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 , 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 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 , given 3 temporal coinci- equations of general relativity, Albert Einstein predicted (The Antares Collaboration) the existence of gravitational waves. He found that the existence of gravitational waves. This discovery,FIG. 1. GW skymap in equatorial coordinates, showing dences. Therefore, the probability that at least one of the the linearized weak-field equations had wave solutions: along with emerging astrophysical understanding [22], the44 reconstructed75 probability92 density58 contours of54 the GW72 3 neutrino82 candidates is directionally coincident with the transverse waves of spatial strain that travel at the speed of led to the recognition that direct observationsM. G. of Aartsen, the K. Abraham, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, 66 88 54 66 73 56 88 3 light, generated by time variations of the mass quadrupole amplitude and phase of gravitational waves wouldD. enable Altmann,eventT. at Anderson, 50%, 90%I. Ansseau, and 99%G. Anton, CL, andM. Archinger, the reconstructedC. Arguelles, di-T. C. Arlen,90% CL skymap of GW150914 is 1 (1 0.014) 0.04. moment of the source [1,2].Einsteinunderstoodthat studies of additional relativistic systems and provideJ. Au new↵enberg,rections43 X. of Bai, high-energy80 S. W. Barwick, neutrino69 V. Baum, candidates73 R. Bay,49 J. detected J. Beatty,60, by 61 J. Ice- Becker Tjus,52 ⇡ gravitational-wave amplitudes would be remarkably tests of general relativity, especially in theK.-H. dynamic Becker,91 E. Beiser,72 S. BenZvi,89 P. Berghaus,92 D. Berley,59 E. Bernardini,92 A. Bernhard,75 strong-field regime. Cube (crosses) during a 500s time window around the GW small; moreover, until the Chapel Hill conference in D. Z. Besson,70 G. Binder,50, 49 D. Bindig,91 M. Bissok,43 E. Blaufuss,59 J. Blumenthal,43 D. J. Boersma,90 Experiments to detect gravitational waves began with ± 1957 there was significant debate about the physical 82 event. The63 neutrino52 directional84 uncertainties73 90 are <721 and are55 92 Weber and his resonant mass detectors in theC. 1960s Bohm,[23],M. B¨orner, F. Bos, D. Bose, S. B¨oser, O. Botner, J. Braun, L. Brayeur, H.-P. Bretz, B. Constraints on the source reality of gravitational waves [3]. N. Buzinsky,not65 shown.J. Casey,47 GWM. Casier, shading55 E. Cheung, indicates59 D. theChirkin, reconstructed72 A. Christov,67 probabil-K. Clark,85 L. Classen,66 Also in 1916, Schwarzschild published a solution for the followed by an international network of cryogenic reso- nant detectors [24]. Interferometric detectorsS. Coenders, were first75ityG. H. density Collin,56 ofJ. M. the Conrad, GW56 event,D. F. Cowen, darker88, 87 regionsA. H. Cruz corresponding Silva,92 J. Daughhetee, to 47 J. C. Davis,60 field equations [4] that was later understood to describe a 72 64 55 73 76 68 black hole [5,6], and in 1963 Kerr generalized the solution suggested in the early 1960s [25] and the 1970sM. Day,[26].AJ. P. A. M. de Andr´e, C. De Clercq, E. del Pino Rosendo, H. Dembinski, S. De Ridder, 72 higher probability.55 Neutrino55 numbers51 refer to64 the first column72 We73 used the non-detection of coincident neutrino can- to rotating black holes [7]. Starting in the 1970s theoretical study of the noise and performance of suchP. detectors Desiati,[27]K., D. de Vries, G. de Wasseige, M. de With, T. DeYoung, J. C. D´ıaz-V´elez, V. di Lorenzo, work led to the understanding of black hole quasinormal and further concepts to