Revealing the mass of dust formedin the ejecta of SNe with ALMA
ALMAで探る超新星爆発時におけるダスト形成量

Takaya Nozawa(IPMU, University of Tokyo)
Collaborators;
M. Tanaka (IPMU), I. Sakon (University of Tokyo),
T. Kozasa, T. Minamidani (Hokkaido University),
K. Maeda, T. Moriya, K. Nomoto (IPMU) …
2011/1/31

1-1. SNe are important sources of dust?
・ Theoretical studies－ at dust formation : ~0.1-1 Msun in CCSNe (SNe II-P)(Nozawa+03; Todini & Ferrara 2001; Cherchneff & Dwek 2010)－ after destruction of dust by reverse shock :~0.01-0.5 Msun (Nozawa+07; Bianchi & Schneider 2007)

dust amount needed to explain massive dust at high-z!
・ Observational works－ MIR observations of dust-forming SNe : < 10-3 Msun(e.g., Ercolano+07; Sakon+09; Kotak+09)－ submm observations of SNRs : >1 Msun
(Dunne+03; Morgan+03; Dunne+09; Krause+05)－ MIR-FIR observation of Cas A SNR : 0.02-0.075 Msun
(Rho+08; Sibthorpe+09; Barlow+10)

1-2. Dust in Cassiopeia A
Nozawa+10, ApJ, 713, 356

・ total mass of dust formed
Mdust = 0.167 Msun・ shocked dust : 0.095 Msun
Md,warm ~ 0.008 Msun
・ unshocked dust :Md,cool ~ 0.072 Msun
with Tdust ~ 40 K

AKARI corrected 90 μm image

AKARI observation
Md,cool = 0.03-0.06 Msun
Tdust = 33-41 K(Sibthorpe+10)

Herschel observation
Md,cool = 0.075 Msun
Tdust ~ 35 K (Barlow+10)

1-3. Missing-dust problem in CCSNe
Tanaka, TN, +11, submitted to ApJ
theory1-4. Possible targets : SNRs in LMC and SMC
Tanaka, TN, +11, submitted to ApJextragalactic

Massive dust can behidden if Tdust < 100 K

2-1. Possible target (1): SN 1987A
on 4 Oct 2003
Gemini T-ReCS(λ = 10.36 μm)
2 pixels : 0.18”(Bouchet+04)
AKARI24 μm(Seok+08)

・ SN1987A in LMC－ Type-II peculiar－ age : 24 yr－ diameter : 2”(= 0.5 pc @ 50 kpc)
・ dust mass in ejecta－ Mdust > 1x10-4 Msun
(Wooden+93)－ Mdust = 0.23 Msun
(Kozasa+91)－ Mdust > 10-4 Msun
(Bouchet+04)

・ dust mass in ER－ Mdust=10-6-10-5 Msun
On 6 Jan and 1 Feb 2005 (Bouchet+06)(Seok+08, Dwek+08)

2-2. Expected detectability of SN 1987A

・ Case of Tdust = 50 K
5.0 mJy @ 450 μm (B9)
0.5 mJy @ 850 μm (B7)
0.1 mJy @ 1.3 mm (B6)・ Case of Tdust = 20 K
1.23 mJy @ 450 μm (B9)0.16 mJy @ 850 μm (B7)0.04 mJy @ 1.3 mm (B6)Rayleigh-Jeans law : Bν(T) = 2 ν2 k T / c2
Mdust = 0.1 Msun ➔ Fν(T) ∝ Mdust3-1. Possible target (2) : SNR 1E0102.2-7219
Spitzer; Stanimirovic+05

24 μm

70 μm

・ SNR 1E0102.2 in SMC－ O-rich (Type Ib?)
－ age : ~1000 yr－ diameter : ~40”(= 12 pc @ 60 kpc)
－ similar to Cas A
・ hot dust mass
－ Mdust = 8x10-4 Msun
(Stanimirovic+05)

Md,warm = 3x10-3 Msun

－ Mdust = 0.014 Msun
(Rho+09)・ cold dust mass
－ Md,cold < 0.6 Msun
with Tdust = 20 K
Sandstrom+09(Sandstrom+09)

3-2. Expected detectability of 1E0102.2-7219
Md,warm = 0.008 Msun
Md,cool = 0.072 Msun
with Tdust = 43 K

・ for the whole SNR
2.0 mJy @ 450 μm
0.24 mJy @ 850 μm
0.06 mJy @ 1.3 mm
・ one pixel resolution

R ~ 0.84”x(250m/L)
x(345GHz/ν)・ field of view~ 17” x (345GHz/ν)・ L = 25 m, diameter : ~40”
－ 450μm(675GHz) ➔ R=4” ➔ (0.02mJy/pixel) ➔ t = 78 d
－ 850μm(345GHz) ➔ R=8” ➔ (0.01mJy/pixel) ➔ t = 22 d
－ 1.3mm(230GHz) ➔ R=12” ➔ (0.005mJy/pixel) ➔ t = 25 d

4-1. Possible target (3) : Type Ia SNRs in LMC
AKARI, 24 μm (Seok+08)0509-67.5 (400 yr)

0519-69.0 (600 yr)

Spitzer, 24μm 70μm

Mdust < 1x10-3 Msun

Mdust < 3x10-3 Msun
(Borkowski+06)

・ shock-heated interstellar dust
➔ dust destruction by SNe

・ SNRs 0509-67.5 and0519-69.0 in LMC－ Type Ia SNRs
－ age : ~500 yr－ diameter : ~40”
・ There is no evidence
for dust formation innormal Type Ia SNe・ possible maximum
dust mass :Mdust = 0.1-0.2 Msun・ conservative upper
limit of dust mass :Mdust ~ 0.05 Msun
(Nozawa+11 to be submitted)4-2. Possible target (4) : SNR N49 in LMC
・ SNR N49 in LMC－ Mstar ~ 20 Msun
－ age : ~6000 yr－ diameter : 50”

・ SNR interacting with MCs－ Md,warm = 0.1-0.4 Msun
－ Md,cold ~ 10 Msuninteracting region (E blob) : 10”

ALMA(Herschel; Otsuka+10)

・ synchrotron emission➔ contribution and distribution

ALMA5. Summary
Revealing cold dust mass in SNe with ALMA !!
・ Possible targets : young SNRs in LMC and SMC－ SN 1987A in LMC
most feasible, but many competitors …
－ 1E0102.2-7219 in SMCtoo extended ➔ seems to be very hard
－ Type Ia SNRs 0509-67.5 and 0519.69.0 in LMC
if detected, very exciting, but most unfeasible …
－ N49 in LMC
synchrotron emission and/or radiation frominterstellar dust may be detectable