X-ray and Radio observations of (interacting) SNe

Keiichi Maeda
Kyoto University
keiichi.maeda@kusastro.Kyoto-u.ac.jp

MIAPP WS on Interacting SNe,
16 February, 2023

Outline• General concepts of X and radio from the interaction.
• Overall properties of different SN types.
– Mass-loss sequence. SNe IIn diverse. Asymmetric CSM (IIn/Ia-CSM).
Ibn very different than SNe IIn in the mass-loss history.

• Infant phase (~< 10 days).
– Radio complementary to optical search for the “confined CSM”. Can go to
the “less-dense” CSM. At least one SN Ic (2020oi) w/ “sub-yr” variability.

• Late-phase / late-interaction (> yrs).
– SN⇒SNR depends on the mass-loss history. Ia SNR = “young”. Do we see
the outer edge of the CSM (probably yes in some, but no others)?

• One of my recent favorites: SN IIL 2018ivc.
– Interaction power dominating. Infant to late-time interaction. Boundary
b/w a single and binary?

A Rough Picture (to be tested)
Progenitor

Mass loss
RSG

IIP/L

Dense CSM
in the vicinity

IIn

YSG

IIb

LBV?
CE?
BSG

Ib
Ic
Decreasing
radiusMass stripping sequence
WR
Single star or binary?
Timing?
More CSM Mass-loss mechanisms?
(where?) CSM – where and how much?

Mass loss process?
Smith 2017

X & Radio: Unique probe to the CSM
Young (< ~Years)
Extragalactic (> 10 Mpc)

Thermal: opt－IR

Shock wave

Radio: Synchrotron
X: Inverse Compton (low density)
Thermal (high density CSM)

Examples of SN radio data (SESNe)

SN IIb 2011dh:
Soderberg+ 2012
SN IIb 1993J:
Weiler+ 2007

Model example: SESN

Overall properties of ejecta and CSM
Multi-band light curves

SED evolution
Day 100

Day 10Day 1

νpeak ∝t-1

50 GHz5 GHz

tp ∝ν-1

Steady-state
mass loss (ρ∝r-2)# Cooling & free-freeabsorption omitted

Generally, higher-ν peaks earlier (becoming optically thin earlier):⇒ inner CSM information obtained easier at higher frequency.
“For steady-state mass-loss”, tp∝ν⇒ represented by a single frequency (frequently @ ~5 GHz).

Overall properties of ejecta and CSM
Model example (type IIb/Ib/Ic SNe): Model example (type IIb/Ib/Ic SNe):Fixed ejecta + different CSM density Fixed CSM + different ejecta properties
10-5 M yr-1
(vw/1000 km s-1)
10-6

2M, 5x1051 erg(high vel.)

10-4
2M,
1051 erg

Larger E/M

DenserCSM

Optically Optically
thin
thick
Steady-state
mass loss (ρ∝r-2)

5M, 1051 erg(low shock vel.)# Cooling & free-freeabsorption omitted

Rise ⇒ decay: peak = Synchrotron self-absorption (SSA)
Peak properties (tp, Lp) ⇔ CSM density + ejecta properties# can roughly constrain the acceleration mechanism by SED and evolution.

Radio Supernova Phase SpacePeak time vs. Peak L
Chevalier+ 06

V↑
V=constρCSM↑
Mass loss↑@100GHz~10d~1d@30Mpc10 SNe/yr@10Mpc0.4 SNe/yr
D for 1mJy

Bietenholz+2021

Time scale at ~5GHz (reduced by 5GHz/100GHz for mm)

X-rayDwarkadas+ 14

Generally, IIP ⇒ IIb/Ib/Ic ⇒ IIL ⇒ IIn
ρCSM
E/M

X-ray emission mechanism(s)Chevalier+Fransson
2006/2017
Forward Shock(FS)
Reverse Shock(RS)

FS: high T, low ρ, hard X
RS: low T, high ρ, soft X
Mostly thermal, but
possibly additional inverse
Compton (IC) at FS.

Fransson+ 96
FS

RS
FS

RS

See Chevalier+Fransson 2006, 2017 – everything is there.

