Ricap18 7th Roma International Conference on Astroparticle Physics

4 Sept 2018, 17:30 → 7 Sept 2018, 20:00 Europe/Rome

Roma Tre University

Mario De Vincenzi (ROMA3)

RICAP-18 will be the seventh edition of the RICAP Conference. The Conference, entirely dedicated to the study of high-energy cosmic rays, has been traditionally organized by the INFN sections and Physics Departments of the three public Universities of Roma (University “La Sapienza”, University Roma “Tor Vergata” and University “Roma Tre”). The 2018 edition will be host by the Department of Mathematics and Physics of the "Roma Tre" University.

Slides

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Tuesday, 4 September

18:00 → 20:00 Welcome and Registration

Wednesday, 5 September

08:30 → 09:00 Registration

09:00 → 11:10 Multimessenger search for HE CR souces

Convener: Mario De Vincenzi (ROMA3)

09:00 Greetings from local authorities

09:10 Neutrino sources in light of recent IceCube results

The field of neutrino astronomy is undergoing a rapid evolution. After the discovery of a diffuse flux of astrophysical TeV-PeV neutrinos in 2013, the IceCube observatory has recently found first evidence for neutrino emission of blazars that undergo an episode of enhanced electro-magnetic emission. I will summarize these recent neutrino observations, highlight their relations to cosmic rays and gamma rays, and discuss candidate sources of the diffuse neutrino emission.

Speaker: Markus Ahlers (Niels Bohr Institute)

Slides Ahlers_RICAP2018.pdf

09:40 10 years of Fermi-LAT successes and recent results

The Fermi Gamma-ray Space Telescope was launched 10 years ago, and since then it has observed the sky mainly in survey mode. In these years the main instrument on board, the Large Area telescope (LAT), has provided unprecedented results on Galactic and extragalactic science. Last year, the LAT collaboration released a catalog of sources detected at energies above 10 GeV, and many follow-up studies have been published. In the near future a new list based on 8 years of data above 100 MeV will be released, which is expected to contain more than 5000 sources. Among them, about a third remain unassociated, meaning that there is not a known counterpart at other energies. What are these gamma-ray sources? I will present a more in-depth look at them discussing their gamma-ray properties and possible interpretations. In this talk I will also show the huge mine of information contained in catalogs and concentrate on the extragalactic sources such as Active Galactic Nuclei reviewing the main recent results.

Speaker: Elisabetta Cavazzuti (T)

Slides RICAP_Cavazzuti.pdf

10:10 AGILE status and results

The gamma-ray satellite AGILE is dedicated to the observation of astrophysical sources of photons in the 30 MeV - 30 GeV energy range. The satellite launched in April 2007 has completed its 11th year of operations, and continues its mission with high efficiency. In this talk, we will review the main AGILE scientific results and the perspectives for the future search of counterparts to gravitational waves and neutrinos.

Speaker: Francesco Verrecchia (ASI Science Data Center)

Slides RICAP2018_AGILE_v3.pdf

10:40 INTEGRAL highlights and perspectives for GW counterparts search

The INTernational Gamma-ray Astrophysical Observatory is providing outstanding science data to the whole international scientific community since its injection in orbit. INTEGRAL has been observing the gamma-ray sky since October 2002, discovering 1000+ high-energy sources, pioneering γ-ray polarization, detecting radioactivity from extragalactic supernovae, and shedding new light on the enigmatic positron annihilation in the Galactic Centre Region, with its putative link to light dark matter. With its 870 kg of detectors and shield scintillators, the observatory is virtually omnidirectional, and thanks to the highly elliptical orbit, the entire sky is accessible with a duty cycle of 90%. Between the positive detection of GW170817, and the upper limits established for the BH merger events (invariably the most stringent upper limits for electromagnetic counterparts), INTEGRAL was able to observe the extended source regions of all but one GW event (six out of seven as of today). We will finally summarize the scientific perspectives of the INTEGRAL observations during the LVC O3.

Speaker: Pietro Ubertini (ROMA2)

Slides PU_INTEGRAL_RICAP2018_v4-sep-2018r.pdf

11:10 → 11:40 coffee break

11:40 → 13:10 Recent results for HE CR and Gamma

Convener: Aldo Morselli (ROMA2)

11:40 Ultra High Energy Cosmic Rays: Origin, Composition and Spectrum.

We will review the physics of Ultra High Energy Cosmic Rays, discussing the latest experimental results and theoretical models aiming at explaining the observations in terms of spectra, mass composition and possible sources.

Speaker: Roberto Aloisio (Gran Sasso Science Institute)

Slides Aloisio-RICAP.pdf

12:10 Results from the Pierre Auger Observatory

The status of the observation of Ultrahigh-Energy cosmic rays by the Pierre Auger Observatory will be reported. The resulting spectrum, composition and anisotropies provide important constraints for the origin of these particles. The recent dipole detection suggest that above the ankle CRs are predominantly of extragalactic origin. Searches of anisotropies on smaller angular scales have been performed at the highest energies. The trends towards heavier composition for increasing energies together with the observed suppression in the spectrum at the highest energies can help to discriminate between scenarios with a maximum rigidity at the sources and those in which the suppression is just a propagation effect. Upper bounds on photon and neutrino fluxes have been set.

Speaker: Prof. Esteban Roulet (Centro Atómico Bariloche)

Slides Roulet_rome18r.pdf

12:40 Cosmic Ray PeVatrons: young stars versus dead stars

The identification of major contributors to the locally observed Cosmic Rays would be a decisive step towards the understanding of the origin of Galactic CRs. The gamma-ray observations have revealed two major classes of CR factories in our Galaxy - Supernova Remnants (SNRs) and the Young Stellar Clusters (YSCs). In the context of the available energetics and the acceleration efficiency, both populations can support the production rate of CRs. The same is true for the speeds of outflows (stellar winds and SNR shocks) of several thousand km/s, which is a critical condition for effective utilization of the diffusive shock acceleration mechanism in the PeVatron regime. We argue that the recent gamma-ray observations give preference to YSCs compared to SNRs as long as it concerns the multi-TeV to PeV domain.

Speaker: Prof. Felix Aharonian (DIAS & MPIK)

Slides RICAP-Aharonian_r.pdf

13:10 → 14:10 Lunch

14:10 → 16:10 CR: 1

Convener: Roberta Sparvoli (ROMA2)

14:10 The PAMELA mission: results after ten years in space

For nearly ten years, from 2006 to 2016, PAMELA (a Payload for Antimatter-Matter Exploration and Light-nuclei Astrophysics) has been making high-precision measurements of the charged component of the cosmic radiation opening a new era of precision studies in cosmic-ray physics. The measured antiparticle component of the cosmic radiation shows features that can be interpreted in terms of dark matter annihilation or pulsar contribution. The measurements of the energy spectra of protons, electrons, helium and light nuclei challenges our basic vision of the mechanisms of production, acceleration and propagation of cosmic rays in the galaxy. The study of the time dependence of the various components of the cosmic radiations clearly shows solar modulation effects as well as charge sign dependence. PAMELA measurement of the energy spectra during solar energetic particle events fills the existing energy gap between the highest energy particles measured in space and the ground-based domain. Finally, by sampling the particle radiation in different regions of the magnetosphere, PAMELA data provide a detailed study of this structure surrounding the Earth. In this talk I will review the PAMELA experiment and its scientific results.

Speaker: Matteo Martucci (ROMA2)

Slides RICAP18_PAMELA.pdf

14:30 Solar modulation of the helium nuclei during the period from 2006 to 2014 with the PAMELA space experiment

Precision measurements of the Z = 2 component in the cosmic radiation provide crucial information about the origin and propagation of the second most abundant hadronic species in cosmic rays inside the Galaxy. Moreover, the solar modulation of light-nuclei like helium can be compared to the widely studied modulation of protons, to spot possible dependencies on charge and mass; such nuclei undergo different processes with respect to Z = 1 particles and this could be reflected on a difference in propagation parameters. The helium nuclei spectra measured by PAMELA down to 80 MeV from July 2006 to September 2014 over a three-months time basis are hereby presented, offering a detailed insight of Z = 2 particles behavior in both solar cycle 23rd and 24th.

Speaker: Nadir Marcelli (ROMA2)

14:50 New solar modulation modeling of the galactic proton measured by the AMS02 and PAMELA experiments

The flux of Galactic Cosmic Rays near Earth is not representative of the Local Interstellar Spectrum at energies below ~30 GeV due to a variety of physical processes arising in their propagation through the heliosphere. The changes in the GCR intensities and energy spectra are related to the solar activity, and are referred to as CR solar modulation. A thorough understanding of solar effects on the GCR is therefore relevant both to infer the LIS spectrum characteristics and to investigate the dynamics of charged particles in the heliosphere. We present a newly developed numerical modulation model to study the transport of galactic protons in the heliosphere. The model makes use of the stochastic differential equations approach to solve the Parker’s transport equation in four dimensions (time, energy, and two spatial dimensions) with realistic models of heliospheric magnetic field and solar wind and up-to-dated LIS flux. The model was applied to the 27-day averaged galactic proton flux recently released by the PAMELA and AMS02 experiments, covering overall an extended time period from mid-2006 to mid-2017. The time evolution of the model parameters and their relationship with solar activity proxies is shown. As we will discuss, our data-driven approach, based on the availability of new precision measurements, leads to new insights on the solar modulation phenomena

Speaker: Emanuele Fiandrini (PG)

15:10 Observation of the Energy Dependence of Primary and Secondary Cosmic Rays with the AMS Detector on the International Space Station

Precision study of cosmic nuclei provides detailed knowledge on the origin and propagation of cosmic rays. AMS is a multi-purpose high energy particle detector designed to measure and identify cosmic ray nuclei with unprecedented precision. It is able to provide precision studies of nuclei simultaneously to multi-TeV energies. In 7 years on the Space Station, AMS has collected more than 120 billion both primary and secondary cosmic rays. Primary cosmic rays, such as p, He, C and O, are believed to be mainly produced and accelerated in supernova remnants, while secondary cosmic rays, such as Li, Be and B are thought to be produced by collisions of heavier nuclei with interstellar matter. Primary cosmic rays such as He, C, and O are found to have identical rigidity dependence, similarly to secondary cosmic rays (such as Li, Be and B) which share the same the same spectral shape. The peculiar case of Nitrogen being a mixture of a primary and secondary component will also be shown.

