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

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

May 20, 2023 160 likes •573 views

Toward Detection of First Supernovae - - Masaomi Tanaka 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

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SLIDE 1

Toward Detection of First Supernovae

  • 初代星超新星の検出に向けて -

Masaomi Tanaka 田中 雅臣

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SLIDE 2

First Star

Taniguchi-san’s talk (e.g., Bromm+01, Stiavelli+09, Bromm & Yoshida 11, Rydberg+11)

10 11 12 13 14 15 16 17 18 19 40 45 50

z mAB

Pop III 300 Msun (2 um)

JWST (5σ) 100hr

L ~ 106 - 107.5 Lsun (for 100-1000 Msun)

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SLIDE 3

First Supernova L ~ 108-10 Lsun

Smartt 2012 1010 Lsun 109 Lsun 108 Lsun 107 Lsun Observed magnitude @ z = 4

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SLIDE 4

Toward Detection of First Supernovae

  • Massive star evolution and

supernova emission

  • Superluminous supernova
  • Survey for first supernovae
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SLIDE 5

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

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SLIDE 6

300 20 40 60 80 100 120 140 50 100 150 200 250 300 MCO/M MMS/M (b) Z = 0.02 Z = 0.01 Z = 0.004 Z = 0.001 Z = 10-4

M(56Ni) > 1 M, CCSN

M(56Ni) > 3 M, CCSN PISN PISN SN 2007bi

Yoshida+14, see Yoon+12 and Chatzopoulos+12 for the effect of rotation

initial mass Final CO core mass

PISN CCSN

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SLIDE 7

Yoshida+14

50 100 150 200 50 100 150 200 250 300 Mf/M MMS/M (a) Z = 0.02 Z = 0.01 Z = 0.004 Z = 0.001 Z = 10-4 Mf = MMS

initial mass Final mass wind mass loss pulsational pair instability

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SLIDE 8

Core-collapse supernova

Element distribution after explosion Shock breakout (~ 1d for red supergiant) Ek ~ Eint ~ 1051 erg

56Ni O He C

0.1 Msun

Tominaga+

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SLIDE 9

Pair-instability supernova

Element distribution after explosion

56Ni O16 Mg C

50 100 150 200

50 100 150 Enclosure Mass [M ]

  • 8
  • 6
  • 4
  • 2
  • 8
  • 6
  • 4
  • 2

B200 R200

Chen+14 Si

4 Msun Explosive O/Si burning Enuc ~ 1053 erg Ek ~ 1052 erg

  • 8
  • 6
  • 4
  • 2

log [x]

(Takahashi-san’s talk)

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SLIDE 10

1010 Lsun 109 Lsun IIn

  • 22
  • 20
  • 18
  • 16
  • 14
  • 12

50 100 150 200 250 300 350 Absolute R-band magnitude Days after the explosion

100d 1 year II Ibc 108 Lsun 107 Lsun 1011 Lsun

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SLIDE 11

Energy source of SN (1) radioactivity

p n 56Ni

decay

56Co gamma 56Fe

decay

gamma

0.1 Msun ejection => ~ 5 x 108 Lsun @ 20d

~1 week ~100 d L = [1.7 × 109e(t/8.8d) + 3.8 × 108e(t/111d)] M56Ni 0.1M

  • L
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SLIDE 12

tb ~ 1d for RSG (R ~ 1000 Rsun) tb ~ 0.001d for WR (R ~ 1 Rsun) (negligible)

Energy source of SN (2) internal energy

L ∼ Eint tb t 1 ∆t ∼ 3 × 108L

  • Eint

1051erg tb 1d t 100d 2

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SLIDE 13

Energy source of SN (3) kinetic energy

L ∼ 109L α 0.1 Ek 1051erg ∆t 1yr

  • Moriya+14

dense CSM SN

High mass loss rate (> 10-3 Msun/yr) ~100 yr before the explosion

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SLIDE 14

1010 Lsun 109 Lsun IIn=CSM 0.1

  • 22
  • 20
  • 18
  • 16
  • 14
  • 12

50 100 150 200 250 300 350 Absolute R-band magnitude Days after the explosion

II=RSG 0.65 Ibc=WR 0.25 108 Lsun 107 Lsun 1011 Lsun

(2) internal energy (3) kinetic energy (1) radioactive energy (56Ni)

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SLIDE 15

First supernovae...

Mesinger+06 29 mag @4.5um SN/ JWST FOV number for 1 yr survey 30 mag JWST tsurvey = 1 yr, texp = 0.1 - 1 d Number of fields = tsurvey/2texp

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SLIDE 16
  • Massive star evolution and

supernova emission

  • Superluminous supernova
  • Survey for first supernovae

Toward Detection of First Supernovae

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SLIDE 17

1010 Lsun 109 Lsun

  • 22
  • 20
  • 18
  • 16
  • 14
  • 12

50 100 150 200 250 300 350 Absolute R-band magnitude Days after the explosion

108 Lsun 107 Lsun 1011 Lsun

  • 22
  • 20
  • 18
  • 16
  • 14
  • 12

50 100 150 200 250 300 350 Absolute R-band magnitude Days after the explosion

SN 2006gy

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SLIDE 18

Kinetic-energy powered

absorption line SN 2006gy emission line =Type IIn CSM interaction emission line

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SLIDE 19

1010 Lsun 109 Lsun 108 Lsun 107 Lsun 1011 Lsun

  • 22
  • 20
  • 18
  • 16
  • 14
  • 12

50 100 150 200 250 300 350 Absolute R-band magnitude Days after the explosion

56Ni decay

  • 22
  • 20
  • 18
  • 16
  • 14
  • 12

50 100 150 200 250 300 350 Absolute R-band magnitude Days after the explosion

SN 2007bi

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SLIDE 20

Possibly PISN??

