Supernova Rate and Supernova Followup Observation 2017 Nov

Supernova Rate and Supernova Follow-up Observation 2017 Nov 24 김상철(Sang Chul KIM) 한국천문연구원(KASI) 1 1

Supernova Rate and Supernova Follow-up Observation 2017 Nov 24 김상철(Sang Chul KIM) 한국천문연구원(KASI) ※ Most of slides on the SN Rate are from those at the KAS meeting (2017 Apr 13) of Prof. Bon-Chul Koo (SNU) 2 2

When will be the next Galactic SN? (베텔지우스가 초신성 폭발한다면…) https: //www. youtube. com/watch? v=v. Xf. Ki. D 9 di. NU 3

Introduction – Stellar Evolution • Mass Final Stages • Low-mass stars White Dwarfs (WDs) SN Ia • Massive (≥ 8 M⊙) stars core-collapse SN http: //earthspacecircle. blogspot. kr/2013/07/stellar-evolution. html 4

Supernova (SN) types • Supernovae : Brightest objects in galaxies (MV = -14 ∼ -22) • Typical types No H lines (pop II) Type I a Ib Ic WD + Giant/MS/He * (Single Degenerate, SD) WD + WD (Double Degenerate, DD) H lines (pop I) Type II Core collapse SNe Ia (thermonuclear stellar explosion) (WD originated SNe) 백색왜성 기원 초신성 CC SNe 핵붕괴 초신성 http: //dujs. dartmouth. edu/2008/05/type-ia-supernovae-properties-models-and-theories-of-their-progenitor-systems http: //wwwmpa. mpa-garching. mpg. de/mpa/research/current_research/hl 2013 -8 -en. html http: //spiff. rit. edu/richmond/sdss/sn_survey. html 5

Supernova (SN) types • Supernovae : Brightest objects in galaxies (MV = -14 ∼ -22) • Typical types No H lines (pop II) Type I a H lines (pop I) Type II Ib Ic WD + Giant/MS/He * (Single Degenerate, SD) WD + WD (Double Degenerate, DD) Core collapse SNe Ia (thermonuclear stellar explosion) (WD originated SNe) 백색왜성 기원 초신성 CC SNe 핵붕괴 초신성 http: //dujs. dartmouth. edu/2008/05/type-ia-supernovae-properties-models-and-theories-of-their-progenitor-systems http: //wwwmpa. mpa-garching. mpg. de/mpa/research/current_research/hl 2013 -8 -en. html http: //spiff. rit. edu/richmond/sdss/sn_survey. html 6

Supernovae taxonomy Type Sub-types I Ia No H Si II (6150Å) absorption near peak light Ib/c Ib Weak/no Si absorption He I (5876Å) emission Ic Weak/no He II II-P/L/n H II-P/L II-P No narrow lines Plateau in light curve(LC: mag vs time) II-L Linear decrease in LC Some narrow lines Pe iar e N S IIb : IIn : H lines nearby (1015 cm) CSM Ibn : He lines Spectrum changes to become like type Ib l. Ic-BL : sometimes associated with GRBs and/or hypernova (broad lines : (2 -3)× 10 u c 4 ultra-bright type II : ~1051 erg radiation energy. Ia : changing rapidly Superluminous SNe, pair-instability SNe, Superluminous Ia Subluminous SNe, Subluminous Ia Super-Chandrasekhar Ia : mass ˃ Chandrasekhar limit Ia-IIn : CSM Iax : Ia w/lower L, less E, less ejecta mass https: //en. wikipedia. org/wiki/Supernova Kilonova/macronova, SN imposters, magnetar km/s) – dwarf gal http: //astronomy. swin. edu. au/cosmos/S/Supernova+Classification 7

Number ratio 76% 21% Volume-limited sample Ideal magnitude-limited sample Li+11 (MN 412 1441) 8

SN Rate Estimation for the Milky Way 1) 2) 3) 4) … Historical SNe in the Galaxy SN statistics of galaxies Star Formation Rate Radioactive 26 Al mass + SN Rate of the Local Group 9

(1) SN Rate from Historical SNe l Simple estimation • SN 1006, Crab (1054), 3 C 58 (1181), Tycho (1572), Kepler (1604) 5 SN/1000 yrs × (10/3)2 ∼ 5 SN/100 yrs l Published results +7. 4 • 5. 7± 1. 7 SN/100 yrs (Strom 94 AA 288 L 1) -2. 7 • 4. 6 +7. 3 SN/100 yrs (Adams+ 13 Ap. J 778 164) -2. 6 • 3. 4 +1. 4 CC SN/100 yrs -0. 8 • 1. 4 SN Ia/100 yrs 10

