observations of supernovae through the kno...• using 9 telescopes with 0.43m – 2.1m in korea,...

1https://www.scientificamerican.com/article/found-the-most-powerful-supernova-ever-seen/

http://www2.mpia-hd.mpg.de/IRSPACE/Tycho_release/tycho1572/Tycho_observation_image.pdf

Observations of Supernovae through the KNO

2020 Aug 28 (Fri)(Sang Chul KIM)

Korea Astronomy & Space Science Institute (KASI)

4th Workshop on Korean Neutrino Observatory (UNIST)

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김상철

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Neutrinos from Supernovae (SNe)

(1) Neutrinos from thermonuclear explosions in core collapse SNe

(2) Various SN survey projects

- Korean projects for the SN follow-up observations

(3) SN Rate Estimation for the Milky Way and the Local Group

- KNO observations of neutrinos from MW/LG SNe

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4

×

(1) Neutrinos from Core Collapse SNe• At final stage of massive ( ) star evolution, at T 3 109 K Si-burning starts

producing 56Ni

• Then, the Fe core collapses and SN explosion occurs when the explosion energy is larger than the binding energy of the stellar envelope

• (Explosion energy 1053 erg) > (Binding energy 1049 - 1051 erg)

• Most ( 99%) of the energy is released as neutrinos, some of them interact with infalling matter

https://www.researchgate.net/publication/306091657

=8 M⊙ ~

~

à

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(1) Neutrinos from Core Collapse SNe• 1053 erg Most ( 99%) of the energy is released as neutrinos, some of them

interact with infalling matter

https://www.researchgate.net/publication/306091657https://www.researchgate.net/publication/306091657

à ~

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(1) Neutrinos from Core Collapse SNe• Neutrino from each nucleosynthesis stage

Woosley & Janka 2005 NatPh, 1, 147

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Three Phases of Neutrino Emission

Georg G. Raffelt 2017 CNNP Conference (Catania) (https://agenda.infn.it/event/12166/contributions/12610/attachments/9378/10583/HALO_HALO-1kT_CNNP.pdf)

• Shock breakout

• De-leptonization of outer core layers

• Shock stalls 150 km

• Neutrinos powered by infalling matter

• Cooling on neutrino diffusion time scale

Spherically symmetric Garching model (25 M ) with Boltzmann neutrino transport

~

⊙

8

Neutrino : Luminosities and EnergiesHoriuchi+18 (MNRAS 475 1363)

Collapse of a 35 M star1-Dim

Neutrinoluminosity

Mean energy

Shape parameter

Collapse of a 23 M star2-Dim

Black hole Neutron star

⊙ ⊙

?µ ?µ

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Neutrinos from Core Collapse SNe• Neutrino comes out first from the core collapse (CC), at least a few

hours before the optical emission

• SN energy

99% comes as neutrinos

1% comes as kinetic energy

0.01% optical emission

• Neutrino telescope can give fast alert to optical and other observatories

• Sciences from SN early detection

- progenitors

- explosion mechanism

- fast decay optical transients

•

•

•

~

~

?

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SN Explosion

Tarantula Nebula

d~49.97 kpc (Pietrzynski+ 13 Nature 495 76)

1987 Feb 23.316 (UT)

B3 I (supergiant)

Peak : +2.9 mag

(B-V) = +0.085

Teff = 16,000 K

L = 105 L

Minitial 20 M (N. Smith 2007 AJ 133 1034)

SN 1987A (IIP, LMC)

⊙

⊙à ~

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SN 1987A – Bolometric Light Curve

Arnett et al. (1989, ARAA, 27, 629)

△

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SN 1987A in the LMC

1987 Feb 23, 07:35:35 (UT), distance = 50 kpc

Irvine-Michigan-Brookhaven-3 (8kton)

Courtesy Soo-Bong Kim

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小柴昌俊

Neutrino Detector – Kamiokande II•

•

Upgrade operation since 1985Observed solar neutrinosObserved 11 neutrinos from Supernova (SN) 1987A – 50 kpc (163,000 ly) away in the Large Magellanic Cloud (LMC)