Detailed study:
SN IIb 1993J

Fransson+Bjornsson 96

Roughly ρ∝r-2

If CSM edge,~ 5000 yrs
before the SN

Hard X (FS)Soft X (RS)
Chandra+09

Outline• General concepts of X and radio from the interaction.
• Overall properties of different SN types.
– Mass-loss sequence. SNe IIn diverse. Asymmetric CSM (IIn/Ia-CSM).
Ibn very different than SNe IIn in the mass-loss history.

• Infant phase (~< 10 days).
– Radio complementary to optical search for the “confined CSM”. Can go to
the “less-dense” CSM. At least one SN Ic (2020oi) w/ “sub-yr” variability.

• Late-phase / late-interaction (> yrs).
– SN⇒SNR depends on the mass-loss history. Ia SNR = “young”. Do we see
the outer edge of the CSM (probably yes in some, but no others)?

• One of my recent favorites: SN IIL 2018ivc.
– Interaction power dominating. Infant to late-time interaction. Boundary
b/w a single and binary?

Radio Supernova Phase SpacePeak time vs. Peak L
Chevalier+ 06

V↑
V=constρCSM↑
Mass loss↑@100GHz~10d~1d@30Mpc10 SNe/yr@10Mpc0.4 SNe/yr
D for 1mJy

Bietenholz+2021

Time scale at ~5GHz (reduced by 5GHz/100GHz for mm)

SNe II vs. SNe Ib/c

Chevalier+ 2006

Chevalier+Fransson 2006

SNe IIP~(0.1-1) 10-5 M yr-1
In line withSN IIP = RSG, Ib/c = WR?
SNe Ib/Ic~(1-30) 10-5 M yr-1

SN IIn 2010jl
10jl, bol

10jl, X

10jl, NH

Chandra+15< 400 days: ρ∝r-2,
0.02-0.2 M/yr (KM+ 13)> 0.1 M/yr, vw~100 km/s
(Fransson+ 14),
0.8 M/yr (Ofek+ 14)> 400 days: break
MCSM > Mej? Ofek+14
CSM breakout? Fransson+ 14- Then MCSM >~ 3M (only inthe final ~ 30 yrs).
And hints of asymmetric CSM(Fransson+ 14).

06jd, bol

SN IIn 2006jd
06jd, X
Chandra+12

Chandra+15

Lx ~ 0.1 x Lbol (X-bright)
CSM flatter than r-2… diversity(different evolution than 10jl)
Asymmetric CSM?
(emission≠absorption)

SN IIn 2017hcc
Lx < 0.001 x Lbol @ < 100 day
Increasing mass-loss toward the
SN in the last decade?
Asymmetric CSM?
(Lbol >> Lx, Lradio: X/radio faint)

Chandra+ 22

0.1 0.02<10-3 M/yr

Moran+ 23
Chandra+ 22

CSM geometry?
Optical spectral evolution?

Polarization (optical)
IIn up tp 5%≫ non—int. SNe
17hcc

Kumar+ 19

Smith+ 15

CSM geometry?
Key to understanding the
mass-loss mechanism, butchallenging (point source).
X-ray from SNe IIn:
Disappearing absorbed+ Emerging unabsorbed.
“Torus” (~ AGN, but w/ time
evolution).

Katsuda, KM+ 16

Hard-X
critical.

Ia-CSM 2020eyj
Delayed interaction w/ He-rich CSM
Low mass, low-metallicty star-forming galaxy
Kool+ 22

Ia-CSM 2020eyj# No X-ray detection at ~ 800 daysby SWIFT, < 2.4e41 erg/s.

Kool+ 22

Mdot ~ 10-3 – 10-2
Mcsm ~ 0.3-1# solar mass/yr

CSM Properties
in Ia-CSM?

Uno+ 23ab

Yang, …, KM+ 23

A few M(?), asymmetric/axisymmetricUno, KM+ 23a
Uno, Nagao, KM+ 23b

SNe Ibn (and Icn?)

X: rising due to decreasing κ to X(⇒composition, X(C) > 0.1 for 06jc)

Chugai 09

r-3
r-2

Increasing toward the SN
Typically MCSM ~ 0.2M

KM+Moriya 23

Outline• General concepts of X and radio from the interaction.
• Overall properties of different SN types.
– Mass-loss sequence. SNe IIn diverse. Asymmetric CSM (IIn/Ia-CSM).
Ibn very different than SNe IIn in the mass-loss history.