improve them [28]H.,ledto Dujmovic,of Table84 J. P. Dumm,I. 82 M. Dunkman,88 B. Eberhardt,73 T. Ehrhardt,73 B. Eichmann,52 S. Euler,didates90 by Antares and IceCube to derive a stan- proposals for long-baseline broadband laser interferome- modes [8–10], and in the 1990s higher-order post- P. A. Evenson,76 S. Fahey,72 A. R. Fazely,48 J. Feintzeig,72 J. Felde,59 K. Filimonov,49 C. Finley,82 S. Flis,82 ters with the potential for significantly increased sensi- https://www.ligo.caltech.edu/page/detection-companion-papers dard frequentist neutrino spectral fluence upper limit for Newtonian calculations [11] preceded extensive analytical C.-C. F¨osig,73 T. Fuchs,63 T. K. Gaisser,76 R. Gaior,57 J. Gallagher,71 L. Gerhardt,50, 49 K. Ghorbani,1072 D. Gier,43 tivity [29–32]. By the early 2000s, a set of initial detectors studies of relativistic two-body dynamics [12,13]. These L. Gladstone,72 M. Glagla,43 T. Gl¨usenkamp,92 A. Goldschmidt,50 G. Golup,55 J. G. Gonzalez,76 D. G´ora,GW15091492 at 90% CL. Considering no spatially and tem- advances, together with numerical relativity breakthroughs was completed, including TAMA 300 in Japan, GEO 600 in Germany, the Laser Interferometer Gravitational-WaveD. Grant,65sourceZ. Grith, directional72 C. Ha,50, 49 distributionC. Haack,43 A. Haj is Ismail, uniform.68 A. Hallgren, For90 temporalF. Halzen,72 E. Hansen,porally62 coincident neutrino candidates, we calculated the in the past decade [14–16], have enabled modeling of 43 43 72 51 54 91 59 binary black hole mergers and accurate predictions of Observatory (LIGO) in the United States, andB. VirgoHansmann, in T. Hansmann, K. Hanson, D. Hebecker, D. Heereman, K. Helbing, R. Hellauer, coincidence,91 64 we searched44 within59 a 500 s91 time window75 source53 fluence that on average would produce 2.3 de- their gravitational waveforms. While numerous black hole Italy. Combinations of these detectors made jointS. Hickford, obser- J. Hignight, G. C. Hill, K. D. Ho↵man, R.± Ho↵mann, K. Holzapfel, A. Homeier, vations from 2002 through 2011, setting upper limits on a72, 88 75 59 82 82 84 57 candidates have now been identified through electromag- K. Hoshina,around⇤ F. Huang, GW150914.M. Huber, W. Huelsnitz, P. O. Hulth, K. Hultqvist, S. In, A. Ishihara,tected neutrino candidates. We carried out this analysis variety of gravitational-wave sources while evolving into netic observations [17–19], black hole mergers have not E. Jacobi,92 G.The S. Japaridze, relative46 M. di Jeong,↵erence84 K. Jero, in72 propagationB. J. P. Jones,56 M. time Jurkovic, for75 A.GeV Kappes,66 T.as Karg, a92 function of source direction, and independently for previously been observed. a global network. In 2015, Advanced LIGO became the72 66 72, 77 88 72 43 72 84 first of a significantly more sensitive networkA. of advanced Karle, U. Katz, M. Kauer, A. Keivani, J. L. Kelley, J. Kemp, A. Kheirandish, M. Kim, 92neutrinos83 and GWs50, 49 (which travel74 at the76 speed of51 light in 43 Antares73 and IceCube. detectors to begin observations [33–36].T. Kintscher, J. Kiryluk, S. R. Klein, G. Kohnen, R. Koirala, H. Kolanoski, R. Konietz, L. K¨opke, *Full authorFIG. 