Masatoshi Koshiba ( ) – 2002 Nobel Prize in Physics (w/Raymond Davis Jr., Riccardo Giacconi)for his work directing the Kamoka experiments, and in particular for the first-ever detection of astrophysical neutrinos

http://www.nobelprize.org/nobel_prizes/physics/laureates/2002/

à§§

http://mulli2.kps.or.kr/~pht/11-11/021108.htm

1987년 2월 23일 07h 35m 35s (UT)

(1914-)(1926-)

(1931-))

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1058 Neutrinos from SN 1987A• Kamiokande II – 11 events (12.44 seconds)• Irvine-Michigan-Brookhaven (IMB, Lake Erie, 5.58 sec) – 8 events

Kamiokande II

IMB data

K II : Hirata+ 87 Phys. Rev. Lett. 58, 1490

IMB : Bionta+ 87 Phys. Rev. Lett. 58, 1494

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SN survey projects• intermediate Palomar Transient Factory (iPTF)

Zwicky Transient Factory (ZTF)

• All Sky Automated Survey for SAS-SN)• 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 0.5m 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 (HiTS)

• 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 (tpweb2.phys.konan-u.ac.jp/~tominaga/HSC-SN/)

• XAO (Xinjiang Astronomical Observatory) and THU (Tsinghua University) Supernova Survey (XTSS)

• Intensive Monitoring Survey of Nearby Galaxies (IMSNG, Seoul National University, Myungshin Im)

• KMTNet Supernova Program (KSP)

à

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ZTF

• Palomar Transient Factory (PTF), intermediate PTF (iPTF)

(2017 ) Zwicky Transient Facility (ZTF, )• Palomar Observatory : 1.2m Samuel Oschin Telescope (47 deg2 field-of-view), 1.5m

telescope, 5m Hale Telescope

• Wide field and fast readout electronics an order of magnitude faster (than PTF) time-domain survey

• Young SNe, transients, variable stars, binary stars, active galactic nuclei (AGNs), tidal disruption events (TDEs), moving objects like asteroids or comets

• Scan = 3750 deg2/hour, up to 20.5 mag

• Northern hemisphere + Galactic plane

1.2m Samuel Oschin Telescope https://www.ztf.caltech.edu/page/science

à

à

~ https://www.ztf.caltech.edu/

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ASAS-SN• All Sky Automated Survey for SuperNovae (ASAS-SN)• www.astronomy.ohio-state.edu/~assassin/index.shtml• Ohio State University• Automatic observations using 14cm robotic telescopes (7.8”/px) in N

(Haleakala, Texas) and S (CTIO, South Africa) hemispheres survey the entire sky once a day, 8 – 18 mag

• Search for SNe and transients e.g. superluminous SN ASASSN-15lh• Other objects were also discovered – TDEs, Galactic novae, cataclysmic

variables, stellar flares, asteroids, comets, etc.

https://twitter.com/SuperASASSN/status/928342328414220289/photo/1 Dong+16 Sci 351 257

MU

à

à

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IMSNG• Intensive Monitoring Survey of Nearby Galaxies (IMSNG, Seoul

National University, Myungshin Im)• Using 9 telescopes with 0.43m – 2.1m in Korea, Australia, USA (LOAO, McDonald),

Uzbekistan

• Optical monitoring observations of 60 nearby (D < 50 Mpc, b>20 ) galaxies, brighter than MNUV=-18.4 AB mag

• Cadence a few hours

Im + 19 (JKAS 52, 11)

°

~

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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”

CTIO SAAO

SSO

Africa

Chile

Australia

Antarctica

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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”

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Korea Microlensing Telescope Network

Chilean Site

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××

Korea Microlensing Telescope Network

Wide Field CCD Imager: 2 2 Field of View ° ´ °

ØØØ

ØØØØ

Four e2v Mosaic CCD Chips340M pixels (18K 18K), each 10 µm0.40 arcsec/pixel, 2 degree 2 degree FOVMechanical cooling (-110 ? )32 readout channelsFilters : BVRI (3 sites), g’r’i’z’ Ha (Chile)Quantum effie : 85% in V, 80% in I∼ ∼

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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

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Supernova Sciences!

