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# Cassiopeia A: Dust factory revealed via submillimetre polarimetry

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(Impact Factor: 5.11). 09/2008; 394(3). DOI: 10.1111/j.1365-2966.2009.14453.x
Source: arXiv

ABSTRACT

If Type-II supernovae - the evolutionary end points of short-lived, massive stars - produce a significant quantity of dust (>0.1 M_sun) then they can explain the rest-frame far-infrared emission seen in galaxies and quasars in the first Gyr of the Universe. Submillimetre observations of the Galactic supernova remnant, Cas A, provided the first observational evidence for the formation of significant quantities of dust in Type-II supernovae. In this paper we present new data which show that the submm emission from Cas A is polarised at a level significantly higher than that of its synchrotron emission. The orientation is consistent with that of the magnetic field in Cas A, implying that the polarised submm emission is associated with the remnant. No known mechanism would vary the synchrotron polarisation in this way and so we attribute the excess polarised submm flux to cold dust within the remnant, providing fresh evidence that cosmic dust can form rapidly. This is supported by the presence of both polarised and unpolarised dust emission in the north of the remnant, where there is no contamination from foreground molecular clouds. The inferred dust polarisation fraction is unprecedented (f_pol ~ 30%) which, coupled with the brief timescale available for grain alignment (<300 yr), suggests that supernova dust differs from that seen in other Galactic sources (where f_pol=2-7%), or that a highly efficient grain alignment process must operate in the environment of a supernova remnant. Comment: In press at MNRAS, 10 pages, print in colour

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Available from: Steve John Maddox, Sep 27, 2012
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• "For example, observations of the SNR Cas A result in a few times 10 −5 M ⊙ of hot dust (>170 K) and a few times 10 −2 M ⊙ of warm and cold dust (< 150 K) for the entire SNR (e.g., Arendt et al, 1999; Douvion et al, 2001b; Hines et al, 2004; Krause et al, 2004; Rho et al, 2008). An amount of ∼ 1M ⊙ of dust at a temperature of ∼ 20 K was recently suggested by Dunne et al (2009). Observations with the Herschel Space Observatory result in a resolved cool dust component (∼ 35 K) in the unshocked interior of Cas A with an estimated mass of 7.5 × 10 −2 M ⊙ of dust (Barlow et al, 2010). "
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##### Article: Carbon Monoxide in the Cassiopeia A Supernova Remnant
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ABSTRACT: We report the likely detection of near-infrared 2.29 $\mu$m first overtone Carbon Monoxide (CO) emission from the young supernova remnant Cassiopeia A (Cas A). The continuum-subtracted CO filter map reveals CO knots within the ejecta-rich reverse shock. We compare the first overtone CO emission with that found in the well-studied supernova, SN 1987A and find $\sim$30 times less CO in Cas A. The presence of CO suggests that molecule mixing is small in the SN ejecta and that astrochemical processes and molecule formation may continue at least ~300 years after the initial explosion. Comment: Accepted for the publication in ApJ Letter
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