From shock breakout to peak and beyond: Extensive panchromatic observations of the type Ib supernova 2008D associated with swift x-ray transient 080109

M. Modjaz, W. Li, N. Butler, R. Chornock, D. Perley, S. Blondin, J. S. Bloom, A. V. Filippenko, R. P. Kirshner, D. Kocevski, D. Poznanski, M. Hicken, R. J. Foley, G. S. Stringfellow, P. Berlind, D. Barrado Y Navascues, C. H. Blake, H. Bouy, W. R. Brown, P. ChallisH. Chen, W. H. De Vries, P. Dufour, E. Falco, A. Friedman, M. Ganeshalingam, P. Garnavich, B. Holden, G. Illingworth, N. Lee, J. Liebert, G. H. Marion, S. S. Olivier, J. X. Prochaska, J. M. Silverman, N. Smith, D. Starr, T. N. Steele, A. Stockton, G. G. Williams, W. M. Wood-Vasey

    Research output: Contribution to journalArticle

    Abstract

    We present extensive early photometric (ultraviolet through near-infrared) and spectroscopic (optical and near-infrared) data on supernova (SN) 2008D as well as X-ray data analysis on the associated Swift X-ray transient (XRT) 080109. Our data span a time range of 5 hr before the detection of the X-ray transient to 150days after its detection, and a detailed analysis allowed us to derive constraints on the nature of the SN and its progenitor; throughout we draw comparisons with results presented in the literature and find several key aspects that differ. We show that the X-ray spectrum of XRT 080109 can be fit equally well by an absorbed power law or a superposition of about equal parts of both power law and blackbody. Our data first established that SN 2008D is a spectroscopically normal SN Ib (i.e., showing conspicuous He lines) and showed that SN 2008D had a relatively long rise time of 18days and a modest optical peak luminosity. The early-time light curves of the SN are dominated by a cooling stellar envelope (for Δt0.1-4days, most pronounced in the blue bands) followed by 56Ni decay. We construct a reliable measurement of the bolometric output for this stripped-envelope SN, and, combined with estimates of E K and M ej from the literature, estimate the stellar radius R of its probable Wolf-Rayet progenitor. According to the model of Waxman etal. and Chevalier & Fransson, we derive R W07 = 1.2 0.7R and R CF08 = 12 7 R , respectively; the latter being more in line with typical WN stars. Spectra obtained at three and four months after maximum light show double-peaked oxygen lines that we associate with departures from spherical symmetry, as has been suggested for the inner ejecta of a number of SN Ib cores.

    Original languageEnglish (US)
    Pages (from-to)226-248
    Number of pages23
    JournalAstrophysical Journal
    Volume702
    Issue number1
    DOIs
    StatePublished - 2009

    Fingerprint

    supernovae
    shock
    x rays
    near infrared
    power law
    ejecta
    symmetry
    stellar envelopes
    wolves
    cooling
    estimates
    oxygen
    light curve
    envelopes
    luminosity
    stars
    radii
    output
    decay
    detection

    Keywords

    • Distances and redshifts
    • Galaxies
    • General
    • Individual
    • Individual (NGC 2770)
    • Supernovae

    ASJC Scopus subject areas

    • Space and Planetary Science
    • Astronomy and Astrophysics

    Cite this

    From shock breakout to peak and beyond : Extensive panchromatic observations of the type Ib supernova 2008D associated with swift x-ray transient 080109. / Modjaz, M.; Li, W.; Butler, N.; Chornock, R.; Perley, D.; Blondin, S.; Bloom, J. S.; Filippenko, A. V.; Kirshner, R. P.; Kocevski, D.; Poznanski, D.; Hicken, M.; Foley, R. J.; Stringfellow, G. S.; Berlind, P.; Barrado Y Navascues, D.; Blake, C. H.; Bouy, H.; Brown, W. R.; Challis, P.; Chen, H.; De Vries, W. H.; Dufour, P.; Falco, E.; Friedman, A.; Ganeshalingam, M.; Garnavich, P.; Holden, B.; Illingworth, G.; Lee, N.; Liebert, J.; Marion, G. H.; Olivier, S. S.; Prochaska, J. X.; Silverman, J. M.; Smith, N.; Starr, D.; Steele, T. N.; Stockton, A.; Williams, G. G.; Wood-Vasey, W. M.

    In: Astrophysical Journal, Vol. 702, No. 1, 2009, p. 226-248.

