjacent molecular cloud/H II region, which confirms the processing of the PAH molecules. These detections, most notably the 15 ∼ 20 μm features, are the first of its kind for supernova remnants to our knowledge (Tappe et al 2006). The 15 ∼ 20 μm features in Figure 2a are interpreted as PAH CCC out-of-plane bending modes (cf.…”

Section: Pah Detection From the Supernova Remnant N132dmentioning

confidence: 70%

“…In the optical, the large-scale morphology of the gas in N132D shows highly red-shifted oxygen-rich ejecta in the center and shocked interstellar clouds in the outer rim. We have previously presented Spitzer IRAC, MIPS and an IRS spectrum of N132D (Tappe et al 2006). Here we present IRS-LL mapping of N132D covering the entire SNR, and IRS staring of SL observations toward 4 positions.…”

Section: Pah Detection From the Supernova Remnant N132dmentioning

confidence: 95%

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PAH and Dust Processing in Supernova Remnants

Rho

Andersen

Tappe

et al. 2011

EAS Publications Series

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Abstract. I present observations of shock-processed PAHs and dust in supernova remnants (SNRs). Supernova shocks are one of the primary sites destroying, fragmenting and altering interstellar PAHs and dust. Studies of PAHs through supernova shocks had been limited because of confusion with PAHs in background emission. Spitzer observations with high sensitivity and resolution allow us to separate PAHs associated with the SNRs and unrelated, Galactic PAHs. In the young SNR N132D, PAH features are detected with a higher PAH ratio of 15-20/7.7 μm than those of other astronomical objects, and we suggest large PAHs have survived behind the shock. We present the spectra of additional 14 SNRs observed with Spitzer IRS and MIPS SED covering the range of 5-90 μm. Bright PAH features from 6.2 to 15-20 μm are detected from many of SNRs which emit molecular hydrogen lines, indicating that both large and small PAHs survive in low velocity shocks. We observe a strong correlation between PAH detection and carbonaceous small grains, while a few SNRs with dominant silicate dust lack PAH features. We characterize PAHs depending on the shock velocity, preshock density and temperature of hot gas, and discuss PAH and dust processing in shocks and implication of PAH and dust cycles in ISM.

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“…Further, the dust-to-gas mass ratio in SNR 1987A has decreased over time -a sign of ongoing grain destruction. Tappe et al (2006) also found infrared emission from dust in the young SNR N132D, but also inferred that the observed dust was from the swept-up ISM. They found a dust-to-gas mass ratio of about of tenth of the average ratio for the LMC.…”

Section: Dust Production and Destructionmentioning

confidence: 85%

Supernova remnants in the Magellanic Clouds

Williams¹

2008

Proc. IAU

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Abstract. At the 1998 IAU Symposium on the Magellanic Clouds, Dr. Robert Petre observed that we were reaching a time where it was possible "to study the MC SNRs at a level of detail comparable with many Galactic remnants", while retaining the benefits of a global view in the MCs. Over the past decade, many researchers have taken advantage of these newly accessible populations. New MC-wide surveys at various wavelengths have enabled broader searches for SNR candidates, extending our census of MC SNRs to less prominent objects -older SNRs, SNRs in complex regions, et cetera. The use of light-echoes has provided a new avenue to probe young SNRs. Higher spatial and spectral resolutions in many wavelength regimes have enabled detailed studies of individual remnants, revealing progenitor types, pulsar-wind nebulae, expansion details, and environmental effects.Perhaps the newest conceptual development is the increasing use of the MC SNRs to study physical problems of wider significance to many fields of astronomy. For example, researchers have examined the energy and hot gas inputs of MC SNRs to the ISM, including their collective effects within superbubbles, in order to evaluate their effects on stellar feedback cycles in a galaxy. Other scientists have investigated the fraction of SNR energies going to the acceleration of cosmic rays, which has significant implications for the role of SNRs in cosmic-ray production. Most recently, the onslaught of Spitzer data has led to new exploration of dust in MC SNRs, allowing us to probe dust creation, depletion, and destruction in the MC SNR populations. In summary, the study of SNRs in the MCs appears to have "come of age" over the past decade, becoming a mature field with rich potential for future scientific work.

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Shock Processing of Interstellar Dust and Polycyclic Aromatic Hydrocarbons in the Supernova Remnant N132D

Cited by 69 publications

References 54 publications

Evolving Gas and Dust in the Galaxy and Galaxies to be seen by SPICA

Evolving Gas and Dust in the Galaxy and Galaxies to be seen by SPICA

PAH and Dust Processing in Supernova Remnants

Supernova remnants in the Magellanic Clouds

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