Speaker: Valerio Formato (PG)

Slides AMS-RICAP-VFormato.pdf

15:30 Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

The fluxes and flux ratios of charged elementary particles in cosmic rays are presented in the absolute rigidity range from 1 to 1000 GV. In the absolute rigidity range ∼60 to ∼500 GV, the antiproton, proton, and positron fluxes are found to have nearly identical rigidity dependence and the electron flux exhibits different rigidity dependence. Below 60 GV, the antiproton-to-proton, antiproton-to-positron, and proton-to-positron flux ratios each reaches a maximum. Particular emphasis is made on new observations of the properties of elementary particles in the rigidity range above 500 GV.

Speaker: Francesco Nozzoli (TIFP)

Slides 2018-09-05Nozzoli-RICAP_web.pdf

15:50 Precision Measurement of the Monthly Cosmic Ray Fluxes with the Alpha Magnetic Spectrometer on the ISS

The precision measurements of the monthly cosmic ray fluxes with Alpha Magnetic Spectrometer on the International Space Station are presented. Individual electron, positron, proton and helium spectra have been measured for each Bartel's rotation period (27 days) in the time range from May 2011 to May 2017. This period covers the ascending phase of solar cycle # 24 together with the reversal of the Sun's magnetic field polarity through the minimum. The fluxes reveal a characteristic time dependence below 20 GeV. The data show a strong charge-sign dependent effects corresponding with the polarity reversal of the solar magnetic field.

Speaker: maura graziani (KIT, Karlsruher Institut für Technologie)

Slides presentazione_maura_RICAP2018_finale_vero.pdf

14:10 → 16:10 Neutrinos

Convener: Dr Juan de Dios Zornoza (IFIC)

14:10 AGILE Gamma-ray Sources Coincident with Cosmic Neutrino Events

Using data obtained by the gamma-ray imager on board of the AGILE satellite, we systematically searched for transient gamma-ray sources above 100 MeV in temporal and spatial coincidence with high-energy neutrino IceCube events. We found some significant gamma-ray transients possibly associated with HESE neutrinos recently detected by the IceCube experiment. In this talk, we review the AGILE results and we will show that the probability of this association to be by chance is very low. One of the sources detected by AGILE is related to the blazar AGN TXS 0506+056. For the other sources, there are no obvious known counterparts.

Speaker: Dr Fabrizio Lucarelli (INAF-OAR & ASI-SSDC)

Slides AGILE-Neutrinos_Lucarelli_final.pdf

14:30 Measurement of the cosmic ray Moon shadow with the ANTARES detector.

The ANTARES detector is the largest neutrino telescope currently in operation in Mediterranean sea. One of the main goals of the ANTARES telescope is the search for point-like neutrino sources, so both the pointing accuracy and the angular resolution of the detector need a proper direct estimation. One possibility to evaluate the pointing performance of the detector is to analyse the shadow of the Moon, i.e. the deficit in the atmospheric muon flux in the direction of the Moon induced by absorption of cosmic rays. The ANTARES data taken between 2007 and 2016 shows a Moon shadow evidence of about 3.5σ significance. This is the first measurement of the ANTARES angular resolution and absolute pointing for atmospheric muons using a celestial calibration source. The presented results confirm the good pointing performance of the detector as well as the predicted angular resolution.

Speaker: Matteo Sanguineti (GE)

Slides Moon_RICAP.pdf

14:50 Anagraphical picture of high energy Galactic Neutrino

The TeV/PeV neutrino emission from our Galaxy is related to the population of cosmic-ray accelerators, their activity duration, the maximal energy of injected cosmic rays as well as their propagation and the massive molecular clouds presence. Interesting upper limits on diffuse hadronic emission from the Galactic plane, the Fermi Bubbles and the more massive molecular cloud regions were set in the last years with the actual sensitivity of IceCube and ANTARES telescopes close to the expected neutrino emissivity. No evidence of Galactic point-like component excess has been observed up to now by high energy neutrino telescopes pointing out the subdominant component respect to the diffuse ones. This result is also determined by the fact that PeV injection of Supernovae Remnants last for a short period of time (~ hundred of years). All these aspects will be discussed in this presentation.

Speaker: Antonio Marinelli (PI)

Slides Galactic_neutrino_A_Marinelli.pdf

15:10 Search for tau neutrinos with the MAGIC telescopes: the quest continues

MAGIC, a system of two Cherenkov telescopes located at the Roque de los Muchachos Observatory (2200 a.s.l.) in the Canary Island of La Palma, has lately been engaged in an unconventional task: the search for a signature of particle showers induced by earth-skimming cosmic tau neutrinos arising from the ocean, in the PeV to EeV energy range. When pointing at the Sea, the MAGIC telescopes can collect data in a range of about 5 deg in zenith and 80 deg in azimuth: the analysis of the shower images from 30 hours of data, together with the simulations of upward-going tau neutrino showers, shows that the air showers induced by tau neutrinos can be discriminated from the hadronic background coming from a similar direction. We have calculated the point source acceptance and the expected event rates, assuming an incoming tau neutrino flux consistent with IceCube measurements, and for a sample of generic neutrino fluxes from photo-hadronic interactions in AGNs and GRBs. A 90% C.L. upper limit on the tau-neutrino point source flux of 2.0x10^-4 GeV cm^-2 s^-1 has been obtained. The presented results can also be important for future Cherenkov experiments such as the Cherenkov Telescope Array. This next generation ground-based observatory can have a much better possibility to detect tau neutrinos, given its larger FOV and much larger effective area.

Speaker: Dr Marina Manganaro (University of Rijeka)

Slides tau_neutrinos_RICAP_2018_v4.pdf

15:30 Particle propagation in clumpy media

The presence of dense clumps in the environment where a supernova remnant (SNR) expands might have a strong impact in shaping the observed hadronic gamma-ray spectrum. I will here present a detailed numerical study about the penetration of relativistic protons into clumps which are engulfed by a SNR shock, taking into account the magneto-hydrodynamical properties of the background plasma. In such a scenario, the spectrum of protons inside clumps results much harder than that in the diffuse inter-clump medium: this effect has strong implications for the formation of the spectrum of hadronic gamma rays, which does not reflect anymore the acceleration spectrum of protons, resulting substantially modified by propagation effects. For the Galactic SNR RX J1713-3946.7, I will show that a hadronic scenario including dense clumps inside the remnant shell is able to reproduce the broadband gamma-ray spectrum from GeV to TeV energies. Moreover, small clumps crossed by the shock could provide a natural explanation to the X-ray variability observed in some hot spots of RX J1713-3946.7. The detection of neutrinos from this source would represent a smoking gun for the hadronic origin of the observed radiation: in this view, I will explore the potentials of the upcoming KM3NeT. Finally I will discuss the detectability of gamma-ray emission from clumps with CTA.

Speaker: Silvia Celli (GSGC)

Slides Celli_Ricap18.key

15:50 Prospects on CCSN neutrino detection with the KM3NeT telescopes

Core Collapse Supernovae (CCSN) are explosive phenomena that may occur at the end of the life of massive stars, releasing over 99% of the energy through emission of neutrinos with energies on the 10 MeV scale. While the explosion mechanics is not fully understood, neutrinos are believed to play an important role in it. The only detection as of today are the 24 neutrinos from supernova SN1987A. Future observations with large detectors will provide an unprecedented potential for the study of these phenomena, and lead to important breakthroughs across the fields of astrophysics, nuclear and particle physics. For a galactic CCSN, the KM3NeT ORCA and ARCA detectors in the Mediterranean will observe a significant number of neutrinos via the detection of Cherenkov light, mostly induced from inverse beta decay interactions over a large instrumented seawater volume. The selection of photons in coincidence between the 31 photomultipliers of KM3NeT optical modules allows to separate the signal from the optical background sources (K40 decays, bioluminescence and atmospheric muons). The KM3NeT sensitivity for the detection of a galactic CCSN and the potential to resolve the neutrino time profile have been estimated exploiting detailed MC simulations covering the event generation and the detector response. Specific criteria are proposed for the online triggering and the participation in the SNEWS global alert network.

Speaker: Marta Colomer Molla (IFIC, Univ. Valencia / APC, Univ Paris Diderot)

Slides RICAP2018_last_CCSN.pdf

14:10 → 16:10 g-rays

Convener: Dr Emmanuel Moulin (CEA Saclay)

14:10 Instruments optimizations for low energy Gamma-ray detection

There is an experimental gap in the study of the non-thermal universe in the photon energy range from 300 kev to 100 MeV. We have analized the performence of a detector with unprecedent sensitivity, angular and energy resolution and combined with polarimetric capability to study of the most powerful Galactic and extragalactic sources and with a line sensitivity in the MeV energy range two orders of magnitude better than previous generation of instruments that can determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy.

Speaker: Gonzalo Rodriguez Fernandez (ROMA2)

Slides eASTRO_Gonzalo.Rodriguez_RICAP2018.pdf

14:30 Future high-energy missions' polarimetric prospects

High-energy astrophysics polarimetry may greatly benefit from e-ASTROGAM mission proposal legacy or from AMEGO future mission, since so far limited polarimetric measurements were performed in this domain, measured by instruments that were not designed or optimized for polarimetry. These space observatory is composed by semiconductor tracker, calorimeter, and an anticoincidence system, operating up to GeV energy band. The Compton (up to ~2 MeV) polarimetric potential of these mission concepts was analysed by mass model simulations using MEGAlib simulation tools [3], for different tracker, calorimeter and anticoincidence system configurations as well as for different the detector types (scintillators and semiconductors) within the mission mass and power margins. Background and main gamma-ray sources were modelized. Polarimetric modulation factor and Minimum Detectable Polarization was estimated for each source within the mission time frame.

