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

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Presentation on theme: "SN 2012fr in NGC 1365 Mark M. Phillips, Carlos Contreras, Eric Hsiao, Nidia Morrell, Kevin Krisciunas, Peter Brown, and Max Stritzinger."— Presentation transcript:

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: ) Optical Spectropolarimetry: Maund et al. (2013; arXiv: ) 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 (~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 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 Δm 15 (B) = 0.84 ± 0.03

5 Near-IR Light Curves S-correctedUncorrected

6 Low Host Dust Reddening Lira Relation Keck HIRES Spectrum

7 UVOIR Bolometric Light Curve Fit to Rise Time (L ∝ t 2 ) 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(B max ) = to +98 days

9 High-Velocity Si II and Ca II Si II λ6355Ca II triplet

10 Velocity Evolution of Si II and Ca II

11 Velocity Evolution of Si II: Comparison with Other SNe Ia

12 Spectropolarimetry 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? [Maund et al. (2013)]

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

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

15 Look-Alikes: 2009ig and 2012fr

16 From Blondin et al. (2012)

17

18 Branch Classification Systems

19 (2012) Data from Swift satellite:

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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