Supernovae and related objects unveiled by TMT
Koji Kawabata (Hiroshima Univ., Japan)

From a Japanese proposal in fields of Stars and Local Galaxies

Pictures: left, Maeda+ 10, right ed. Kodama+Japanese science proposal for Stars and Local Galaxies fields
discussed by sub working group
In Stars and Local Galaxies
Lead author:
Aoki, Wako (NAOJ)
Contributors:
Chiba, Masashi (Tohoku Univ.)
Kawabata, Koji (Hiroshima Univ. )Komiyama, Yutaka (NAOJ)
Maeda, Keiichi (IPMU, Univ. Tokyo)
Matsuura, Mikako (London Univ.)
Nogami, Daisaku (Kyoto Univ.)Tominaga, Nozomu (Konan Univ.)
Yoshida, Naoki (IPMU, Univ. Tokyo)
Japanese science white paper for TMT : Edited by Tad Kodama

Main Items of proposal: Stars and Local Galaxies☺Trace stellar activity and explosions☺Decipher galaxy formation and evolution via high-res. observation
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Supernovae (SNe) and gamma-ray bursts (GRBs)
Time variability of stars and binaries
Stellar evolution and cycles of matter
1st and 2nd generation stars
Formation of local galaxies
Detailed stellar population in nearby galaxies

Absolute magnitude

Light curves of various types of SNe
Ia: thermonuclear burning
Others: core-collapse-19-17

PhotosphericEarly, bright phase
See photosphere

Optically thin
Nebular spectra

Late, fainter phase
See inner core effectively

App. mag App. mag
at 100Mpc at z = 0.5+16+23+18+25+20+27+22+29+24+31

Filippenko 1997

TMT may contribute to late-phase (detailed) obs. for nearby
SNe and early-phase obs. for moderately distant SNeMajor problems on SNe• Explosion mechanism and progenitors– Core-collapse (CC) SNe: Outward shock wave, 3D effects– Thermonuclear (Type Ia) SNe: Spectroscopic diversity, 3D effects– Connection between SNe and GRBs
– Nature of Faint supernovae/New type explosions• Nucleosynthesis, products back to ISM (dust, etc.)

Main items on SNe and GRBs in our proposal• GRBs and SNe: Progenitors of normal GRBs
• Geometry of SN explosion– Spectroscopic approach– Polarimetric approach• High Spatial Resolution Spectroscopy of Nearby SNe and SNRs
• Faint supernovae• Supernovae in the High-Redshift Universe

SNe as Progenitors of long GRBs: Introduction• A part of long GRBs appear associated with energetic SNe Ic• Spectroscopically confirmed SNe associated with long GRBs––––SN 1998bw (bright, energetic SN Ic) - GRB 980425 (z=0.0085; X-ray rich; Eiso<<Etyp)
SN 2003dh (bright energetic SN Ic) – GRB 030329 (z=0.168)
SN 2003lw (bright energetic SN Ic) – GRB 031203 (z=0.105; Eiso<<Etyp )SN 2006aj (mildly-energetic SN Ic) – GRB 060218 (z=0.033; X-ray flash; Eiso<<Etyp)06aj98bwHCOMassive star

Envelope-stripped(mass-loss in WR
phase / binaryinteraction)
H,He layers off

02ap
normal Ic OI CaII
Spectra of SNe Ic (hypernovae)(Nomoto+ 06)

Type Ic SN
H,He-deficient
High-vel. ejecta
Forming BH/GRB

Diversity of GRB-SNe: The scenario is universal?
• Consensus “Long-duration GRBs originate from energetic SNe Ic”?
However,Sample SN-GRBs are still few and quite atypical.
• Eiso = 1048-1049 erg << Eiso,typ ~ 1051 erg• z < ~0.1 << ztyp ~ 1-2 (restricted to nearest GRBs; outlier?)

Difference between `GRB-associated energetic SNe Ic’ (like 98bw) and `nonGRB energetic SNe Ic‘ (like 03jd). e.g., metalicity of host galaxy (Modiaz+ 08)

Thus, a part of observational facts can be no longer explained onlyby the simple scenario.
• Diversity of Progenitors for long-duration GRBs
GRB 060505 and GRB 060614 (z <~ 0.1):
Afterglow observed, but SN is too faint (<1/100 of typical luminosity)
Every nearby long GRB is NOT associated with bright SNe.

GRBs and SNe: Progenitors of normal GRBs: Observation Plan
With TMT (IRIS/AO and/or WFOS)
Optical and NIR Spectroscopy for SN components of GRBs up toz=1-2 at ~1 month from GRB
SN 1998bw at z=1: Imax=24mag, Jmax=23mag, Hmax=23mag
S/N~5 with R~1000: Exp time ~1hr in I-band, 3hr in J-band, 5hr in H-band~5 GRBs/year at z<1

AO is so effective to avoid contamination of host galaxy backgroundMarginal spectroscopy for GRB
021211 (z=1.0; Della Valle+ 04)

SN 1998bw (Galama+ 98)

GRBs and SNe: Progenitors of normal GRBs: SummaryHigh quality spectra for SN componentsof normal GRBs at z > 0.1 (up to ~2)(TMT IRIS/AO, WFOS)
8000

12000Ǻ at z = 1

More GRB-associated supernova samples

Clarify connection between GRBs and SNe: Progenitor of GRBs, Physical process of GRB-jet ejection,
 Massive star evolution…

