2019/02/06

Formation of dust andmolecules in supernovae
Takaya Nozawa(National Astronomical Observatory of Japan)

SN 1987A

Cassiopeia A

SNR 0509-67.5

1-1. Introduction
Question : Can supernovae (SNe) produce
molecules and dust grains?

Nozawa 2014, Astronomical Herald

2-1. Thermal emission from dust in SN 1987A
60day

200day415day615daylight curve(optical luminosity)

Whitelock+89- dust starts to form in theejecta at ~400 days

755day- dust mass ay 775 day:> ~10-4 Msun
(optically thin assumed)
Wooden+93

2-2. CO and SiO detection in SN 1987A
CO first overtone: 2.29-2.5 μm
CO fundamental: 4.65-6.0 μm
SiO fundamental: 7.6-9.5 μm

97 day200daySN Ic 2000ew, Gerardy+2002

415day615day58 day755daySN II-pec 1987A, Wooden+1993

SN II-P 2016adj, Banerjee+2018

2-3. CO and SiO masses in SN 1987A
COGerardy+2002, see also Banerjee+2018‐CO emission is seen in various
types of CCSNe from ~50 day

Liu+95SiO‐CO/SiO masses in SN 1987A
Mco > ~4x10-3 Msun
MSiO > ~7x10-4 Msun
Liu & Dalgarno 1996

2-4. Dust mass in Cassiopeia A (Cas A) SNR○ Estimated mass of dust in Cas A
・ warm/hot dust (80-300K)(3-7)x10-3 Msun (IRAS, Dwek et al. 1987)~7.7x10-5 Msun (ISO, Arendt et al. 1999)
0.02-0.054 Msun (Spitzer, Rho+2008)➜ Mdust = 10-4-10-2 Msun
consistent with >10-4 Msun in SN 1987A

Dwek+1987, IRASRho+2008
Spitzer

Arendt+1999, ISO

3-1. Dust formation in Type IIb SN○ SN IIb model (SN1993J-like model)- Meje = 2.94 Msun
MZAMS = 18 Msun
MH-env = 0.08 Msun

- E51 = 1- M(56Ni) = 0.07 Msun

3-2. Equations for dust formation calculations
・ Nucleation rate

Formation rate of stable
nuclei per volume

・ Grain growth

Growth rate of dust is independent of its size

・ Mass conservation

3-3. Results of dust formation calculations
mass distribution

Nozawa+2010

condensation time

- condensation time of dust
300-700 d after explosion- total mass of dust formed
・ Mdust = 0.167 Msun in SN IIb
・ Mdust = 0.1-1 Msun in SN II-P

➜ 5-10% of metal mass

3-4. Comparison with IR observations of Cas A
Cassiopeia AHerschel FIRobservation

0.008Msun of shockedwarm dust

0.07Msun of unshockedcool dust

Nozawa+2010

FIR observations with Herschel revealed thepresence of 0.06 Msun of cool dust inside Cas ABarlow+2011

4-1. Herschel detects cool dust in SN 1987A~180K~10-5 Msun
~20K
~0.5 Msun

Matsuura+2011, Science

Herschel detected cool (20K) dustof 0.4-0.7 Msun toward SN 1987A!
➜ Consistent with theoreticalprediction of Mdust =0.1-1 Msun

4-2. Resolving cool dust in SN 87A with ALMA
ALMA Cycle 0 Proposal‘Detecting cool dust in SN1987A’Band 7 (850 μm)

Band 9 (450 μm)（TN, Tanaka, et al.)2 arcsec

CASA simulation
with extended
config. (4 hrs)

0.1 Msun of silicate➔ 5σ detection at Band 9 !!

4-3. Successful ALMA proposals for SN 1987A

This proposal was ranked
in the highest priority !!

Our proposal was
not executedBand 9extended configuration

Band 3, 6, 7, 9
compact configuration

4-4. ALMA reveals dust formed in SN 1987A
ALMA, 1.4 mm

ALMA, 870 µm

ALMA, 450 µm

HST optical (HI)Chandra, X-ray

Indebetouw+2014

Our CASA simulation
Band 7 (850 μm)

SED of 25-years old SN 1987A

Band 9 (450 μm)

ALMA spatially resolves cool(~20K) dust of ~0.5 M sun formedin the ejecta of SN 1987A➔ SNe could be production
factories of dust grains

4-5. CO detection in SN 1987A with ALMA

Kamenetzky+13‐CO properties
blue: Hαgreen: [SiI]+[FeII] (1.64 µm)
red: CO(2-1)

Vco ~ 2200 km/s
Mco > 0.01 Msun
Tco > 14 K

‐For ALMA full operation,
3D maps of CO and SiO

4-6. 3D-structure of CO and SiO emission

Abellan+2017

4-7. CO detection in Cassiopeia A SNRAKARI IRC spectra

Herschel PACS

Rho+12- Mco ~ 6x10-7 -x10-6 Msun
- Tco = 400 K and 2400 K- knot density: 106-7 /cm3

CO was not destroyed by theshock or was reformed recently
Wallstrom+13

5-1. Observed dust mass in CC-SNe/SNRs
reverse shock
destruction??
missingcold dust?

Dust mass
increasing
with time?

??