• Infant phase (~< 10 days).
– Radio complementary to optical search for the “confined CSM”. Can go to
the “less-dense” CSM. At least one SN Ic (2020oi) w/ “sub-yr” variability.

• Late-phase / late-interaction (> yrs).
– SN⇒SNR depends on the mass-loss history. Ia SNR = “young”. Do we see
the outer edge of the CSM (probably yes in some, but no others)?

• One of my recent favorites: SN IIL 2018ivc.
– Interaction power dominating. Infant to late-time interaction. Boundary
b/w a single and binary?

“Flash”
optical spectroscopy
Recombination from the massive
CSM near the SN???
→ So far mostly for SNe II(RSG). Potentially biased
toward the dense CSM.
Gal-Yam+ 14, Khazov+ 16,
Yaron+ 17, Bruch+ 21/22“First day”

Narrow Emission (CSM)
Broad Absorption (SN)
Yaron+ 17
iPTF13dqy= SN2013fs

Mass loss in the final decades for some SNe IIP (RSG)
SN II (RSG)
Optical detection
10-3 M/yr (w/ vw=10 km/s

⇒ final 30 yrs)

Radio non-detection

10-6 M/yr

Yaron+ 17
iPTF13dqy = SN2013fs

1015cm ⇒final ~30 yrs for the
RSG wind (~ 10 km/s)

Dense CSM within 1015cm (Type II SN = RSG progenitor)

Early optical LCs (IIP)
Peaks in multi bands
Confined CSM?
# mass-loss rate different for different
models (typically ~ 0.1 M/yr by
Morozova+, but ~ 10-3 M/yr by Moriya+).
⇒Need something independent.

Morovova+ 17
Forster+ 18

Radio (High freq.) within 10 days of SN
100 GHz-3
1010-2 M/yr
10-4

SNe IIP (RSG) w/ “confined” CSM(+ outer low-density CSM).
Issues in the optical window:

Matsuoka, KM, Lee,
Yasuda 2019

250 GHz- Interpretation complicated.
- Bias toward the dense(st) CSM.
- Probable bias toward SNe II (RSG).
mm obs. overwhelms these difficulties:
ALMA cycles 5-7, 9 (KM+)- No CSM, no radio (⇔ optical).
- Optically thin (⇔cm suppressed).
Need: Quick observations within~ a week (challenging but doable).

Going closer to the CSM @ 1015cm (given “SN” age)~ 30 yrs for an RSG (SNe II)
moment of explosion ~ 0.3 yrs for a WR (SNe Ib/c)Fe

Type IIFor given mass-loss rate,

ρCSM x 0.01 (no trace in the optical).

SNe II:Red Supergiant (H envelope)
RSG
TypeExtendedIa⇒ vw~ 10km/s

Ca

Ca

O

Type Ib
Fe

Na Si

O

WR-likeType Ic
SNe Ib/Ic
Wolf-Rayet-like star (He/CO)
Compact ⇒ vw ~ 1000 km/s

From mass-loss “rate” to “history”
LC w/ cooling and free-free abs.

SED changed by the cooling
Day 17

InverseComptoncooling

w/o coolingfν∝ν-1w/ coolingFν∝ν-1.5

free-freeabsorption
Steady-state
mass loss (ρ∝r-2)

Need to take into account the cooling and free-free absorption.
These processes provide an additional “constraint” to robustly
constrain parameters for electron acceleration physics (reasonably
accurate estimate on the ejecta and CSM properties).

From mass-loss “rate” to “history”
LCs for different CSM slope

SED
Day 17

s=1.5
s=2
s=2.5

ρ∝r-s

SED slope is independent from the CSM distribution.
Temporal evolution ⇒ CSM density distribution.
Optically-thin regime important.

Project w/ ALMA
• We want optically-thin emission⇒high frequency.
– CSM density is higher for the inner region = earlier epoch(shock expands).

• Synchrotron emission: fν∝ν-1 to ν-1.5⇒ (relatively) faint point source.
• SN embedded in a host galaxy (SF region + AGN)
⇒ high spatial resolution.
• Need:high-sensitivity + angular resolution at >~ 100 GHz.

