NEUTRINOS ON ICE THE SEARCH FOR THE COSMIC-RAY SOURCES FE KRAUSS, J. WILMS, M. KADLER, M. KRETER
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1 NEUTRINOS ON ICE THE SEARCH FOR THE COSMIC-RAY SOURCES FE KRAUSS, J. WILMS, M. KADLER, M. KRETER
2 COSMIC RAYS 2a
3 COSMIC RAYS 1896: Henri Becquerel discovery of radioactivity 1909: Theodor Wulf ascends Eiffel tower with electrometer 1912: Victor Hess balloon flight 5.3 km (17400 feet) Flux of charged particles from space 3a
4 COSMIC RAYS Energy Flux Tanabashi et al. (2018) 3b
5 WHERE ARE COSMIC RAYS COMING FROM? Energy Flux Galactic Extragalactic Tanabashi et al. (2018) 3c
6 ACTIVE GALACTIC NUCLEI (AGN) 4a
7 ACTIVE GALACTIC NUCLEI (AGN) Supermassive black hole M Accretion disk Relativistic jet 5a
8 Blazar flat-spectrum radio quasar (FSRQ) BL Lac Radio galaxy 5b
9 ACTIVE GALACTIC NUCLEI (AGN) 0.05 pc AU 5c
10 HERCULES A 500 kpc AU 6a
11 FINDING CR SOURCES 7a
12 How do we find sources of cosmic rays? Neutrinos AGN jets: multiwavelength information 8a
13 νfν [10 12 erg s 1 cm 2 ] radio optical X-ray γ-ray Frequency [Hz] Krauß F. et al. (2014) 9a
14 νfν [10 12 erg s 1 cm 2 ] ATCA TANAMI Planck 2MASS WISE UVOT BAT XRT Fermi/LAT 2FGL Frequency [Hz] Krauß F. et al. (2014) 9b
15 νfν [10 12 erg s 1 cm 2 ] ATCA TANAMI Planck Synchrotron 2MASS WISE UVOT BAT XRT Fermi/LAT 2FGL Frequency [Hz] Krauß F. et al. (2014) 9c
16 νfν [10 12 erg s 1 cm 2 ] ATCA TANAMI Planck 2MASS WISE UVOT Big Blue Bump BAT XRT Fermi/LAT 2FGL Frequency [Hz] Krauß F. et al. (2014) 9d
17 νfν [10 12 erg s 1 cm 2 ] ATCA TANAMI Planck 2MASS WISE UVOT XRT BAT Fermi/LAT 2FGL Leptonic (SSC, EC)? Hadronic? Frequency [Hz] Krauß F. et al. (2014) 9e
18 π 0 p p UV γ 10a
19 γ-ray γ π 0 p p UV γ Mannheim (1993), Mannheim (1995), Mücke (2000) 10b
20 π + n p UV γ Mannheim (1993), Mannheim (1995), Mücke (2000) 10c
21 ν µ ν e e + µ + ν µ π + e n ν e p? p UV γ The search for cosmic neutrinos Mannheim (1993), Mannheim (1995), Mücke (2000) 10d
22 THE SEARCH FOR COSMIC NEUTRINOS c IceCube 11a
23 ICECUBE RESULTS IceCube Collaboration (2013, 2013, 2014, 2015) 12a
24 ICECUBE RESULTS 16 neutrinos IceCube Collaboration (2013, 2013, 2014, 2015) 12b
25 PEV NEUTRINOS : IC 14 AND IC 20 IceCube Collaboration (2013) 13a
26 IDENTIFYING NEUTRINO COUNTERPARTS Step 1: Find possible counterparts 14a
27 IDENTIFYING NEUTRINO COUNTERPARTS 15a
28 IDENTIFYING NEUTRINO COUNTERPARTS Six bright blazars coincident with PeV neutrinos No clear association 16a
29 IDENTIFYING NEUTRINO COUNTERPARTS Step 2: Calculate neutrino emission 17a
30 IDENTIFYING NEUTRINO COUNTERPARTS νfν [10 12 erg s 1 cm 2 ] ATCA BAT TANAMI WISE Ced Planck UVOT XRT Frequency [Hz] Fermi/LAT 2FGL νlν [erg s 1 ] Mannheim (1993), Mannheim (1995), Mücke (2000) Fν (E ν ) de ν = F γ (E) de 17b
31 ASSUMPTIONS OF NEUTRINO CALCULATION All of high-energy emission is of hadronic origin All of the neutrinos emitted at one energy (delta-peak) Calculated numbers are maximum possible number 18a