Speaker: Mr André Filipe Ventura Cortez (Laboratório de Instrumentação e Física Experimental de Partículas)

14:50 The Astri program

The Cherenkov Telescope Array (CTA) will be the largest ground-based very high-energy gamma-ray detection observatory in the world with more than one hundred telescopes located in the Northern and Southern Hemispheres (La Palma, Canary Islands and currently proposed at Paranal, Chile). The energy coverage, in the southern CTA array, will extend up to 300TeV thanks to a large number (up to 70) of small size telescopes, with their primary mirrors of about 4 meters in diameter and large field of view of the order of 9 degrees. In the CTA project framework Italy is giving an important contribution in the development of the telescope array through the ASTRI program. The first aim of the program was to design, realize and deploy a prototype of the CTA small-size telescopes named the ASTRI SST-2M, The prototype telescope is now installed in Italy at the INAF Observatory on Mt. Etna (Sicily) and is entering in its commissioning and science verification phase. During this phase, that includes scientific observations of known sources such as the Crab Nebula and a few blazars, the prototype performance will be crosschecked with the predictions of Monte Carlo simulations. The next step of the program will be the production of a set at least nine end-to-end ASTRI telescopes named ASTRI mini-array, proposed as one of the first seed of CTA telescopes at the south site. This effort is led by INAF in synergy with the Universidade de Sao Paulo (Brazil) and the North-West University (South Africa). ASTRI telescopes are characterized by an optical system based on a dual-mirror Schwarzschild-Couder design and by a curved focal plane covered by silicon photomultiplier sensors managed by a fast front-end electronics. The telescope prototype, developed by the Italian National Institute for Astrophysics, INAF, follows an end-to-end approach that includes the internal and external calibration systems, control/acquisition hardware and software, data reduction and analysis software, and the data archiving system.

Speaker: Dr Salvatore Scuderi (INAF-IASFMI)

Slides ASTRI_RICAP2018r.pdf

15:10 SiPM optical modules for the Schwarzschild- Couder Medium Size Telescopes proposed for the CTA observatory

Silicon Photomultipliers (SiPMs) are excellent devices to detect the faint and short Cherenkov light emitted in high energy atmospheric showers, and therefore suitable for use in Imaging Air Cherenkov Telescopes. The high density NUV SiPMs (NUV-HD3) produced by Fondazione Bruno Kessler (FBK) in collaboration with INFN were used to equip optical modules for a possible upgrade of the prototype Schwarzschild-Couder Telescope camera, in the framework of the Cherenkov Telescope Array project. SiPMs are 6x6mm2 devices based on 40x40μm2 microcells optimized for photo-detection at the Near Ultra Violet wavelengths. More than 40 optical modules, each composed by a 4x4 array of SiPMs, were assembled. In this contribution we report on the development and on the assembly of the optical modules, their validation and integration in the the camera.

Speaker: Emanuele Fiandrini (PG)

Slides RICAP_2018_sct__Fiandrini_sh_r.pdf

15:30 The Large Magellanic Cloud with the Cherenkov Telescope Array

The Large Magellanic Cloud with the Cherenkov Telescope Array Abstract The CTA Consortium1, represented by Mabel Bernardos2 Co-Authors: María Benito3, Elena Fedorova4, Fabio Iocco3, Salvatore Mangano2, Olga Sergijenko5. The Large Magellanic Cloud (LMC) is a spiral galaxy, satellite of the Milky way with a high star formation activity. It represents a unique laboratory for studying an extended and spatially resolved star-forming galaxy through gamma-ray observatories. Therefore, the LMC survey is one of the key science projects for the Cherenkov Telescope Array (CTA), the next generation ground-based gamma-ray observatory. In this talk I will present the work performed over the last year by the CTA working group dedicated to the Large Magellanic Cloud, in order to offer a first characterization of the LMC at TeV energies. We have performed detectability forecasts based on the expected CTA performance for all sources in the region of interest of the LMC with known emission at GeV energies and above. Based on previous observations made by Fermi LAT and H.E.S.S. we have characterized all point sources, extended sources and diffuse emission produced by cosmic-ray propagation, extrapolating their spectra to CTA energies. Finally, we have characterized the signal expected by different annihilation mechanisms of dark matter particles within the LMC, drawing the detection sensitivity for this target in the mass-cross section plane. 1 See https://www.cta-observatory.org/consortium_authors/authors_2018_08.html 2 Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas(CIEMAT), Madrid, Spain. 3 ICTP-South American Institute for Fundamental Research, Instituto de Física Teórica - UNESP, São Paulo, Brazil. 4 National Academy of Sciences of Ukraine, Kiev, Ukraine. 5 Ivan Franko National University of Lviv Astronomical Observatory, Lviv, Ukraine.

Speaker: Mrs Mabel Bernardos (CIEMAT)

Slides LMCwithCTAv3.pdf

15:50 GIANT MOLECULAR CLOUDS AS PROBES OF CR PROTONS WITH FERMI-LAT

The accumulation and effective mixture of relativistic particles during their propagation through the interstellar magnetic fields results in the formation of the so-called "sea" of galactic Cosmic Rays (CRs). The level and the energy distribution of the CR sea is determined by the operation of all galactic accelerators over the confinement time of CRs in the Galactic Disk. The homogeneity of CRs, however, can be violated on smaller scales, in the form of excess fluxes over the CR sea, caused by the injection of fresh relativistic particles by young accelerators into the interstellar medium (ISM). CRs interacting with Giant Molecular Clouds with masses larger than 10^5 Solar masses produce “enhanced” gamma-ray emission which can be used to probe the level of the CR sea throughout the Galactic Disk. I present the analysis of more than 9 years data of Fermi-LAT on a sample of 18 molecular clouds located at different distances from the Galactic Center. The CR density derived from the gamma-ray data are in a good agreement with the direct CR measurements, confirming that the CR fluxes reported by the AMS collaboration do represent the level of CR; meanwhile in some regions, in particular in the 4-6 kpc molecular ring the CR flux is enhanced and the energy spectrum is noticeably harder compared to the AMS-02 measurements.

Speaker: Ms Giada Peron (Max Planck Institute of Nuclear physics)

Slides GiadaPeronRicap2018.pdf

16:10 → 16:40 coffee break and poster session

16:40 → 18:40 CR: 2

Convener: Roberta Sparvoli (ROMA2)

16:40 Helium flux and elemental composition of galactic Cosmic Rays with the DAMPE space mission

DAMPE (DArk Matter Particle Explorer) is a space mission project promoted by the Chinese Academy of Sciences (CAS), in collaboration with Universities and Institutes from China, Italy and Switzerland. The detector is collecting data in a stable sun-synchronous orbit lasting 95 minutes at an altitude of about 500 km. It has been launched in December 17th, 2015, from the Jiuquan Satellite Launch Center, in the Gobi Desert. The main goals of the mission are: indirect search for Dark Matter, looking for signatures in the electron and photon spectra with energies up to 10 TeV; analysis of the flux and composition of primary Cosmic Rays with energies up to hundreds TeV; high energy gamma-ray astronomy. Preliminary results about the Helium flux and Cosmic Rays composition will be presented and discussed.

Speaker: Margherita Di Santo (LE)

Slides RICAP_2018_MARGHERITADISANTO.pdf

17:00 Proton energy spectrum with the DAMPE experiment

The DAMPE (DArk Matter Particle Explorer) experiment, in orbit since December 17th 2015, is a space mission whose main purpose is the detection of cosmic electrons and photons up to energies of 10 TeV, in order to identify possible evidence of Dark Matter in their spectra. Furthermore it aims to measure the energy fluxes and the elemental composition of the galactic cosmic rays nuclei up to at least 30 TeV. The  proton spectrum  at the end of two years of data taking, will be presented and discussed

Speaker: Antonio De Benedittis (LE)

Slides RICAP_Proton_energy_spectrum_with_the_DAMPE_experiment.pdf

17:20 The future of the high energy cosmic ray direct detection: HERD

The High Energy cosmic Radiation Detection (HERD) facility will be one of the future space astronomy payloads onboard the upcoming Chinese space station. The ambitious aim of HERD is the direct detection of cosmic rays towards the "knee" region (~ 1 PeV), with a detector able to measure electrons, photons and nuclei with an excellent energy resolution (1 % for electromagnetic components at 200 GeV and 20 % for nuclei at 100 GeV - PeV), an acceptance 10 times larger than the one of present generation missions (~ 1 m^2 sr), and long lifetime (> 10 years). The primary objectives of HERD are the indirect search for dark matter particles and the precise measurement of energy distribution and composition of primary cosmic rays from 30 GeV up to PeV in order to determine the origin of the "knee" structure in the spectrum. Moreover, HERD will monitor the high energy gamma ray sky, from 500 MeV, thus observing gamma-ray bursts, active galactic nuclei and galactic microquasars. HERD will be composed of a homogeneous electromagnetic calorimeter made of 7500 LYSO crystals, surrounded by a particle tracker, a plastic scintillator detector and a transition radiation detector. Two possible trackers are under study: a 5-side tracker made of silicon micro-strip detectors and a 4-side scintillating fiber tracker surmounted by a silicon micro-strip tracker. The total weight of HERD will be around 4 t with a volume of (2.3 × 2.3 × 2.6) m^3. The entire project: design, perspectives, expected performances in terms of energy sensitivity and acceptance as well as some alternative sub-detectors that are under investigation will be presented in this contribution.