(2) SN Rate from SN statistics l Simple estimation • Sbc, LB = (2. 6 ± 0. 6) × 1010 L⊙ ∼ 3 SN/100 yrs ※ (Cappellaro+99 A&A 351 459) l Published results +0. 8 • 2. 5 -0. 4 SN/100 yrs (Tammann+ 94 Ap. JS 92 487) • 2. 8 ± 0. 6 SN/100 yrs (W. Li+ 11 MN 412 1441) 11

(3) SN Rate from Star Formation Rate (SFR) l Simple estimation ∙ • M* ∼ 1. 3 ± 0. 2 M⊙/yr ∙ × f(M > 8 M ) / 〈M〉 ∼ 1. 4 CC SNe/100 yrs M * ⊙ 『Physics of the IS and IG Medium』 (Draine 2011) l Published results • 1 -2 CC SN/100 yrs (Reed 05 AJ 130 1652) 12

(4) SN Rate from 26 Al (τlife∼ 1 Myr) l Simple estimation • M(26 Al) ∼ 2. 8 M⊙ M(26 Al) / 〈Y〉/ τlife ∼ 1. 9 CC SN/100 yrs Diehl+ 2006 (Nature 439 45, Supplement 5) l Published results • 1. 9 ± 1. 1 CC SN/100 yrs (Diehl+ 06 Nature 439 45) 13

Other Methods l Pulsar distribution • ∼ 3. 2 -3. 7 SN/100 yrs (Faucher-Giguère & Kaspi 06 Ap. J 643 332) l No neutrino burst • Large Volume Detector (LVD) operation during last 21 years (1992 June – 2013 Dec) (Agafonova+ 15 Ap. J 802 47) ≤ 11. 4 CC SN/100 yrs 14

Summary of Milky Way SN Rate Method Historical SN CC SN 3. 4 +7. 3 -2. 6 SN Ia +1. 4 -0. 8 All SNe 4. 6 +7. 4 -2. 7 SN statistics 2. 30± 0. 48 0. 54± 0. 12 2. 84± 0. 60 Authors Adams+13 W. Li+11 SFR 1 -2 ⋯ ⋯ Reed 05 26 Al 1. 9± 1. 1 ⋯ ⋯ Diehl+06 Pulsar 3. 2 -3. 7 ⋯ ⋯ Faucher-Giguère & Kaspi 06 No neutrino burst ≤ 11. 4 ⋯ ⋯ Agafonova+15 Galactic CC SN rate ∼ 2 -3 SN/100 yrs 15

SN Rate of the Local Group l Local Group • R ≤ 1 Mpc • Milky Way, M 31, M 33 and ≥ 30 dwarf galaxies l ‘Historical’ SNe • 1987 A (LMC), SN 1885 A (M 31) l SN statistics • M 31, M 33 : 0. 83, 0. 62 CC SN/100 yrs (Tammann+94) • LMC, SMC : 0. 45, 0. 11 CC SN/100 yrs (Tammann+94) l SNR statistics • 0. 25 -0. 46 SN/100 yrs for the LMC+SMC (Maoz, Badenes 10 MN 407 1314) • 0. 31 SN/100 yrs for M 33 (Sarbadhicary+17 MN 464 2326) 16

Supernova Follow-up Observation 17

Various SN survey projects • intermediate Palomar Transient Factory (i. PTF) • All Sky Automated Survey for Super. Novae (ASAS-SN, www. astronomy. ohio • • • • state. edu/~assassin/index. shtml) Public ESO Spectroscopic Survey for Transient Objects (PESSTO) Pan-STARRS Survey for Transients (PSST) Aqueye+ (182 cm Copernico telescope in Asiago Cima Ekar) Asiago Transient Classification Program ATLAS survey (twin 0. 5 m telescope system on Haleakala and Mauna Loa, surveying up to 60, 000 square degrees per night) Catalina Real-Time Transient Survey, CRTS (crts. caltech. edu) - SNHunt (nesssi. cacr. caltech. edu/catalina/current. html) High Cadence Transient Survey (Hi. TS) Katzman Automatic Imaging Telescope (KAIT) Kepler, La Silla-QUEST (LSQ) MASTER Global Robotic Net (master. sai. msu. ru/en/) Optical Gravitational Lensing Experiment (OGLE, ogle. astrouw. edu. pl) PMO-Tsinghua Supernova Survey (PTSS) Swift Optical/Ultraviolet Supernova Archive (SOUSA) transient survey with Subaru/Hyper Suprime-Cam (tpweb 2. phys. konan-u. ac. jp/~tominaga/HSCSN/) XAO (Xinjiang Astronomical Observatory) and THU (Tsinghua University) Supernova Survey (XTSS) • Intensive Monitoring Survey of Nearby Galaxies (IMSNG) • KMTNet Supernova Program (KSP) 18

