s e r in TyPe Ia Supernovae: Keiichi Maeda · 2011. 4. 14. · Spectroscopic Typing⇒Progenitor H...
Transcript of s e r in TyPe Ia Supernovae: Keiichi Maeda · 2011. 4. 14. · Spectroscopic Typing⇒Progenitor H...
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in TyPe Ia Supernovae: An Origin of Their Observational Diversities?
Keiichi MaedaInst. for the Phys. and Math. of the Universe (IPMU),
University of Tokyo
s e r
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Observational Characteristics of Supernovae
• > 500 discoveries a year (557 for 2006, 584 for 2007).
–Only a part (nearby) observed in detail.
• Distance > ~ 10 Mpc (extragalactic).
–Point sources. – Typical maximum mag. V > ~ 16 mag (roughly).
• Most of obs. = Optical.
– Imaging + spectra (time-dep.)
Supernova Physics(e.g., exp. mech.)
Interpretation
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Spectroscopic Typing⇒Progenitor
H
Si
He
Type II
Type Ia
Type Ib
Type Ic
Fe
Fe
FeS
SiFeO
Na
Si
O
Ca
CaSi
C+O
He
H-rich
Fe
Si
C+O
He
H-rich
Fe
Si
C+O
He
H-rich
Fe
Ib/c: massive He/CO star。
Ia:white dwarf(thermonuclear)。
Emission process is the same.
SN explosion Nucleosynthesis
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Emission Process in SNe Ia (and Ib/c)
• Power source: 56Ni⇒56Co⇒56Fe.8.8 day 113 day ⇒ ~ 1 MeV γ (+ e+)
Log (Optical Luminosity)
Time
R = V t
ρ ∝ R-3∝t-3
Early Phase Late Phase
~ 50 day
~ 20 day
Thick
Thin
~ 200 day
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Type Ia Supernovae and cosmology
• Thermonuclear runaway of a white-dwarf (WD).
– An explosion of a Chandrasekhar-mass WD.
– No central remnant left.
• “Homogeneous” light curves→standard candles.
– Light curve time scale∝Luminosity← 56Ni mass.
– ΩΛ ~ 0.73!
e.g., Nomoto+ 1984 (“w7 model”)
e.g., Phillips 1993 (“Phillips relation”)
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Theory, Observation, then Unification?
• Observational diversities. – KM+, 2010, Nature, 466, 82.
– KM+, 2011, MNRAS, in press
s e r
• Off-set SN Ia model. – KM+, 2010, ApJ, 712, 624.
• observational evidence. – KM+, 2010, ApJ, 708, 1703.
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Asymmetric explosions?
• Details of the exp. not yet clarified.
• “spherical” explosion is standard, but it
does not have to be in theories.
Dipole Convection in progenitor WD (Kuhlen+ 06)
Kasen, Roepke, Woosley, 2009
Δm15 (Light curve time scale)
Peak
B
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But NO observational evidence• Theorists have started thinking about the
“asymmetric” explosion in these days. • Roepke+07, Jordan+08, Kasen+09.
• Big problem here. – (Some) models may explain some observations, which
can however be explained by SPHERICAL models as well.
• We need direct evidence, which contradicts any spherical models.
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Where to look into? High-density Ash!
• Example: Ignition at an offset (near the center).
time
KM, Roepke, Fink, Hillebrandt, Travaglio, Thielemann, 2010, ApJ, 712, 624
Def. Ash = STABLE Fe+Ni, High Density
Det. Ash = 56Ni (SN power!), Low Density
Deflagration Detonation Fe-peak elements
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How? Late-time spectra
• Just simple… Doppler shift diagnostic of
homologously expanding & transparent ejecta.
• Simple, but not easy… faint (radioactive decay⇒~ 21 – 23 mag)
• Successful for SNe Ib/c to show their asymmetric nature. • KM, Kawabata, Mazzali+, 2008, Science, 319, 1220.
• Modjaz+08, Taubenberger+09.
week ~ month year
ExpansionRedshift
Blueshift No shift
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Doppler shift diagnostics for SNe Ia
• STABLE Fe+Ni, high density… “Def. Ash”– Low ionization(+1), low temperature (~ 5000K).
• Representative = [Fe II]7155, [Ni II]7378.
• 56Ni, low density… “Det. Ash”– High ionization(+2), high temperature (~ 10000K).
• Representative = [Fe III]4701.
Jn
n
n
n
nn
Je
i
i
i
ie
eff
1114
Ionization / particle
56Ni/Co/Fe: radioactive input
e
exeline
T
TnnL exp0
Thermal Balance
Excitation T of a line
KM, Taubenberger, Sollerman+, 2010, ApJ, 708, 1703
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It is there! The first evidence of asymmetry
Center = Rest. Center ≠ Rest.
