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)
1
김상철
2
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
3
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
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
5
(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 ~
6
(1) Neutrinos from Core Collapse SNe• Neutrino from each nucleosynthesis stage
Woosley & Janka 2005 NatPh, 1, 147
7
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
9
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
•
•
•
~
~
?
10
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 ~
11
SN 1987A – Bolometric Light Curve
Arnett et al. (1989, ARAA, 27, 629)
△
12
SN 1987A in the LMC
1987 Feb 23, 07:35:35 (UT), distance = 50 kpc
Irvine-Michigan-Brookhaven-3 (8kton)
Courtesy Soo-Bong Kim
13
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/
১
http://mulli2.kps.or.kr/~pht/11-11/021108.htm
1987년 2월 23일 07h 35m 35s (UT)
(1914-)(1926-)
(1931-))
14
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
15
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
16
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
17
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/
18
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
19
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)
°
~
20
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
21
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”
22
Korea Microlensing Telescope Network
Chilean Site
23
××
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∼ ∼
24
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
25
Supernova Sciences!
25 17
LSST Science Book (arXiv: 0912.0201)
26
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
27
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
※
28
SN Type : Ia vs CC
Li+11 (MN 412 1441)
Volume-limited sample Ideal magnitude-limited sample
76% 21%
29
×
±
(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
•
•
•
~
30
± ×
±
(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)
•
*
•
~
~
·· ⊙
⊙ 〈 〉
『 』
32
±
(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
33
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
34
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
35
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)
•
•
•
•
•
•
•
=
36
Probability to Observe Galactic SNe
Courtesy Bon-Chul Koo
e.g. in 30 years
37
SN burst observation by HK
Courtesy Soo-Bong KimBest scenarios for KNO!
38
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
Courtesy Soo-Bong Kim
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)
※
41
Neutrinos from Supernovae (SNe)
• SN Relic Neutrino (SRN)Figure from Shin’ichiro Ando
Now
• Failed SNe
Kochanek+08 (ApJ 684 1336)
5
?
?
42
(Diffuse Supernova Neutrino Background)
Courtesy Soo-Bong Kim
(Supernova Relic Neutrino)SRN
43
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.
45
Neutrino Sources
Katz & Spiering (2012, Progress in Particle and Nuclear Physics, 67, 651)
46
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
47
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
48
Supernova Taxonomy
Cappellaro & Turatto (astro-ph/0012455)
49
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
50
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
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