Dietrich Baade (ESO) Peter Hoeflich (FSU) Ferdinando Patat (ESO) Lifan Wang (LBNL)

Dietrich Baade (ESO)Peter Hoeflich (FSU)Ferdinando Patat (ESO)Lifan Wang (LBNL)J. Craig Wheeler (Austin)

The Best SN of 2005?

SN 2005df

• UV – Swift• Optical photometry and spectropolarimetry• Mid-IR

• Structure of the ejecta

Optical Light Curves

Si II line atV~25000 km/sec

Fine structuresare found

Polarizationis strong At blue shiftedabsorptionfeatures

-12

-09

+09

+08

+05

+00

-03

-07

-08

+04

OI CaII

Ca

Example 3: SN 2004dt

A high velocity SN Distorted envelope

HVS NVC

Wavelength

Rel

. Flu

x

SN 2004dt - IME only

Wang et al. 2004

Line/Polarization Profiles

Peak blueshifted by 4000 km/sec

SN 2006X

HVS

NVC

HVS

NVC

O I of SN 2006X

Example 2: SN 2001el

Detached Ca Shell/Clump/RingDay -4 Day 19

SN 2001el

Si II Ca IIDay -4 Day 19 Day -4 Day 19

-2X104 0 2X104

Velocity(km/sec)

-2X104 0 2X104

Velocity(km/sec) -2X104 0 -2X104 0 Velocity(km/sec) Velocity(km/sec)

Q-U diagram for axially symmetric geometry

V1V3

V2

Q

U

Principle axis

V4

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

Pf=N1/2p0fi

Brownian Motion

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 (~3f i%) P ≈ f N~1/23%/(1-f) ~ 0.5%, N ~ 36 for f ~ 0.5, fi~f/N=0.014dc- diameter of a typical clump ~ 2,400 km/sec

∑pifi fiN1/2 fN-1/2

P = ———— ~ ——p0 = —— p0 1-∑fi 1-f 1-f

Pf=N1/2p0fi

Brownian Motion1) 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/clumpsmoved outside the surfaceof the photosphere at a later epoch.

Polarization position angles: A corkscrew in the ejecta?

U

Q

v1

Q

U

v4

Q

U

v3

Q

U

v2

Polarization position angles: corkscrews in the ejecta?

U

QQLoops/arcs on Q-U diagram

Absorbing clumps at different velocity

In velocity space,the radial elongation of the clumps determines the correlation of theobserved polarization at different velocities.

10,0

00 k

m/s

ec

15,0

00 k

m/s

ec

20,0

00 k

m/s

ec

Each velocity layerintercepts ~16 clumpsif the volume in frontof the photosphereis packed with clumpsof diameter of 5,000 km/sec

The volume in front of thephotosphere is big enoughto hold about 48 clumps of diameter ~5,000 km/secThe radial extension

of typical clumps has tobe ~ 5,000 km/sec toexplain the observedpolarization profile.

Peak blueshifted by 4000 km/sec

Si II 3859 Si II 6355

Mg II 4481

O I 7773

SN 2001elSi II Ca II

Day -4 Day 19 Day -4 Day 19

-2X104 0 2X104

Velocity(km/sec)

-2X104 0 2X104

Velocity(km/sec) -2X104 0 -2X104 0 Velocity(km/sec) Velocity(km/sec)

SN 2005df

08/06/200508/08/200508/09/2005

08/10/200508/14/200508/17/200508/21/200508/22/2005

08/25/200508/26/2005

Chemical Structure

Correlation

Correlation

Summary

1. High velocity component is always asymmetric2. The normal velocity component is symmetric, to a level below 5%3. The chemical burning is different for HV and NV events

1) The HV probably burned C to oxygen2) 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 layeredLow 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-expansion2) Progenitor3) Rotation; magnetic field

No high velocity shell

No high velocity shell High velocity shell withstrong 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