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SN 2012fr in NGC 1365

SN 2012fr in NGC 1365. Mark M. Phillips, Carlos Contreras, Eric Hsiao, Nidia Morrell, Kevin Krisciunas, Peter Brown, and Max Stritzinger. The Type Ia SN 2012fr in NGC 1365. Optical Spectroscopy: Childress et al. (2013; arXiv:1302.2926)

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SN 2012fr in NGC 1365

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  1. SN 2012fr in NGC 1365 Mark M. Phillips, Carlos Contreras, Eric Hsiao, Nidia Morrell, Kevin Krisciunas, Peter Brown, and Max Stritzinger

  2. The Type Ia SN 2012fr in NGC 1365 Optical Spectroscopy: Childress et al. (2013; arXiv:1302.2926) Optical Spectropolarimetry: Maund et al. (2013; arXiv:1302.0166) Optical/NIR Imaging: Contreras et al. (2013; in preparation) NIR Spectroscopy: Hsiao et al. (2013; in preparation)

  3. SN 2012fr • Discovered by TAROT on images taken by its robotic telescope at La Silla observatory, Chile, on 2012 Oct 27.05 (~6-12 hours after explosion) • Hosted by the nearby galaxy NGC1365, a barred spiral ~18 Mpc distant in the Fornax cluster (has a Cepheid distance) • The first optical spectrum obtained with the ANU 2.3 m/WiFeS on 2012 Oct 28.53 showed that the supernova was a very young type Ia with high-velocity Si II and Ca II • The CSP started optical imaging on Oct 30.16, and near-IR imaging and spectroscopy on Oct 31.16

  4. Optical Light Curves Δm15(B) = 0.84 ± 0.03

  5. Near-IR Light Curves S-corrected Uncorrected

  6. Low Host Dust Reddening Lira Relation Keck HIRES Spectrum

  7. UVOIR Bolometric Light Curve UVOIR Bolometric Light Curve Fit to Rise Time (L∝ t2) Rise time of ~16 days from explosion to maximum. In left Fig, others from top down: 91T, 92A, 94ae 91bg.

  8. Optical Spectroscopic Coverage 69 spectra obtained between t(Bmax) = -14.5 to +98 days

  9. High-Velocity Si II and Ca II Si II λ6355 Ca II triplet

  10. Velocity Evolution of Si II and Ca II

  11. Velocity Evolution of Si II: Comparison with Other SNeIa

  12. Spectropolarimetry [Maund et al. (2013)] • Low (< 0.1%) continuum polarization • HV components of Si II and Ca II are highly polarized at earliest epoch; polarization decreases as these features weaken • At +2 days, the polarization angles of the LV components of Si II and Ca II are identical and oriented at 90° relative to the HV Ca II component, meaning they have orthogonal distributions in the plane of the sky • Observations are perhaps more consistent with the pulsating delayed detonation model?

  13. Near-IR Spectroscopic Coverage of SN 2012fr 31 spectra obtained between t(Bmax) = -11.5 to +108 days

  14. SN 2012fr: Optical + Near-IR, -7 days No HV components in the near-IR? HV Ca II HV + LV Si II HV Ca II Mg II Fe III?

  15. Look-Alikes: 2009ig and 2012fr

  16. From Blondin et al. (2012)

  17. (2012)

  18. Branch Classification Systems

  19. Data from Swift satellite: (2012)

  20. Summary of Observational Characteristics of SN 2012fr • Fast rise to max; slow decline after max • Strong HV components of Si II and Ca II absorption at early epochs • Nearly flat evolution of LV Si II λ6355 expansion velocity • “Normal” luminosity

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