すばるHSCで探る銀河系外
可視光突発天体浦田裕次（台湾国立中央大学）

CTAに関連することがほとんどないです。

時間領域の天文学 in 台湾
Subaru/HSC
Lulin Observatory in TW

CFHT/WIRCam

Pan-STARRS1

SMA

時間領域の天文学 in 台湾
Fermi unID sources

Ultra-Luminous SN(PS1-11ap)

Subaru/HSC

CFHT(IR)

赤外超過?!

Lulin 1m

Pan-STARRS1(opt)
Kataoka et al. 2012

GRB120326A
Tidal Disruption FlareSw J1644+55

赤外線追跡

CFHT

Burrows et al. 2011

235GHz (SMA)

サブミリ波残光の最速の検出
Lulin 1m + SMA etcUrata et al. in prep

今日の話

HSC/SSP Transient team! Taiwan : Y. Urata, M.F. Tsai, P. Tsai, Tang (NCU),
K.Y. Huang (ASIAA), A. Kong(NTHU)! Japan: N. Yasuda, R. Quimby, M. Moriya, N. Yoshida(IPMU),
T. Morokuma (Tokyo U), M. Tanaka(NAOJ),
N. Tominaga(Kounan-U), J. Okumura (Kounan-U)! Princeton : P. Price目次! すばる Hyper-Suprime-Cam! 計画中のサーベイと突発天体! 可視光突発天体を見つける方法! Pre-sciencesすばる Hyper-Suprime-Cam! Subaru : one of largest aperture
telescope 8.2 m at MaunaKea! Prime focus : Wide field observations(imaging and spectroscopy)! Current instruments @Prime Focus
Suprime-Cam (SC) FOV 34’ x 27’

HSCSC	SC	

FOV of HSC 1.5 deg in diameter

HSC : Upgrading of SC about 10 times!

HSC

SC → HSCSC	Suprime-Cam (SC)Hyper-Suprime-Cam(HSC)

CCD Type

MIT/LL(2000-2008)
Hamamatsu (2008~)

Hamamatsu(Fully-Depleted)

Number of chip

10116
(4 guiding, 8 focusing)

Pixel size

15um (~0.”20)

15um (~ 0.”17)FOV

34’ x 27’90’ (Diameter)Gain

2.5-3.7 e/ADU

3.0 e/ADU

Readout noise

10e

TBD

Readout time

18s

20s

Number of filter

106Filter exchanging time

300s

600s (900s)

AΩ (Survey Power)

13.295

HSC (Hardware)

Consist of three partPrime Focus Unit (PFU)
CameraWide Field Corrector (WFC)HSC will be ready soon !
Significantly earlier than LSST!

• 116 CCD in total• 1.5 deg FOV (diameter)

High sensitivity CCD

http://anela.mtk.nao.ac.jp/hscblog/builder/http://anela.mtk.nao.ac.jp/hscblog/builder/Schedule! 2011/08

Ship WFC unit to Hawaii! 2011/12

Camera completed! 2012/08

Engineering First light!

! 2012/10

Science First light! 2012/10

Submission of the SSP proposal! 2013

Expected HSC SSP survey start! 2018

Expected HSC SSP survey end

The survey will be significantly earlier than LSST

Subaru Strategic Program(SSP)! Subaru is the open use telescope! HSC will be one of the open use instruments! Subaru proposal system:!
!
!

Normal Program up to 5 nights
Intensive Program (IP) up to 20 nights / several semester(Max 10 nights / semester)
Subaru Strategic Program (SSP) New!
100-300 nights / 3-5 years (max 60 nights / year)
For newly developed instrument, we can submit a proposal forthis category.
HiCIAO : “SEED” (Exoplanet, 5years - 120 nights)
FMOS : “ FastSound“ (BAO, 2 years - 40 nights)

Only one or less program will be selected for SSP.

HSC SSP! Establish HSC/SSP consortium (Japan, Taiwan, Princeton)! The science driver is cosmology (Dark Energy)!
! Planning three layer (wide, deep ultra-deep) survey with grizy andnarrow band filters! Aiming 300 nights survey over 5 years

Time domain survey!

Variable stars!

Proper motion stars!

AGN (Wide, Deep, & Ultra-deep)

Key science!

SNIa cosmology (z>1) (Deep & Ultra-deep)

Key science!

Supernova rate (z<1) (Deep & Ultra-deep)!