But see Moriya+10, Yoshida+11 for core-collapse interpretation

−50 50 100 150 200 250 300 350 −23 −22 −21 −20 −19 −18 −17 −16 −15 Time since explosion (d) Data 80M 90M 100M 110M 120M

b

PISN models

− − − Absolute MR (mag)

Gal-Yam+09

M(56Ni) ~ 3 Msun

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SLIDE 21 3,000 3,500 4,000 4,500 5,000 5,500 6,000 6,500 7,000 7,500 8,000 0.05 0.1 0.15 0.25 0.3 0.2 0.35 0.4 Rest-frame wavelength (Å) SN 2007bi, 54 d after peak SN 1999as SYNOW ft Ca II Mg II Fe II Mg II Ca II [Ca II] Scaled Fλ (erg s–1 cm–2 Å–1)

3,000 3,500 4,000 4,500 5,000 5,500 6,000 6,500 7,000 7,500 8,000 0.05 0.1 0.15 0.25 0.3 0.2 0.35 0.4 Rest-frame wavelength (Å)

SN 2007bi, 54 d after peak SN 1999as SYNOW ft

Ca II Mg II Fe II Mg II Ca II [Ca II] Scaled Fλ (erg s–1 cm–2 Å–1)

Observed

Gal-Yam+09 Hydrogen!

Theory

Dessart+13

Spectrum: No hydrogen

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SLIDE 22

PISN without H...?

3000 4000 5000 6000 7000 8000 9000 wavelength (angstroms) 0.5 1.0 1.5 2.0 relative flux mgI mgII mgI siII [caII] OI OI

Kasen+11

SN 2007bi model

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SLIDE 23

1010 Lsun 109 Lsun 108 Lsun 107 Lsun 1011 Lsun

  • 22
  • 20
  • 18
  • 16
  • 14
  • 12

50 100 150 200 250 300 350 Absolute R-band magnitude Days after the explosion

  • 22
  • 20
  • 18
  • 16
  • 14
  • 12

50 100 150 200 250 300 350 Absolute R-band magnitude Days after the explosion

Not 56Ni!!

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SLIDE 24

What powers this type...??

Quimby+11

  • Not 56Ni
  • Not internal energy (no H)
  • Not (clearly) interaction
  • magnetar...???
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SLIDE 25

1010 Lsun 109 Lsun 108 Lsun 107 Lsun 1011 Lsun

  • 22
  • 20
  • 18
  • 16
  • 14
  • 12

50 100 150 200 250 300 350 Absolute R-band magnitude Days after the explosion

(1) Kinetic energy (3) Mystery (2) Radioactivity 0.65 0.25 0.1

~10-3

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SLIDE 26

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

(1 x 10-2 if Salpeter)

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SLIDE 27
  • Massive star evolution and

supernova emission

  • Superluminous supernova
  • Survey for first supernovae

Toward Detection of First Supernovae

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SLIDE 28

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

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SLIDE 29

PISN model

Dessart+13 Quimby+11

Observed SLSN

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SLIDE 30

“Genuine” PISN may be difficult

5 10 15 20 redshift 16 18 20 22 24 26 28 30 Peak Apparent Magnitude R250 R200 R150 B250 B200 He130 He100

@ 2 um

Kasen+11, see also Dessart+13

NIR survey WFIRST/WISH

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SLIDE 31

“Observed” SLSNe are detectable @ z > 10

MT, Moriya, Yoshida+13

NIR survey WFIRST/WISH

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SLIDE 32

MT, Moriya, Yoshida+13

23 24 25 26 27 28 29 30 1 2 3 4 5 6 7 8 9 10 AB magnitude Wavelength (µm)

z = 3 6 10 15 20

26 mag WFIRST/WISH SPICA JWST

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SLIDE 33

Survey simulation

RSLSN(z) = fSLSN ρ∗(z) R Mmax,SN

Mmin,SN ψ(M)dM

R Mmax

Mmin Mψ(M)dM

10-3

star formation rate

Quimby+13

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SLIDE 34

10-1 100 101 102 103 5 10 15 20 Number of SNe per bin Redshift

WISH WFIRST-e + 3µm WFIRST-e WFIRST Euclid

100 deg2 40 deg2 6.5 deg2

WFIRST WISH Euclid 2019~

Up to z ~ 10 with planned strategy

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SLIDE 35

AB = 26.5 mag (@ 1-4 um) 2000 deg2 6 visits in 0.5 yr

20 40 60 80 100 120 140 8 10 12 14 16 18 20 N Redshift

26.5 mag 25.5 To detect supernovae @ z ~ 15

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SLIDE 36

Salpeter

Studying IMF by number count

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SLIDE 37

!! 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

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SLIDE 38

Superluminous supernovae at z ~ 5-6

10-1 100 101 102 103 104 105 106 5 10 Number of SNe per bin Redshift

LSST LSST deep drilling HSC Deep HSC UltraDeep

3 deg2 30 deg2 100 deg2 20000 deg2

Transient survey with Subaru/HSC (2014-)

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SLIDE 39

Subaru and Hyper Suprime-Cam

104 CCDs ~ 900 Megapixel

3m 3t ! 8.2m

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SLIDE 40

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 deg2)
  • Lower-redshift survey is critical
  • progenitor, metallicity dependence,

and completeness

  • Survey with Subaru is ongoing