Speaker: Dr Chiara Perrina (University of Geneva)

Slides HERD_RICAP18_C_Perrina.pdf

17:40 In-flight performance of the HEPD detector on-board CSES

The CSES (China Seismo-Electromagnetic Satellite) mission, will investigate the dynamics of the ionosphere by monitoring electric and magnetic fields, plasma disturbances and trapped particle fluctuations, searching for a correlation with the geophysical activity. The High-Energy Particle Detector (HEPD), developed by the Italian National Institute for Nuclear Physics (INFN) in collaboration with other Italian institutes and universities, is devoted to the measure of electrons (3-200 MeV) and protons (30-300 MeV) with the possibility of discriminate precipitating trapped particles. The HEPD consists of two planes of double-side silicon micro-strip detectors for the reconstruction of the incident particle direction, a segmented layer of plastic scintillators for the trigger, a calorimeter constituted by a tower of plastic scintillator counters and a LYSO matrix and a veto system. CSES was launched from the Jiuquan Satellite Launch Center (China) on the 2nd of February 2018. The HEPD has been powered a few days after launch for a health check and the beginning of the commissioning phase. In the commissioning period (February-July 2018) different payload configurations have been tested in order to optimize the detector configuration in flight. Topic of this talk is the in-flight performance of the HEPD apparatus.

Speaker: Dr Alessandro Sotgiu (ROMA2)

18:00 CaloCube and “Tracker In Calorimeter” projects for the direct measurement of high energy charged astro-particles and gamma rays.

Measurements of high energy cosmic rays in the “knee” region (about 10^15 eV) are currently available only with ground detectors: new observations of cosmic particles up to this energies with direct measurements are one of the main goals of the next generation space experiments. To achieve those aim, a large acceptance, good energy resolution and particle identification are needed. CaloCube is the design of a space borne calorimeter which is capable to accepts particles coming from any direction, increasing the acceptance with respect to traditional telescopes. A good performance for both hadronic and electromagnetic showers is achieved with a 3-D sampling capability: the basic picture of CaloCube is a cubic homogeneous calorimeter which consists of cubic scintillating crystals. MC simulations, concerning different materials and geometrical configurations, and several beam test with different versions of the CaloCube prototype have been employed to optimize both the detector design and the data analysis method. Taking advantage of the CaloCube project, the space experiment HERD (“High Energy Cosmic Radiation Detection”) will include a large acceptance cubic calorimeter with cubic LYSO crystals. It will be installed on-board of the Chinese space station around 2025. Beside the charged particle observations, high energy gamma rays provide direct information about the galactic cosmic ray sources. A new project named “Tracker In Calorimeter” (TIC) was approved by INFN in 2017 with the main purpose of the optimization of the calorimeter design for the reconstruction of the gamma ray direction, without the requirement of additional not homogeneous pre-shower detector. A TIC prototype was recently assembled and tested at the PS-CERN accelerator.

Speaker: Nicola Mori (FI)

16:40 → 18:40 direct search for DM and underground experiments

Convener: Mario De Vincenzi (ROMA3)

16:40 Xenon-1T

Speaker: Dr Ran Budnik (Columbia university)

17:00 Direct search for light dark matter with the CRESST-III experiment

The CRESST-III (Cryogenic Rare Event Search with Superconducting Thermometers) experiment, located in the Gran Sasso underground laboratory (LNGS, Italy), aims at the direct detection of dark matter (DM) particles. Scintillating CaWO$_4$ crystals operated as cryogenic detectors at mK temperatures are used as target material for elastic DM-nucleus scattering. The simultaneous measurement of the phonon signal from the CaWO$_4$ crystal and the emitted scintillation light in a separate cryogenic light detector provides particle discrimination on an event-by-event basis. This technology is particularly sensitive to small energy deposits induced by light dark matter particles, allowing the experiment to probe the low-mass region of the parameter space for spin-independent DM-nucleus scattering with high sensitivity. In early 2018 CRESST-III completed an initial data taking campaign reaching nuclear recoil thresholds of well below 100 eV. This unprecedented low threshold provides a significant boost in sensitivity beyond CRESST-II which achieved a threshold of 0.3 keV allowing for the first time to probe dark matter masses as low as 500 MeV/c$^2$. New results of CRESST-III will be presented accompanied by a brief status update on the ongoing CRESST-III measurement campaign.

Speaker: Paolo Gorla (LNGS)

Slides RICAP_CRESST_Gorla.pdf

17:20 Directional dark matter search with nuclear emulsion technology

Direct Dark Matter searches are nowadays one of the most fervid research topics with many experimental efforts devoted to the search for nuclear recoils induced by the scattering of Weakly Interactive Massive Particles (WIMPs). Detectors able to reconstruct the direction of the nucleus recoiling against the scattering WIMP are opening a new frontier to possibly extend Dark Matter searches beyond the neutrino background. Exploiting directionality would also prove the galactic origin of Dark Matter with an unambiguous signal-to-background separation. Indeed, unlike the background sources, the angular distribution of recoiled nuclei is expected to be centered around the direction of the Cygnus constellation. Current directional experiments are based on gas TPC whose sensitivity is limited by the small achievable detector mass. In this talk we present the discovery potential of a directional experiment based on the use of a solid target made of newly developed nuclear emulsions and of optical read-out systems reaching unprecedented nanometric resolution.

Speaker: Giovanni De Lellis (NA)

Slides NEWSdm_RICAP.pptx

17:40 Underground Nuclear Astrophysics: present and Future of the LUNA experiment

The evolution of all the celestial bodies is regulated by gravitation and thermonuclear reaction rates, while the Big Bang nucleosynthesis is the result of nuclear processes in a rapidly expanding Universe. The LUNA Collaboration has shown that, by exploiting the ultra low background achievable deep underground, it is possible to study the relevant nuclear processes down to the nucleosynthesis energy inside stars and during the first minutes of Universe. In this talk the main results obtained by LUNA are overviewed, as well as the scientific program of LUNA with the forthcoming 3.5 MV underground accelerator. In particular I will discuss the recent study of the d(p,gamma)3He reaction, whose cross section has been measured inside the Big Bang Nucleosynthesis energy region. The importance of this measurement in Cosmology, particle physics and theoretical nuclear physics is also discussed.

Speaker: Carlo Gustavino (ROMA1)

Slides Gustavino_ricap.pdf

18:00 The Recoil Directionality (ReD) experiment

Directional sensitivity to nuclear recoils would provide a smoking gun for a possible discovery of dark matter in the form of WIMPs. A hint of directional dependence of the response of a dual-phase liquid argon Time Projection Chamber (TPC) was found in the SCENE experiment. Given the potential importance of such a capability in the framework of dark matter searches, a new dedicated experiment, ReD (Recoil Directionality), was designed in the framework of the DarkSide Collaboration, in order to scrutinize this hint. A small dual-phase liquid argon TPC is irradiated with neutrons produced by the p(Li7,Be7)n reaction from the TANDEM accelerator of the INFN Laboratori Nazionali del Sud (LNS), Catania, such to produce Ar nuclear recoils in the range of interest for Dark Matter searches. Energy and direction of nuclear recoils are inferred by the detection of the elastically-scattered neutron by a set of scintillation detectors. Golden scattering events can be further selected by gating of the associated Be7, which is detected by a telescope made of two Si detectors. As an additional valuable by-product, ReD can be operared to study the response of the TPC to very low-energy nuclear recoils (in the keV range). After a commissioning phase of the TPC at INFN Naples, the ReD set-up was deployed and integrated on a beam line of the LNS. Initial beam time was granted in June-July 2018, allowing for the first characterization and for the integration of the three detector systems (TPC, liquid scintillators, Si telescope). This contribution will describe the performance of the detectors achieved during the first test-beam, the current status of ReD and the perspectives for physics measurements during the forthcoming beam-time.

Speaker: Dr Simone Sanfilippo (ROMA3)

Slides Sanfilippo_ricap2018v2.pdf

18:40 → 19:40 Posters session

18:40 CSES-LIMADOU: HEPD Ground Segment at ASI-SSDC

The CSES space mission, an international collaboration between China and Italy, aims at monitoring the perturbations originated by electromagnetic emissions in the ionosphere, magnetosphere and in the Van Allen radiation belts, and at investigating possible correlations with seismic events. The Italian collaboration, named LIMADOU, contributed to the mission with the realization of the High Energy Particle Detector (HEPD), an instrument developed on the basis of a long experience in developing advanced space detectors for charged and neutral particles and gamma rays – in a wide range of energies – for applications in solar physics as well as in extra-galactic astrophysics and cosmology. The CSES Satellite was launched from the Jiuquan Satellite Launch Center on February 2, 2018 and the expected mission lifetime is of 5 years. Satellite data are transferred to the Institute of Crustal Dynamics (ICD) of the China Earthquake Administration (CEA) in Beijing, China. After the donwling HEPD raw data are transferred as soon as possible to the Italian Ground Segment. In the IGS, HEPD raw data are processed from level0 to level2 after calibration and equalization and are then stored in an high-availability processing server and stored in a high-resilience storage. In this poster we present a schematic of the HEPD detector data structure and the processing pipeline that has been built at the Italian Space Agency – Space Science Data Center.

Speaker: Mr Matteo Merge' (ROMA2)

18:41 The HEPD Segmented Calorimeter

The core of the High-Energy Particle Detector (HEPD), on board of the China Seismo-Electromagnetic Satellite (CSES), is a segmented calorimeter, which is composed with an upper tower of plastic scintillator counters and a bottom array of LYSO large crystals. Electrons with energy below 100 MeV, protons and light nuclei, below few hundreds of MeV/nucleon are fully contained within this calorimeter. Mainly the LYSO array (density 7.3, thickness around 29.2 g/cm^2) extends the HEPD energy range, allowing those measurements (solar energetic particles, low-energy cosmic rays) which are more related to astroparticle physics topics. Two identical copies of HEPD, and then of its calorimeter, exist: the Flight (FM) and the Qualification (QM) models. While the FM has achieved the orbit on board of the CSES satellite in February 2018, the Qualification Model, is used, at ground, for tests and calibrations. A report on the characterization of this compact particle space detector and on preliminary studies and results, will be given.

