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Faint Supernova or Super-AGB star?: SN 2008S in context. Margaret Meixner STScI Masaaki Otsuka STScI/ASIAA David Riebel JHU SEEDS consortium. SN2008S: Spitzer IRAC 3.6 micron. Day 17. Day 180. Wesson et al. (2009). - PowerPoint PPT Presentation
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Faint Supernova or Super-AGB star?: SN 2008S in context
Margaret Meixner STScIMasaaki Otsuka STScI/ASIAA
David Riebel JHUSEEDS consortium
SN2008S: Spitzer IRAC 3.6 micron
Wesson et al. (2009)
Day 17 Day 180
WHIRC (WIYN High Resolution InfraRed Camera) field: SN 2008S & SN 2002hh
Otsuka et al. submitted
SEEDS: The Search for Evolution of Emission from Dust in Supernovae
• Science Goal is to quantify the rate of dust production in Type-II SNe
• Track Type-II SNe light curves to very late times and look for simultaneous 3 observational signatures:– Sudden dimming of optical light (HST)– Brightening of mid-IR light (Spitzer)– Blue shifting of spectral lines (Hα, Gemini GMOS)
SN2008S Near-IR light curve
Otsuka et al. submitted
Otsuka et al. submitted
SN2008S Near-IR light curve
Otsuka et al. submitted
SN2008S Near-IR light curve
SN2008S: a faint supernova?
Otsuka et al. submitted
SEEDS sample & progenitor mass
SEEDS sample & light echo
SEEDS sample & dust production
SN2008S: a Super-AGB star? comparison to AGB stars in LMC
Riebel & Meixner 2011
Riebel & Meixner 2011
SN2008S: a Super-AGB star? comparison to AGB stars in LMC
SN2008S: Progenitor SED model carbon rich super-AGB star
Wesson et al. (2009)
Silicates
Amorphouscarbon
T~380 KL~3.2×104 LM~10 MMloss~5x10-7 M yr-1
Mtot ~0.01 M
SN 2008S illumination
Wesson et al. (2009)
Day 17
Day 180
SN2008S: Day 17 SED
Wesson et al. (2009)
T~550 KL~2.2×106 LLTOT~1.5×107 L
Amorphouscarbon
SN2008S: Day 180 SED
Wesson et al. (2009)
T~450 KL~3.6×105 LLTOT~1.2×106 L
Amorphouscarbon
Stellar Sources of Dust: Massive Stars
March 2011 Herschel & Characteristics of Dust in Galaxies - Meixner
Object classProgenitormass
Example sources
Dust Mass (M or Myr-1)
Dust composition
Gas-to-dust ratio/refs
Supernovae SN 2002hhSN 2003gdSN 2004etSN 2007itSN 1987A
0.1 <0.02 1.5×10-3
<10-4
~0.7
Amorphous silicates?,Amorphous carbon?
Barlow et al. 2002Sugerman et al. 2006Fabbri et al. 2011, sub.Andrews et al. 2011Otsuka et al. 2011, sub.Matsuura et al. 2011, acc.
Red Super Giant, 8-40 M
BetelgeuseMuCephVYCMaNML Cyg
3-10×10-10 5-8×10-9 1×10-6
6×10-6
Metal Oxides,Amorphous silicates,Metallic iron?
Verhoelst et al. 2009De Wit et al. 2008
Asymptotic Giant Branch stars, carbon rich, 2-4 M
VHyaIRC+10216AFGL 3068SN2008S?
2×10-9
2×10-8
1.6×10-7
5×10-7
Amorphous carbon, PAHs,MgS, SiC
700 Groenewegen 1998Jura 1986Jura & Kleinman 1989Wesson et al. 2009
Asymptotic Giant Branch stars, oxygen rich 0.8-2; 4-8 M
MiraW HyaRX BooOH 44.8-2.3OH 26.5+0.6
5.5×10-10
2×10-9
2×10-9
2.8×10-7
1.2×10-6
Silicates, amorphous & crystalline
280De Beck et al. 2010
Conclusions: SN 2008S• Most likely a Super-AGB star
– T~380 K– L~3.2×104 L
– M~10 M
– Mloss~5x10-7 M yr-1
– Mtot ~0.01 M (2x104 yr)
• Carbon rich circumstellar dust, interesting, unusual• Significant dust contributor in galaxies:
– Dust produced in “pre-explosion” phase– Massive enough could evolve fast enough to be important in early universe– May not destroy its own dust as with SNe
• Important to keep monitoring this field to see if we recover a progenitor