Toward Detection of First Supernovae - - Masaomi Tanaka - PowerPoint PPT Presentation

Toward Detection of First Supernovae - 初代星超新星の検出に向けて - Masaomi Tanaka 田中 雅臣

L ~ 10 6 - 10 7.5 Lsun First Star (for 100-1000 Msun) Pop III 300 Msun 50 (2 um) m AB 45 40 10 11 12 13 14 15 16 17 18 19 JWST (5 σ ) z 100hr Taniguchi-san’s talk (e.g., Bromm+01, Stiavelli+09, Bromm & Yoshida 11, Rydberg+11)

First Supernova L ~ 10 8-10 Lsun 10 10 Lsun 10 9 Lsun 10 8 Lsun 10 7 Lsun Observed magnitude @ z = 4 Smartt 2012

Toward Detection of First Supernovae • Massive star evolution and supernova emission • Superluminous supernova • Survey for first supernovae

100 150 200 250 Mass Metallicity (mass loss) & Rotation core-collapse direct collapse supernova (CCSN) (SN? GRB?) pair-instability supernova (PISN)

Final CO core mass 140 ( b ) Z = 10 -4 120 100 PISN SN 2007bi Z = 0.001 M CO / M � PISN 80 Z = 0.004 PISN 60 M ( 56 Ni) > 3 M � , CCSN CCSN 40 Z = 0.01 M ( 56 Ni) > 1 M � , CCSN 20 Z = 0.02 0 300 0 50 100 150 200 250 300 initial mass M MS / M � Yoshida+14, see Yoon+12 and Chatzopoulos+12 for the effect of rotation

Final mass 200 M f = M MS ( a ) Z = 10 -4 pulsational 150 pair instability M f / M � wind 100 Z = 0.001 mass loss Z = 0.004 50 Z = 0.01 Z = 0.02 0 0 50 100 150 200 250 300 initial mass M MS / M � Yoshida+14

Core-collapse supernova Tominaga+ 0.1 Msun He 56Ni O C Shock breakout (~ 1d for red supergiant) Element distribution E k ~ E int ~ 10 51 erg after explosion

Pair-instability supernova (Takahashi-san’s talk) Chen+14 B200 50 100 150 200 O16 56Ni C -2 -2 4 Msun -2 -4 -4 -4 Si Mg log [x] -6 -6 -6 -8 -8 -8 R200 50 100 150 Enclosure Mass [M ] Explosive O/Si burning Element distribution E nuc ~ 10 53 erg after explosion E k ~ 10 52 erg

10 11 Lsun -22 10 10 Lsun Absolute R-band magnitude -20 IIn 10 9 Lsun -18 II -16 Ibc 10 8 Lsun 100d -14 1 year 10 7 Lsun -12 0 50 100 150 200 250 300 350 Days after the explosion

Energy source of SN (1) radioactivity gamma gamma p n decay decay 56Ni ~1 week 56Co ~100 d 56Fe � M 56Ni � L = [1 . 7 × 10 9 e ( � t/ 8 . 8d) + 3 . 8 × 10 8 e ( � t/ 111d) ] L � 0 . 1 M � 0.1 Msun ejection => ~ 5 x 10 8 Lsun @ 20d

Energy source of SN (2) internal energy � 1 � t b L ∼ E int ∆ t t � � t b � � 2 � � � E int t ∼ 3 × 10 8 L � 10 51 erg 1d 100d t b ~ 1d for RSG (R ~ 1000 Rsun) t b ~ 0.001d for WR (R ~ 1 Rsun) (negligible)

Energy source of SN (3) kinetic energy dense CSM SN Moriya+14 High mass loss rate (> 10 -3 Msun/yr) ~100 yr before the explosion � � ∆ t � α � � � E k L ∼ 10 9 L � 10 51 erg 0 . 1 1yr

10 11 Lsun (3) -22 kinetic energy (2) 10 10 Lsun internal Absolute R-band magnitude -20 energy (1) IIn=CSM radioactive 10 9 Lsun -18 energy ( 56 Ni) 0.1 -16 10 8 Lsun -14 Ibc=WR II=RSG 10 7 Lsun 0.25 0.65 -12 0 50 100 150 200 250 300 350 Days after the explosion

First supernovae... number for SN/ 1 yr survey JWST FOV 29 mag @4.5um 30 mag JWST t survey = 1 yr, t exp = 0.1 - 1 d Mesinger+06 Number of fields = t survey /2t exp

Toward Detection of First Supernovae • Massive star evolution and supernova emission • Superluminous supernova • Survey for first supernovae

10 11 Lsun -22 -22 SN 2006gy 10 10 Lsun Absolute R-band magnitude Absolute R-band magnitude -20 -20 10 9 Lsun -18 -18 -16 -16 10 8 Lsun -14 -14 10 7 Lsun -12 -12 0 0 50 50 100 100 150 150 200 200 250 250 300 300 350 350 Days after the explosion Days after the explosion

Kinetic-energy powered SN 2006gy emission line =Type IIn absorption line CSM interaction emission line

10 11 Lsun -22 -22 10 10 Lsun 56 Ni decay Absolute R-band magnitude Absolute R-band magnitude -20 -20 SN 2007bi 10 9 Lsun -18 -18 -16 -16 10 8 Lsun -14 -14 10 7 Lsun -12 -12 0 0 50 50 100 100 150 150 200 200 250 250 300 300 350 350 Days after the explosion Days after the explosion

Possibly PISN?? M( 56 Ni) ~ 3 Msun b − 23 PISN models Data 80 M − 22 90 M 100 M 110 M − 21 Absolute M R (mag) 120 M − − 20 − 19 − − 18 − 17 − − 16 Gal-Yam+09 − 15 − 50 0 50 100 150 200 250 300 350 Time since explosion (d) But see Moriya+10, Yoshida+11 for core-collapse interpretation