    Research output: Contribution to journalArticle

    Modjaz, M, Li, W, Butler, N, Chornock, R, Perley, D, Blondin, S, Bloom, JS, Filippenko, AV, Kirshner, RP, Kocevski, D, Poznanski, D, Hicken, M, Foley, RJ, Stringfellow, GS, Berlind, P, Barrado Y Navascues, D, Blake, CH, Bouy, H, Brown, WR, Challis, P, Chen, H, De Vries, WH, Dufour, P, Falco, E, Friedman, A, Ganeshalingam, M, Garnavich, P, Holden, B, Illingworth, G, Lee, N, Liebert, J, Marion, GH, Olivier, SS, Prochaska, JX, Silverman, JM, Smith, N, Starr, D, Steele, TN, Stockton, A, Williams, GG & Wood-Vasey, WM 2009, 'From shock breakout to peak and beyond: Extensive panchromatic observations of the type Ib supernova 2008D associated with swift x-ray transient 080109', Astrophysical Journal, vol. 702, no. 1, pp. 226-248. https://doi.org/10.1088/0004-637X/702/1/226
    Modjaz, M. ; Li, W. ; Butler, N. ; Chornock, R. ; Perley, D. ; Blondin, S. ; Bloom, J. S. ; Filippenko, A. V. ; Kirshner, R. P. ; Kocevski, D. ; Poznanski, D. ; Hicken, M. ; Foley, R. J. ; Stringfellow, G. S. ; Berlind, P. ; Barrado Y Navascues, D. ; Blake, C. H. ; Bouy, H. ; Brown, W. R. ; Challis, P. ; Chen, H. ; De Vries, W. H. ; Dufour, P. ; Falco, E. ; Friedman, A. ; Ganeshalingam, M. ; Garnavich, P. ; Holden, B. ; Illingworth, G. ; Lee, N. ; Liebert, J. ; Marion, G. H. ; Olivier, S. S. ; Prochaska, J. X. ; Silverman, J. M. ; Smith, N. ; Starr, D. ; Steele, T. N. ; Stockton, A. ; Williams, G. G. ; Wood-Vasey, W. M. / From shock breakout to peak and beyond : Extensive panchromatic observations of the type Ib supernova 2008D associated with swift x-ray transient 080109. In: Astrophysical Journal. 2009 ; Vol. 702, No. 1. pp. 226-248.
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    abstract = "We present extensive early photometric (ultraviolet through near-infrared) and spectroscopic (optical and near-infrared) data on supernova (SN) 2008D as well as X-ray data analysis on the associated Swift X-ray transient (XRT) 080109. Our data span a time range of 5 hr before the detection of the X-ray transient to 150days after its detection, and a detailed analysis allowed us to derive constraints on the nature of the SN and its progenitor; throughout we draw comparisons with results presented in the literature and find several key aspects that differ. We show that the X-ray spectrum of XRT 080109 can be fit equally well by an absorbed power law or a superposition of about equal parts of both power law and blackbody. Our data first established that SN 2008D is a spectroscopically normal SN Ib (i.e., showing conspicuous He lines) and showed that SN 2008D had a relatively long rise time of 18days and a modest optical peak luminosity. The early-time light curves of the SN are dominated by a cooling stellar envelope (for Δt0.1-4days, most pronounced in the blue bands) followed by 56Ni decay. We construct a reliable measurement of the bolometric output for this stripped-envelope SN, and, combined with estimates of E K and M ej from the literature, estimate the stellar radius R ⊙ of its probable Wolf-Rayet progenitor. According to the model of Waxman etal. and Chevalier & Fransson, we derive R W07 ⊙ = 1.2 0.7R ⊙ and R CF08 ⊙ = 12 7 R ⊙, respectively; the latter being more in line with typical WN stars. Spectra obtained at three and four months after maximum light show double-peaked oxygen lines that we associate with departures from spherical symmetry, as has been suggested for the inner ejecta of a number of SN Ib cores.",
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    TY - JOUR

    T1 - From shock breakout to peak and beyond

    T2 - Extensive panchromatic observations of the type Ib supernova 2008D associated with swift x-ray transient 080109

    AU - Modjaz, M.

    AU - Li, W.

    AU - Butler, N.

    AU - Chornock, R.

    AU - Perley, D.

    AU - Blondin, S.

    AU - Bloom, J. S.

    AU - Filippenko, A. V.

    AU - Kirshner, R. P.

