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

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

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

4. Optical Light Curves

5. +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

6. OI
CaII

8. Si II - Photospheric

9. Si II – High V

10. O I

11. Ca
Ca II

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

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

15. Line/Polarization Profiles
Peak blueshifted
by 4000 km/sec

16. SN 2006X
HVS
HVS
NVC
NVC
Ca II

17. O I of SN 2006X
O I NOT poplarized

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

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

21. 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

22. 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/ fN-1/2
P = ———— ~ ——p0 = —— p0
1-∑fi f f

23. 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.

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

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

26. 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.

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

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

29. 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

31. Chemical Structure

32. Correlation

33. Correlation

34. 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

35. Mid-IR

36. Mid-IR

37. Mid-IR – Day 135

38. SN 2003hv – Day 375

41. 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 – 8000 km/sec;
2) The core is likely asymmetric