Spectrum: No hydrogen Observed Theory 0.4 SN 2007bi, 54 d after peak SN 1999as 0.35 SYNOW f t Hydrogen! 0.4 0.3 SN 2007bi, 54 d after peak Scaled F λ (erg s –1 cm –2 Å –1 ) SN 1999as 0.35 SYNOW f t 0.3 [Ca II ] Scaled F λ (erg s –1 cm –2 Å –1 ) 0.25 [Ca II ] 0.25 0.2 0.2 Mg II Ca II 0.15 Mg II Ca II 0.15 0.1 Ca II Mg II Fe II 0.05 0.1 0 3,000 3,500 4,000 4,500 5,000 5,500 6,000 6,500 7,000 7,500 8,000 Rest-frame wavelength (Å) Ca II Mg II Fe II 0.05 0 3,000 3,500 4,000 4,500 5,000 5,500 6,000 6,500 7,000 7,500 8,000 Rest-frame wavelength (Å) Gal-Yam+09 Dessart+13

PISN without H...? 2.0 1.5 SN 2007bi relative flux [caII] 1.0 mgII mgI mgI 0.5 siII model OI OI 3000 4000 5000 6000 7000 8000 9000 wavelength (angstroms) Kasen+11

10 11 Lsun -22 -22 10 10 Lsun Not 56 Ni!! Absolute R-band magnitude Absolute R-band magnitude -20 -20 10 9 Lsun -18 -18 -16 -16 10 8 Lsun -14 -14 10 7 Lsun -12 -12 0 0 50 50 100 100 150 150 200 200 250 250 300 300 350 350 Days after the explosion Days after the explosion

What powers this type...?? - Not 56 Ni - Not internal energy (no H) - Not (clearly) interaction - magnetar...??? Quimby+11

10 11 Lsun (3) Mystery -22 (1) Kinetic energy 10 10 Lsun Absolute R-band magnitude -20 ~10 -3 (2) Radioactivity 10 9 Lsun -18 0.1 0.65 -16 10 8 Lsun -14 0.25 10 7 Lsun -12 0 50 100 150 200 250 300 350 Days after the explosion

100 150 200 250 Mass 50 2 x 10 -2 direct collapse CCSN (SN? GRB?) 10 -3 Superluminous PISN (1 x 10 -2 if Salpeter) supernovae

Toward Detection of First Supernovae • Massive star evolution and supernova emission • Superluminous supernova • Survey for first supernovae

Type brightness color progenitor Normal SN x x O SLSN O ? O (kinetic energy) (bright in UV) (need CSM) SLSN ~ PISN(?) x ? O (radioactivity) (faint in UV) (H?) SLSN O O ?? (??) (bright in UV)

Observed SLSN PISN model Quimby+11 Dessart+13

“Genuine” PISN may be difficult 30 28 Peak Apparent Magnitude 26 NIR survey WFIRST/WISH 24 22 R250 R200 20 R150 B250 B200 18 He130 He100 @ 2 um 16 0 5 10 15 20 redshift Kasen+11, see also Dessart+13

“Observed” SLSNe are detectable @ z > 10 NIR survey WFIRST/WISH MT, Moriya, Yoshida+13

23 z = 3 SPICA 24 6 25 AB magnitude 10 26 26 mag 27 15 WFIRST/WISH 28 20 29 JWST 30 1 2 3 4 5 6 7 8 9 10 Wavelength ( µ m) MT, Moriya, Yoshida+13

Survey simulation star formation rate 10 -3 R M max , SN M min , SN ψ ( M )d M R SLSN ( z ) = f SLSN ρ ∗ ( z ) R M max M min M ψ ( M )d M Quimby+13

WFIRST Up to z ~ 10 with planned strategy 10 3 WISH 100 deg 2 WFIRST-e + 3 µ m Number of SNe per bin WFIRST-e Euclid 6.5 deg 2 WFIRST 10 2 2019~ 40 deg 2 Euclid 10 1 10 0 WISH 10 -1 0 5 10 15 20 Redshift

To detect supernovae @ z ~ 15 140 120 100 26.5 mag 80 N 60 25.5 40 20 0 8 10 12 14 16 18 20 Redshift AB = 26.5 mag (@ 1-4 um) 2000 deg 2 6 visits in 0.5 yr

Studying IMF by number count Salpeter

!! Caveats !! • Star formation rate => Needs galaxy survey (z >~ 10) • “Mysterious” objects • Progenitor (minimum mass?) • Metallicity dependence => # of SN/SFR as a function of redshift • Completeness => Needs well-controlled “missed” fraction

Transient survey with Subaru/HSC (2014-) Superluminous supernovae at z ~ 5-6 10 6 20000 deg 2 LSST 10 5 100 deg 2 LSST deep drilling Number of SNe per bin 30 deg 2 HSC Deep 10 4 3 deg 2 HSC UltraDeep 10 3 10 2 10 1 10 0 10 -1 0 5 10 Redshift

Subaru and Hyper Suprime-Cam 104 CCDs ~ 900 Megapixel 8.2m 3m 3t !

Summary • “Normal” supernovae: difficult to detect @ z > 6 • “Superluminous” supernovae • kinetic powered, radioactively powered, and... • Detail of the progenitor is still mystery • Planned NIR survey can detect SLSNe up to z ~ 10 • Late 2010 and 2020- • z ~ 15 with dedicated NIR survey (2000 deg 2 ) • Lower-redshift survey is critical • progenitor, metallicity dependence, and completeness • Survey with Subaru is ongoing