Geometry of SN explosion: Introduction
Explosion mechanism of SNe (core-collapse/thermonuclear=Ia)-- Essential, but still unclear-- Explosion does not occur in simulation (CC; Mzams > 10-15M8)-- Diversity in velocity/composition structure (Ia; e.g., Maeda+ 10)

Recently, many studies indicate that Effects in multi-dimesional
structure can be a key ingredient in the explosion physics.
 Standing Accretion Shock Instability, SASI (CC) Magnetic field, rotation effect (CC) Off-center ignition (Ia)

Non-spherical SN explosion
Numerical simulation of SASI (Blondin+ 04)

Geometry of SNe: Spectroscopic approach 1• Late-phase spectra (>0.5 year): Ejecta becomes optically-thinand line emission brings information at innermost part(composition, expansion velocity).
• 8-10m telescopes are revealing possible general asphericity
for envelope-stripped SNe (SNe Ib/Ic).
• [OI]6300,6363 is blend. Mg I]4571 is more useful, but faintnear polar (single peak)Profile of[O I] 6300,6363
near equator
double peaks

Mazzali+ 05; Maeda+ 08

Maeda+ 08

Geometry of SNe: Spectroscopic approach 2 and Obs. Plan
• For SNe Ia, recent studies pointed the correlation between thevelocity dispersion in the early phase and Fe/Ni line velocity inlate phase, which can be explained by off-center ignition.
With TMT (IRIS/AO and/or WFOS)
Much larger sample for both CC/Ia.
CC: Explosion mechanism for each type(Type Ic – Ib – IIb – II)
Nearby Ia: Detailed explosion mechanism
from Opt-NIR-MIR spectra
Distant Ia: Difference from nearby SNe Ia,validity of standard candle (z~0.15)

Fe, Nidelayed detonation
Off-center ignition explosion model(Maeda+ 10)

Geometry of SNe: Polarimetric approach

Polarization proves asymmetry of ejecta(photosphere/chemical inhomogeneity) forearly, photospheric phase of SNe.
Photospheric asphericity and polarization
Not only CC SNe but also SNe Ia show largepolarization across absorption lines, being
different with elements. However, wellobserved samples are still lacking.

in QU diagram (Wang & Wheeler 08)

Polarimetry needs much number ofphotons (∆p~0.1%) and TMT will be ideal
photon collector. But, the problem is no
optical and NIR polarimeter being planned
for TMT (instrumental polarization ofLine polarizatin vs. decline rate of SNe Ia(Tanaka+ 10; Wang+ 08; Leonard+ 05;
tertially mirror in Nasmyth foci ~4%).
Chornock&Filippenko 08)

Geometry of SNe: Summary
Late-phase spectroscopy - Emission line profile, velocity
Early-phase spectropolarimetry – Chemical structure(TMT IRIS/AO, WFOS, possible polarimeter)
3D structure of SN ejecta: Velocity, composition, etc.

Explosion mechanism and nucleosynthesis:
CC: How outgoing shock wave is produced?
Ia: Is off-center ignition universal? How transition fromdeflagration to detonation occurs?

Spatial Resolusion Spectroscopy of Nearby SNe and SNRs
SN 1987A – only young SN which has been spatially-resolved
With TMT (IRIS/AO and/or IRMOS/AO)
Spectroscopy of young, nearby ~5-10 SNRs (after 1980 at <10Mpc)

2D spectroscopy of SN 1987A remnant; different asymmetry between central
ejecta and circumstellar ring (Kjær+ 10)

Faint supernovae
Suffering from selection effect / Can be a larger population
Potential roles for resolving some major problems of SNe• Ia: SN 2002cx-like, SN 2008ha – incomplete Ia?
• Ib: Ca-rich, O-deficient: helium detonation, or CC of less massive• IIP: Fall-back to black hole? Less massive core-collapse?
2-5 mag
2fainterWith TMT (WFOS)
Spectroscopy of larger samples of faint SNe→ From case studies to comprehensive
understanding of stellar evolution
Light curves of faint SNe (KK+ 10)

Supernovae in the High-Redshift Universe
Exploring high-z universe, e.g., SFR, from unbiased, individual stars(SFR from galaxy observation may miss faint diffuse galaxies)
 Bright SN IIn (+SNe IIL, PISN) --- MR ~ -22 mag Shock breakout --- Mbol ≤ -23 mag, easy to observe because ∆t/(z+1)

With TMT (IRIS and/or WFOS)
Spectroscopy of candidates of high-z supernovae found by survey
program coordinated with other telescopes (Subaru, LSST, PanSTARRS,etc)

Light curve of typical SNe at rest frame(Smith+ 07; Patat+ 01; Catchpole+ 87;
Tominaga+ 09). The time scale is prolonged

by 1/(z+1) for high z SNe.

Conclusion 1/2• TMT spectroscopy for SNe associated with moderately-distant
GRBs and explore progenitors of normal GRBs
• TMT spectroscopy (and spectropolarimetry, if possible) for
SNe to diagnose 3D structure and explosion engines• High spatial-resolution spectroscopy of young, nearby SNRs
• Faint supernovae to complete stellar evolution model• Supernovae in the High-Redshift UniverseConclusion 2/2
Opt: WFOS (R~500-1000)
NIR: IRIS w/ AO (R~500-2000), IRMOS (R~2000)

Mostly, no multiplicity is required
Polarimetric capability is desirable, if possible

To maximize the opportunity,
Simultaneous wide-band spectroscopy (Opt-NIR),
AO-assisted instruments (red band – NIR) is desirable→ X-shooter-like instrument at the AO port is ideal (mostly formoderately distant SNe)