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LSST Science Book (arXiv: 0912.0201)

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SN Rate Estimation for the Milky Way

+ SN Rate of the Local Group

1) Historical SNe in the Galaxy

2) SN statistics of galaxies

3) Star Formation Rate

4) Radioactive 26Al mass

…

This part (SN rate estimation) is from the presentation of Prof. Bon-Chul Koo (SNU) at the

Korean Astronomical Society meeting on 2017 Apr 13

※

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SN Type : Ia vs CC

Li+11 (MN 412 1441)

Volume-limited sample Ideal magnitude-limited sample

76% 21%

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×

±

(1) SN Rate from Historical SNel

à

l

Simple estimation

SN1006, Crab (1054), 3C58 (1181), Tycho (1572), Kepler (1604)

5 SN/1000 yrs (10/3)2 5 SN/100 yrs

Published results

5.7 1.7 SN/100 yrs (Strom 94 AA 288 L1)4.6 SN/100 yrs (Adams+ 13 ApJ 778 164)

• 3.4 CC SN/100 yrs

• 1.4 SN Ia/100 yrs

+7.4-2.7

+7.3-2.6+1.4

-0.8

•

•

•

~

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± ×

±

(2) SN Rate from SN statisticsl

à

l

Simple estimation

Sbc, LB = (2.6 0.6) 1010 L3 SN/100 yrs

Published results

2.5 SN/100 yrs (Tammann+ 94 ApJS 92 487)

2.8 0.6 SN/100 yrs (W. Li+ 11 MN 412 1441)

+0.8

-0.4

(Cappellaro+99 A&A 351 459)

•

•

•

⊙

※

~

31

±

×

(3) SN Rate from Star Formation Rate (SFR)l

à

l

Simple estimation

M* 1.3 0.2 M /yr

M f(M > 8 M ) / M 1.4 CC SNe/100 yrs

Published results

1-2 CC SN/100 yrs (Reed 05 AJ 130 1652)

Physics of the IS and IG Medium(Draine 2011)

•

*

•

~

~

·· ⊙

⊙ 〈〉

『』

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±

(4) SN Rate from 26Al ( 1 Myr)t life~l

à

l

Simple estimation

M(26Al) 2.8 M

M(26Al) / / 1.9 CC SN/100 yrs

Published results

1.9 1.1 CC SN/100 yrs (Diehl+ 06 Nature 439 45)

Diehl+ 2006 (Nature 439 45, Supplement 5)

•

life

•

~

~ ⊙

〈Y〉τ

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Other Methodsl

l

à

Pulsar distribution

3.2-3.7 SN/100 yrs (Faucher-Gigu re & Kaspi 06 ApJ 643 332)

No neutrino burst

Large Volume Detector (LVD) operation during last 21 years (1992 June – 2013 Dec) (Agafonova+ 15 ApJ 802 47)

= 11.4 CC SN/100 yrs

•

•

~ e

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Milky Way SN Rate - Summary

à Galactic CC SN rate 2-3 SN/100 yrs

26

+7.3-2.6

+1.4

-0.8+7.4-2.7

~

? ?

? ?

? ?

? ?

Method CC SN SN Ia All SNe Authors

Historical SN

3.4 1.4 4.6 Adams+13

SN statistics 2.30±0.48 0.54±0.12 2.84±0.60 W. Li+11

SFR 1-2 Reed 05

Al 1.9±1.1 Diehl+06

Pulsar 3.2-3.7 Faucher-Gigu re & Kaspi 06

No neutrinoburst

=11.4 Agafonova+15

e

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SN Rate of the Local Groupl

l

l

l

Local Group

R = 1 Mpc

Milky Way, M31, M33 and 100 dwarf galaxies (McConnachie 12 AJ 144 4)

‘Historical’ SNe

1987A (LMC), SN 1885A (M31)

SN statistics

M31, M33 : 0.83, 0.62 CC SN/100 yrs (Tammann+94)

LMC, SMC : 0.45, 0.11 CC SN/100 yrs (Tammann+94)

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 M33 (Sarbadhicary+17 MN 464 2326)

•

•

•

•

•

•

•

=

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Probability to Observe Galactic SNe

Courtesy Bon-Chul Koo

e.g. in 30 years

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SN burst observation by HK

Courtesy Soo-Bong KimBest scenarios for KNO!

