超新星・突発現象研究の現状と今後:
High-z and low-z
Cosmology
Star Formation History

Stellar Evolution
Explosion Physics

SN Feedback
Metal, Dust, Cosmic Ray, …

Keiichi Maeda (Kavli IPMU, U. Tokyo）

Exploring high-z and z-evolutionz = 2.05

z = 3.90

Super-Luminous SNe(SLSNe):
Massive star(?)< - 21 mag,long lasting (~ year)

Cooke+ 2012, CFHT Legacy Deep (stacking)
SN SCP 0401, Z = 1.71
HST Survey + HST spec.

Rubin+ 2013, HST survey + spec. (8 orbits)

SN Ia:White Dwarf~ - 19 - 20 mag,~ monthExploring high-z and z-evolution
Horiuchi et al.
2011

RateTotani et al. 2008

0.1 Gyr
SN rate - SFR

Delay time
10 GyrDelay time (progenitors’ life time)

SFR tracer? (⇒ Star formation, Galaxy evolution)
Different SN populations? (⇒ Stellar evolution)
Change in SN properties? (⇒ Cosmology)

High-z SNe @ optical (future)Moriya+ 2012; Tanaka+ 2012

SLSNeSNe Ia

z=3z=5

HSC survey expectation (Yasuda+)

8m-survey ⇒ spec. requires
30-m class.
TMT in the future (or JWST).
Tominaga+ 2011

Shockbreakout inSNe IIp(from RSG)

Evolution w/ redshift?
Cooke+
2011

z~0.5

Low-z

Evolution in rest “UV”? Local sample limited.
⇒ Rest flame “optical” (used for cosmology), need 30m(or NIR space).

SN Ia Cosmology
Riess+ 2007

Conley et al. 2011

Future: w… cosmological constant or not?
Ground, optical: DES, HSC, LSST (+ spec., TMT in the future?)
Space, NIR: WFIRST, WISH
(Ground, NIR at z < 0.2?: TAO… calibration sample, K-cor. etc.)

Causes of systematics?
020 40days• Studying local samples
will be kept important.
– Systematics.
– How and where ?
• Extinction?
• Different Populations?

– z-evolution, host-depend.?
B-V @ peak

Intrinsic variation in explosion
mech. can mimic extinction.

KM+ 2011

HSC, PFSLine shift in latephase (intrinsic)

Rest-frame NIR SN Ia Cosmology
MBDecline rate

As distance indicators,MH ext.
Rest optical: “standardized”
corrected Rest J, H: “standard”
Non-ext.
correctedExtinction unimportant
By B. Kirshner

Currently: Pan Starrs (opt)+ HST w(NIR), up to z ~ 0.5

Future: NIR survey (WFIRST,WISH) also low redshift?
Local samples for K-cor. (TAO?)-1

Effect of Rv in opticalfor w-determination
3.1-1.2

2.5
1.7
25 SNe @ z = 0.35

Clarifying natures @ low-z
Wide-field Untargeted
Example: PTF
Survey: 1.2m, 7 deg2 (~ KISS)
Identification: 1.5m, low-R IFU
Follow-up: Keck etc.
Filling up time-luminosity space
Expected future upgrade:
Survey 7 deg2⇒40 deg2
… will fully “kill” the local
Universe transient space?
(both in time and luminosity)

Just after the explosion
270R⇒Giant4R
1.5R
2R⇒Wolf Rayet

0.03R

Cao+ 2013, SN Ibc iPTF13bvn
Progenitor < a few R ⇒ WR

Bersten+ 2012, SN IIb 2011dh~ 250R ⇒ Yellow supergiant

Quick follow-up by 1m: e.g., OISTER

Just after the explosion
SNe IIp (RSG progenitor)

Quick ToO by 2 - 4m.
Kyoto 3.8m
SNe Ia< a few day
0.25 day
1 day
time

Shock breakout
Surface composition
Unexplained features⇒ Important for theory

How progenitor-SN properties related?
MR, max

Draut+ 2012

EnergySNe Ib/c
Model

Decline rate

Mms

Future (on-going): Unbiased + large sample⇒ IMF, single/binary evolution, etc.
Intensive follow-up required. Resource will be on-line(Kyoto, TAO). Strategy? (for competition)

Explosion Mechanism (~ 1 year)
Core-collapse
KM+ 2008
SubaruType Ia SNe
KM+ 2010
Gemini+Different type of
explosion geometry

BlueRedExplosion Mechanism (~ 1 year in IR)
NIR is better (e.g., less blending than opt)
⇒ IRCS+AO188 for 8 nights in 2011-2012 (KM+, to come),
but limited to a few very nearby SNe ⇒ TMT?
Can also be done in mid-IR.
(almost no blending, very
low temperature regions).
SPICA(also strong for dust:Tanaka+ 2012)
KM+ 2010

Dust Formation… Origin of dust in Universe
SN IIn 2010jl@ ~550 day

KM+ 2013 Subaru IRCS+LGSAOA minute of dust formation… NIR (~1000 – 2000K)
Photometry is OK, but spectra provide complete view.
(e.g., dust size + optical depth require spectra).
Optical also necessary.
TAO, kyoto 3.8m (but south and north)Synergy w/ High Energy Astrophysics• SN-GRB relation (z < 0.2 w/ 8m, z > 1 w/ 30m).
• Hard X, soft-γ– Radioactive decay emission (only SN 1987A so far).
• Nearby SNe Ia possible w/ Astro-H (2015-) (KM+ 2012)
SN Ia standard candle• Radio, soft X Progenitor– Mass loss + particle acceleration (KM 2012, 2013).
– Speed of breakout shock wave (KM 2013)
Shock breakout– A few program running.
• KM+, Alma cycle 1; Alak+, Chandra + VLA cycle 15.

– ALMA, SKA, …

Summary• High redshift.
– SN populations and evolution. SFR.
– SN Ia Cosmology. Rest-NIR. Systematics (low-z).
• Main drivers – HSC + upcoming (in relatively long term).

• Low redshift.
– Basis for high-z study.
– Surveys begin filling up “t-L” space.
– Intensive follow-up required ⇒ unbiased picture.
– Lots of question… progenitor, explosion.
• Main drivers – existing and near future.