Ultra-Luminous Supernova ( z up to 4~6) (Deep & Ultra-deep)!

Bright SNIIn (z up to ~6) (Ultra-deep)!

Orphan GRB (Deep & Ultra-deep)!

Tidal Disruption Flare (Deep & Ultra-deep)!

SNe Shock break out (z>0.5) (Wide, Deep & Ultra-deep)!

Unknown objects…..

Time domain survey!

Variable stars!

Proper motion stars!

AGN (Wide, Deep, & Ultra-deep)

Key science!

SNIa cosmology (z>1) (Deep & Ultra-deep)

Key science!

Supernova rate (z<1) (Deep & Ultra-deep)!

Ultra-Luminous Supernova ( z up to 4~6) (Deep & Ultra-deep)!

Bright SNIIn (z up to ~6) (Ultra-deep)!

Orphan GRB (Deep & Ultra-deep)!

Tidal Disruption Flare (Deep & Ultra-deep)!

SNe Shock break out (z>0.5) (Wide, Deep & Ultra-deep)!

Unknown objects…..

Advantages of HSC!

Large Aperture
Other SN surveys except for LSST use 4m telescopes
SNIa samples are limited to z<0.9→ Extend to z~1.2!
!

!

Wide Field!

!

Higher sensitivity in red bands (z, y-bands)!
!
!

!

Most energy of SNIa@z=1 fall in i, z, and y-band
Ultra-Luminous SNe at z~6Bright SNIIn at z~6High spatial resolution!

!

2 FoV of HSC is comparable to the survey area of SNLS

SNe are point sources

Coordinated SSP survey only enables multi-band and multi-epoch time
domain survey

時間変動天体サーベイ
1. 大口径望遠鏡・宇宙望遠鏡でのdeep サーベイのデータ分割- Hubble Space Telescope (HST, 2.4m) / WFPC2, ACS, WFC3
- Subaru (8.2m)/Suprime-Cam (SDF, SXDS), Hyper Suprime-Cam- CFHT (3.6m)/MegaCam: Supernova Legacy Survey (SNLS)- JWST (6.5m)/NIRCam- WISH (1.5m), Euclid (1.2m), WFIRST (1.1-2.4m)
2. (中小口径)望遠鏡をほぼ占有- ROTSE(0.45m)- Kiso (1.05m)/KWFC: Kiso Supernova Survey (KISS), KWFC Intensive Survey Of the
Galactic Plane (KISOGP)- Palomar 48-inch Oschin (1.2m)/CFH12k: Palomar Transient Factory (PTF)- Pan-STARRS (PS, 1.8m)- SkyMapper (1.35m)- SDSS (2.5m): SDSS-II Supernova Survey- Microlensing Observations in Astrophysics (MOA, 1.8m)- CTIO Blanco (4m)/Dark Energy Camera (DECam): Dark Energy Survey (DES)- Large Synoptic Survey Telescope (LSST, 8.4m)

Orphan GRB afterglow
GRB collimated Jet

Energetics Eiso ~ 1053-54 → Jet corrected ~ 1051
Achromatic temporal break in afterglow light curves(but Chromatic breaks,
no jet breaks....)

On-axis Orphan(Nakar+02)
Failed GRBs
(Huang+02)
Short GRBs

Nakar +02

Off-axisNo γ-rays
Afterglows show rise and fall
After jet break, the properties are similar

Off-axis orphan GRB afterglow = direct evidence of jet collimation

Orphan afterglow survey! Wider survey fields in optical!
!

Swift/BAT 120 x 90 deg :Typical opt imager several 10 arcmin)! Deep imaging (r ~ 26.5 mag)
→ 8 m class telescopes! Cadence of the survey (days scale)

Temporal color evolution! Long-term monitoring(monthly~ year)

Subaru, LSST
http://cosmo.nyu.edu/afterglowlibrary/index.html

Orphan afterglow survey
z=4.0! Wider survey fields in optical!
!

Swift/BAT 120 x 90 deg :Typical opt imager several 10 arcmin)! Deep imaging (r ~ 26.5 mag)
→ 8 m class telescopesz=2.0
z=1.0
z=0.5

Limits of 2m Telescopes (e.g. Pan-STARRS)! Cadence of the survey (days scale)

Temporal color evolution! Long-term monitoring(monthly~ year)

Subaru, LSST
http://cosmo.nyu.edu/afterglowlibrary/index.html

Orphan afterglow survey! Wider survey fields in optical!
!