Speaker: Dr Vincenzo Vitale (ROMA2)

18:42 Status and first results from the ARCA and ORCA lines of the KM3NeT experiment

KM3NeT is a submarine Cherenkov neutrino telescope under construction at two sites in the Mediterranean Sea. The detector at the Italian site, close to the Sicilian coast and named ARCA, will be devoted to the detection of high-energy astrophysical neutrinos, while the detector at the French site, in the Toulon bay and named ORCA, will collect mainly atmospheric neutrinos to study the neutrino mass hierarchy. The telescope will be a network of strings anchored to the sea floor and instrumented with multi-PMT digital optical modules (DOM). The geometry of the detectors has been adapted to their physics goals: in ARCA, every string is 700 m high and has 18 DOMs, one every 36 m, with the inter-string distance of about 90 m; while in ORCA the strings are 200 m high, with an inter-DOM spacing of only 9 m and an inter-line spacing of ~23 m. The first two lines of ARCA have been deployed in December 2015 and May 2016 respectively, the first string of ORCA has been deployed in sept 2017. The first results of ARCA intra-DOM calibrations using K40 decays together with the first reconstructed atmospheric muons and the first data-MC comparison for ORCA will be presented.

Speaker: Paolo Fermani (ROMA1)

18:43 MC simulation of HEPD detector - performances and beam test analysis

The High-Energy Particle Detector (HEPD) is an instrument devoted to the measurement of electron, proton and light nuclei from few MeV up to hundreds MeV. HEPD has been developed by the Italian Limadou collaboration in the framework of the Chinese CSES (China Seismo-Electromagnetic Satellite) space mission. The HEPD will give a strong contribution to the CSES mission by measuring the precipitation of trapped particles and by studying the solar-terrestrial environment through mechanisms like coronal mass ejections and solar energetic particle emissions. CSES satellite was successfully launched on the 2nd of February 2018 and injected into a circular Sun-syncronous orbit with 98° inclination and 500 km altitude. Expected lifetime is 5 years. Two models of the detector have been entirely integrated in the clean rooms of WiZard laboratory at University of Rome Tor Vergata: a Qualification Model (QM) for calibration tests and a Flight Model (FM) for the space mission. Beam tests have been carried out before the launch with electrons, protons and nuclei up to Oxygen for both QM and FM. In this poster the main features of the HEPD Monte Carlo simulation and some results of the detector performances based on MC simulations are reported. Particular importance will be given to MC nuclei data analysis.

Speaker: Luca Carfora (ROMA2)

18:44 Integration and testing of the Mini-EUSO UV telescope

The Mini-EUSO telescope is designed to observe the UV emission of the Earth from the vantage point of the International Space Station in low Earth orbit. Mini-EUSO will map the earth in the UV range (300 - 400 nm) offering the opportunity to study a variety of atmospheric events such as Transient Luminous Events (TLEs) and meteors, as well as searching for strange quark matter and bioluminescence. The instrument comprises a compact telescope with a large field of view (±22°), based on an optical system employing two Fresnel lenses for increased light collection. The light is focused onto an array of 36 multi-anode photomultiplier tubes and the resulting signal is converted into digital, processed and stored via the electronics subsystems on-board. In addition to the main detector sensible in the UV range (300 - 400 nm), Mini-EUSO contains two ancillary cameras for complementary measurements in the near infrared (1500 - 1600 nm) and visible (400 - 780 nm) range. The integration of the instrument, currently underway at the University of Rome Tor Vergata, is at an advanced stage in order to be compliant with a launch opportunity in the early 2019. The on ground test results will be presented.

Speaker: Giorgio Cambiè (University of Rome Tor Vergata)

18:45 Mini-EUSO: a telescope on board the International Space Station for the observation of terrestrial and cosmic UV emissions

The Mini-EUSO instrument is a UV telescope to be placed inside the International Space Station (ISS), looking down on the Earth from a UV-transparent window in the Russian Zvezda module. Mini-EUSO will map the earth in the UV range (300 - 400 nm) with a spatial resolution of 6 - 11 km and a temporal resolution of 2.5μs. The main Mini-EUSO objectives are the study a variety of atmospheric phenomena such as Transient Luminous Events (TLEs), meteors and meteoroides, the search for Strange Quark Matter (SQM) and bioluminescence. Furthermore, Mini-EUSO could represent the first step in a roadmap of potential debris removal via laser ablation. Moreover, the high-resolution mapping of the UV emissions from Earth orbit allows Mini- EUSO to serve as a pathfinder for the study of Extreme Energy Cosmic Rays (EECRs) from space by the JEM-EUSO Collaboration. Mini-EUSO is a compact telescope, with a large field of view, based on an optical system employing two Fresnel lenses, a focal surface composed of 36 multi-anode photomultiplier tubes and an acquisition and storage system. In addition to the main UV detector, Mini-EUSO contains two ancillary cameras for complementary measurements in the near infrared and visible range.

Speaker: Laura Marcelli (ROMA2)

18:46 e-Astrogam Mission Polarimetric Optimization

High-energy astrophysics polarimetry may greatly benefit from e-ASTROGAM (enhanced ASTROGAM) mission proposal legacy, since so far limited polarimetric measurements were performed in this domain, measured by instruments that were not designed or optimized for polarimetry. This space observatory is composed by a Silicon tracker, a calorimeter, and an anticoincidence system, operating in the 0.3 MeV up to 3 GeV energy band. The Compton (up to ~2 MeV) polarimetric potential of e-ASTROGAM mission concept was analysed by mass model simulations using MEGAlib simulation tools [3], for different tracker, calorimeter and anticoincidence system configurations as well as for different the detector types (scintillators and semiconductors) within the mission mass and power margins. Background and main gamma-ray sources were modelized. Polarimetric modulation factor and Minimum Detectable Polarization was estimated for each source within the mission time frame.

Speaker: Mr Rui Curado da Silva (LIP)

18:47 Variability studies of GRB light curves and neutrino flux prediction for multi-collision zone model

Gamma-Ray Bursts are the most powerful explosions in the Universe. They constitute highly beamed sources of gamma rays and possibly also of high-energy neutrinos and protons. In the fireball model, blobs of plasma, emitted from a central engine, collide within a relativistic jet forming shocks, where particle acceleration is expected to act. However, an open issue is represented by the way in which the central engine operates. In order to shed light on this topic, the information on the temporal behaviour of individual GRBs is very precious. For the analysis here presented, the most luminous GRB detected by Konus/WIND until now was selected, namely GRB 110918A. Through the NeuCosmA code, simulating multi-zone collisions during the GRB prompt emission, a synthetic light curve consistent with the observed one has been obtained, in order to study how characteristic parameters of the inner engine activity influence the light curve. This is achieved varying the input parameters values in the simulation. In agreement with other previous studies, it was obtained that the inner engine is more variable than the observed light curve and dependence relations between parameters have been found. Furthermore, the empirical mode decomposition method is applied and its stability is analysed.

Speaker: Ms Angela Zegarelli (INFN, Roma1)

18:48 Preliminary Studies on Supernova neutrinos with JUNO detector

Observation of supernovae through their neutrino emission is a major fundamental point to understand both supernova dynamics and neutrino physical properties. JUNO is a 20 kton liquid scintillator detector, under construction in Jiangmen, China. The main aim of the experiment is to determine neutrino mass hierarchy by precisely measuring the energy spectrum of reactor electron antineutrinos at a distance of ∼ 53 km from the reactors. However due to its properties, JUNO has the capability of detecting a high statistics of SN events too. Where existing data from SN neutrino consists only of a few events coming from the SN 1987A, the detection of a SN burst in JUNO from a progenitor star at ∼ 10 kpc will yield ∼ 5 × 10 3 IBD events from electron antineutrinos, plus several hundreds on other CC and NC interaction channels from all neutrino species. In this work, a preliminary study of the SN neutrino events, with the JUNO detector is presented. The reconstruction of the supernova neutrino energy spectra is based on a probabilistic unfolding method.

Speaker: Mrs Cristina Martellini (Roma Tre Univ)

18:49 e-mu discrimination at high energy in the JUNO detector

The neutrino oscillation physics can be studied by using atmospheric neutrinos as source. JUNO is a large liquid scintillator detector with low energy threshold and excellent energy resolution. The detector performances allow the atmospheric neutrino oscillation measurements. In this work, a discrimination algorithm for different reaction channels of neutrino-nucleon interactions in the JUNO liquid scintillator , in the GeV/sub-GeV energy region, is presented. The atmospheric neutrino flux is taken as reference, considering \nu_e and \nu_\mu. Depending on the nature of the interaction, neutrinos can produce their corresponding charged lepton plus hadronic particles in the final state, if they undergo a charged-current (CC) interaction, or can generate only secondary hadrons, if they undergo a neutral-current (NC) interaction. When the energy of the event is high enough, namely \gtrsim 1 GeV, muons travel for a longer distance inside the matter with respect to electrons. Additionally, muons have the property of being unstable particles and decaying in an electron plus two neutrinos, which translates in a late energy emission inside a particle detector. These differences make \nu_\mu CC events more elongated in time with respect of \nu_e CC events, which indeed appear point-like. Hadronic particles are all unstable, thus adding late energy releases to all the events. The different temporal behaviour of the classes of events have been exploited to build a time profile-based discrimination algorithm. The results show a good selection power for \nu_e CC events, while the \nu_mu CC component suffers of an important contamination from NC events at low energy, which is now under study.

Speaker: Giulio Settanta (ROMA3)

Thursday, 6 September

08:30 → 10:30 GW and CR measurements

Convener: Prof. dafne guetta (ORT Braude College)

08:30 Gravitational Waves: where we are, where we go

We review shortly the results obtained during the two science runs O1 and O2 with the advanced gravitational wave detectors LIGO and Virgo. Then, we focus on the middle and long term evolution of the gravitational wave detectors on the Earth with emphasis to their perspectives for the advancement on fundamental physics and astronomy.

Speaker: Fulvio Ricci (ROMA1)

Slides 01_Ricci_RICAP_2018_v1.pdf

09:00 Main scientific results of the DAMPE mission

The DArk Matter Particle Explorer (DAMPE) is a space mission, resulting from the collaboration of Chinese, Italian, and Swiss institutions. Since December 2015, DAMPE orbits at the altitude of 500 km and collects data regularly. The detector is made of four sub-detectors: top layers of plastic scintillators, a silicon-tungsten tracker, a deep BGO calorimeter (32 radiation lengths), and a bottom boron-doped scintillator to detect delayed neutrons. The main goal of the mission is the search of indirect signals of Dark Matter in the electron and photon spectra with energies up to 10 TeV. Furthermore DAMPE is studying cosmic charged and gamma radiation. The calorimeter depth and the large effective acceptance allow to measure cosmic ray fluxes in the range from 20 GeV up to hundreds of TeV. An overview of the latest results about electron and positron flux, light component (p+He) of charged cosmic rays, and gamma rays will be presented.

