https://kicp-workshops.uchicago.edu/uheap2016/ 1 Welcome to Chicago 2 Local Information Front door opening time 8:30 - 17:30 without keys. This room (ERC 401) is available during all three days. Please feel free to use. Wifi: uchicago-guest Username: ucguest_2758 We are Password: dk79t here. Please keep your belongings with you. Smoking is prohibited in the building. Warm jacket needed. 3 We are here. Lunch 4 We are here. Lunch Quantum Cafe 1st flour hutchinson commons (food court) Sky lobby food court 7th flour Please come back at 2 pm. 5 To Speakers HDMI/Thunderbolt connectors are available. 30 minutes slot: 25 minutes talk + 5 minutes discussion 15 minutes slot: 12 minutes talk + 3 minutes discussion Please copy your presentation in USB. We will upload your slide in workshop page. 6 In UHEAP 2016 workshop, Social networking, please say hello to all participants. Encourage an informal discussion in receptions. Discuss a roadmap of future prospects in this workshop in UHE Astroparticle physics, Next 5-10 years Next 10-20 years. 7 Physics Goal and Future Prospects Origin and Nature of Ultra-high Energy Cosmic Rays and Particle Interactions at the Highest Energies 5 - 10 years Exposure and Full Sky Coverage Detector R&D “Precision” Measurements TA×4 + Auger Radio, SiPM, AugerPrime Low energy enhancement JEM-EUSO : pioneer detection from Low-cost (Auger infill+HEAT+AMIGA, space and sizable increase of exposure Detectors TALE+TA-muon+NICHE) 10 - 20 years Next Generation Observatories In space (100×exposure): EUSO-Next Ground (10×exposure with high quality events): Giant Ground Array, FAST 419 The post-trial p-value is 28%. For the analysis done using the high-energy cascades 420 (Figure 6b), the smallest pre-trial p-value is obtained at an angular distance of 22◦, 421 for which 575 pairs are observed while 490.3 were expected on average. The post-trial 4 422 p-value is 5.0 10− assuming an isotropic flux of CRs. ⇥ 419 The post-trial p-value is 28%. For the analysis done using the high-energy cascades 420 (Figure 6b), the smallest pre-trial p-value is obtained at an angular distance of 22◦, 421 for which 575 pairs are observed while 490.3 were expected on average. The post-trial 4 IceCube, Auger, TA 422 p-value is 5.0 10− assuming an isotropic flux of CRs. ⇥ All Sky SurveyHotspot/Warmspot with TA&PAO Oversampling with 20°-radius circle No correction for Northern TA : 7 years 109 events (>57EeV) E scale difference Southern Auger : 10 years 157 events (>57EeV) b/w TA and PAO !! SouthernUHECR hotspot is seen oversampling at Cen A(Pre-trial ~3.6 σ) 12 Figure 7: Maps in Equatorial and Galactic coordinates showing the arrival directions of the IceCube with 20°-radius circle cascades (black dots) and tracks (diamonds), as well as those of the UHECRs detected by the Pierre Auger Observatory (magenta stars) and Telescope Array (orange stars). The circles around the showers indicate angular errors. The black diamonds are the HESE tracks while the blue diamonds stand for the tracks from the through-going muon sample. The blue curve indicates the Super-Galactic plane. http://arxiv.org/abs/1511.09408 9 18 Figure 7: Maps in Equatorial and Galactic coordinates showing the arrival directions of the IceCube cascades (black dots) and tracks (diamonds), as well as those of the UHECRs detected by the Pierre Auger Observatory (magenta stars) and Telescope Array (orange stars). The circles around the showers indicate angular errors. The black diamonds are the HESE tracks while the blue diamonds stand for the tracks from the through-going muon sample. The blue curve indicates the Super-Galactic plane. 18 Selected for a Viewpoint in Physics week ending PRL 116, 061102 (2016) PHYSICAL REVIEW LETTERS 12 FEBRUARY 2016 New Partner Observation of Gravitational Waves from a Binary Black Hole Merger 11 B. P. Abbott et al.* High-energy Neutrino follow-up search of Gravitational Wave Event (LIGO Scientific Collaboration and Virgo Collaboration) GW150914 with ANTARES and IceCube (Received 21 January 2016; published 11 February 2016) 1 2 3 4 1 5 6 p-value6 1 Fpois(Nobserved 2,Nexpected =4.4) = 0.81, On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave S. Adri´an-Mart´ınez, A. Albert, M. Andr´e, G. Anton, M. Ardid, J.