Limits of 8m telescope (e.g. Subaru)

Swift/BAT 120 x 90 deg :Typical opt imager several 10 arcmin)! Deep imaging (r ~ 26.5 mag)
→ 8 m class telescopes! Cadence of the survey (days scale)

z=4.0
z=2.0z=1.0
z=0.5
Temporal color evolution! Long-term monitoring(monthly~ year)

Subaru, LSST
http://cosmo.nyu.edu/afterglowlibrary/index.html

Orphan afterglow survey! Wider survey fields in optical!
!

z=4.0
z=2.0
z=1.0
z=0.5

Swift/BAT 120 x 90 deg :Typical opt imager several 10 arcmin)! Deep imaging (r ~ 26.5 mag)!

Median redshift of GRB z~2→ 8 m class telescopes

Temporal color evolution! Cadence of the survey (days scale)! Multi-color monitoring(monthly~ year)

Subaru, LSST
田中さん
http://cosmo.nyu.edu/afterglowlibrary/index.html

Planned Cadence• Example for Deep & Ultra deep
• Optimize to SNIa hunting• 1st year : Making reference images forimage subtraction• 2nd year : SNe Ia. Orphan GRB etc
hunting• 3rd year : Long term monitoring for
Luminous SNe, SNIIn, AGN• 4th year : SNe Ia. Orphan GRB etc
hunting• 5th year : Long term monitoring for
Luminous SNe, SNIIn, AGN
FilterLimit(5σ)

g

26.9

r

26.6i26.6z

25.7Planned Survey! Three layer (wide, deep ultra-deep) survey with grizy! Aiming 300 nights survey over 5 years (2013 – 2018)

Time Domain Survey
Limit for 1 visit
FilterLimit (5σ)

g26.9

r26.6

i26.6z25.7

350 SNIa (180@z>1)

HSCDeep

HSC
Ultra-Deep30

4Epoch (each filter) 12

28

Totani andPanaitescu(2002)

35

9

Nakar&Piran(2002)

52

Rossi+08

10.14

FOV (sq. deg)

Expected
1- 44 events(Total)

HSC & Radio Follow-ups
Simulated light curves (Etotal=1053 erg, z=1, θjet=0.1 rad)Subaru/HSC

EVLA(1hr)

Optical r’ Θ = Θobs
Jet

8.5GHz Θobs = ΘJet
Θobs = 2ΘJetΘobs = 2ΘJetΘobs = 3ΘJet
Θobs = 3ΘJet

EVLA を使うと off axis 角などが精度よく求まる

探査方法
!

PSF合わせた画像引き算!

光度曲線の生成!

母銀河の同定!

母銀河内での位置の測定!

赤方偏移の測定!

(Phot-z, Spec-z)!

絶対等級の測定!

突発天体/変動天体の分類

PSF matched image subtraction

PSF matched image subtraction は、HSC analysis pipelineの一部に組み込まれる

光度曲線の作成

母銀河の同定

Photometric redshift

AB mag

25

28

400

600
800
Wavelength (nm)1000

GRB母銀河

Jakobsson et al. 2011

HSCで見つかる Orphan GRBは、 z ~2 くらいまでHSCのpre/late-imagingで母銀河は、ほぼ同定されるはず！

GRB母銀河のPhot-Z

GRB９８０３２９

Urata et al. 2004

Christensen et al. 2004

Pre-searches with SC
Subaru Deep Field (SDF)	 Subaru-XMM Deep Survey (SXDS)	
Observations	

2001-2007	

2002-2005, 2008-2010	

FOV (deg2)	

0.25 ( = 0.14 HSC)	

1.3 (5FOV of SC = 0.73 HSC)	

Cadence 	

20 epochs / 6 yrs 	

8-10 epochs/ 4yrs	

Filters	

BVRiz + Narrow Bands	

BVRiz +Narrow bands	

Others	

UV, NIR, MIR	X, UV, NIR, MIR, FIR, sub-mm, radio	
SDF

SXDS

HSC
Deep

HSC
Ultra-Deep

FOV (sq. deg)

0.25

1.330

4Epoch2081228

Totani+02

0.47

0.75

359Nakar+02

0.07

0.11

52

Rossi+08

0.01

0.02

10.14

SDF-05M05

Urata et al. 2012ApJL submitted

Unusual Long and Luminous Optical Transient
検出 2005年3月5日
SDSSもたまたま検出 (2005年1月18日)
継続時間 > 800 days in the obs frame
母銀河からのoffset
ΔRA=+0.”15, Δdec=-0.”24• 母銀河 Rc ~ 26 mag• zphot ~ 0.65 (+0.02 -0.03)••••