A nearby SN Ic 2020oi @ M100 (~ 14 Mpc)
Rho+ 20

Discovery on 7
Jan 2020@ ~ 1 day of
explosion.
Discover within a few days of SN explosion is now common⇒ quick follow-up possible. ALMA ToO triggered (@ 100 GHz).
SN Ic = Compact C+O star, vw ~ 1000 km/s:
CSM @ < 1015cm ⇒ mass loss @ <1 yr before SN.

ALMA ToO obs. at 100 GHz (band 3):First infant SN seen by ALMA
5.4 days
0-1.5 mJy

8.4 days
0-1.5 m Jy

18.4 days
0-0.3 mJy

51.3 days
0-0.3 mJy

KM+,
2021

SN 2020oi in the optically thin limit

KM+, 2021
Low freq. data (VLT, etc)from Horesh+ 2020

Optically thin @ 100 GHz from the beginning.
Spectral fattening: Inverse Compton (IC) cooling to adiabatic.
Optically thin & cooling effect well understood⇒ reconstruction of the CSM density distribution.

First infant SN seen by ALMA: SN Ic 2020oi
Multi-band LC

Derived mass-loss history
SNe IIKM+ 2021

VLA data from Horesh+ 2020, ALMA from KM+ 2021.
Overall mass-loss rate in the final few yrs for SN Ic 2020oi~ the (enhanced) mass-loss rate in the final decades for SN II.

Sub-year timescale variability toward the SN.

Outline• General concepts of X and radio from the interaction.
• Overall properties of different SN types.
– Mass-loss sequence. SNe IIn diverse. Asymmetric CSM (IIn/Ia-CSM).
Ibn very different than SNe IIn in the mass-loss history.

• Infant phase (~< 10 days).
– Radio complementary to optical search for the “confined CSM”. Can go to
the “less-dense” CSM. At least one SN Ic (2020oi) w/ “sub-yr” variability.

• Late-phase / late-interaction (> yrs).
– SN⇒SNR depends on the mass-loss history. Ia SNR = “young”. Do we see
the outer edge of the CSM (probably yes in some, but no others)?

• One of my recent favorites: SN IIL 2018ivc.
– Interaction power dominating. Infant to late-time interaction. Boundary
b/w a single and binary?

Late-phase: SN to SNR
Expectation:“SNe II”: bright ⇒ faint“SESNe”: faint ⇒ bright
Mass-loss history recorded in
the SNR phase.
SNR samples may be biased.

Yasuda, Lee,KM 2021/2022“II” (MS⇒RSG)“II” (MS⇒RSG)“SESN”(MS⇒RLOF⇒He)“SESN”(MS⇒RLOF⇒He/CO)

SNe Ia SNR: CSM around Kepler
Ia-CSM
91T
KeplerKepler SNR
Katsuda, Moti, KM+ 2015

Ejecta abundance & hist. LC⇒bright 91T-like, no Ia-CSM
CSM properties⇒Mass loss history:> 0.3M @ 2pc (104-5 yrs)

PTF 11kx ~ 1 M 0.01pc(Ia-CSM) (~ 100 – 1000 yrs)

SNe Ia SNR:
Tycho environment

Deceleration
Interaction w/
Molecular cloud.
Progenitor systems
born in a MC.
Tanaka, …, KM+ 2021

Type IIn 1996cr

Continuous distribution
rather than distinct shell(s)~shell, not disk?

Bietenholz+ 2023

~ 1500 yrs back if
vw ~ 100 km/s

Extreme IIn-like SN?
MAXI counterpart ~ 3 yrs before
the 5GHz peak. Engine-driven?
Otherwise, looks like an extreme
end of SNe IIn? (Dillon’s talk?)

Dong+ 21

SESNe w/ strong and “delayed” CSM interaction

Margutti+ 17

Observationally rareso far (?), ~ 10%.
Can be intrinsicallycommon.

A case for SN Ib 2014C

Margutti+ 17

Anderson+ 17

2014C: keep evolving
Dense CSM passed through, thenLess-dense (but still dense) “r-2”CSM.
ρCSM∝r-2

Tinyanont, …, KM+ 19

Outline• General concepts of X and radio from the interaction.
• Overall properties of different SN types.
– Mass-loss sequence. SNe IIn diverse. Asymmetric CSM (IIn/Ia-CSM).
Ibn very different than SNe IIn in the mass-loss history.

• Infant phase (~< 10 days).
– Radio complementary to optical search for the “confined CSM”. Can go to
the “less-dense” CSM. At least one SN Ic (2020oi) w/ “sub-yr” variability.