1. list The given gravitational-wave at the end of eventthe article. GW150914 observed by the LIGOA Hanford century (H1, after left column the fundamental panels) and Livingston predictions (L1,C. Kopper, rightof Einstein65GeneralS. Kopper,91 Relativity)D. J. Koskinen, traveling62 M. Kowalski, to51, Earth 92 K. Krings, from75 G. the Kroll, source73 M. Kroll, is 52 G. Kr¨uckl,The73 obtained spectral fluence upper limits as a func- column panels) detectors. Times are shown relative to September 14, 2015and at Schwarzschild, 09:50:45 UTC. For visualization,we report the all time first series direct areJ. filtered detection Kunnen, of55 S. Kunwar,92 N. Kurahashi,79 T. Kuwabara,57 M. Labare,68 J. L. Lanfranchi,88 M. J. Larson,62 Publishedwith by a 35 the–350 American Hz bandpass Physical filter Societyto suppress under large the fluctuations terms of outside the detectors’ most sensitive frequency band, and band-reject tion of source direction are shown in Fig. 2.We gravitational waves and the first direct observation of aexpected64 to be 83 1 s. We note43 that43 the relative57 propa-55 81 the Creativefilters to Commons remove the Attribution strong instrumental 3.0 License spectral. Further lines seen distri- in the Fig. 3 spectra. Top row, left: H1 strain. Top row, right: L1 strain.D. Lennarz, M. Lesiak-Bzdak, M. Leuermann, J. Leuner, L. Lu, J. L¨unemann, J. Madsen, 2 0.5 binary black hole system merging to form a single black 55 64 ⌧ 52 77 57 50 59 bution ofGW150914 this work arrived must maintain first at L1 attribution and 6.9−þ0.4 toms the later author(s) at H1; for and a visual comparison, the H1 data are also shown, shifted in time byG. this Maggi,gationK. B. M. time Mahn, betweenM. Mandelartz, neutrinosR. Maruyama, and GWsK. Mase, mayH. change S. Matis, inR. Maunu,consider a standard dN/dE E source model, as amount and inverted (to account for the detectors’ relative orientations). Second row: Gravitational-wave strain projected onto each the published article’s title, journal citation, and DOI. hole. Our observations provide unique accessF. McNally, to the 72 K. Meagher,54 M. Medici,62 M. Meier,63 A. Meli,68 T. Menne,63 G. Merino,72 T. Meures,54 / detector in the 35–350 Hz band. Solid lines show a numerical relativity waveform for a system with parameters consistent with those alternative gravity models [47, 48]. However, discrepan- well as a model with a spectral cuto↵ at high energies: recovered from GW150914 [37,38] confirmed to 99.9% by an independent calculation based on [15]. Shaded areas show 90% credibleS. Miarecki,50, 49 E. Middell,92 L. Mohrmann,92 T. Montaruli,67 R. Morse,72 R. Nahnhauer,92 U. Naumann,91 2 0031-9007regions=16 for=116(6) two independent=061102(16) waveform reconstructions. One (dark 061102-1 gray) models the signal Published using binary by black the Americanhole template Physical waveforms Societycies64 from General83 Relativity65 could in50 principle be probed91 dN/dE59 E exp[ (E/100TeV)]. For each spectral [39]. The other (light gray) does not use an astrophysical model, but instead calculates the strain signal as a linear combinationG. of Neer, H. Niederhausen, S. C. Nowicki, D. R. Nygren, A. Obertacke Pollmann, A. Olivas, 91 54 86 76 88 43 86 / sine-Gaussian wavelets [40,41]. These reconstructions have a 94% overlap, as shown in [39]. Third row: Residuals after subtractingA. the Omairat,withA. O’Murchadha, a joint GW-neutrinoT. Palczewski, detectionH. Pandya, byD. V. comparing Pankova, L. the Paul, ar-J. A. Pepper,model, the upper limit shown in each direction of the sky filtered numerical relativity waveform from the filtered detector time series. Bottom row:A time-frequency representation [42]C.of P´erez the de los Heros,90 C. Pfendner,60 D. Pieloth,63 E. Pinat,54 J. Posselt,91 P. B. Price,49 G. T. Przybylski,50 p strain data, showing the signal frequency increasing over time. is the more stringent limit provided by one or the other M. Quinnan,rival88 C. times Raab,54 L. against R¨adel,43 M. the Rameez, expected67 K. Rawlins, time45 