Photometric redshift

800 daysAB mag

25

光度曲線

28400

600
800
Wavelength (nm)1000

• 最大光度 -20 mag (-19等以上が~500日)• 放射エネルギー~ 1 x 1051 erg• 暗い母銀河 MV = -16.3 mag(SMCと同じくらい暗い)• SED@~88日 黒体放射 T~6400K

SDF05-M05の起源• 母銀河からのoffset
AGN / TDF を棄却• Ultra-Luminous SNe
暗い母銀河は、共通
光度、時間発展は異なる• 特異なSN IIn
暗い母銀河を持つ傾向
光度、時間発展はまちまち（共通の特徴はない）
SED 黒体放射 半々
BB温度 ~ 20,000K(SDF-05M05 T~6400K)• 新種の突発天体の可能性もSED@~90日

Peculiar SN Iin （SN1９９７cy）

SDF05-M05の起源

SDF05-M05の起源• 特異なSN IIn との比較
暗い母銀河を持つ傾向
光度、時間発展はまちまち（共通の特徴はない）

特異なSN IIn SED 黒体放射 半々
BB温度 ~ 20,000 K (SDF-05M05 T~6400K)

Peculiar SN Iin （SN1９９７cy）

SDF05-M05の起源• AGN/TDF
母銀河からのoffset
AGN / TDF を棄却• Ultra-Luminous SNe
暗い母銀河は、共通光度、時間発展は異なる• 特異なSN IIn ▲暗い母銀河を持つ傾向
光度、時間発展はまちまち（共通の特徴はない）
SED 黒体放射 半々
BB温度 ~ 20,000K(SDF-05M05 T~6400K)• 新種の突発天体の可能性●?

SED@~90日

Peculiar SN Iin （SN1９９７cy）

Pan-STARRS1 未同定突発天体の母銀河探査! Pan-STARRS 100-150 突発天体/月 (分光ID~10%)! Pan-STARRS1 MDS は、すばるのDeep pre-imagingが豊富
結構似たような天体がたくさん?! 暗い(>24 mag) 母銀河 、ゆっくりな時間発展）

PS1-MD04(= COSMOS) 33 天体 （2.5年）
すばる Suprime-Cam Deep imaging
z-bandB-bandPS1-11ma

100日

突発天体の可視光の分光観測があると良いが。。。

• 4つのPS1 MDS fields と HSCのDeep/UD fieldは、同じ。
9年(Pan-STAARS1 4 年 + すばる 5 年)のモニター観測Ultra-Luminous Supernova 	
!

New category of transient
discovered in 2006 (SCP06F6)!

Peak absolute magnitude nearly -22mag!

!

Slow light curve evolution!

Brighter than -21 mag for ~100days!

Host less/faint (probably metalpoor host)!

Some are related with some kind ofsupernova!

Recent optical surveys (e.g.
PanSTARRS, PTF) are finding
many!	

Pastorello et al. 2010 ApJL 724, 16	39	

12/09/26	

Variable AGNの可能性

諸隈さんのPPT- HST studies @ CDF-South (Sarajedini+2003,2006,2010, Cohen+2006, [Trevese+2008], [Villforth+2010,2012])- Subaru study @ SXDS (TM+2008b, Morimoto+2012 in prep.)- 1% of galaxy cores show variability (months to years)- several tens % are undetected in X-ray (XMM, Chandra)- variability-selected AGN exist everywhere in CM diagram- low-L AGN in bright galaxies- no clear environmental dependence (Villforth+2012)
Villforth+2012

variability-selected AGN / X-ray sources

Sarajedini+2003

まとめ! すばる Hyper-Suprime-Cam を用いた突発天体探査を準備中! Orphan GRB afterglowをはじめて発見できる可能性大! 既にあるすばるのdeep observationsからいくつかの新種の突発天体を発見!
!
!

Unusual Long & Luminous event SDF-05M05を発見
特異なSNIInと相違 (新種の突発天体の可能性も)High-z ULSN candidates! Pan-STARRS1 と すばる(SC/HSC)で新たな発見の可能性! 日本を中心にLSSTよりもはるかに先に、突発天体の探査を行える！
! 将来的には、すばる/HSC + 30m telescopesの連携