[Fe III]4700 [NiII]7378[FeII]7155Obs. Obs. Obs.Model Model
Different Angles
• No-shift in [Fe III] does not necessarily support spherical explosions!
• Got to see lower ionization+lower Tex lines.
KM, Taubenberger, Sollerman+, 2010, ApJ, 708, 1703
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Evidences… not model dependent. • Purely observational statements.
No correlation w/ epoch. The shift does not evolve for each SN. Large variation of the Doppler shift.
→ Offset + viewing angle.
Correlation w/ epoch. The shift evolves with time. Little variation for given epoch. → Radiation transfer. Spherical.
[Fe II]/[Ni II]
[Fe III]
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A strong case: 2003hv
• Two categories in lines.– No shift.– blue-shift.
• The shift behavior
as expected.
56Ni, low ρ
Steble Fe+Ni, high ρ
Obs. from Motohara+06, Gerardy+07, Leloudas+ 09
Looks like spherical, if you look
at only this line! (as people did.)
Toy model
Computation by 3D nebular code by KM+ 2006
opt opt
opt NIR
NIR IR
ObsOff-set
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Tackling Observational Diversities• Expectation.
– SNe Ia look different for different viewing direction.
• Any implications in Observations?– Spectral Evolution Diversity.– Peak Color Diversity.
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Time R = vt(outer=faster)
Time
Velocity of absorbing materials decreases with time.
The way different for different SNe.
Spectral evolution diversity
SN 2002bo
Rapid evolution
SN 1998bu
Slow evolution
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Spectral evolution diversity
HVG
LVG
• Spectral evolution does not correlate with the “luminosity”. – The no-correlation noticed by Benetti+05, raising a challenge to
the concept of “SNe Ia = uniform class = good standard candles”
Days
Si II absorption velocity Si II absorption velocity / day
Light curve time scale = Luminosity indicator
HVG
LVG
HVG/LVG = High/Low Velocity Gradient
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Just a viewing angle!
Wavelength Shift of [Fe II]7155+[Ni II] 7378 = viewing angle
Speed of the spectral evolution (Velocity Gradient)
• Prob. for chance coincidence
= 0.06%
HVG all viewed at the direction
OPPOSITE to the deflagration ash.
KM, Benetti, Stritzinger+, 2010, Nature, 466, 82
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“typical” SN Ia configuration
Distribution of wavelength shift
Number ratios HVG/LVG
• One assumption:
• Off-set = 3,500 km s-1 for the deflagration ash is generic.
• Two independent information
points to the same config.
• 105-110o for the transition angle.
Shift = -3,500 km s-1 ×cosθLVG: -3,000 < θ < 1,000 km s-1
HVG: 1,000 < θ < 3,000 km s-1
θ0= acos(-1000/3500)
HVG:LVG = 1:2 (numbers)1-cosθ0/1+cosθ0= LVG/HVG = 2
θ0
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Diversity in Color?
• Why does it matter? – Essential in SN cosmology.
• Observed color + magnitude → distance.
– extinction = observed color – intrinsic color.
– distance = obs. mag. – absolute mag. – extinction
• Intrinsic color depends on
– Light curve shape.
– +alpha → color diversity.
“Low-reddening SNe”
KM, Leloudas, Stritzinger+, 2011, MNRAS, in press
Light Curve Shape
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• “low-reddening SNe” → observed color ~ intrinsic.
– Either in E/S0 or in the outskirts.
• “Viewing direction” → intrinsic color variation (?).
– C.f., HVGs are red (Pignata+ 08, Wang+09).
“Low-reddening SNe”
Light Curve (LC) Shape
Observed color w/ LC correction
Nebular velocity shift
residual
Intrinsic color variation from asymmetryKM, Leloudas, Stritzinger+, 2011, MNRAS, in press
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Host extinction: Real or Artifact?
• A part (not all) of the previously derived “host extinction” may be due to “intrinsic color”.
– Host extinction should be revised.“Low-reddening” SNe (host morphology) No selection for reddening
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Asymmetry → Observational Diversities
θ0
+ Bluer color
+ Redder color
First-order
Not seriously affecting
distance measurement (random/statistic effect )
Second-order
Better distance calibration?
(color/extinction estimate)
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Conclusions
• Is a generic feature.
– Late-time spectra have provided the first evidence.
• Strong support for the “one-sided” nature.
–Solves a part of “diversities” in SNe Ia.
• A simple answer to the diversities in spectral evolution/color.
• Would not introduces z-dependent systematic errors in cosmology (it is a random effect).
• However, might affect the extinction. May introduce some (z-independent) systematics?
• Unification of further diversities?
s e r