Korea Microlensing Telescope Network (KMTNet): Three new 1. 6 -m wide-field telescopes in the southern hemisphere, providing 24 -h sky coverage. “Star never sets on the KMTNet” Africa CTI O SAA O Chile Antarctica Australia SS O 19

Korea Microlensing Telescope Network (KMTNet): Three new 1. 6 -m wide-field telescopes in the southern hemisphere, providing 24 -h sky coverage. “Star never sets on the KMTNet” 20

Korea Microlensing Telescope Network Chilean Site 21

Korea Microlensing Telescope Network Wide Field CCD Imager: 2 2 Field of View Ø Four e 2 v Mosaic CCD Chips Ø 340 M pixels (18 K× 18 K), each 10 μm Ø 0. 40 arcsec/pixel, 2 degree × 2 degree FOV Ø Mechanical cooling (-110 ℃) Ø 32 readout channels Ø Filters : BVRI (3 sites), g’r’i’z’ Hα (Chile) Ø Quantum effie : ∼ 85% in V, ∼ 80% in I 22

SN survey projects - Sciences • Type classification – Ia, Ib, Ic, IIP, IIL, IIn, IIb, Ibn, Ic. BL, Iax, . Ia, SL SN, PI SN, Ia-IIn, SN imposter, kilonova, macronova, etc. - Ia – SD, DD - distance indicator • Shock Breakout (SBO) • Explosion mechanism • Nucleosynthesis heavier than Fe • Stellar evolution, mass loss 23

Supernova Sciences! LSST Science Book (ar. Xiv: 0912. 0201) 24 17 24

Shock Breakout (SBO) Core collapse of massive stars (˃8 M⊙) (Illustration by R. J. Hall) 25

Shock Breakout (SBO) 26

SBO – Kepler SNe KSN 2011 a (IIP) Blue points : 30 -min cadence Red dots : 1 day medians KSN 2011 d (IIP) Garnavich+16 Ap. J 820 23 27

SBO – Kepler SNe KSN 2011 a (IIP) KSN 2011 d (IIP) Blue points : 30 -min cadence Red dots : 6 -hr medians Garnavich+16 Ap. J 820 23 28

SBO – Kepler SNe KSN 2011 d (IIP) Blue points : 30 -min cadence Red dots : 3. 5 -hr medians Garnavich+16 Ap. J 820 23 Best fit photospheric model LC Nakar & Sari (2010) SBO model (R=490 R⊙) 29

Early detection of SN SN 2011 fe (Ia, M 101) (D=6. 4 Mpc) Exploding primary * : Mg Teff < a few × 105 K No MS/RG Geneneracy-supported compact objects (WD/NS) Companion secondary * : No Roche-lobe overflowing RG/MS Bloom+12 0. 17 d (4. 1 hr) 0. 48 d (11. 52 hr) PTF (Nugent+11, Nat 480 344) SN primary (exploding) star parameters : radius, density, Temperature… Ap. J 744 L 17 30

Early detection of SN SN 2013 fs (IIP, NGC 7610) (=i. PTF 13 dqy) d=50. 95 Mpc 3 hr Yaron+17 Nat. Ph (Nature. Physics), 13, 510 31

Companion interaction of SN Ia companion SN Ia Ia Fig 3 : SN signatures of companion interaction Kasen 10 Ap. J 708 1025 32

Early bolometric light curve(LC) Bolometric LC Mg’ YSG SN 2011 dh (IIb, M 51) Bersten+12 Radius effect – noticeable before t~5 days (compact 2 R⊙ vs extended 270 R⊙) Ap. J 757 31 33

Early bolometric light curve(LC) Models - Same explosion energy - Different initial radius : SN 2011 dh (IIb, M 51) Bersten+12 Ap. J 757 31 34

Early bolometric light curve(LC) SN 2014 J (Ia, M 82) (D=3. 5 Mpc) progenitor, R=1. 7 R⊙ Goobar+15 Companion, R=4. 0 R⊙ Ap. J 799 106 35

Very early light curve(LC) SN 2015 F (Ia, NGC 2442) (d = 23. 9 ± 0. 4 Mpc) 0. 43 m Lee Sang Gak Tel. Daily cadence Progenitor : WD Companion star : (MS, WD ? ) M. Im+15 Ap. JS 221 22 36

SN early detection • Sciences from SN early detection - progenitors - explosion mechanism - fast decay optical transients • Neutrino detection comes first from the CC • 99% of SN energy emerge as neutrinos (kinetic energy ∼ 1%, optical emissions ∼ 0. 01%) • Neutrino telescope can give fast alert to optical and other λ observatories 37