Speaker: Paolo Bernardini (LE)

Slides talk_RICAP.pdf

09:30 The Lesson of PAMELA

PAMELA is a medium-sized space experiment for the detection of cosmic rays that took data for 10 years from 2006 to 2016. Composed of a magnetic spectrometer and several auxiliary detectors it has been completely realized, at a very reasonable cost, by the collaboration: its different parts at Physics Departments in Italy, Russia, Sweden and Germany and finally the integration in the clean rooms of INFN at Rome Tor Vergata University. The reduced dimensions of the instrument required high performance of the individual detectors to obtain high-precision measurements over a range of energy from tens of MeV/n to 1 TeV/n. In ten years of data taking in space, the experiment PAMELA has shown very interesting features in cosmic rays, namely in the fluxes of protons, helium, electrons, that might change our basic vision of the mechanisms of production, acceleration and propagation of cosmic rays in the Galaxy. In particular, remarkable and stimulating have been the measurements of cosmic antiproton and positron fluxes that have allowed the nature of dark matter to be probed in a new way, suggesting new ideas and setting strong constraints to the models. The continuous particle detection allowed for a constant monitoring of the solar activity and detailed study of the solar modulation for a long period, giving important improvements to the comprehension of the heliosphere mechanisms. PAMELA also measured the radiation environment around the Earth, and discovered an antiproton radiation belt.

Speaker: Piergiorgio Picozza (INFN and University of Rome Tor Vergata)

Slides Picozza_RICAP_The_Lesson_of__PAMELAr.pdf

10:00 The AMS-02 detector on the International Space Station - Status and highlights, after 7 years on orbit

The AMS-02 detector is operating on the International Space Station (ISS) since May the 19th, 2011. More than 120 billion events have been collected by the instrument in the first 7 years of data taking. This unprecedented amount of data is being used to perform accurate measurements of the different Cosmic Rays components. In this contribution, the published results and the highlights of the on-going analyses will be presented.

Speaker: Matteo Duranti (PG)

Slides Duranti-AMSHighlight-RICAP2018_nobackup.pdf

10:30 → 11:00 coffee break and poster session

11:00 → 13:00 Search for HE astrophysical neutrinos

Convener: Antonio Capone (ROMA1)

11:00 IceCube Upgrade and Gen2

Since its discovery of the astrophysical neutrino flux, the IceCube Neutrino Observatory has continued to provide invaluable knowledge about both potential neutrino sources and neutrino properties at the GeV-PeV scale through its detection of neutrino interactions via Cherenkov radiation in the deep South Pole ice. In addition, IceCube is a strong partner in the field of multi-messenger astronomy, which involves rapid follow-up of neutrino events with good pointing precision. I will report on the plans for the IceCube-Upgrade, which aims to deploy new optical modules into the deep ice along with improved calibration devices. This Upgrade will greatly improve our understanding of the detector medium, allowing for reduced uncertainties in angular and energy reconstruction, and thereby more precise measurements of neutrino properties, and more precise pointing towards potential astrophysical sources. In addition, the Upgrade will allow for in-situ testing of new optical modules currently under development for the future IceCube-Gen2 detector.

Speaker: Dr Summer Blot (DESY)

Slides ICU&Gen2_SBlot_RICAP2018.pdf

11:30 Review of the results of the ANTARES neutrino telescope

Neutrino astronomy is in an exciting moment. The discovery of a cosmic flux of high energy neutrinos by IceCube heralds a new era in which neutrinos have finally joined the multi-messenger study of the Universe. This new important window complements more “traditional” probes (as cosmic rays or photons), given the particular combination of characteristics of neutrinos (neutral, stable and weakly interacting). The ANTARES detector, built in the Mediterranean Sea, has succeeded in two key points. First, it has shown the feasibility of the technique of underwater neutrino telescopes, which offers important advantages in terms of performance (better angular resolution, better visibility of the Galaxy if built in the Northern Hemisphere). This has paved the way for the next step, KM3NeT, already in construction. Second, the physics harvest of ANTARES is very rich, including many results that show the particular advantages of being in the Mediterranean mentioned above. The analyses performed include the search for point sources, diffuse fluxes, transient phenomena, dark matter, etc. In this talk we will review this long list of achievements.

Speaker: Dr Juan de Dios Zornoza (IFIC)

Slides RomeRICAP-sep18-antares.pptx

12:00 Baikal-GVD: first results and prospects

Next generation cubic kilometer scale neutrino telescope Baikal-GVD is currently under construction in Lake Baikal. The detector is specially designed for search of high energies neutrinos whose sources are not yet reliably identified. Since April 2018 the telescope has been successfully operated in complex of three functionally independent clusters i.e. sub-arrays of optical modules (OMs) where now are hosted 864 OMs on 24 vertical strings. Each cluster is connected to shore by individual electro-optical cables. The effective volume of the detector for neutrino initiated cascades of relativistic particles with energy above 100 TeV has been increased up to about 0.15 km^3. Preliminary results obtained with data recorded in 2016 and 2017 are discussed.

Speaker: Dr Olga Suvorova (INR RAS)

Slides 07_OSuvorova_RICAP2018.pdf

12:30 Multimessenger Probes of High-energy Sources

With the contemporary operation of the IceCube and Advanced LIGO facilities, we are now able to observe the universe using two new, distinct astrophysical messengers. In addition to photons from radio waves to gamma-rays, we can now, for the first time, simultaneously observe the sky with high-energy neutrinos and gravitational waves . This new era of multimessenger astrophysics offers a unique view of the universe and provide powerful insights into the workings of some of the most energetic and enigmatic objects in the cosmos. In this talk I will overview some of the possible high energy astrophysical sources.

Speaker: Prof. dafne guetta (ORT Braude College)

Slides Dafne2018.pdf

13:00 → 13:10 Group photo

13:10 → 14:10 Lunch and Poster session

14:10 → 15:10 Multimessengers searches

Convener: Dr Fabrizio Lucarelli (INAF-OAR & ASI-SSDC)

14:10 The MAGIC experiment : results and future prospects

MAGIC is a system of two 17 meter Imaging Air Cherenkov Telescopes, located at the Observatorio Roque de los Muchachos at an altitude of 2200 meters on the Canary island of La Palma. MAGIC detects gamma rays in the very-high-energy regime between a few tens of GeV and tens of TeV. In this presentation, I will present the latest highlights achieved by the instrument from galactic and extragalactic observations, as well as the most recent results on dark matter and fundamental physics. I will also show results of the MAGIC transient follow-up program, with special emphasis on the very recent VHE gamma-ray measurement of the flaring blazar TXS 0506+056 coincident with the high-energy neutrino IceCube-170922A.

Speaker: Dr Ruben Lopez-Coto (INFN-Padova)

Slides 2018_09_06_MAGIC.pdf

14:40 Pushing the Energy and Cosmic Frontiers of Particle Physics with High-Energy Astrophysical Neutrinos

The astrophysical neutrinos recently discovered by IceCube have two unique features. First, they have the highest detected neutrino energies --- from TeV to PeV. Second, they travel the longest distances --- up to a few Gpc. Motivated by this, the decades before discovery saw many proposals for using these neutrinos to measure fundamental particle-physics properties, possibly tiny in size, at energy scales unreachable by any other means. Those exciting proposals have now become a reality. Today, we can perform robust particle-physics tests, in spite of prevalent astrophysical unknowns. In this talk, I will showcase examples of doing fundamental neutrino physics at the most extreme scales, including some of the most stringent tests of physics beyond the Standard Model.

Speaker: Dr Mauricio Bustamante (Niels Bohr Institute)

Slides 2018-09-06-Bustamante-RICAP.pdf

15:10 → 15:40 coffee break and Poster session

15:40 → 17:00 CR: 3

Convener: Silvia Celli (GSGC)

15:40 Measurement of the cosmic ray spectrum with the Pierre Auger Observatory

The Pierre Auger Observatory is the world's largest detector for extensive air showers initiated by cosmic rays with energies above 0.3 EeV. Equipped with 1660 water-Cherenkov stations, the surface detector array spans an area of 3000 square kilometers. The combination with 27 fluorescence telescopes, which overlook the atmosphere and measure the calorimetric energy allows for a hybrid detection. The all-sky flux of cosmic rays is obtained by combining four independent data sets. The surface detector array provides three data sets, two formed by dividing the data into two zenith angle ranges, and one obtained from a nested, denser detector array. The fourth measurement is obtained with the fluorescence detector. In this talk, the spectral features are discussed in detail and the systematic uncertainties are addressed.

Speaker: Ms Daniela Mockler (Karlsruhe Institute of Technology)

Slides Mockler_RICAP.pdf

16:00 Studies of the UHECR mass composition with the FD and SD of the Pierre Auger Observatory

The Pierre Auger Observatory is the largest detector of ultra-high energy cosmic rays (UHECR) built so far. With the Fluorescence Detector (FD) of the Auger Observatory, a direct measurement of the depth of maximum of shower profiles, $X_{\rm max}$, is performed using the ultraviolet light emitted by nitrogen as the shower develops in the atmosphere. With data on $X_{\rm max}$ collected during more than a decade of operation we report on the inferences on the mass composition of UHECRs in the energy range $E=10^{17.2}-10^{19.6}$~eV and on the measurements of the proton-air cross section for energies up to $10^{18.5}$~eV. The FD operates only during moonless nights and has a duty cycle of around 15\%, thus to gain a larger statistics other mass sensitive observables measured with the Surface Detector (SD), having almost 100\% duty cycle, can be used. Here we present the results on $X_{\rm max}$ (SD) obtained using the information on the particle arrival times recorded by the SD stations allowing us to extend the $X_{\rm max}$ measurements up to $10^{20}$~eV. The inferences on mass composition, in particular using the data of the SD, are subject to systematic uncertainties due to uncertainties in the description of hadronic interactions at ultra-high energies. We discuss this problem with respect to the properties of the muonic component of extensive air-showers as derived from the SD data.

