Papers › High Density Circumstellar Interaction in the Luminous Type IIn SN 2010jl: The first 1100 days
High Density Circumstellar Interaction in the Luminous Type IIn SN 2010jl: The first 1100 days
Claes Fransson, Mattias Ergon, Peter J. Challis, Roger A. Chevalier, Kevin France, Robert P. Kirshner, G. H. Marion, Dan Milisavljevic, Nathan Smith, Filomena Bufano, Andrew S. Friedman, Tuomas Kangas, Josefin Larsson, Seppo Mattila, Stefano Benetti, Ryan Chornock, Ian Czekala, Alicia Soderberg, Jesper Sollerman
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HST and ground based observations of the Type IIn SN 2010jl are analyzed, including photometry, spectroscopy in the ultraviolet, optical and NIR bands, 26-1128 days after first detection. At maximum the bolometric luminosity was ∼3×10⁴³ erg/s and even at 850 days exceeds 10⁴² erg/s. A NIR excess, dominating after 400 days, probably originates in dust in the circumstellar medium (CSM). The total radiated energy is > 6.5×10⁵⁰ ergs, excluding the dust component. The spectral lines can be separated into one broad component due to electron scattering, and one narrow with expansion velocity ∼100 km/s from the CSM. The broad component is initially symmetric around zero velocity but becomes blueshifted after ∼50 days, while remaining symmetric about a shifted centroid velocity. Dust absorption in the ejecta is unlikely to explain the line shifts, and we attribute the shift instead to acceleration by the SN radiation. From the optical lines and the X-ray and dust properties, there is strong evidence for large scale asymmetries in the CSM. The ultraviolet lines indicate CNO processing in the progenitor, while the optical shows a number of narrow coronal lines excited by the X-rays. The bolometric light curve is consistent with a radiative shock in an r⁻² CSM with a mass loss rate of ∼0.1 M_sun/yr. The total mass lost is > 3 M_sun. These properties are consistent with the SN expanding into a CSM characteristic of an LBV progenitor with a bipolar geometry. The apparent absence of nuclear processing is attributed to a CSM still opaque to electron scattering.
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