• Late-phase / late-interaction (> yrs).
– SN⇒SNR depends on the mass-loss history. Ia SNR = “young”. Do we see
the outer edge of the CSM (probably yes in some, but no others)?

• One of my recent favorites: SN IIL 2018ivc.
– Interaction power dominating. Infant to late-time interaction. Boundary
b/w a single and binary?

A case for (peculiar) SN IIL 2018ivc
Bostroem+ 2020

Pre-SN progenitor limit:< 12M or > 50M(relatively) faintRapid decay (~ rapid transient)
Emission lines

KM+, 2023a

ALMA ToO + DDT

100 GHz250 GHz~4 day[0:10 mJy]

[0:5 mJy]~7day~17 day

Ejecta properties must be similar
to SNe IIb (w/ H-env. of ~ 1M)Consistent w/ Mms < 12M in abinary.

~200 day[0:0.5 mJy]

[0:0.2 mJy]

Infant phase ≠ a single power-law
No solution possible with a single ρ∝r-2 CSM.
Flat (inner) → Steep (outer) CSM distribution.

> 20 dayρ∝r-2.5< 20 dayρ∝r-1.6

Model: ~ SN IIb 1993J ejecta + dense CSM

Any hint in other observables? Yes… in the optical.

CSM interaction also seen in the optical?

The optical emission also shows the flat-to-steep evolution.

Optical/X-ray emission by
the CSM interaction
CSM interaction dominates in all the wavelengths.

w/ the same
CSM used for radio.

SN-CSM interaction
model from
KM+Moriya 2022

CSM distribution and mass-loss history

Somewhat dense, butsimilarity to SN IIb 1993J.
Ejecta properties alsosimilar.
Mass-loss rate
~10-4 M yr-1.
KM+ in prep.

A variant of (canonical)
SN IIb 1993J?

IIP⇒IIL⇒IIb transition in the binary evolution?
Ouchi+KM
2017 (c.f.,Yoon)

Ouchi+KM
2017

past

SN

High-mass loss rate.
Expected rate~ 10% of SNe IIb(roughly ok with the observed
fraction).
Detached shell?

SN 2018ivc: resurrection

SN Ib
2014C

Keeps looking at it : archival + DDT

Mutie+ ATel #15521

SN IIL (~ SN IIb?)
2018ivc
KM+, 2023b

The first example of the rebrightening in mm (to my knowledge).
The second example of the “SN IIb” late-time interaction clearlyseen in the radio (as far as I am aware of).

Modeling for large-scale CSM distribution

Outer CSM denser thanthe extrapolation fromthe inner region (~ x10).
Higher mass-loss rate
toward the past.

Modeling for large-scale CSM distribution

C-burn.
~10-3 M yr-1 @ ~ 1,000 yrs before the SN, then kept ~ 10-4 M yr-1.
Sudden mass loss at the carbon burning phase (following the expansion).
Boundary between the “binary” and “single” in the orbital separation.
・ Prediction (e.g., Ouchi & Maeda 2017; also work by Yoon et al.):Huge mass-loss at he beginning of the interaction.
Mass-ratio inverted → stable (but high-mass loss) RLOF.
# CE as an alternative? The “inflation” may change the picture quantitatively.

ALMA Cycle 9 (Oct 2022-) + ATCA + GMRT

Rapid ToO for infant CCSNe.
Cycle 9 targets: one SN II and one SN Ib/Ic (ALMA back in March).

Summary• General concepts of X and radio from the interaction.
• Overall properties of different SN types.
– Mass-loss sequence. SNe IIn diverse. Asymmetric CSM (IIn/Ia-CSM).
Ibn very different than SNe IIn in the mass-loss history.

• Infant phase (~< 10 days).
– Radio complementary to optical search for the “confined CSM”. Can go to
the “less-dense” CSM. At least one SN Ic (2020oi) w/ “sub-yr” variability.

• Late-phase / late-interaction (> yrs).
– SN⇒SNR depends on the mass-loss history. Ia SNR = “young”. Do we see
the outer edge of the CSM (probably yes in some, but no others)?

• One of my recent favorites: SN IIL 2018ivc.
– Interaction power dominating. Infant to late-time interaction. Boundary
b/w a single and binary?