Late-time interaction incore-collapse supernovae
Dan Milisavljevic
Purdue University
MIAPbP – Interacting Supernovae
February 14, 2023

Late-time emission =years to decades after explosion (mostly)

What can we learn?
1. Probe mass loss hundreds to thousands of years prior toexplosion.
2. Emission from outer layers of metal-rich ejecta. Over timeever-deeper layers will slowly reveal themselves.
3. Connections to supernova remnants where we have much
more detailed and resolved information.

SN 2010jlFantasy

Credit: ESO/M. KornmesserSN 2010jlReality

Credit: J. Brimacombe

REALITY!
Cassiopeia A
SN 1680 (approx)

Cassiopeia A
SN 1680 (approx)

Credit: Patnaude & DepasqualeForward shock

Reverse-shockedejecta

Central Compact Object

3D Reconstruction of a SN Debris Field
Cas A’s distribution of opticallyemitting ejecta exhibits largescale coherent structure thatwas imprinted early in theexplosion

Milisavljevic & Fesen (2015, Science)Milisavljevic & Fesen (2013)

The SN 1993J—Cas A connection enables interpretation of emission line
substructure in unresolved sources

Milisavljevic & Fesen (2017)

The SN 1993J—Cas A connection enables interpretationof emission line substructure in unresolved sources

Not random clumps! Coherent, large-scale
structure (here observed as rings)
http://www.physics.purdue.edu/kaboom/casa-webapp/model.html

How far back can we follow the SN-SNR
transition?

Milisavljevic & Fesen 2017

How far back can we follow the SN-SNR
transition?

Milisavljevic et al. (2012)

Pinpointing the SN-SNR transition

Milisavljevic & Margutti 2018

Milisavljevic & Fesen 2017

Reverse shock excites outer high-velocity ejectaBlack, DM, et al. 2017

Pinpointing the SN-SNR transition

Weil et al. (2020)

Line profile reflects geometry and dust (andclumping and…)

Weil et al. (2020)

Changes in features follows progression of reverse
shock into inner layers of ejecta
SN 1979C

Milisavljevic+ 2009

Emission line profiles as probes of ejecta
geometry and dust

Milisavljevic et al. 2012

Milisavljevic & Fesen (2008)

SNR-4449-1 in NGC 4449

Remnant is strongly interacting with dense, circumstellar wind loss material from a > 20 M progenitor star.

Late-time emission as diagnostic of progenitor systems
Striking similarity between SNe 2013df and
1993J in the (candidate) progenitors andthe CSM environments, and the contrast
with SN 2011dh, suggests that SNe IIb witha more extended progenitor haveexperienced a much stronger mass loss inthe final centuries toward the explosion.

Maeda, Hattori, DM et al. (2015)

Late-time emission as diagnostic of progenitor systems
Striking similarity between SNe 2013df and
1993J in the (candidate) progenitors andthe CSM environments, and the contrast
with SN 2011dh, suggests that SNe IIb witha more extended progenitor haveexperienced a much stronger mass loss inthe final centuries toward the explosion.

Maeda, Hattori, DM et al. (2015)

SN
SN2014C:
2014C:Supernova
SupernovaMetamorphosis
Metamorphosis

Radical Frontiers of Stellar Evolution

Dan Milisavljevic

SN 2014C: Supernova Metamorphosis
SN Ib that initially expanded in cavity, then encountered H-rich shell
approximately 1 Msun in mass approximately 5 x 1016 cm from the explosion site.

Hα
SN 2014C
t = 373 d
SN 2008D (Ib)t ~ 1 year

SN 2014C
t = 113 d(B)SN 2008D (Ib)t ~ 6 months

SN 2014Ct = -2 d(A)(C)

Scaled ﬂambda + constant

Scaled ﬂambda + constant

(C)

(B)

(A)

Hα emission
dominates
spectrum

Emergent Hαemissionv ~ 1400 km/s

Weak Hαemission withv < 250 km/s

SN 2008D (Ib)t ~ max

4000

5000

6000
7000
8000
rest wavelength [angstroms]

9000

6200

Optical

6400
6600
6800
rest wavelength [angstroms]

7000

Adapted from Milisavljevic et al. (2015)

X-ray
Margutti, Kamble, DM+ 2017

Multi-wavelength characterization
As forward shock plows through circumstellar material, X-ray and radio emission is
produced that probes the mass loss environment.