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CC SN Rate

Ando et al. (2005, PRL, 95, 171101)

SN burst – Position accuracy

※ Gadolinium trichloride (GdCl3) addition (0.2%) increases detection efficiency (J. F. Beacom & M.

R. Vagins 2004 Phys. Rev. Lett. 93, 171101)

1 degree at 10 kpc16


à

~

40±

Neutrino Observation TimescaleY. Suwa (2019 ApJ 881 139)

Observable timescale of neutrinos (s)

Dis

tanc

e to

the SN

(kpc

)

LMC : d = 51.2 3.1 kpc (Panagia et al. 1991 ApJL 380 L23)

(12.4 s)

※

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• SN Relic Neutrino (SRN)Figure from Shin’ichiro Ando

Now

• Failed SNe

Kochanek+08 (ApJ 684 1336)

5

?

?

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(Diffuse Supernova Neutrino Background)


(Supernova Relic Neutrino)SRN

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Summary

• Core-collapse supernovae in the Milky Way and Nearby Galaxies (probably in the Local Group) within a few Mpc

• Detection of failed explosion to form BHs

• Supernova relic neutrinos (SRN) SRN energy spectrum measurement, history of SN bursts, cosmic SFR

Neutrino research – Supernovae Science

à

4444

Thank you.

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Neutrino Sources

Katz & Spiering (2012, Progress in Particle and Nuclear Physics, 67, 651)

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백색왜성 기원 초신성 핵붕괴 초신성

Supernova (SN) types

•

•

http://dujs.dartmouth.edu/2008/05/type-ia-supernovae-properties-models-and-theories-of-their-progenitor-systemshttp://wwwmpa.mpa-garching.mpg.de/mpa/research/current_research/hl2013-8/hl2013-8-en.htmlhttp://spiff.rit.edu/richmond/sdss/sn_survey/sn_survey.html

Supernovae : Brightest objects in galaxies (MV = -14 -22)∼

Typical typesNo H lines (pop II) Type I H lines (pop I) Type II

Core collapse

SNe Ia (thermonuclear stellar explosion) CC SNe

(WD originated SNe)

WD + Giant/MS/He *

(Single Degenerate, SD)WD + WD

(Double Degenerate, DD)

a Ib Icà à

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백색왜성 기원 초신성 핵붕괴 초신성

Supernova (SN) types

•

•

http://dujs.dartmouth.edu/2008/05/type-ia-supernovae-properties-models-and-theories-of-their-progenitor-systemshttp://wwwmpa.mpa-garching.mpg.de/mpa/research/current_research/hl2013-8/hl2013-8-en.htmlhttp://spiff.rit.edu/richmond/sdss/sn_survey/sn_survey.html

Supernovae : Brightest objects in galaxies (MV = -14 -22)∼

Typical typesNo H lines (pop II) Type I H lines (pop I) Type II

Core collapse

SNe Ia (thermonuclear stellar explosion) CC SNe

(WD originated SNe)

WD + Giant/MS/He *

(Single Degenerate, SD)WD + WD

(Double Degenerate, DD)

a

Ib

Ic

à à

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Supernova Taxonomy

Cappellaro & Turatto (astro-ph/0012455)

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SuperNova Early Warning System (SNEWS)

• Similar to “Seismic waves in(on) the Earth”

Seismic wave Speed

5-8 km/s

파동 통과물질 피해

Primary wave , , Minor

Secondary wave 3-4 km/s Huge

종파 고 액 기체

횡파 고체

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SuperNova Early Warning System (SNEWS)

• http://snews.bnl.gov/

• A network of 7 neutrino detectors

- Borexino, Daya Bay, KamLAND, HALO, IceCube, 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 1987A – arrived 3 hours before the photons

à

observations of supernovae through the kno...• using 9 telescopes with 0.43m – 2.1m in korea,...

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