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    A decade of ejecta dust formation in the Type IIn SN 2005ip

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    Author
    Bevan, A
    Wesson, R
    Barlow, M J
    De Looze, I
    Andrews, J E
    Clayton, G C
    Krafton, K
    Matsuura, M
    Milisavljevic, D
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2019-06
    Keywords
    radiative transfer
    methods: statistical
    supernovae: general
    supernovae: individual
    SN 2005ip
    ISM: supernova remnants
    
    Metadata
    Show full item record
    Publisher
    OXFORD UNIV PRESS
    Citation
    A Bevan, R Wesson, M J Barlow, I De Looze, J E Andrews, G C Clayton, K Krafton, M Matsuura, D Milisavljevic, A decade of ejecta dust formation in the Type IIn SN 2005ip, Monthly Notices of the Royal Astronomical Society, Volume 485, Issue 4, June 2019, Pages 5192–5206, https://doi.org/10.1093/mnras/stz679
    Journal
    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
    Rights
    © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    In order to understand the contribution of core-collapse supernovae to the dust budget of the early Universe, it is important to understand not only the mass of dust that can form in core-collapse supernovae but also the location and rate of dust formation. SN 2005ip is of particular interest since dust has been inferred to have formed in both the ejecta and the post-shock region behind the radiative reverse shock. We have collated eight optical archival spectra that span the lifetime of SN 2005ip and we additionally present a new X-shooter optical-near-IR spectrum of SN 2005ip at 4075 d post-discovery. Using the Monte Carlo line transfer code DAMOCLES, we have modelled the blueshifted broad and intermediate-width H alpha, H beta, and He I lines from 48 to 4075 d post-discovery using an ejecta dust model. We find that dust in the ejecta can account for the asymmetries observed in the broad and intermediate-width H alpha, H beta, and He I line profiles at all epochs and that it is not necessary to invoke post-shock dust formation to explain the blueshifting observed in the intermediate-width post-shock lines. Using a Bayesian approach, we have determined the evolution of the ejecta dust mass in SN 2005ip over 10 yr presuming an ejecta dust model, with an increasing dust mass from similar to 10(-8) M-circle dot at 48 d to a current dust mass of similar to 0.1 M-circle dot.
    ISSN
    0035-8711
    EISSN
    1365-2966
    DOI
    10.1093/mnras/stz679
    Version
    Final published version
    Sponsors
    European Research Council (ERC) [SNDUST 694520]; STFC Ernest Rutherford fellowship [ST/L003597/1]; ESO programme(s) [097.D-0525(A)]
    ae974a485f413a2113503eed53cd6c53
    10.1093/mnras/stz679
    Scopus Count
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    UA Faculty Publications

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