Neutrinos From Supernovae John Beacom, The Ohio State University
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 1 SN 1987A: Our Rosetta Stone
IMB
KamII
Observation: Type II supernova Observation: The neutrino progenitors are massive stars precursor is very energetic
Theory: Core collapse makes a proto-neutron star and neutrinos
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 2 What Does This Leave Unknown? Total energy emitted in neutrinos? Partition between flavors? Emission in other particles? Spectrum of neutrinos? Neutrino mixing effects? ! Supernova explosion mechanism? Nucleosynthesis yields? Neutron star or black hole? Electromagnetic counterpart? Gravitational wave counterpart? ! and much more!
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 3 Plan of the Talk
✔ Introduction: Three detection modes
Revolutionizing MeV neutrino astronomy
Milky Way burst
Nearby galaxy mini-burst
Diffuse Supernova Neutrino Background
Concluding perspectives
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 4 Introduction: Three Detection Modes
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 5 Basic Features of MeV Neutrino Detection
Detectors must be massive: Effectiveness depends on volume, not area Example signals:
+ ⌫ + e ⌫ + e ¯ + p e + n ! e !
Detectors must be quiet: Need low natural and induced radioactivities Example background:
A(Z, N) A(Z +1,N 1) + e +¯⌫ ! e
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 6 Distance Scales and Detection Strategies
N >> 1 : Burst N ~ 1 : Mini-Burst N << 1 : DSNB
Rate ~ 0.01/yr Rate ~ 1/yr Rate ~ 108/yr high statistics, object identity, cosmic rate, all flavors burst variety average emission
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 7 Simple Estimate: Milky Way Burst Yields Super-Kamiokande (32 kton water) ~ 104 inverse beta decay on free protons ~ 102 - 103 CC and NC with oxygen nuclei ~ 102 neutrino-electron elastic scattering (crude directionality) KamLAND, MiniBooNE, Borexino, SNO+, etc (~ 1 kton oil) ~ 102 inverse beta decay on free protons ~ 102 neutron-proton elastic scattering ~ 10 - 102 CC and NC with carbon nuclei ~ 10 neutrino-electron elastic scattering IceCube (106 kton water) Burst is significant increase over background rate Possibility of precise timing information
Much larger or better detectors are being proposed now
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 8 Simple Estimate: Extragalactic Mini-Burst Yields
Yield in Super-Kamiokande ~ 1 (Mpc/D)^2
A 5000-kton detector could see mini-bursts from galaxies within several Mpc, where the supernova rate is above one per year
New considerations for such a detector as a dense infill for IceCube!
Kistler, Ando, Yuksel, Beacom, Suzuki (2011); builds on Yoichiro Suzuki’s ideas for Deep-TITAND
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 9 Simple Estimate: DSNB Event Rate
Super-Kamiokande rate in Kamiokande-II rate in a ~ 1 s-1 every 10 second interval special 10 second interval
NSN Mdet dN dN 4⇥D2 DSNB * dt ⇠ dt NSN Mdet DSNB 87A ⇥ 4⇥D2 ⇤ 87A ⇥ ⇤ For the DSNB relative to SN 1987A: 2 -10 NSN up by ~ 100 Mdet up by ~ 10 1/D down by ~ 10
DSNB event rate in Super-Kamiokande is a few per year
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 10 Revolutionizing MeV neutrino astronomy
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 11 First: Get Multi-kton-Scale Neutrino Detectors Super-K JUNO DUNE
32 kton water 20 kton oil 34 kton liquid argon Japan China United States running building proposing Excellent prospects for coverage of all neutrino flavors
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 12 Second: Enable Super-K Selection of Nuebar
The signal reaction produces a neutron, but most backgrounds do not
