The Best SN of 2005? Dietrich Baade (ESO) Peter Hoeflich (FSU) Ferdinando Patat (ESO) Lifan Wang (LBNL) J. Craig Wheeler (Austin)

Historical Image from Song Dynasty SN 1006 at Discovery – Historical Image from Song Dynasty

SN 2005df UV – Swift Optical photometry and spectropolarimetry Mid-IR Structure of the ejecta

Optical Light Curves

+09 +08 +05 +04 +00 -03 -07 -08 -09 -12 Fine structures are found Polarization is strong At blue shifted absorption features +00 -03 -07 -08 -09 -12 Si II line at V~25000 km/sec

OI CaII

Si II - Photospheric

Si II – High V

O I

Ca Ca II

Example 3: SN 2004dt HVS NVC A high velocity SN Distorted envelope

SN 2004dt - IME only Rel. Flux Wavelength Wang et al. 2004

Line/Polarization Profiles Peak blueshifted by 4000 km/sec

SN 2006X HVS HVS NVC NVC Ca II

O I of SN 2006X O I NOT poplarized

Example 2: SN 2001el Day -4 Day 19 Detached Ca Shell/Clump/Ring

Si II Ca II SN 2001el Day -4 Day 19 Day -4 Day 19 Velocity(km/sec) -2X104 0 2X104 Velocity(km/sec) -2X104 0 2X104 Velocity(km/sec) -2X104 0 -2X104 0 Velocity(km/sec) Velocity(km/sec)

Q = (I0-I90)/(I0+I90) U = (I45-I135)/(I45+I135) Q-U diagram for axially symmetric geometry V3 V4 V2 V1 U Principle axis Q Q = (I0-I90)/(I0+I90) U = (I45-I135)/(I45+I135) Theorem: For axially symmetric geometry, the Q-U vectors form a straight line on the Q-U Diagram

Brownian Motion Pf=N1/2p0fi ∑pifi fiN1/2 fN-1/2 f - total area covering factor of clumps (≤1) fi - area covering factor by a typical clump (~f/N) N - total number of clumps (=f/fi) pifi - polarized flux due to individual clump (~3fi%) P ≈ f N~1/23%/(1-f) ~ 0.5%, N ~ 36 for f ~ 0.5, fi~f/N=0.014 dc- diameter of a typical clump ~ 2,400 km/sec ∑pifi fiN1/2 fN-1/2 P = ———— ~ ——p0 = —— p0 1-∑fi 1-f 1-f

Brownian Motion Pf=N1/2p0fi 1) When N is sufficiently large P will be a stable vector that does not show big, random fluctuations with time. 2) In the case of a small number of large clumps, P is again a stable quantity as such clumps will shield the photosphere at all epochs These vectors/clumps moved outside the surface of the photosphere at a later epoch.

Polarization position angles: A corkscrew in the ejecta? U Q v1 Q U v2 Q U v3 Q U v4

Polarization position angles: corkscrews in the ejecta? Absorbing clumps at different velocity U Loops/arcs on Q-U diagram Q Q

of the clumps determines the correlation of the In velocity space, the radial elongation of the clumps determines the correlation of the observed polarization at different velocities. Each velocity layer intercepts ~16 clumps if the volume in front of the photosphere is packed with clumps of diameter of 5,000 km/sec Peak blueshifted by 4000 km/sec 10,000 km/sec 15,000 km/sec 20,000 km/sec The volume in front of the photosphere is big enough to hold about 48 clumps of diameter ~5,000 km/sec The radial extension of typical clumps has to be ~ 5,000 km/sec to explain the observed polarization profile.

Si II 6355 Si II 3859 Mg II 4481 O I 7773

SN 2001el Si II Ca II Day -4 Day 19 Day -4 Day 19 Velocity(km/sec) -2X104 0 2X104 Velocity(km/sec) -2X104 0 2X104 Velocity(km/sec) -2X104 0 -2X104 0 Velocity(km/sec) Velocity(km/sec)

SN 2005df 08/06/2005 08/08/2005 08/09/2005 08/10/2005 08/14/2005 08/17/2005 08/21/2005 08/22/2005 08/25/2005 08/26/2005

Chemical Structure

Correlation

Correlation

Summary High velocity component is always asymmetric The normal velocity component is symmetric, to a level below 5% 3. The chemical burning is different for HV and NV events The HV probably burned C to oxygen The NV did not burn C at the outer layer (this is why C is found only in some NV) 4. The core is likely asymmetric

Mid-IR

Mid-IR

Mid-IR – Day 135

SN 2003hv – Day 375

Deflagration Delayed Detonation Observed Turbulent/clumpy geometry at all velocities Significantly reduced asymmetry at the central part of the ejecta No significant asymmetry below photosphere Clumpy chemical Layered chemical structure layered Low energy Sufficient energy High speed layer? The seed for significant asymmetry At the outermost layer, the turbulent plumes/bubbles generated during the deflagration may survive Asymmetry in 1) pre-expansion 2) Progenitor 3) Rotation; magnetic field No high velocity shell High velocity shell with strong asymmetry Comparable level of asymmetry at all velocities Stronger asymmetry at outer layers 1) Asymmetry decreases from 30000 – 8000 km/sec; 2) The core is likely asymmetric