Speaker: Mr Juan Miguel Carceller (University of Granada)

Slides 2_pres.pdf

16:20 Status of the AugerPrime upgrade of the Pierre Auger Observatory

The Pierre Auger Observatory has been very successful to determine many aspects of the highest-energy cosmic rays including, among others, the flux suppression at energies above 4x10^19 eV, stringent upper limits on photon and neutrino fluxes at ultra-high energies and an unexpected evolution of the mass composition with energy. We expect an extension of the frontiers of our knowledge on these aspects from a major upgrade of the Observatory. The upgrade, known as AugerPrime, will include an addition of a 4 m^2 Surface Scintillator Detector atop each Water Cherenkov station of the Surface array. The new detectors will provide us with an unprecedented opportunity of performing a complementary measurement of the shower particles and thus determine the primary mass composition with good accuracy on an event-by-event basis. AugerPrime will also include an upgrade of electronics, installation of the AMIGA Underground Muon Detector and a change of observation mode of the Fluorescence Detector, which will increase its current duty cycle by about 50%. Current status of the upgrade with the main focus on the Surface Scintillator Detectors will be presented following a brief description of the physics motivation for the upgrade.

Speaker: Niraj Dhital (Institute of Nuclear Physics PAN)

Slides 3_RICAP2018.pdf

16:40 Ultrahigh-Energy multi-messengers at the Pierre Auger Observatory

The study of correlations between observations of different messengers from extreme sources of the Universe has emerged as an outstanding way to make progress in their understanding. The Pierre Auger Observatory is capable of significant contributions as an ultra-high energy particle detector, particularly through its capability to search for inclined showers produced by neutrinos. We describe the neutrino searches made with the Observatory with particular emphasis on the recent results following the detections of gravitational waves from binary mergers with Advaced LIGO and VIRGO, leading to competitive limits.

Speaker: Mr Francisco Pedreira (Universidad de Santiago de Compostela)

Slides 4_Pedreira_Auger_multi-messenger.pdf

15:40 → 17:00 Direct and indirect search for DM

Convener: Carlo Gustavino (ROMA1)

15:40 A Unified Program of Argon Dark Matter Searches: DarkSide-20k and The Global Argon Dark Matter Collaboration

Experimenters from four different argon dark matter searches have joined their forces in the the “Global Argon Dark Matter Collaboration” to carry out a unified program for dark matter direct detection. The participants are researchers currently working on the ArDM experiment at LSC; on the DarkSide-50 experiment at LNGS; on the DEAP-3600 experiment at SNOLab; and on the MiniCLEAN experiment at SNOLab. In 2015/2016 The DarkSide-50 experiment at LNGS produced two zero-background science results, along with a comparison of the results obtained with both atmospheric and underground argon fills, demonstrating the ability of large experiments to eliminate background from betas/gammas at the tens of tonne-year exposure. Early in 2018, the DarkSide Collaboration announced results from a 2-years campaign with DarkSide-50, resulting again in a zero-background, null observation of heavy (>50 GeV/c2) dark matter and in the best exclusion limits for light (<10 GeV/c2) dark matter. The DEAP-3600 experiment at SNOLAB is the first tonne-scale experiment to achieve both stable operations and an extended physics run. DEAP-3600 has been collecting physics data with over 3 tonnes of argon since late 2016 and published its first results in 2017. Researchers from the four experiments will jointly carry out as the single next step at the scale of a few tens of tonnes the DarkSide-20k experiment. DarkSide-20k was approved in 2017 by the Italian INFN, by the host laboratory LNGS, and by the US NSF. DarkSide-20k is also officially and jointly supported by the three underground laboratories LNGS, LSC, and SNOLab. DarkSide-20k is a 20-tonne fiducial volume dual-phase TPC to be operated at LNGS with an underground argon fill, designed to collect an exposure of 100 tonne×years, completely free of neutron-induced nuclear recoil background and all electron recoil background. DarkSide-20k is set to start operating by 2021 and will have sensitivity to WIMP-nucleon spin-independent cross sections of 1.2 × 10−47 cm2 for WIMPs of 1 TeV/c2 mass, to be achieved during a 5 year run. An extended 10 year run could produce an exposure of 200 tonne×years, with sensitivity for the cross-section of 7.4 × 10−48 cm2, for the same WIMP mass. DS-20k will explore the WIMP-nucleon cross-section down to the edge of the ’neutrino floor’, where coherent neutrino-nucleus scattering from environmental neutrinos induce nuclear recoils in the detector. A second step in the program is the construction and operation of a detector with a fiducial mass of a few hundred tonnes, capable of collecting an exposure of several thousands of tonne×years, completely free of all backgrounds on top of CNNS. This follow-up experiment would also be capable of performing a set of very high precision measurement of several solar neutrino sources (location and laboratory t.b.d.). This includes exquisitely precise measurements of pep, CNO, as well as low energy 8B neutrinos, all in the region of transition between the vacuum- and matter-dominated regions of solar neutrino oscillations.

Speaker: Prof. Cristiano Galbiati (GSGC)

16:00 Search for Dark Matter using Low-energy Antimatter with the GAPS experiment

The GAPS experiment will be designed to carry out dark matter studies by searching for low-energy cosmic-ray antiparticles (in particular antideuterons). The antideuteron flux, resulting from secondary interactions of primary cosmic rays with the interstellar medium, is very low; novel theoretical studies beyond the standard model of particle physics (i. e., SUSY etc.) predict dark matter candidates, which could led to a significant enhancement of the antideuteron flux, mostly at low energy ranges. The detector will consist of a series of Si(Li) planes of solid state detectors and a time of flight system. Low-energy (< 300 MeV/n) antideuterons will be slowed down in the Si(Li) material, forming an excited exotic atom that will create a characteristic annihilation pion star after de-excitation processes through X-ray transitions. This unique signature will be crucial for a nearly background-free event detection. The GAPS experiment is designed to utilize a series of long-duration balloon flights from Antarctica, and is currently scheduled by NASA for its first Antarctic flight in late 2020.

Speaker: Matteo Martucci (ROMA2)

Slides RICAP18_GAPS.pdf

16:20 Latest results on dark matter searches with H.E.S.S.

The nature of dark matter (DM) is one of the most debated questions of contemporary physics. Ground-based arrays of Cherenkov telescopes such as the High Energy Spectroscopic System (H.E.S.S.) search for DM signatures through the detection of very-high-energy (VHE, E > 100 GeV) gamma rays. DM particles could self-annihilate in dense environments producing VHE gamma rays in the final states that would be eventually detected by H.E.S.S.. The H.E.S.S. observation strategy to search for DM focuses towards the Galactic Centre (GC) region and nearby dwarf galaxies satellite of the Milky Way. The GC dataset provides the most stringent constraints on the DM annihilation cross section in the mass range 300 GeV - 70 TeV for the continuum and line DM signals. Searches have been carried out towards classical and ultra-faint dwarf galaxies to test specific DM models such as the Wino. The latest results towards the GC and dwarf galaxies will be shown.

Speaker: Ms Lucia Rinchiuso (CEA Irfu)

Slides RICAP_LR.pdf

16:40 The Quest for Dark Matter in Dwarf Galaxies with Cherenkov Telescopes

The problem of dark matter detection is of paramount importance for modern astrophysics, since it would allow to fully characterize the properties of the ``missing'' mass in the Universe. So far, in fact, its existence is only based on the indirect observations of the gravitational effects on astronomical objects. Efforts to identify plausible dark matter particle candidates essentially fail without any direct hint about their physics. Recently, a framework for the astronomical search of dark matter signals has been arising from the possibility that dark matter particles self-interact to produce Standard-Model pairs, that subsequently annihilate into final-state gamma photons. The observation of such photons is a task potentially at reach of next-generation Cherenkov telescopes. In this talk, I will illustrate the capabilities of future Cherenkov instruments to detect gamma rays from dark matter self-interaction by observing low-background, dark-matter dominated astronomical sources such as the dwarf spheroidal galaxies.

Slides Saturni_RICAP18_dSph_rid_r.pdf

17:00 → 19:00 Visit of Museum "Centrale Montemartini"

20:15 → 23:00 Social Dinner

Friday, 7 September

09:00 → 11:00 CR and Gamma

Convener: Ms Giada Peron (Max Planck Institute of Nuclear physics)

09:00 VERITAS Status and Recent Results

VERITAS, an array of four 12 m-diameter imaging atmospheric Cherenkov telescopes, located at the Fred Lawrence Whipple Observatory in southern Arizona, is one of the most sensitive instruments currently in operation for gamma-ray astronomy in the 85 GeV to 30 TeV energy range. The VERITAS collaboration conducts a multi-faceted science program which includes studies of Galactic and extragalactic particle accelerators, deriving constraints on cosmological fields and fundamental physics, indirect searches for dark matter and measurements of cosmic rays. Target-of-opportunity observations have high priority and VERITAS operates an extensive follow-up program of both self-generated triggers and multi-messenger alerts received from other instruments. In this talk I will discuss the operational status of VERITAS and present an overview of our scientific program with select recent results highlighted.

Speaker: Dr John Quinn (University College Dublin)

Slides Quinn_VERITAS_RICAP18r.pdf

09:30 The Cherenkov Telescope Array: Current Status and Science Goals

The Cherenkov Telescope Array (CTA) is the major ground-based gamma-ray observatory planned for the next decade and beyond. Consisting of two large atmospheric Cherenkov telescope arrays (one in the southern hemisphere and one in the northern hemisphere), CTA will have superior energy and angular resolutions, a much wider energy range, and up to an order of magnitude improvement in sensitivity, as compared to existing instruments. The CTA science program will be rich and diverse, covering the major aspects of cosmic particle acceleration, understanding extreme environments, and probing physics frontiers beyond the Standard Model. This talk will outline the science goals for CTA and will cover the most recent status of the project.