Beacom and Vagins (2004): First proposal to use dissolved gadolinium in large light water detectors showing it could be practical and effective
Neutron capture on protons Gamma-ray energy 2.2 MeV Hard to detect in SK + ¯e + p e + n ! Neutron capture on gadolinium Gamma-ray energy ~ 8 MeV Easily detectable coincidence separated by ~ 4 cm and ~ 20 µs
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 13 12 many nucleons of 16O significantly deviate - by about a dation. Some of us have been supported by funds from factor of four - from predictions. the Research Foundation of Korea (BK21 and KNRC), the Korean Ministry of Science and Technology, the Na- tional Research Foundation of Korea (NRF- 20110024009 VIII. ACKNOWLEDGMENT ), the European Union FP7 (DS laguna-lbno PN-284518 and ITN invisibles GA-2011-289442), the Japan Society We gratefully acknowledge the cooperation of the for the Promotion of Science, the National Science and Kamioka Mining and Smelting Company. The Super- Engineering Research Council (NSERC) of Canada, and Kamiokande experiment has been built and operated the Scinet and Westgrid consortia of Compute Canada; from funding by the Japanese Ministry of Education, This work is also supported by the National Natural Sci- Culture, Sports, Science and Technology, the U.S. De- ence Foundation of China (Grants No.11235006). partment of Energy, and the U.S. National Science Foun-
[1] T. Hagner et al.,Astropart.Phys.14,33(2000). Simulation program for particle physics experiments, [2] S. Abe et al.,(KamLANDCollaboration),Phys.Rev. GEANT : user guide and reference manual, CERN-DD- C81, (2010) 025807. 78-2(1978). [3] B. Bellini et al., (Borexino Collaboration), J. Cosmol. [25] A. Hoecker, P. Speckmayer, J. Stelzer, J. Therhaag, Astropart. Phys. 08 (2013) 049. E. von Toerne, and H. Voss, PoS A CAT 040 (2007); [4] J. F. Beacom and M. R. Vagins, Phys. Rev. Lett., 93: arXiv: physics/0703039. 171101 (2004). [26] P. Speckmayer, A. Hoecker, J. Stelzer, and H. VossJ. [5] K. Abe, et al.,(Hyper-Kamiokandeworkinggroup), Phys.: Conf. Ser. 219, 032057 (2010). arXiv:1109.3262. [27] H. Watanabe et al.,(Super-KamiokandeCollaboration), [6] M. Askins, et al.,(WATCHMANCollaboration), Astropart. Phys., 2009, 31:320. arXiv:1502.01132. [28] D. Cokinos and E. Melkonian, Phys. Rev. C 15, 1636 [7] L. Agostino, et al.,(MEMPHYSCollaboration),J.Cos- (1977). mol. Astropart. Phys. 1301 (2013) 024. [29] A. Ferrari, P. R. Sala, A. Fasso, and J. Ranft, FLUKA: [8] C. Adams, et al.,(LBNECollaboration), Amulti-particletransportcode,CERN-2005-10(2005), arXiv:1307.7335. INFN-TC-05-11, SLAC-R-773. [9] S. Fukuda et al.,(TheSuper-KamiokandeCollabora- [30] G. Battistoni et al.,AIPConf.Proc.896,31(2007). tion), Phys. Rev. Lett. 86, 5651 (2001). [31] S. Ando, K. Sato and T. Totani, Astropart. Phys. 18, 307 [10] J. Hosaka et al, (Super-Kamiokande Collaboration), (2003). Phys. Rev. D 73, 112001 (2006). [32] T. Totani and K. Sato, Astropart. Phys. 3, 367 (1995). [11] K. Abe et al.,(TheSuper-KamiokandeCollaboration), [33] R. A. Malaney, Astropart. Phys. 7, 125 (1997). Phys. Rev. D 83, 052010 (2011). [34] D. H. Hartmann and S. E. Woosley, Astropart. Phys. 7, [12] K. Bays et al.,(TheSuper-KamiokandeCollaboration), 137 (1997). Phys. Rev. D 85, 052007 (2012). [35] M. Kaplinghat, G. Steigman, and T. P. Walker, Phys. [13] S. W. Li and J. F. Beacom, Phys. Rev. C 89, 045801 Rev. D 62, 043001 (2000). (2014). [36] L. Strigari,Fate of the GADZOOKS! Proposal M. Kaplinghat, G. Steigman, and T. Walker, [14] S. W. Li and J. F. Beacom, Phys. Rev. D 91, 105005 JCAP, 0403:007 (2004). (2015). [37] T. Totani, K. Sato, and Y. Yoshii, Astrophys. J. 460, 303 [15] S. W. Li and J. F. Beacom, arXiv:1508.05389. For about 10 years:(1996). [16] D. R. Tilley, J. H. Kelley, J. L. Godwin, D. J. Millener, Vagins[38] S. Horiuchi,and colleagues developed experimental aspects J. F. Beacom, and E. Dwek, Phys. Rev. D J. E. Purcell, C. G. Sheu, and H. R. Weller, Nucl. Phys. Beacom and colleagues developed theoretical aspects79, 083013 (2009). A745,155(2004). [39] M. Fukugita and M.Kawasaki, Mon. Not. Roy. Astron. [17] H. Zhang et al.,(Super-KamiokandeCollaboration),As- SuperSoc.