NEUTRINOS ON ICE 3LAC COUNTERPAR TS TO ICECUBE NEUTRINOS ABOVE 100 TEV

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1 NEUTRINOS ON ICE 3LAC COUNTERPAR TS TO ICECUBE NEUTRINOS ABOVE 100 TEV FE KRAUSS J. WILMS, K. MANNHEIM, K. DESOKAR, M. KADLER, M. KRETER Papers in PDF link to journal article, slides available at

2 COSMIC RAYS 1896: H. Becquerel discovery of radioactivity 1909: T. Wulf Eiffel tower and electrometer 1912: V. Hess balloon flight 5.3 km (17400 feet) Flux of charged particles from space 2a

3 COSMIC RAYS Energy Flux Energy Flux Tanabashi et al. (2018) 2b

4 WHERE ARE COSMIC RAYS COMING FROM? Energy Flux Energy Flux Galactic Extragalactic Tanabashi et al. (2018) 2c

5 Blazars 3a

6 BLAZAR SED νfν [10 12 erg s 1 cm 2 ] radio optical X-ray γ-ray Frequency [Hz] Krauß F. et al. (2014) a

7 B LAZAR SED c Wikipedia Krauß F. et al. (2014) 4b

8 BLAZAR SED νfν [10 12 erg s 1 cm 2 ] radio optical Synchrotron X-ray γ-ray Frequency [Hz] Krauß F. et al. (2014) c

9 BLAZAR SED νfν [10 12 erg s 1 cm 2 ] radio optical Big Blue Bump X-ray γ-ray Frequency [Hz] Krauß F. et al. (2014) d

10 BLAZAR SED νfν [10 12 erg s 1 cm 2 ] radio optical X-ray γ-ray Leptonic (SSC, EC)? Hadronic? Böttcher (2013) Frequency [Hz] Krauß F. et al. (2014) e

11 HOW HADRONIC ARE BLAZARS?

12 HOW HADRONIC ARE BLAZARS? IceCube collaboration (2018) 6a

13 HOW HADRONIC ARE BLAZARS? Consistent with IceCube? 6b

14 WHAT IS THE HADRONIC CONTRIBUTION? 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] Krauß F. et al. (2014) 7a

15 WHAT IS THE HADRONIC CONTRIBUTION? 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] Krauß F. et al. (2014) 7b

16 WHAT IS THE HADRONIC CONTRIBUTION? 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] Krauß F. et al. (2014) 7c

17 HOW HADRONIC ARE BLAZARS? νfν [10 12 erg s 1 cm 2 ] ATCA BAT TANAMI WISE Ced Planck UVOT XRT Fermi/LAT 2FGL νlν [erg s 1 ] Consistent with IceCube? Frequency [Hz] Contribution to the high-energy spectrum 8a

18 HOW HADRONIC ARE BLAZARS? νfν [10 12 erg s 1 cm 2 ] ATCA BAT TANAMI WISE Ced Planck UVOT XRT Fermi/LAT 2FGL νlν [erg s 1 ] Consistent with IceCube? Frequency [Hz] Contribution to the high-energy spectrum SIMILAR FOR ALL SOURCES? 8b

19 SUMMARY What is the average percentage of hadronic emission? 4% Are all sources equally hadronic?? 9a

20 METHOD IceCube Collaboration (2013, 2013, 2014, 2015) 10a

21 METHOD 16 neutrinos IceCube Collaboration (2013, 2013, 2014, 2015) 10b

22 I DENTIFYING NEUTRINO SOURCES Unfeasible for most neutrinos Calculate neutrino emission for large number of sources 11a

23 PREVIOUS RESULTS Calorimetrically blazars can explain IceCube events Krauß et al. (2014) First coincidence of blazar outburst and neutrino: PKS and IC 35 Kadler, Krauß et al. (2016), Nature Physics (TXS and IC A) 12a

24 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 13a

25 NEUTRINOS > 100 TEV IC events R Galactic Plane h 46 8h 39 4h 0h h h 48 12h FGL sources Krauß et al. (2018) 14a

26 NEUTRINOS > 100 TEV ν Fν [erg s 1 cm 2 ] Swift/XRT Fermi/LAT PKS ν Lν [erg s 1 ] 179 χ Frequency [Hz] Krauß et al. (2018) 15a

27 NEUTRINOS > 100 TEV ν Fν [erg s 1 cm 2 ] Swift/XRT Fermi/LAT PKS ν Lν [erg s 1 ] 179 χ Frequency [Hz] N ν,all = cosmic neutrinos Kadler, Krauß F. et al., Nature Physics (2016) Krauß F. et al. (2018) 15b

28 NEUTRINOS > 100 TEV ν Fν [erg s 1 cm 2 ] Swift/XRT Fermi/LAT PKS ν Lν [erg s 1 ] 179 χ Frequency [Hz] N ν,all = cosmic neutrinos 4% of emission hadronic FIRST CONSTRAINT ON HADRONIC CONTRIBUTION TO SED 15c

29 MULTIWAVELENGTH MODELING OF TXS Leptonic model (Gao et al., 2018; Keivani et al., 2018) 16a

30 MULTIWAVELENGTH MODELING OF TXS Hadronic model (Gao et al., 2018; Keivani et al., 2018) 16b

31 CONCLUSION Blazars on average 4% hadronic No 5σ associations yet! Unclear whether different sources are less/more hadronic 17a

32 BACKUP 18a

33 ASSUMPTIONS OF NEUTRINO CALCULATION 1.) All of high-energy emission is of hadronic origin 2.) All of the neutrinos emitted at one energy (delta-peak) Calculated numbers are maximum possible 19a

34 NEUTRINOS > 100 TEV Fermi/LAT flux unreliable proxy of N ν Krauß et al. (2018) 20a

35 NEUTRINOS > 100 TEV Fermi/LAT flux unreliable proxy of N ν Krauß et al. (2018) 20b

36 ALL 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 21a

37 RESULTS FOR IC 35: VARIABILITY γ-ray flux F MeV [10 6 cm 2 s 1 ] MJD Kadler, Krauss et al. (2016), Nature Physics 22a

38 RESULTS FOR IC 35: VARIABILITY γ-ray flux F MeV [10 6 cm 2 s 1 ] MJD Kadler, Krauss et al. (2016), Nature Physics 22b

39 RESULTS FOR IC 35: VARIABILITY γ-ray flux F MeV [10 6 cm 2 s 1 ] MJD Kadler, Krauss et al. (2016), Nature Physics 22c

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 23a

41 CHANCE COINCIDENCE OF TXS Significance of association: pre-trial: 4.1σ post-trial: 3.0σ But: signalness 0.5 Expected neutrinos during flare: 1.19 (Kreter, Kadler, Krauss et al., in prep.) 24a

42 CHANCE COINCIDENCE OF TXS Joint probability: Null hypothesis: IC 35 & IC170922A are not from blazars p IC170922A/TXS = σ p IC35/PKS = σ p joint,fisher σ (Kadler, Krauss, Kreter et al., in prep.) Multiwavelength modeling & previous neutrino data 25a

43 NEUTRINOS BEFORE IC170922A log 10 p IC40 IC59 IC79 IC86a IC86b IC86c IceCube A Gaussian Analysis Box-shaped Analysis σ 3σ 2σ 1σ flare post-trial: 3.5σ IceCube (2018) 26a

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