NIR/MIR
Matsuura+2011
FIR/submm
Balow+2010
extinction

Gomez+2012

Dust mass formed in the ejecta is dominated by cold dust

5-2. Questions for dust formation in SNe(1) What fraction of newly formed dust cansurvive the destruction by reverse shock?
- theory: ~5-50 % (Mdust ~ 0.01-0.1 Msun per CCSN)- obs.: very hard to detect dust from more extended SNRs

(2) When do the majority of grains form?
- theory (1-3 yr) vs obs (~10-20 yr)- JWST will not be able to resolve this question- ALMA can disclose it if CCSNe happen in MW and L/SMC(3) Can dust (and molecules) form in SNe Ia?

6-1. No dust in the ejecta of Type Ia SNRs
Cas A (Type IIb)

Kepler (Type Ia)
70 μm

Tycho (Type Ia)

100 μm

250 μmHerschel
100 µmimage

850 μmBarlow+2011

160 μm500 μmCOGomez, Clark, TN, +2012

Herschel detected no cool dust in Galactic Type Ia
SNRs, Kepler and Tycho (Mdust < ~10-3 Msun)

6 cm

6-2. No evidence for dust formation in SNe Ia〇 Hard to observe SNe Ia in IR- SNe Ia fade more rapidly➜ Luminosity is small at >100 day- SNe Ia hardly occur in nearbygalaxies➜ too far to be detected in MIR- SN 2011fe and SN 2014J➜ Spitzer stopped MIR obs in 2009

MIR obs of SN 2005bf
at day 200 and 400(Gerardy+2007)

6-3. MIR Observations of SN 2014J with Subaru
N11.7 Band (at 370 day, 8000 sec)
SN 2014J （optical）
Subaru/COMICS

T. Nozawa et al. unpublished〇 No detection of SN 2014J with Subaru/COMICS
・ No massive amounts of dust grains formed in the ejecta(Mdust < ~0.1 Msun)
・ No massive circumstellar dust grains around SN 2014J

6-4. Suppressed formation of dust in SNe Ia?
W7 SN Ia model (C-deflagration)(Nomoto+1984; Thielemann+1986)

Condensation time

Mdust ~ 0.1 Msun

Nozawa+2011〇 SNe Ia are harsher than CCSNe?
M(56Ni) ~ 0.6 Msun ➜ 10 times higher than that of CCSNedust and molecules can be destroyed by energetic
photons and electrons prevailing in the ejecta

6-5. Can ALMA detect dust in SNe Ia?
- extragalactic SNe are too far (D > 1 Mpc) to detect thethermal emission from cool dust in ejecta with ALMA

- young Galactic SNRs are too extended (θ > 1 arcmin)for good spatial resolution of ALMA (~0.1 arcsec)

young (compact) SNRs in LMC/SMC !
〇 SNR 0509-67.5

HαX-ray- Type Ia SNe- age : ~400 yr- in LMC (d=50 kpc)

Borkowski+2006

6-6. SNR 0509-67.5 is too extended!
Band 3 with ACA

Band 3
Band 9 with ACA

SN 1987A

30 arcsec

6-7. Fe grains formed in SNR 0509?
optical image of SNR 0509-67.5 in LMC
Radius of the central circle :1.5” = 1.1x1018 cm @ 50 kpc

Vexp = 850 km/s @ 410 yrcorresponds to Fe core !

Supposition
Diffuse emission within thecentral circle may be opticallights scattered by Fe grainsformed in the ejecta

Schaefer & Pagnotta+2012

6-8. Expected SEDs of Fe grain emission
ALMA Cycle 2 Proposal“Detecting cool dust in Type Ia
supernova remnant 0509-67.5”

ranked as priority grade B

If the source is detected, this is the first detectionof the formation of massive dust grains in SNe Ia !

6-9. ALMA Observation of SNR 0509-67.5
HST （optical）

ALMA （Band 6, 1.2 mm）

HST （H band）

ALMA

Nozawa et al., unpublishedPagnotta+2014〇 No detection in Band 6・ Massive Fe grains are not formedin Type Ia SNe (< ~0.1 Msun）
5 σ limit

・ Diffuse source is a backgroundgalaxy at z=0.031 (Pagnotta+2014)

7-1. Next challenge to SNe Ia?
Aiming at first detection of molecules in SNe Ia

Band 6Band 330 arcsec

7-2. Explosion mechanism of SNe Ia
Detection of molecules can gives insight into
- explosion mechanism of SNe Ia- physical condition of the expanding ejecta
Deflagration

unburned carbon : 0.05 M sun

Detonation

unburned carbon : <0.01 M sun7-3. Summary of this talk‐CCSNe are production factories of dust and molecules➜ Theoretical calculations predicts 0.1-1 Msun of dust formed➜ ALMA and Herschel confirmed the presence of a large
amount of dust in the ejecta of CC-SNe/SNRs➜ Still unclear what fraction of dust grains can survive thedestruction in reverse shocks and be injected into the ISM‐hard to detect thermal emission from cool dust in any
SNe/SNRs other than SN 1987A with ALMA
➜ even the youngest SNR in LMC/SMC are too extended➜ if SNe happen in MW or L/SMC, we see cool dust with ALMA

‐There is no evidence for the formation of dust andmolecules in SNe Ia