-K 2015: 340, L7Yes (2003). tropart. Phys. 60 (2015) 41. [40] C. Lunardini, Phys. Rev. Lett. 102, 231101(2009). [18] K. Abe, et al., (Super-Kamiokander Collaboration), [41] Ref. [4] proposed adding a 0.2% gadolinium solution into Nucl. Instr. Meth, A 737 (2014). the SK water. After exhaustive studies, on June 27, [19] S. Yamada, et al.,IEEETrans.Nucl.Sci.,57(2010)428. 2015, the SK Collaboration formally approved the con- [20] Z. Conner, PhD thesis, University of Maryland, 1997. cept, officially initiating the SuperK-Gd project, which [21] S. Desai, PhD thesis, Boston Univesity, 2004. will enhance anti-neutrino detectability (along with other [22] http://www.nndc.bnl.gov. physics capabilities) by dissolving 0.2% gadolinium sul- [23] http://www.tunl.duke.edu/nucldata/GroundStatedecays/. fate by mass in the SK water. [24] R. Brun, R. Hagelberg, M. Hansroul, and J. C. Lassalle, Will greatly increase sensitivity for many studies
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 14 Third: Remove Spallation Backgrounds
detector backgrounds
Super-K is already adopting Li-Beacom techniques Expect to reduce backgrounds in all MeV detectors by ~ 10
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 15 Localizing Spallation Production
Li and Beacom 2015a,b Almost all isotopes are produced in individual showers These showers can be localized by their Cherenkov light
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 16 Milky Way Burst
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 17 The Flavor Problem Need all flavors to measure the total emitted energy Need all flavors to test effects of neutrino mixing
4 ⌫¯e Precise (~ 10 events in Super-K)
⌫µ, ⌫⌧ , ⌫¯µ, ⌫¯⌧ Inadequate (~ 102 events in oil)
⌫e Inadequate (~ 102 events in Super-K)
How will we ensure complete flavor coverage?
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 18 Focus on Measuring Nue
Super-K JUNO DUNE ~ 102 events ~ 102 events ~ 103 events 10 10 16 e + O ν 12 8 8 e + C erg] 6 + e- erg] 6
52 e 52 x x [10 [10
tot 4 tot 4 e e ν E E - ? ? ν e + e 2 allowed 2 solid: Gd dashed: no Gd 0 0 0 5 10 15 20 25 30 0 5 10 15 20 25 30
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 19 The Waiting Problem
Will we be ready to detect a Milky Way supernova?
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 20 All-Sky Optical Monitoring to Leverage Connection to astronomy crucial, but optical data are lacking Enter OSU’s “Assassin” (All-Sky Automated Survey for SN)
Dominating discovery rate of supernovae in nearby universe
Discovering and monitoring optical transients to 17th mag. See also Adams, Kochanek, Beacom, Vagins, Stanek (2013)
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 21 The Aftermath What are the conditions in the proto-neutron star?
Horowitz et al. (2017) Li, Beacom, Roberts (in prep.)
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 22 Nearby Galaxy Mini-Burst
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 23 The Variations What are the properties of core collapse in extremes?
0.15 SN (4 Mpc) DSNB (1 day) Invisible (1 day)
H2O 0.1
H O + GdCl 0.05 2 3 dN/dE 1/[MeV Mton]
0 0 10 20 30 40 50 Visible Energy [MeV] Idea from Ando, Beacom, Yuksel (2005) Nakazato and collaborators
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 24 The Verifications What are the varieties and rates of transients?
