Supernovae and Neutrinos: The Crossroads John Beacom, The Ohio State University
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 1 Gateway: Astrophysics Neutron stars Black holes GW sources Cosmic rays Chemical elements Galaxy feedback
Supernovae
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 2 Gateway: Particle Physics s Origin of mass Mixing, CP violation Collective effects Dark matter New forces New particles
Neutrinos
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 3 Crossroads Origin of mass Neutron stars Mixing, CP violation Black holes Collective effects GW sources Dark matter Cosmic rays New forces Chemical elements New particles Galaxy feedback
X Neutrinos
Supernovae
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 4 Why a Crossroads?
To understand supernovae only neutrinos can reveal these extreme conditions
To understand neutrinos only these extreme conditions can reveal particle properties
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 5 Crossroads: Past Versus Future
Are we ready?
For Milky Way burst detection? To precisely detect the DSNB? To detect extragalactic minibursts?
To advance multimessenger astrophysics? To probe physics beyond the standard model? To make neutrino astronomy real?
What should we do differently?
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 6 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 Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 7 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 Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 8 Distance Scales and Detection Strategies
N >> 1 : Burst N ~ 1 : Mini-Burst N << 1 : DSNB
Gpc kpc Mpc
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 Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 9 Scientific Opportunities: MW Burst
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 10 Question 1: The Source What are the mechanisms of core collapse?
Idealized; simple Realistic; complex
Oak Ridge group (2015)
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 11 Question 2: The Messengers How do neutrinos mix in core collapse?
Idealized; simple Realistic; complex
Trapping Decoupling Free-streaming 11 1.51.5 n fwd (0) n
11 n bwd G ne (z,t) (z,t) (z,t)
eq ee n fwd eq ee ne eq ee r r 0.50.5 r (z) / 0.50.5 n bwd n G Dighe and Smirnov (1999); Raffelt slide 00 00 0 10001000 20002000 0 10001000 20002000 z z Capozzi, Dasgupta, Mirizzi, Sen, Sigl (2019)
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 12 The Flavor Problem: Experiment 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 KL+)
⌫e Inadequate (~ 102 events in Super-K)
How will we ensure complete flavor coverage?
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 13 Multi-kton-Scale Neutrino Detectors Super-K JUNO DUNE
32 kton water 20 kton oil 40 kton liquid argon Japan China United States running building preparing Together, excellent potential for MeV neutrino astronomy
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 14 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
DUNE uncertain due to cross section, detector response Need better understanding of neutrino+nucleus!
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 15 The Timeline Problem
present and near future beyond that
large detectors maybe not time used to measure anymore neutrino mixing
Who will build detectors for supernova neutrinos?
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 16 What is Needed?
Interactions: Understand neutrino-nucleus cross sections This should include differential cross sections, particle emission, etc.
Detectors: Understand detection response, especially DUNE
Coordination: Ensure full coverage, especially flavors
Simulations: Robust predictions to at least 10 seconds
Theory: Solution of flavor mixing problem Costs and benefits of “flavor censorship”
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 17 Question 3: The Consequences What are the dynamics of the supernova?
Idealized; simple Realistic; complex
Core collapse leads to Luminosity (erg/s) Type II SN (= red supergiants)
shock breakout an outgoing shock of 1045 51 internal energy radioac5ve energy total energy ~ 10 erg 44 10 cooling envelope 1043 plateau ~0.5hr Light signal has total 1042 Luminosity 49 @ UV & op5cal tail energy ~ 10 erg 1041
1040 0.1 d 1d 10 d 100 d 1000 d 5me
Tanaka (2017)
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 18 Question 4: The Multimessengers How do these signals reveal the dynamics?
Idealized; simple Realistic; complex 54 Astronomers detect the νe 52 νe ]) νx optical light -1 50 GW EM 48 pre-SN νe Physicists detect the 46 SBO 44 plateau neutrinos 42
Log (luminosity [erg s 40 progenitor Nobody detects 38 9 6 3 0 -2 0 2 4 6 8 anything else Log (time relative to bounce [s]) Nakamura et al. (2016)
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 19 The Waiting Problem
Will we be ready to detect a supernova neutrino burst?
