SciNeGHE 2016 High-energy gamma-ray experiments at the dawn of gravitational wave astronomy

18 Oct 2016, 08:00 → 21 Oct 2016, 19:35 Europe/Rome

11^th Workshop on Science with the New generation
of High Energy Gamma-ray Experiments

 

The 2016 edition of the SciNeGHE workshops will focus on the study of high-energy gamma-ray sources, including Gamma Ray Bursts, blazars, pulsars, supernova remnants, from a multiwavelength and multimessenger perspective. Particular attention will be given to the connections with gravitational waves, both from the observational and theoretical point of view.

Cosmic messengers, such as photons, neutrinos and cosmic rays, are the key to understand the physics of estreme astrophysical sources such as blazars, pulsars, supernova remnants, and mergers of neutron stars and/or black holes.

The first direct detection of gravitational waves from the merger of two massive black holes has inaugurated the era of gravitational wave astronomy and opened a new chapter in the multimessenger study of the Universe.

Space missions like Fermi, Swift, INTEGRAL and AGILE, and ground-based instruments like H.E.S.S., MAGIC, VERITAS and HAWC have revolutionized our view of the gamma-ray sky. They have discovered new populations of gamma-ray emitters and contributed to probe the high-energy acceleration and emission mechanisms at play in these sources. Furthermore, the second generation of ground-based interferometers like Advanced LIGO and Advanced Virgo, will add complementary informations to fully decypher the laws governing these intriguing and powerful cosmic sources.

Following the tradition of the SciNeGHE workshops, there will be updates on current and planned space-borne and ground-based gamma-ray experiments, and reviews on the status and results of cosmic ray, neutrino and gravitational wave detectors.

The workshop will be organized in plenary sessions of review and contributed talks and poster presentations.
Special attention will be given to contributions from Ph.D. students and young postdocs. In particular three Young Scientist SciNeGHE Awards of €500,00 each will be given to the best contributions by talented young researchers (Ph.D. students or young researchers within their 6 year of Postdoc).

During the workshop, there will be the opportunity to visit the Virgo interferometer at the European Gravitational Observatory (EGO) in Cascina, near Pisa.
 

The 11th edition of the SciNeGHE!

Thank you for attending this year's conference. We are hoping to seeing you during the 12th SciNeGHE edition in La Palma, Canary Islands, in 2018!

More information at scineghe2016@pi.infn.it

European Gravitational Observatory

Slides

• P1050615.JPG
• poster_scineghe2016-160dpi.pdf
• poster_scineghe2016.png
• poster_scineghe2016_96dpi.pdf
• scineghe2016_1st_announcement_v9.pdf
• scineghe2016_2nd_announcement_v1.pdf
• scineghe2016_3rd_announcement.pdf

Tuesday, 18 October

08:00 REGISTRATION

1 Welcome

2 Review Talk: gravitational wave astronomy: present,past,future

Speaker: Eugenio Coccia (ROMA2)

Slides Scineghe_Coccia.pdf

Session Ia: High-Energy experiments: reports and connections with Gravitational Waves

Convener: Luca Baldini (PI)

3 Searches for Gamma-ray Counterparts to Gravitational-Wave Sources with the Fermi Gamma-ray Space Telescope

A new era for astronomy has begun as the first detection of Gravitation Wave (GW) event arising from the coalescence of two stellar-mass Black Holes (BH) was announced by LIGO/VIRGO. Searches for electromagnetic (EM) counterpart of GW event is of fundamental importance, as it increases the confidence in the GW detection and helps characterize the parameters of the merger. The Fermi gamma-ray space telescope has the best sensitivity to simultaneously observe a large fraction of the sky from 10 keV to more than 300 GeV, providing the unique capability of rapidly covering the entire probability region from a LIGO candidate. In this talk, I will present the strategy for follow-up observations of GW event with the Fermi Large Area Telescope (LAT), focusing on the results from the first observing run O1, where LAT upper limits were reported. As advanced LIGO and VIRGO begin operations, we eagerly anticipate the detection GW in coincidence with a gamma-ray signal from the Fermi Gamma-ray Burst Monitor (GBM) and the LAT, likely from a short Gamma-Ray Burst (GRB) arising from the merger of two neutron stars or a black hole and a neutron star. Offline searches for weak GRBs that fail to trigger onboard Fermi indicate that additional short GRBs can be detected in the GBM data and dedicated analysis of LAT data can result in sub-threshold detections that can greatly improve our knowledge of the source of GW event and affect follow-up strategies for counterpart searches by other observatories.