frameR. Reimann, of43 emission.M. Relich,57 E. Resconi,75 W. Rhode,63 Directionally,M. Richman,79 S. Richter, we searched72 B. Riedel,65 forS. overlapRobertson,44 betweenM. Rongen, the43 C. GW Rott,84 T. Ruhe,detector.63 We see in Fig. 2 that the constraint strongly 061102-2 sky map and the neutrino point spread functions, as- depends on the source direction, and is mostly within 2 1 1 2 rec E dN/dE 10 10 GeV cm . Furthermore, the sumed to be Gaussian with standard deviation µ (see ⇠ Table I). upper limits by Antares and IceCube constrain di↵er- The search identified no Antares neutrino candidate ent energy ranges in the region of the sky close to the GW 2 that were temporally coincident with GW150914. candidate. For an E power-law source spectrum, 90% For IceCube, none of the three neutrino candidates of Antares signal neutrinos are in the energy range from temporally coincident with GW150914 were compatible 3 TeV to 1 PeV, whereas for IceCube at this southern with the GW direction at 90% CL. Additionally, the re- declination the corresponding energy range is 200 TeV to constructed energy of the neutrino candidates with re- 100 PeV. spect to the expected background does not make them We now convert our fluence upper limit into a con- significant. See Fig. 1 for the directional relation of straint on the total energy emitted in neutrinos by the GW150914 and the IceCube neutrino candidates de- source. To obtain this constraint, we integrate emission within [100 GeV, 100 PeV] for the standard dN/dE tected within the 500 s window. This non-detection is 2 / consistent with our± expectation from a binary black hole E source model, and within [100 GeV, 100 TeV] assum- merger. ing neutrino emission with a cuto↵ at 100 TeV. We find non-detection to correspond to the following upper limit To better understand the probability that the de- on the total energy radiated in neutrinos: tected neutrino candidates are being consistent with background, we briefly consider di↵erent aspects of the 2 ul 52 54 Dgw data separately. First, the number of detected neutrino E 10 –10 erg (1) ⌫,tot ⇠ 410 Mpc candidates, i.e. 3 and 0 for IceCube and Antares,re- ✓ ◆ spectively, is fully consistent with the expected back- Note that the wide allowed range is primarily due to the ground rate of 4.4 and 1 for the two detectors, with large directional uncertainty of the GW event. For com- ⌧ Next-Generation Techniques for UHE Astroparticle Physics February 29 - March 2, 2016 @ Chicago, IL WORKSHOP PROGRAMEnjoy UHEAP 2016 workshop Next-Generation Techniques for UHE Astroparticle Physics February 29 - March 2, 2016 @ Chicago,Next-Generation IL Techniques for UHE Astroparticle Physics February 29 - March 2, 2016 @ Chicago, IL

Monday - February 29, 2016 Tuesday - March 1, 2016 Wednesday - March 2, 2016

10:00 AM - 10:10 AM Welcome Address 9:00 AM - 9:30 AM Morning Coffee 9:00 AM - 9:30 AM Morning Coffee James Cronin, Toshihiro Fujii 9:30 AM - 12:15 PM SESSION 3 9:30 AM - 12:30 PM SESSION 5 10:10 AM - 10:15 AM Toshihiro Fujii, Chair : Paolo Privitera Chair: Dan Hooper, Cosmin Deaconu Workshop Information 9:30 AM - 10:00 AM Foteini Oikonomou, Penn State 9:30 AM - 10:00 AM Stijn Buitink, Vrije Universiteit Brussel (VUB) UHECRs and Neutrinos: Expectations for the next 20 years 10:15 AM - 12:00 PM SESSION 1 Radio detection of air showers with LOPES and LOFAR Chair: Eric Oberla 10:00 AM - 10:30 AM Andrew M Taylor, DIAS 10:00 AM - 10:30 AM Radomir Smida, KIT Extragalactic Cosmic Rays in the Knee to Ankle Region 10:15 AM - 10:45 AM Claudio Kopper, University of Alberta Radio