Speaker: Prof. Rene Ong (Univesrity of California)

Slides RICAP2018-Ong-v3.pdf

10:00 The H.E.S.S. experiment : current status and future prospects

In the 15 years since its construction, the H.E.S.S. gamma-ray observatory has allowed the study of the VHE gamma-ray sky at resolutions and sensitivities which were never before possible. During this period H.E.S.S. has discovered a rich zoo of both galactic and extra galactic source classes, made measurements of the galactic cosmic ray spectrum and placed limits of fundamental physical processes. We will present a summary of the latest H.E.S.S. results for these source classes, describing the most interesting new observations and their physical interpretation. Additionally I will detail the latest upgrades and improvements to the H.E.S.S. hardware and data analyses and the future science prospects for the experiment.

Speaker: Dr Mathieu de Naurois (LLR Ecole Polytechnique - IN2P3/CNRS)

Slides RICAP2018_deNaurois_HESSHighlights_Final_NoBackup.pdf

10:30 Astroparticle Physics with H.E.S.S.: past and future

H.E.S.S. is an array of five Imaging Atmospheric Cherenkov Telescopes located in Namibia. It is designed for observations of astrophysical sources emitting very-high energy (VHE) gamma rays in the energy range from a few ten GeVs to several ten TeVs. The H.E.S.S. array consists of four identical 12 m diameter telescopes with a 28 m diameter telescope placed at the center of the array. An ambitious Astroparticle Physics program is being carried out by the H.E.S.S. collaboration searching for New Physics in the VHE gamma-ray sky. This Astroparticle Physics program includes the search for dark matter signals and axion-like particles, and tests of Lorentz invariance. I will present the latest results on dark matter from observations of the Galactic Centre region and nearby dwarf galaxies, the search for Lorentz invariance violation with 2014 Mrk 501 flare observations, and the first measurement of the cosmic-ray electron spectrum up to 20 TeV. The future of the H.E.S.S. Astroparticle Physics program will be discussed.

Speaker: Dr Emmanuel Moulin (CEA Saclay)

Slides Emmanuel_RICAP2018_final.pdf

11:00 → 11:20 coffee break

11:20 → 13:30 Multimessenger search for HE CR souces

Convener: Mrs Maria Isabel Bernardos (CIEMAT)

11:30 The HAWC gamma-ray observatory: results and prospects

The High Altitude Water Cherenkov gamma-ray observatory has surveyed on a daily basis the northern sky since its completion more than three years ago. The accumulated exposure provides the deepest TeV gamma-ray observations over a large fraction of the sky. In this contribution we will highlight some of the most recent results on individual sources and the role of the observatory in the global astro-particle physics community. This year, the observatory extended its instrumented area by a factor of four with a sparse array of water-Cherenkov detectors to enhance the sensitivity above ~10 TeV. In addition, new analysis techniques have recently been developed to improve low-energy sensitivity and energy resolution. The prospects of these recent developments will be presented.

Speaker: Dr Harm Schoorlemmer (Max-Planck-Institut für Kernphysik)

Slides HAWC_Overview_Harm_Schoorlemmer_RICAP2018_r.pdf

12:00 Upgrading Plan Towards Multi-messenger Observation with LHAASO and Construction Status

LHAASO is planning to enhance its sensitivity at energies around 100 GeV by utilize MCP staffed 20" PMT in the Water Cherekove Detector Array. The effective area for gamma ray detection will reach to 1800 m^2 and differential sensitivity to 0.2 CU at 50 GeV. It will be the very useful survey detection for transient phenomena at 50 GeV in the northern sky. LHAASO will play an important role in the multi-messenger observation. The status of the construction of the whole LHAASO array at the 4400 m a.s.l. site is updated as well.

Speaker: Prof. Zhen Cao (Institute of High Energy Physics)

Slides CAO_ZEN_RICAP-2018r.pdf

12:30 Status of the KM3NeT project

KM3NeT is a research infrastructure hosting neutrino telescopes in the Mediterranean Sea. Two detectors with the same technology but different granularity are foreseen: ARCA at a depth of 3500 m offshore Capo Passero, Italy and ORCA at a depth of 2500 m offshore Toulon, France. Both consist of a 3D array of optical sensors modules, equally spaced along flexible vertical lines, the detection units, anchored at the seabed. The ARCA telescope is designed to discover and observe high-energy neutrinos (TeV ÷ PeV) of cosmic origin. It will be the next generation of the underwater kilometre-cube scale neutrino telescopes. Thanks to its geographical location, it will allow for surveying a large part of the sky, including most of the Galactic Plane and the Galactic Centre. The ORCA detector, with an instrumented volume of a few Mton, is optimized to measure neutrinos with energies at the GeV scale. With ORCA, the focus will be the studies of oscillations of atmospheric neutrinos with the main objective of determining the neutrinos mass hierarchy. The KM3NeT Collaboration has started the construction of both detectors. The first detection units were deployed and the analysis is on going to validate the detector performances. In this talk, the status of the ARCA and ORCA detectors and the future prospects of the project will be presented.

Speaker: Carla Distefano (LNS)

Slides ricap-2018.pdf

13:00 Status and perspectives of the radio detection of high-energy cosmic rays

High-energy cosmic rays impinging on the atmosphere of the Earth induce cascades of secondary particles, the extensive air showers. Many particles in the showers are electrons and positrons. Due to interactions with the magnetic field of the Earth they emit radiation with frequencies of several tens of MHz. In the last years huge progress has been achieved in this field through strong activities of various groups, including the LOFAR radio telescope, the Pierre Auger Observatory, or Tunka-REX. The radio technique is now routinely applied to measure the properties of cosmic rays, such as their arrival direction, their energy, and their particle type/mass. Recent results will be discussed and we will outline the potential of future large-scale applications of the radio technique.

Speaker: Joerg Hoerandel (Radboud University Nijmegen)

Slides jrh-radio.pdf

13:30 → 13:50 Lunch

13:50 → 15:30 UHE and HE CR future experiments

Convener: Mr Juan Miguel Carceller (University of Granada, Spain)

13:50 The TAIGA experiment

The TAIGA-experiment (Tunka Advanced Instrument for cosmic ray and Gamma ray Astrophysics) aims at gamma-astronomy in the multi-TeV to PeV energy range, using a new hybrid technology to build multi-km2 gamma telescopes at competitive cost. TAIGA uses the synergy of two complementary air shower detection techniques: widely spaced imaging air Cherenkov telescopes (IACTs) and a Cherenkov light shower front sampling array. The first has good gamma-hadron separation, while the second yields precision reconstruction of shower energy, direction and impact point. This allows for large distances between IACTs of up to 800-1000m, i.e. a cost-effective mono-mode IACT operation. The proof of principle of this new concept is underway with the TAIGA prototype array, that will be commissioned in 2019 in the Tunka valley in Siberia: three IACTs of (10degx10deg), embedded in a 1km2 timing array with 120 detector stations. We present results obtained with the current setup (0.5km2 timing array with first IACT).

Speaker: Dr Ralf Wischnewski (DESY)

Slides taiga_ricap2018_wischnewski_fin_r.pdf

14:20 The science case for a Southern Wide field of view detector.

EAS arrays are wide field-of-view instruments able to monitor all the overhead sky with a close to 100% duty-cycle. Such a detectors are multimessenger observatories by definition allowing a combined study of photon and charged nuclei induced events. All EAS arrays presently in operation or under installation are located in the northern hemisphere. The scientific potential of a next-generation facility in the Southern Hemisphere will be presented and discussed.

Speaker: Giuseppe Di Sciascio (INFN Roma Tor Vergata)

Slides DiSciascio-RICAP2018-final.pdf

14:50 Ultra High Energy Neutrinos with Radio

The optical Cerenkov technique has been tremendously successful and has now measured astrophysical neutrinos up to ~10 PeV. At higher energies, the neutrino fluxes become so low that km^2 detection areas are not enough, and other techniques are needed to cover areas of order 100 km^2 or more. I will give an overview of searches for neutrino-induced showers at the highest energies using radio techniques. I will review complementary strategies for searching for neutrino-induced radio impulses that include viewing the Antarctic ice sheet from the stratosphere, searching from within the Antarctic ice sheet, and searching for the radio signature due to air showers from tau decay products. I will also touch on new ideas under development.

Speaker: Prof. Amy Connolly (Ohio State University)

Slides Connolly_RICAPr.pdf

15:30 → 16:00 Cosmology and CMBR measurements

Cosmology and CMBR measurements

Convener: Mr Juan Miguel Carceller (University of Granada, Spain)

15:30 Balloon-borne experiments for Cosmic Microwave Background studies

Stratospheric balloon experiments play a unique role in current Cosmic Microwave Background (CMB) studies. CMB research has entered a precision phase, harvesting the detailed properties of its anisotropy, polarization and spectrum, at incredible precision levels. These measurements, however, require careful monitoring and subtraction of local backgrounds, produced by the earth atmosphere and the interstellar medium. High frequencies (larger than 180 GHz) are crucial for the measurements of interstellar dust contamination, but are degraded by atmospheric emission and its fluctuations, even in the best (cold and dry) sites on earth. For this reason, new balloon-borne missions, exploiting long-duration and ultra-long duration stratospheric flights, are being developed in several laboratories worldwide. These experiments have the double purpose of qualifying instumentation and validating methods to be used on satellite missions, and produce at a relatively fast pace CMB science synergic to ground based CMB observatories. After a general discussion, I'll focus on the OLIMPO experiment (http://olimpo.roma1.infn.it), recently flown in a long duration flight in the Arctic, as a demonstrator of the power of these missions.

Speaker: Silvia Masi (ROMA1)

Slides Masi_balloons_02.pdf

16:00 → 17:00 Summary and Conference conclusion

16:00 Summary

Speaker: Dr Juan de Dios Zornoza (IFIC)

Slides RomeRICAP-sep18-summary.pptx