15 observed (with SN 2008S-like) 11 observed (without SN 2008S-like) Neutrino bright, optically bright: 15 B-band 15 CCSNe 2.5 cosmic SFR extrapolation Core-collapse supernova NOROT-UV ROT-UV NOROT-H 2 ROT-H Neutrino bright, optically dim: 11 CCSNe 10 Core-collapse to black hole 1.5
B-band NOROT-UV Neutrino dim, optically bright:
1 CCSN rate [/yr] ROT-UV Type Ia supernova 5 NOROT-H Supernova impostor CCSNe in galaxy sample ROT-H 0.5 Neutrino dim, optically dim: 0 0 All the time! 0246 8 10 Distance D [Mpc] Horiuchi et al. (2013)
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 25 Diffuse Supernova Neutrino Background
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 26 What Does Burst Detection Leave Unknown?
Average neutrino emission? Variation between supernovae? Surprise propagation effects? ! Supernova rate of the universe? Black hole formation probability? Surprise sources? !
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 27 Theoretical Framework
Signal rate spectrum in detector in terms of measured energy dN 1 cdt e (E )=N (E ) (1 + z) ⇥[E (1 + z)] R (z) dz dE e p SN dz e Z0 h ih i Third ingredient: Detector Capabilities Second ingredient: Core-collapse (well understood) rate (formerly very uncertain, but now known with good precision)
First ingredient: Neutrino spectrum (this is now the unknown)
See my 2010 article in Annual Reviews of Nuclear and Particle Science
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 28 Measured Spectrum Including Backgrounds
Amazing background rejection: 3.5
] nothing but neutrinos despite
-1 Atm. ν + ν 3 µ µ huge ambient backgrounds MeV -1 2.5 Amazing sensitivity: factor Atm. ν + ν 2 € e e ~ 100 over Kamiokande-II limit and first in realistic DSNB range 1.5 [ (22.5 kton yr) e 1 € No terrible surprises
0.5 dN / dE Challenges: Decrease 0 20 30 40 50 60 70 80 backgrounds and energy
Visible Energy Ee [MeV] threshold and increase Malek et al. [Super-Kamiokande] (2003); efficiency and particle ID energy units changed in Beacom (2011) – use with care
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 29 Benefits of Neutron Tagging for DSNB
Solar neutrinos: 3 eliminated 10 GADZOOKS! -1 2 Reactor ! Spallation daughter decays: 10 e essentially eliminated 1 Supernova !e 10 (DSNB) Reactor neutrinos: Atmospheric !! !e
[(22.5 kton) yr MeV] 0 now a visible signal e 10 dN/dE -1 Atmospheric neutrinos: 10 significantly reduced
-2 10 0 5 10 15 20 25 30 35 40 Measured E [MeV] DSNB: e More signal, less background! Beacom, Vagins (2004) (DSNB predictions now at upper edge of band)
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 30 Super-K With Gd Can Detect the DSNB
Reactor ! ] e 8 MeV -1 Excluded 6 MeV 0.5 by SK 4 MeV SN1987A
MeV (2003) -1 0.4
0.3
0.2 [ (22.5 kton yr) e
0.1 dN / dE
0 10 20 30 40 Ee [MeV] Horiuchi , Beacom, Dwek (2009) Success in Super-K would motivate case for Hyper-K with Gd
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 31 Concluding Perspectives
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 32 The Time for Supernova Neutrinos is Now
N >> 1 : Burst N ~ 1 : Mini-Burst N << 1 : DSNB
Rate ~ 0.01/yr Rate ~ 1/yr Rate ~ 108/yr high statistics, object identity, cosmic rate, all flavors burst variety average emission
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 33 The Time for Neutrino Astronomy is Now
Neutrino Astronomy
MeV—GeV n TeV—PeV n EeV—ZeV n
Efforts: Efforts: Efforts: HK and more IceCube and more ANITA and more
Targets: Targets: Targets: Solar, SN, more GRBs, AGN, more GZK process Surprises Surprises Surprises
Neutrino astronomy must be broad
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 34 The Time for Neutrino Science is Now Neutrino Science
Laboratory n Cosmology n Astronomy n
Efforts: Efforts: Efforts: Fermilab and more CMB and more IceCube and more
Context: Context: Context: Precision Physics, Precision Cosmology, Transient Astronomy, BSM reach BSM reach Multi-messenger
Neutrinos are multi-frontier science
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 35 TeVPA 2017 tevpa2017.osu.edu
I August 7–11, Columbus, OH
I Registration and abstract submission are open
I Pre-meeting mini-workshops on Sunday, August 7
John Beacom, The Ohio State University IceCube Particle Astrophysics, Madison, May 2017 36