32 R EPEAT ATCA TANAMI Ced Planck 2MASS WISE UVOT BAT XRT 2MASS WISE OM UVOT BAT XMM /pn XRT Fermi/LAT 2FGL ATCA TANAMI Ced Planck BAT WISE UVOT Fermi/LAT 2FGL XRT BAT INTEGRAL Fermi/LAT XRT 2FGL E ATCA TANAMI Planck 1045 E MASS WISE UVOT E TANAMI 2MASS WISE UVOT BAT XRT Fermi/LAT 2FGL E ATCA TANAMI Ced Planck BAT WISE UVOT XRT Fermi/LAT 2FGL νlν [erg s 1 ] νfν [10 12 erg s 1 cm 2 ] ATCA TANAMI Ced Planck Fermi/LAT 2FGL νlν [erg s 1 ] νfν [10 12 erg s 1 cm 2 ] 100 FOR ALL COUNTERPARTS Frequency [Hz] 1024 E Frequency [Hz] Krauß et al. (2014) 1024 E Frequency [Hz] a
33 RESULTS 20a
34 RESULTS FOR IC 14 & IC 20 source events Total 1.9±0.4 Krauß et al. (2014) 21a
35 RESULTS FOR IC 14 & IC 20 Correct order of magnitude of predicted neutrino events Calorimetrically blazars can explain IceCube events Large angular uncertainty complicated source identification Krauß et al. (2014) 21b
36 R ESULTS FOR IC 35 2 PeV event r50 = 15.9 IceCube Collaboration (2014) 22a
![γ-ray flux F100 300000 MeV [10 6 cm 2 s 1 ] RESULTS FOR IC 35: VARIABILITY Kadler, Krauss et al.](/docs-images/96/127299602/images/37-1.jpg "(2016), Nature Physics 2010 2010.5 2011 2011.5 2012 2012.5 2013 2013.5 2.5 2 1.5 1 0.")
37 γ-ray flux F MeV [10 6 cm 2 s 1 ] RESULTS FOR IC 35: VARIABILITY Kadler, Krauss et al. (2016), Nature Physics MJD 23a
![γ-ray flux F100 300000 MeV [10 6 cm 2 s 1 ] RESULTS FOR IC 35: VARIABILITY Kadler, Krauss et al.](/docs-images/96/127299602/images/38-1.jpg "(2016), Nature Physics 2010 2010.5 2011 2011.5 2012 2012.5 2013 2013.5 2.5 2 1.5 1 0.")
38 γ-ray flux F MeV [10 6 cm 2 s 1 ] RESULTS FOR IC 35: VARIABILITY Kadler, Krauss et al. (2016), Nature Physics MJD 23b
![γ-ray flux F100 300000 MeV [10 6 cm 2 s 1 ] RESULTS FOR IC 35: VARIABILITY Kadler, Krauss et al.](/docs-images/96/127299602/images/39-1.jpg "(2016), Nature Physics 2010 2010.5 2011 2011.5 2012 2012.5 2013 2013.5 2.5 2 1.5 1 0.")
39 γ-ray flux F MeV [10 6 cm 2 s 1 ] RESULTS FOR IC 35: VARIABILITY Kadler, Krauss et al. (2016), Nature Physics MJD 23c
40 RESULTS FOR IC 35: SED νfν [erg s 1 cm 2 ] ALMA ATCA LBA 2MASS WISE UVOT BAT INTEGRAL Fermi/LAT SMARTS XRT High-fluence outburst Short flare 2LAC range νlν [erg s 1 ] χ Frequency [Hz] N ν = 5.7 (IceCube time range) Kadler, Krauß et al. (2016), Nature Physics 24a
41 RESULTS FOR IC A 22 September 2017: ν alert from IceCube & coincident γ-ray flare from TXS (IceCube, Fermi-LAT et al., 2018) 25a
42 RESULTS FOR IC A 22 September 2017: ν alert from IceCube & coincident γ-ray flare from TXS (IceCube, Fermi-LAT et al., 2018) 25b
43 RESULTS FOR IC A 25c
44 RESULTS FOR IC A Discovery by Y. Tanaka (Hiroshima University) Fast multiwavelength follow-up Detection in VHE with MAGIC TXS at z=0.34 (Paiano et al 2018) 26a
![2 MAGIC significance [σ] 5 10 original GCN Notice Fri 22 Sep 17 20:55:13 UT refined best-fit direction IC170922A IC170922A 50% - area: 0.](/docs-images/96/127299602/images/45-2.jpg "15 square degrees IC170922A 90% - area: 0.97 square degrees 6.6 6 4.6 3FHL 3FGL 78.4 78.0 Fermi-LAT Counts/Pixel R ESULTS 1 0 77.6 77.2 76.8 76.")