-J. Aubert, T. Avgitas, B. Baret, 7 8 5 9 10, 11 10 10, 12 5 − Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwardsJ. in Barrios-Mart´ı, S. Basa, V. Bertin, S. Biagi, R. Bormuth, M.C. Bouwhuis, R. Bruijn, J.where Brunner, Fpois is the Poisson cumulative distribution func- 5 13, 14 15 5 13, 14 16 17 6 frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0 × 10−21. It matches the waveform J. Busto, A. Capone, L. Caramete, J. Carr, S. Celli, T. Chiarusi, M. Circella, A. Coleiro,tion. Second, for the most significant reconstructed muon predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the R. Coniglione,9 H. Costantini,5 P. Coyle,5 A. Creusot,6 A. Deschamps,18 G. De Bonis,13, 14 C. Distefano,9 PHYSICAL REVIEW LETTERS week ending 6, 19 5 2 4 20 21 4 PRL 116,resulting061102 single (2016) black hole. The signal was observed with a matched-filter signal-to-noise ratio12 of FEBRUARY 24 and a 2016C. Donzaud, D. Dornic, D. Drouhin, T. Eberl, I. El Bojaddaini, D. Els¨asser, A. Enzenh¨ofer,energy (Table I), 12.5% of background events will have false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater K. Fehn,4 I. Felis,22 L.A. Fusco,23, 16 S. Galat`a,6 P. Gay,24, 25 S. Geißels¨oder,4 K. Geyer,4 V. Giordano,greater26 muon energy. The probability that at least one propertiesthan of5.1 space-timeσ. The source in the lies strong-field, at a luminosity high-velocity distance of 410the160 coincidentMpc corresponding signal GW150914 to a redshift shownz in Fig.0.091.0 The.03. initial 4 27, 28 6 4 4 29 10 −þ180 −þ0.04 A. Gleixner, H. Glotin, R. Gracia-Ruiz, K. Graf, S. Hallmann, H. van Haren, A.J. Heijboer, regime and confirm predictions of general relativity for the detection5 was4 made by low-latency searches¼ for generic In the source frame, the initial black hole masses are 36þ M and 29þ M , and the final black hole mass is 18 7 4 4 30, 31 13, 14 neutrino4 candidate, out of 3 detected events, has an en- nonlinear dynamics of highly disturbed black holes. −gravitational-wave4 −4 transients [41] and was reported withinY. Hello, J.J. Hern´andez-Rey, J. H¨oßl, J. Hofest¨adt, C. Hugon, G. Illuminati, C.W James, 4 0.5 2 ⊙ ⊙ 62−þ4 M , with 3.0−þ0.5 M c radiated in gravitational waves.three All minutes uncertainties of data define acquisition 90% credible[43]. intervals. Subsequently, 10, 11 21 4 4 4 6, 28 21 ⊙ ⊙ M. de Jong, M. Kadler, O. Kalekin, U. Katz, D. Kießling, A. Kouchner, M. Kreter,ergy high enough to make it appear even less background- These observations demonstrate the existence of binary stellar-massmatched-filter black analyses hole systems. that use This relativistic is the first models direct of com- II. OBSERVATION I. Kreykenbohm,32 V. Kulikovskiy,9, 33 C. Lachaud,6 R. Lahmann,4 D. Lef`evre,34 E. Leonora,26, 35 S. Loucatos,36, 6 3 detection of gravitational waves and the first observationpact of binary a binary waveforms black hole[44] merger.recovered GW150914 as the 8 23, 16 37, 38 1 5 10 like, is39 1 (1 0.125) 0.33. Third, with the GW sky On September 14, 2015 at 09:50:45 UTC, the LIGO most significant event from each detector for theM. observa- Marcelin, A. Margiotta, A. Marinelli, J.A. Mart´ınez-Mora, A. Mathieu, T. Michael, P. Migliozzi, − − ⇡ 2 Hanford,DOI: WA,10.1103/PhysRevLett.116.061102 and Livingston, LA, observatories detected tions reported here. Occurring within the 10-msA. intersite Moussa,20 C. Mueller,21 E. Nezri,8 G.E. P˘av˘ala¸s,15 C. Pellegrino,23, 16 C. Perrina,13, 14 P. Piattelli,9 V.area Popa,15 90% CL of ⌦gw = 590 deg , the probability of a T. Pradier,40 C. Racca,2 G. Riccobene,9 K. Roensch,4 M. Salda˜na,1 D. F. E. Samtleben,10, 11 M. Sanguineti,background30, 31 neutrino candidate being directionally coin- P. Sapienza,9 J. Schnabel,4 F. Sch¨ussler,36 T. Seitz,4 C. Sieger,4 M. Spurio,23, 16 Th. Stolarczyk,36 I. INTRODUCTION The discovery of the binary pulsar system PSRA. B1913 S´anchez-Losa,16 7, 41 M. Taiuti,30, 31 A. Trovato,9 M. Tselengidou,4 D. Turpin,5 C. T¨onnis,7 B. Vallage,cident36, 25 is ⌦gw/⌦all 0.014. We expect 3⌦gw/⌦all di- by Hulse and Taylor [20] and subsequent observationsþ of In 1916, the year after the final formulation of the field C. Vall´ee,5 V. Van Elewyck,6 D. Vivolo,39, 42 S. Wagner,4 J. Wilms,32 J.D. Zornoza,7 and J. Z´u˜niga7 ⇡ its energy loss by Taylor and Weisberg [21] demonstrated rectionally coincident neutrinos, given 3 temporal coinci- equations of general relativity, Albert Einstein predicted (The Antares Collaboration) the existence of gravitational waves.