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 20 How Will We See the Supernova? Connection to astronomy crucial, but optical data are lacking Enter OSU’s “ASAS-SN” (All-Sky Automated Survey for SN)
Host Galaxy log L/L? -3 -2 -1 0 1 100
10
1 Offset (kpc) 0.1 ASAS-SN Other Prof. Amateurs -15 -16 -17 -18 -19 -20 -21 -22 -23 -24 -25 -26
Host Galaxy MKs
Discovering and monitoring optical transients to 18th mag.
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 21 What is Needed?
Detectors: Ensure readiness with practiced alarms
Coordination: Test procedure with practiced alarms, alerts
Pointing: Decide if triangulation works or not This needs a new paper to check Beacom and Vogel (1999) versus Brdar, Lindner, Xu (2018)
Theory: Clear predictions for possible signals
Observers: New facilities for full Milky Way coverage Build on Adams, Kochanek, Beacom, Vagins, Stanek (2013), Nakamura et al. (2016)
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 22 Scientific Opportunities: DSNB
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 23 Question 1: The Template What are the properties of core collapse on average?
Bays et al. [Super-Kamiokande] (2012)
Horiuchi , Beacom, Dwek (2009)
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 24 Question 2: The Multitude What is the cosmic rate of core collapses?
Horiuchi et al. (2011) Lien, Fields, Beacom (2010)
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 25 What is Needed?
3 10 GADZOOKS!
-1 Full deployment of Gd in Super-K 2 Reactor 10 !e
1 Supernova !e 10 (DSNB) Atmospheric Full plans for Gd in Hyper-K
!! !e
[(22.5 kton) yr MeV] 0 e 10
dN/dE See Vagins talk -1 10
-2 10 0 5 10 15 20 25 30 35 40 Measured Ee [MeV]
New ways to reduce backgrounds further Spallation backgrounds: Li and Beacom, 2014+ Atmospheric Backgrounds: Zhou and Beacom, 2019+
Advance, update astrophysical constraints ASAS-SN nearby supernova rate forthcoming Other new data on SFR, direct BH detection, etc.
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 26 Scientific Opportunities: Nearby Galaxies
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 27 Question 1: 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 Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 28 Question 2: 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 Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 29 What is Needed?
Detector of mass > 5 Megaton 2008? 2002bu 1.0 NGC 300-T 2002kg, 04dj 2004am, 08iz 2005af 2008bk 2002hh 2004et 2008S 1999gq 2002ap, 03gd 2008ax 2005cs 2005at 1999gi 1999em 2007gr 1999ev
0.8 N Events 0.6 ≥
0.4 time N ≥ 15 10 7 5 4 3 = hit kept in phase space cut = hit removed in Probability of 0.2 vertex phase space cut
0.0 0246 8 10 Distance [Mpc] Kistler et al. (2011) Boser et al. (2014)
Best hope is a dedicated modification of IceCube
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 30 Concluding Perspectives
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 31 Take-Away Messages
Profound physics questions depend on MeV neutrinos Extreme conditions, neutrino properties, surprises
Need better detectors, signal ID, and backgrounds With theoretical help, can leverage other investments
Next discovery may be the DSNB in Super-K with Gd Construction is already underway
Rich prospects, rich context Interpretation will be complicated
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 32 Crossroads Origin of mass Neutron stars Mixing, CP violation Black holes Collective effects GW sources Dark matter Cosmic rays New forces Chemical elements New particles Galaxy feedback
X Neutrinos
Supernovae Are we ready?
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 33 How to Advance our Goals?
We’re going to need a bigger boat
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 34 The Time for Neutrino Astronomy is Now
Neutrino Astronomy
MeV—GeV n TeV—PeV n EeV—ZeV n
Efforts: Efforts: Efforts: SK, 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 Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 35 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 Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 36 Summoning the Multi-Messenger
Photons Neutrinos
Cosmic Rays Dark Matter
Gravitational Waves
Careful what we wish for!
John Beacom, The Ohio State University Supernova Neutrinos at the Crossroads, Trento, Italy, May 2019 37