Milky Way Supernovae • SN rate ∼ few decades - 100 years • Last (observed) = 1604 Kepler + 관상감 • Last (known) = 1680 Cassiopeia A (Changbom Park et al. 2016 JKAS 49 233) • The World is waiting for a new SN! 38

Super. Nova Early Warning System (SNEWS) • Similar to “Seismic waves in(on) the Earth” Seismic wave 파동 Speed 통과물질 피해 Primary wave 종파 5 -8 km/s 고, 액, 기체 Minor Secondary wave 횡파 3 -4 km/s 고체 Huge 41

Super. Nova Early Warning System (SNEWS) • http: //snews. bnl. gov/ • A network of 7 neutrino detectors - Borexino, Daya Bay, Kam. LAND, HALO, Ice. Cube, LVD, Super-Kamiokande - began automatic operation in 2005 - reports gather + identify SNe at Brookhaven National Laboratory need signals at ≥ 2 detectors within 10 seconds • To make early warning for CC SNe from the Milky Way, or nearby galaxies (e. g. LMC, Canis Major dwarf) • Neutrino pulses from SN 1987 A – arrived 3 hours before the photons 42

SN Explosion SN 1987 A (IIP, LMC) Tarantula Nebula d~49. 97 kpc (Pietrzynski+ 13 Natur 495 76) 1987 Feb 23. 316 (UT) B 3 supergiant Peak : +2. 9 mag (B-V) = +0. 085 43

1058 Neutrinos from SN 1987 A • Kamiokande II – 11 events (13 seconds) • Irvine-Michigan-Brookhaven (IMB, Lake Erie) – 8 events Kamiokande II IMB data K II : Hirata+ 87 Phys. Rev. Lett. 58, 1490 IMB : Bionta+ 87 Phys. Rev. Lett. 58, 1494 44

Neutrino research - Astronomical applications • Solar neutrino • Massive stars during very late evolutionary stages – we can look into the “core” directly and study the stellar interior. • Core-collapse supernovae in the Milky Way or Galaxies in the Local Group (∼long Gamma-Ray Burst) - behind the bulge, Sun - large extinction - good sensitivity larger distance (∼Mpc) - failed SNe • NS + NS merger short GRB + kilo nova • NS + BH merger short GRB • WD + WD merger collapse to a NS without a bright SN • Supernova relic neutrinos (SRN : Neutrinos produced by all of the SN explosions since the beginning of the Universe) – esp. below 20 Me. V SRN energy spectrum measurement, history of SN bursts • Cosmic ray spallation – atmospheric neutrinos • Dark Matter – Weakly Interacting Massive Particles (WIMP) 45

Photon, neutrino – escape from the Sun’s interior Photon and neutrino – travel times out of the center of the Sun 104 -105 yr 2 sec k” l a mw do n a “R 46

Nearby massive stars - nucleosyntheses 1 st step : 1 H + 1 H → 2 H + e+ + νe (→ 1. 44 Me. V) 2 nd step : 2 H + 1 H → 3 He + γ (→ 5. 49 Me. V) rd 3 3 4 1 1 3 step : He + He → He + H (→ 12. 9 Me. V) 12 C + 1 H → 13 N + γ 13 N → 13 C + e+ + ν e 13 C + 1 H → 14 N + γ 14 N + 1 H → 15 O + γ 15 O → 15 N + e+ + ν e 15 N + 1 H → 12 C + 4 He C-burning 12 C + 12 C → 24 Mg + γ (13. 933 Me. V) → 23 Mg + n (-2. 599 Me. V) (endothermic) → 23 Na + p (2. 241 Me. V) 20 → Ne + α (4. 617 Me. V) → 16 O + 2α (-0. 113 Me. V) (endothermic) O-burning 16 O + 16 O → 28 Si + α (9. 954 Me. V) (~60%) → 31 P + p (7. 678 Me. V) (~40%) → 31 S + n (1. 500 Me. V) → 32 S + γ → 24 Mg + 2α http: //www. astro. umd. edu/~richard/ASTR 680/ 28 Si + 4 He ⇔ 32 S + γ 14 2 16 32 S + 4 He ⇔ 36 Ar + γ 16 2 18 36 Ar + 4 He ⇔ 40 Ca + γ 18 2 20 40 Ca + 4 He ⇔ 44 Ti + γ 20 2 22 44 Ti + 4 He ⇔ 48 Cr + γ 22 2 24 48 Cr + 4 He ⇔ 52 Fe + γ 24 2 26 52 Fe + 4 He ⇔ 56 Ni + γ 26 2 28 56 Ni + 4 He ⇔ 60 Zn + γ 28 2 30 47