and microwave detection of extensive air showers at the Pierre Auger Observatory Recent Results from IceCube 10:30 AM - 10:45 AM Break 10:30 AM - 11:00 AM Daisuke Ikeda, Institute for Cosmic Ray Research, University of Tokyo 10:45 AM - 11:15 AM Mariangela Settimo, LPNHE-CNRS Radio detection for the ultra-high energy cosmic rays 10:45 AM - 11:15 AM Mauricio Bustamante, Center for and AstroParticle Physics, The Ohio State Recent Results from the Pierre Auger Observatory University 11:00 AM - 11:15 AM Break Flavor composition of high-energy astrophysical neutrinos: present and future 11:15 AM - 11:45 AM Yuichiro Tameda, Kanagawa University Recent Results from the Telescope Array Experiment 11:15 AM - 11:45 AM Pavel Motloch, KICP, U Chicago 11:15 AM - 11:45 AM Markus Ahlers, UW-Madison & WIPAC Multi-Messenger Aspects of Cosmic Neutrinos Properties of transition radiation induced by particle showers 11:45 AM - 12:00 AM Piotr Homola, Institute of Nuclear Physics, Polish Academy of Sciences, Krakow Brainstorming on a distributed, open and diversified cosmic ray detector 11:45 AM - 12:00 PM Closing Remark 11:45 AM - 12:15 PM Kael D Hanson, University of Wisconsin - Madison (WIPAC) Toshihiro Fujii IceCube Gen2: The Next Generation Neutrino Observatory 12:00 PM - 2:00 PM Lunch 12:15 PM - 2:00 PM Lunch 2:00 PM - 5:15 PM SESSION 2 Chair: Angela Olinto 2:00 PM - 5:15 PM SESSION 4 Chair: 2:00 PM - 2:30 PM Marco Casolino, RIKEN and INFN Perspectives and techniques of UHECR observation from space with EUSO detectors 2:00 PM - 2:30 PM Jordan C Hanson, The A review of UHE neutrino detection using the Askaryan Effect 2:30 PM - 3:00 PM Nonaka Toshiyuki, Institute for Cosmic Ray Research , University of Tokyo Surface detector for TAx4 expansion and status of Muon measurement at TA site. 2:30 PM - 3:00 PM Ryan Nichol, UCL ANITA: Current status and future prospects 3:00 PM - 3:15 PM Radomir Smida, KIT AugerPrime - Primary cosmic ray identification for the next 10 years 3:00 PM - 3:30 PM Thomas Meures, UW-Madison The - status and future plans 3:15 PM - 3:30 PM Sean Quinn, Case Western Reserve Univ. Auger@TA: current progress and future plans 3:30 PM - 3:45 PM Break

3:30 PM - 3:45 PM Break 3:45 PM - 4:15 PM Ke Fang, University of Maryland The Giant Radio Array for Neutrino Detection: Present and Perspectives 3:45 PM - 4:15 PM Lenka Tomankova, Karlsruhe Institute of Technology (KIT) Studying telescope properties using an airborne light source 4:15 PM - 4:45 PM Carl G Pfendner, Ohio State University The ExaVolt Antenna: Concept and Development Updates 4:15 PM - 4:45 PM Thomas Bretz, RWTH Aachen University If you have questions, SiPMs for AugerPrime and IceCube Gen2 4:45 PM - 5:15 PM Stephanie Wissel, Cal Poly SLO Implications for Radio Detection of Cosmic Rays from Accelerator Measurements of please feel free to ask us. Next-Generation4:45 PM - 5:15 Techniques PM forToshihiro UHE Astroparticle Fujii, University Physics of Chicago February 29 - March 2, 2016 @ Chicago, IL Particle Showers in a Magnetic Field Next-Generation Observatory: Fluorescence detector Array of Single-pixel Telescopes Cosmin Deaconu, Toshihiro Fujii, Dan Hooper, 5:15 PM - 7:00 PM Informal Discussion & Reception 5:15 PM - 7:00 PM Welcome Reception Eric Oberla, Angela Olinto, Paolo Privitera, Workshop Program http://kicp-workshops.uchicago.edu/uheap2016/ Workshop Program http://kicp-workshops.uchicago.edu/uheap2016/ 4 of 4 1 of 4 Abigail Vieregg 11 Workshop Program http://kicp-workshops.uchicago.edu/uheap2016/ 3 of 4

Workshop Program http://kicp-workshops.uchicago.edu/uheap2016/ 2 of 4