45 IC A FOR TXS PKS MAGIC PSF Right Ascension TXS PKS Declination Declination 6.2 MAGIC significance [σ] 5 10 original GCN Notice Fri 22 Sep 17 20:55:13 UT refined best-fit direction IC170922A IC170922A 50% - area: 0.15 square degrees IC170922A 90% - area: 0.97 square degrees FHL 3FGL Fermi-LAT Counts/Pixel R ESULTS Right Ascension Only one source consistent with this neutrino event IceCube, Fermi-LAT et al. (2018), Science 27a
46 CAVEATS AND PROBLEMS 28a
47 What about other sources? What do we know about outburst - neutrino associations? How certain are we about outburst associations? 29a
48 SIGNIFICANCE & SIGNALNESS IC 35 IC A r 50 [ ] E ν,total [TeV] Signalness 100% 56.5% Significance 1.9σ 3σ Neither association is significant! 30a
49 NEUTRINOS < 1 PEV 31a
50 NEUTRINOS > 100 TEV IC E deposited MJD α J [ ] δ J [ ] ang. morphology [TeV] res Shower Shower Shower <1.2 Track Shower Shower Shower Shower Shower Shower Shower Shower <1.2 Track Shower Shower <1.2 Track Shower Shower Shower Obtain multiwavelength SEDs for all 3LAC counterparts 32a
51 NEUTRINOS > 100 TEV IC events R Galactic Plane h 46 8h 39 4h 0h h h 48 12h FGL sources Krauß et al., 2018, A&A accepted Calculate neutrino estimates N ν 33a
52 NEUTRINOS > 100 TEV N ν,max,all = 493 maximum number 34a
53 NEUTRINOS > 100 TEV N ν,max,all = 493 N ν,spec,all = 97 maximum number powerlaw neutrino spectrum 34b
54 NEUTRINOS > 100 TEV N ν,max,all = 493 N ν,spec,all = 97 N ν,f,all = maximum number powerlaw neutrino spectrum ν flavors, blazar physics 34c
55 NEUTRINOS > 100 TEV N ν,max,all = 493 N ν,spec,all = 97 N ν,f,all = maximum number powerlaw neutrino spectrum ν flavors, blazar physics Highest expected # neutrino: PKS : 2.7 Only 2 sources above 1 ν Approach underestimates neutrino numbers: full sky 34d
56 NEUTRINOS > 100 TEV Full sky approximation: assume sources similar IC events R Galactic Plane h 46 8h 39 4h 0h h h 48 12h FGL sources deg 2 /41253 deg 2 = a
57 NEUTRINOS > 100 TEV Full sky approximation: assume sources similar N ν,max,fullsky = 493/0.136 = 3637 maximum number 35b
58 NEUTRINOS > 100 TEV Full sky approximation: assume sources similar N ν,max,fullsky = 493/0.136 = 3637 maximum number N ν,spec,fullsky = 712 powerlaw neutrino spectrum 35c
59 NEUTRINOS > 100 TEV Full sky approximation: assume sources similar N ν,max,fullsky = 493/0.136 = 3637 maximum number N ν,spec,fullsky = 712 powerlaw neutrino spectrum N ν,f,fullsky = 178 ν flavors, blazar physics 35d
60 NEUTRINOS > 100 TEV Full sky approximation: assume sources similar N ν,max,fullsky = 493/0.136 = 3637 maximum number N ν,spec,fullsky = 712 powerlaw neutrino spectrum N ν,f,fullsky = 178 ν flavors, blazar physics 178» 10 (16) 35e
61 NEUTRINOS > 100 TEV νfν [10 12 erg s 1 cm 2 ] ATCA BAT TANAMI WISE Ced Planck UVOT XRT Fermi/LAT 2FGL νlν [erg s 1 ] Frequency [Hz] a
62 NEUTRINOS > 100 TEV νfν [10 12 erg s 1 cm 2 ] ATCA BAT TANAMI WISE Ced Planck UVOT XRT Fermi/LAT 2FGL νlν [erg s 1 ] Frequency [Hz] b
63 NEUTRINOS > 100 TEV νfν [10 12 erg s 1 cm 2 ] ATCA BAT TANAMI WISE Ced Planck UVOT XRT Fermi/LAT 2FGL νlν [erg s 1 ] Frequency [Hz] c
64 NEUTRINOS > 100 TEV 10 cosmic events (/16): 8% of emission hadronic Considering unresolved blazars: 4% First constraint on hadronic contribution to SED Is this consistent with previous results? 36d
65 MULTIWAVELENGTH MODELING OF TXS Leptonic model (Gao et al., 2018; Keivani et al., 2018) 37a
66 MULTIWAVELENGTH MODELING OF TXS Hadronic model (Gao et al., 2018; Keivani et al., 2018) 37b
67 CONCLUSIONS AGN & blazars are best (U)HE cosmic ray candidates Two blazar outbursts coincident with neutrino detection First constraint of hadronicness of blazars 38a
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