    AU - Kocevski, D.

    AU - Poznanski, D.

    AU - Hicken, M.

    AU - Foley, R. J.

    AU - Stringfellow, G. S.

    AU - Berlind, P.

    AU - Barrado Y Navascues, D.

    AU - Blake, C. H.

    AU - Bouy, H.

    AU - Brown, W. R.

    AU - Challis, P.

    AU - Chen, H.

    AU - De Vries, W. H.

    AU - Dufour, P.

    AU - Falco, E.

    AU - Friedman, A.

    AU - Ganeshalingam, M.

    AU - Garnavich, P.

    AU - Holden, B.

    AU - Illingworth, G.

    AU - Lee, N.

    AU - Liebert, J.

    AU - Marion, G. H.

    AU - Olivier, S. S.

    AU - Prochaska, J. X.

    AU - Silverman, J. M.

    AU - Smith, N.

    AU - Starr, D.

    AU - Steele, T. N.

    AU - Stockton, A.

    AU - Williams, G. G.

    AU - Wood-Vasey, W. M.

    PY - 2009

    Y1 - 2009

    N2 - We present extensive early photometric (ultraviolet through near-infrared) and spectroscopic (optical and near-infrared) data on supernova (SN) 2008D as well as X-ray data analysis on the associated Swift X-ray transient (XRT) 080109. Our data span a time range of 5 hr before the detection of the X-ray transient to 150days after its detection, and a detailed analysis allowed us to derive constraints on the nature of the SN and its progenitor; throughout we draw comparisons with results presented in the literature and find several key aspects that differ. We show that the X-ray spectrum of XRT 080109 can be fit equally well by an absorbed power law or a superposition of about equal parts of both power law and blackbody. Our data first established that SN 2008D is a spectroscopically normal SN Ib (i.e., showing conspicuous He lines) and showed that SN 2008D had a relatively long rise time of 18days and a modest optical peak luminosity. The early-time light curves of the SN are dominated by a cooling stellar envelope (for Δt0.1-4days, most pronounced in the blue bands) followed by 56Ni decay. We construct a reliable measurement of the bolometric output for this stripped-envelope SN, and, combined with estimates of E K and M ej from the literature, estimate the stellar radius R ⊙ of its probable Wolf-Rayet progenitor. According to the model of Waxman etal. and Chevalier & Fransson, we derive R W07 ⊙ = 1.2 0.7R ⊙ and R CF08 ⊙ = 12 7 R ⊙, respectively; the latter being more in line with typical WN stars. Spectra obtained at three and four months after maximum light show double-peaked oxygen lines that we associate with departures from spherical symmetry, as has been suggested for the inner ejecta of a number of SN Ib cores.

    AB - We present extensive early photometric (ultraviolet through near-infrared) and spectroscopic (optical and near-infrared) data on supernova (SN) 2008D as well as X-ray data analysis on the associated Swift X-ray transient (XRT) 080109. Our data span a time range of 5 hr before the detection of the X-ray transient to 150days after its detection, and a detailed analysis allowed us to derive constraints on the nature of the SN and its progenitor; throughout we draw comparisons with results presented in the literature and find several key aspects that differ. We show that the X-ray spectrum of XRT 080109 can be fit equally well by an absorbed power law or a superposition of about equal parts of both power law and blackbody. Our data first established that SN 2008D is a spectroscopically normal SN Ib (i.e., showing conspicuous He lines) and showed that SN 2008D had a relatively long rise time of 18days and a modest optical peak luminosity. The early-time light curves of the SN are dominated by a cooling stellar envelope (for Δt0.1-4days, most pronounced in the blue bands) followed by 56Ni decay. We construct a reliable measurement of the bolometric output for this stripped-envelope SN, and, combined with estimates of E K and M ej from the literature, estimate the stellar radius R ⊙ of its probable Wolf-Rayet progenitor. According to the model of Waxman etal. and Chevalier & Fransson, we derive R W07 ⊙ = 1.2 0.7R ⊙ and R CF08 ⊙ = 12 7 R ⊙, respectively; the latter being more in line with typical WN stars. Spectra obtained at three and four months after maximum light show double-peaked oxygen lines that we associate with departures from spherical symmetry, as has been suggested for the inner ejecta of a number of SN Ib cores.

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    KW - Galaxies

    KW - General

    KW - Individual

    KW - Individual (NGC 2770)

    KW - Supernovae

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