Two distinct
regions of massloss

Chandra+NuSTAR

Anderson+ 2017
Adapted from Margutti, Kamble, DM+ 2017

See also interesting results by Tinyanont+ 2016 (Spitzer), Vinko et al. (2017), Sun et al. (2020),

Accelerated SN-SNR transition

Emission arises from various regions of shocked andphotoionized CSM and stellar ejecta. Many coronallines
Y_are observed. Emission from reverse-shock-heated metalrich ejecta is observed.
Y_qAccelerated SN-SNR transition

Y_

Y_q

QI”Not the brightest, but the hottest Type IIn Supernova” Smith+ 2009

Where did the H-rich CSM come from?
W-R phase?
Possible if W-R phase isshort and/or asymmetric
WR 134

LBV-like outburst?
Difficult to reconcile. Stellar populationsuggests stars < 10 Msun and littlehydrogen present at time of SN
Eta(PICO)
Car shel
Photoionization-conﬁned

CSM confinement?
Possible if W-R phase is very shortand/or mass-loss is very asymmetricWhere did the H-rich CSM come from?
W-R phase?
Possible if W-R phase isshort and/or asymmetric
WR 134

LBV-like outburst?
Difficult to reconcile. Stellar populationsuggests stars < 10 Msun and littlehydrogen present at time of SN
Eta(PICO)
Car shel
Photoionization-conﬁned

CSM confinement?
Possible if W-R phase is very shortand/or mass-loss is very asymmetric
Sun+ (2020) argue for CE ejection

Where did the H-rich CSM come from?
Emerging picture is that the CSM iscontained within the equatorial plane.
Density is approximately 105 to 106 cm-3.
Disk extends from around 1016 cm to1017 cm. Most estimates are around 1
Msun of material, but see Harris andNugent (2020).
Consistent with Thomas et al. (2022).

Brethauer, Margutti, DM et al. (2022)

“SUPERNOVA 1996cr: SN 1987A’s WILD COUSIN?”
Bauer et al. 2008
The progenitor of SN
1996cr evacuated alarge cavity just prior
to exploding: the blast
wave likely spentapproximately 1-2 yr in
relatively uninhibited
expansion before
eventually striking
dense CSM. The mostConclude that the progenitor changed
evolutionary states immediately prior toexplosion, likely transitioning from a WRlike wind to an even faster, less densewind, resulting in portions of the previous
CSM being swept up to form a wind-blowncavity surrounded by a dense shell.

Late-time interaction is increasingly
recognized across SN types and timescales
SN 2004dk: A Type Ib
that evolved into
Type IIn 12 years
after explosion.
Vinko et al. (2017) haveprogram for Halphamonitoring of nearby
SNe to detect thesesystems.
Mauerhan et al. (2018)

SN 2001em

An early spectrum indicates it exploded as a Type Ib
supernova. Later, the ejecta caught up with a dense
circumstellar H-shell, ejected a few thousand years before
the explosion, triggering interaction between thesupernova ejecta and the dense shell, producing radio, Xray, and Hα emission.

Estimating rates of observed eruptive behavior in SN Ib/c
In a sample of 60 SN Ib/c that haveconstraining radio observations,evidence of eruptions was found in 10%of progenitors during their last ∼ 500
years of evolution, but potentially toevery SN Ib/c progenitor if the process is
intrinsically active over a longer timescale of 5000 yr or more.

Margutti, Kamble, DM+ 2017

Supernova remnants provide detailed information about thenature of supernova explosions.
E0102
E0102Cassiopeia A A
Cassiopeia

G292

15 arcsec

N132D
Crab2 arcmin

Progenitor systems, mass loss,
explosion mechanisms, mixing, dust
formation, collapsed objects, …

Crab Nebula

SN 1054

Hubble Space
Telescope

Crab NebulaMartin, Milisavljevic, Drissen (2021)

SN 1054

Crab Nebula

3C 58

Cassiopeia A

Mercator projections showing
distribution of ejecta for threecore-collapse supernova
remnants.
Nature vs. Nurture:
structure imprinted by the
explosion vs. influence ofinteraction with surroundingenvironment.

Comparing morphology and chemistry between remnants is
now possible and can help resolve Nature vs. Nurture:
explosion dynamics vs. environment
N132D

Cassiopeia A

Milky Way340 yr

LMC
2500 yrboundaryboundary
torus

torus

Law, DM et al. (2020)

Simulations that
follow explosion
physics andinterior structure
Gabler et al. (2021)

Orlando et al. (2020)

Simulations that
follow SN/CSM
interaction
Polin, Duffell, DM (2022)
Galactic Autopsies: Supernovae with JWST

Orlando et al. (2022)
Dan Milisavljevic