TMT Observational study of nearby supernovae with TMT and smaller telescopes

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TMT???????????????????Observational study of
nearby supernovaewith TMT and smaller telescopes
???? Kawabata, Koji, Hiroshima-U ???? Maeda,
Keiichi, IPMU, U-Tokyo ???? Tanaka, Masaomi,
IPMU, U-Tokyo ??? Tominaga, Nozomu,
Konan-U ???? Nomoto, Kenichi, IPMU,
U-Tokyo ???? Yamanaka, Masayuki, Hiroshima-U
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Summary

• Many progress with 8-10m telescopes and smaller
  ones
• Especially in
• late phase (optically thin phase) observations
• spectropolarimetric observations
• distant supernovae (associated with GRBs/XRFs) or
  faint SNe
• New findings of extreme/peculiar SNe, such as
• faint SNe Ia energetic or faint SNe Ib/c

Multi-epoch / multi-telescope observation required
8-10m telescopes are not always sufficient for
pol./late-time obs.
TMT with polarimetry and/or AO (in queue mode) is
desirable
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Light curves of supernova
Ia thermonuclear burning
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-19
Others core-collapse
-17
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Absolute magnitude
Apparent magnitude (100Mpc)
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22
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Filippenko (1997)
Disc. lt1m Spec. 1-2m
Spec. 2-4m
Spec. 8-10m
Multi-epoch observation with small to large
telescope
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Spectral evolution (SN Ic 2007gr)
-7.3d
Photospheric (absorption lines)
-1.3d
photospheric
OI
Nebular (optically-thin emission lines)
45.6d
55.6d
158.4d
374.5d
375.5d
nebular
We can see the explosion center in late phases
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Late-time spectroscopy of energetic SN Ic 2003jd
Mazzali et al, Science (2005)
Double peaked O I for non-GRB, energetic SN
Ic (Single peaked O I for GRB-linked energetic
SN Ic)
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Late-time SNe Ib/c spectra Aspherical explosion
Maeda et al., Science (2008)
High incidence of double peak O I. Consistent
with all Ib/c SNe are aspherical.
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SN 2006gy One of the most luminous SNe

• MV -22 mag? Lbol31044 erg s-1 slow LC
  evolution,
• Total radiation energy 11051erg, comparable
  with Ekinetic
• Type IIn narrow emission lines ? strong CSM
  interaction
• Low X-ray luminosity ? weak CSM interaction
• Energy source is unclear CSM interaction? /
• 56Ni decay? (gt10M? necessary) / high-mass
  star interaction?

Ofek 2007 Smith 2007 Nomoto, Tominaga
2007 Umeda Nomoto 2008 Woosly 2007
Portegies 2007
Kawabata 2009
Smith 2007
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SN 2006gy Late-time photometry
Smith 2008

• Subaru 8.2-m/FOCAS at 400d (undetected at Keck
  in optical)

Luminosity is consistent with 56Ni gt3 M?
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SN 2006gy Late-time spectroscopy at 400d
Subaru/FOCAS
Inconsistent with type IIn/IIa (weak Ha,
strong Ca II) type II/Ib/Ic (no OI ?
core-collapse unlikely?) type Ia energetic Ic
(weak Fe lines ? less 56Ni ?) Dense ejecta
(ne108-109 cm-3) than typical SNe II
Kawabata 2009
Later spectrum is required, but faint even for
8-10m
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SN 2006gz Super-Chandrasekhar mass SN Ia?
Subaru/FOCAS spectroscopy
Maeda 2009

• Late-time obs with Subaru (spec) and Keck
• Not so luminous (i.e., not so large 56Ni mass)
• Weak or no Fe lines (suggesting less 56Ni ?)

Really super-Chandrasekhar mass SN Ia?
Detailed late-time phot/spec are difficult even
for 8-10m
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SN 2009dc Another super-Chandrasekhar mass SN Ia?
Hiroshima 1.5-m/HOWPol
Subaru/FOCAS spectropolarimetry
Yamanaka, submitted
Tanaka, submitted

• Likely more luminous than SN 2006gz (56Ni mass gt
  1.2 M?)
• Polarimetry confirm little deviation from
  spherical symmmetry
• Really super-Chandrasekhar mass?

Early-time polarimetry and late-time spec.
with 8-10m class or larger required
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SN 2005bf Extremely peculiar type Ib SN
Subaru/FOCAS spectroscopy
Subaru obs
Maeda 2007 Tominaga 2005

• Peculiar light curve Difficult to reproduce both
  the main peak luminosity and late-time faintness
• Energy source is a birth of magneter?

Detailed late-time photmetry (easy with large
telescope)
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SN 2005bf Asymmetry revealed by polarimetry
VLT/Subaru spectropolarimetry (Maund 07 Tanaka
09)
Tanaka 2009

• Asymmetry is revealed High polarization in Ca/He
• Jet-like blob penetrating up to He layer?

Multi-epoch, high S/N spectropolarimetry required
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SN 2008ha Most extreme in faint SNe Ia
2002cx-like
Keck/LRIS
Foley 09
Valenti 2009

• Very faint (5 mag fainter than typical Ia) low
  line velocity
• Rapid evolution in LC and spectra, small ejecta
  (0.15 M?)
• Host galaxy similar to core-collapse (cf.
  Moriya 09)

Observational bias? Large telescopes are required
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SN 2005cz Faint Ca-rich type Ib in elliptical
galaxy
Kawabata, submitted

• Undetected in VR bands at 170 days even by
  Subaru
• Ca gt O ? low-mass end of core-collapse SNe?

Late-time observation reveal the central engine
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SN sequence in 56Ni mass main sequence mass
Sauer06, Shigeyama94, Iwamoto94,
Shigeyama90, Blinnikov00, Turatto98,
Iwamoto00, Mazzali00, Nakamura01, Iwamoto98,
Zampieri03, Mazzali02, Mazzali03, Deng05,
Mazzali06, Tominaga05, Maeda07, Mazzali06,
Mazzali08, Tanaka08, Nomoto08, Kawabata
submitted
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Summary

• Many progress with 8-10m telescopes and smaller
  ones
• Especially in
• late phase (optically thin phase) observations
• spectropolarimetric observations
• distant supernovae (associated with GRBs/XRFs) or
  faint SNe
• New findings of extreme/peculiar SNe, such as
• faint SNe Ia energetic or faint SNe Ib/c

Multi-epoch / multi-telescope observation required
8-10m telescopes are not always sufficient for
pol./late-time obs.
TMT with polarimetry and/or AO (in queue mode) is
desirable