ToO Observations with Subaru
Spectropolarimetry of Supernovae
すばる望遠鏡ToO観測

ー超新星爆発の即時偏光分光観測ー

Masaomi Tanaka (U. Tokyo, IPMU)
田中 雅臣（東京大学 数物連携宇宙研究機構）

in collaboration withK. S. Kawabata, T. Hattori. E. Pian, K. Maeda, M.Yamanaka,
K. Nomoto, P. A. Mazzali, K. Aoki, T. Sasaki, and M. Iye

Target of Opportunity (ToO)
Subaru Open Use Policy
Applicants may submit proposals for Target of Opportunity (ToO)
observations of transient and/or rare phenomena with specific or
non-specific objects based on clear observational strategy, such as
nearby supernovae, Gamma-Ray Burst follow-up, etc.
...
You may also submit ToO proposals (excluding GRB observations)to the time-exchange program with Gemini, which will be executedat queue mode.

Acceptance Letter
You have rights of implementing your TOO observations inprinciple in any "Subaru time" in S11B (Subaru open use time andobservatory/engineering time indicated in the schedule as 'S11B-???'or 'Eng'/'obs'/'service'), while "UH/Keck/Gemini times" are NOTallowed.

Spectropolarimetry => SN Explosion Mechanism2D jet+disk

Harikae+09
ï15000ï10000 ï5000

0ï205000

21.00.5

U (%)

U (%)

1

ï1

ï2
ï2

ï10Q (%)

1Loop!

ï50OI

2Iwakami+08

ï15000ï10000 ï5000

1

ï0.5

0.0

Q (%)

05000

Loop0

ï1Ca IIï1.0
ï1.0

Doppler velocity (km sï1)

SN 2009jf(+9.3 days)

0.0
ï0.5

Straight line

ï10

Doppler Velocity (103 km sï1)

Doppler velocity (km sï1)0

ï15

Neutrino
heating?

3D clump

U (%)

MHD jet?

0.5

1.0

ï10Q (%)

1

ToO Spectropolarimetry of SNewith Subaru/FOCASS09A: 1 night
S09B: 2 nights
PI: M. Tanaka
S10A:2nights
Co-I: K. S. Kawabata, T. Hattori. E. Pian, K. Maeda, M.Yamanaka,(S11B: 1 night)
K. Nomoto, P. A. Mazzali, K. Aoki, T. Sasaki, and M. Iye• Boundary conditions• Number of bright SNe ~ 2-4 / semester• Observable for ~ 2 week (“slow” ToO)
• Total observable time window~ 1-2 months / semester• Time exchange?

• No polarimetric instrument in Gemini• No ToO with Keck

FOCAS available
SN discovery
Our observation

S09A: 1 ToO night
2009/0211020

1020301020301020301020301020302009/03
12009/04
12009/05
12009/06
12009/07
1

FOCAS available
SN discovery
Our observation

S09B: 2 ToO nights
2009/081

1020301020301020301020301020

301020302009/091

2009/1012009/11
12009/12
12010/01
1

FOCAS available
SN discovery
Our observation

S10A: 2 ToO nights
2010/021

1020

1020301020301020301020301020302010/0312010/04
12010/05
12010/06
12010/07
1So far, so successful• Triggered 3.5 nights / allocated 5 nights = 70 %• Best response: 0.5 day!!
Thanks to great effort by the observatory(Director, Associate-directors,Terada-san, ...),
Hattori-san (FOCAS support astronomer),and many observers at the summit• Not many nights for FOCAS• Observations at > 2 weeks after the discovery=> low S/N ratio

1. Instrument exchange for “slow” ToO(or explicit policy for the exchange)

Subaru ToO in the Future• Subaru/HSC can be a great discovery
engine of supernovae/transient(~50 per 1 FOV)

(C: Subaru telescope/HSC project)• High-redshift Type Ia supernovae (cosmology)• Very luminous supernovae at z>2• Unknown transients?
20HSC Transient WG
T. Morokuma, N.Yasuda,Y. Urata,
L. Huang, N. Tominaga, T. Moriya,
M. Tanaka, J. Okumura, A. Kong,
N.Yoshida, C-H Tang, M-F Wang,C-H Shen, M-F Tsai

Deep (30 deg2)

15N•

Very unique before LSST

Tanaka, Moriya,
Yoshida+, in prep

5100345500123Redshift456

Spectroscopic identification is crucial7.5 Shock Breakout

Discovery

3Apparent g’ magnitude [mag]5Flux [10-32 W m-2 Hz-1]

4 231020
10-1-2• Redshift• SN type
5-50

10150NUVgri
50

100

Days from the peak [Days]

2013/03?
1HSC

z=0.2 z=1.5 z=2.5
z=0.5 z=2 z=3z=1

22

Tominaga+112426

28

00.5

11.5

Day

Days since bolometric peak (observer frame) [Days]

Figure 7.6:
(Left): Comparison between the GALEX and SNLS observations (points, SNLS-04D2dc,Schawinski et al. 2008) and a SN IIP1051 erg reddened for the host
10 model with Mms = 20M! and E = 1.2 ×20
galaxy extinction with a color excess E(B − V ) = 0.14 mag (lines, Tominaga et al. 2009) (black and red: near UV,green: g-band, blue: r-band, magenta: i-band). The inset enlarges the phase when the SN emitted UV light. (Right):
Apparent g " -band light curve of a shock breakout in AB magnitude system for a SN IIP model with Mms = 40M!
and E = 1051 erg. Limiting magnitudes for a 4σ detection in 3.3 min, 5 min, 10 min, and 20 min integrations arealso shown (dashed line), assuming 0.7” seeing, 1.6 arcsec aperture, and 3 days from New Moon.

30

No spectroscopic
identify the shock breakout with the blue g − r color as described below. Aims of this survey
instruments??
are (1) detecting numerous high-z shock breakouts and obtaining their multicolor light curves, (2)observationally establishing the physics of shock breakouts and confirming that the shock breakouts
2. MoretimeexchangewithKeckGeminitake place universally,(3) derivinga cosmic star formation
history (CSFH)
up to z ∼and1.5 with theRealtime follow-up!

!

shock breakouts, and ultimately (4) developing the totally-new high-z study with shock breakouts.

Summary• ToO spectropolarimetry of nearby supernovae• Triggered 70% of total allocated time
(Best response: 0.5 day!)• Sometimes low S/N <= not many nights for FOCAS• Subaru/HSC can be a great discovery engine• Very unique before LSST

0. Queue mode observations
1. Instrument exchange for “slow” ToO
2. More time exchange with Keck and Gemini