Speaker: Dr Nicola Omodei (Stanford University/KIPAC)

Slides Omodei_Fermi_GW.pdf

4 AGILE observations of Gravitational Wave events

We will present the AGILE capabilities to detect the electromagnetic counterparts of Gravitational Wave (GW) sources recently discovered by LIGO. The follow-up of the events discovered so far and the perspective for future discoveries will be discussed. The combination of Tracker, miniCalorimeter, Anti Coincidence as a gamma-ray imager, makes the AGILE-GRID an optimal instrument for follow-up observations of large localization regions of GW sources. This can be achieved thanks to the following characteristics: 1) a very large FoV (2.5 sr), 2) an accessible sky of about 80% every 7 minutes with a sensitivity of 10-8 erg cm-2 s-1 at E > 30 MeV on ~ 100 s, 3) sub-millisecond trigger for very fast events detectable by MCAL in the range 0.4-100 MeV. In addition to them, the improved localization capability (2-3 arcmin) expected to be provided by the reactivation of the hard X-ray monitor, SuperAGILE.

Speaker: Dr Immacolata Donnarumma (INAF-IAPS)

Slides Donnarumma_Scineghe2016_last.pptx

10:45 Coffee Break

5 Recent results with Fermi GBM

The Fermi Gamma-ray Burst Monitor (GBM) is an all-sky, hard X-ray/soft gamma-ray monitor, ideally suited to detect rare and unpredictable transient events. In the first eight years since the launch of Fermi in 2008 it has triggered on more than 5000 transients, including nearly 1900 gamma-ray bursts (GRBs), many solar flares, bursts from magnetars, and terrestrial gamma-ray flashes (TGFs). Dedicated offline searches over all or parts of the mission have yielded many bursts, non-impulsive steady or variable emission from numerous Galactic sources. Fermi GBM is also an excellent partner in the search for electromagnetic counterparts to gravitational-wave events detected by LIGO/Virgo. The talk will give an overview of recent GBM results, with particular emphasis on the EM follow-up of gravitational-wave events

Speaker: Dr Andreas von Kienlin (MPE)

Slides AvKienlin_SciNeGHE-PisaOct16.pdf

6 INTEGRAL Highlights and perspectives for EM follow-up of Gravitational-Wave and HE Neutrino events

ESA’s INTEGRAL Space Observatory was launched on 17 October 2002 from the Baikonur Cosmodrome (Kazakistan) aboard a Proton rocket as part of the Russian contribution to the mission. To date the spacecraft, ground segment and scientific payload are in excellent state-of-health, and INTEGRAL is continuing its scientific operations. In view of its 14 years successful science outcome, ESA is considering its extension till 2018-2020. INTEGRAL has so far produced an unprecedented harvest of results in the soft gamma-ray band, ranging from the inventory of 1000 energy sources (Bird, et al., APJS, 2015), to the discovery of hundreds of variable soft gamma-ray sources, the mapping of the Aluminium and 511 keV annihilation line in the Galaxy, the evidence of polarized gamma ray emission from the Crab Nebula, strong Gamma-ray burst and the galactic BH Cyg X-1, the first detection of nuclear lines from SN2014J and the detailed study of the high energy emission from the galactic microQSO V404. More recently, INTEGRAL has successfully observed with its All-Sky Monitors SPI-ACS and IBIS-VETO the sky counterpart of the LIGO-VIRGO triggers from GW150914 (V. Savchenko, et al., ApJL, 820, L36, 2016, Abbott, et al, 2016, ApJL, 826, L13, 2016, Abbott, et al, 2016, ApJS, 225, 1, pp8, 2016) and LTV151012, with no evidence of contemporary signals. Similar type of observation has been performed for the EHE Neutrino events IceCube 160806A (GCN 19789) and IceCube-HESE 128340. Following this successful results INTEGRAL has now a better reaction time to perform ToO observations correlated with the above mentioned triggers. This is particularly important in view of the LIGO-VIRGO O2 observations starting soon. This paper summarizes the current INTEGRAL scientific achievements and future prospects, with particular regard to the so called “New astronomies”, i.e. Gravitational Wave and High Energy Neutrinos counterpart search.

Speaker: Dr Pietro Ubertini (ROMA2, IAPS-INAF)

7 Multimessenger astronomy with Swift: results and prospects.

With the recent discoveries of astrophysical neutrinos by IceCube, and Gravitational Waves by Advanced LIGO, we live on the cusp of a new era of astronomical research. Combining these messengers with EM data is vital to maximise the scientific gain, but is challenging. The large position uncertainties, particularly from Gravitational Wave detections, make follow-up difficult, and the chances of finding 'contaminating' transients unrelated to the trigger event non-neglible. In this review, I summarise the results obtained to date by X-ray follow up of neutrino and Gravitational Wave events with the Swift satellite. I also discuss the prospects for the future, particularly optimisations that can be made by EM team to take advantage of the extra information the LIGO team will be providing in their "O2" observing run.

Speaker: Dr Philip Evans (University of Leicester)

Slides Evans_SciNeGHE.pdf

8 A new measurement of cosmic-ray electrons and positrons with the Large Area Telescope

We present an updated measurement of the cosmic-ray electron and positron spectrum between 7 GeV and 2 TeV, based on 7 years of data collected with the Fermi Large Area Telescope (LAT). The LAT is the first space-based instrument to directly explore the region above 1 TeV. At such high energies, the shape of the spectrum can provide useful information about the origin and propagation of cosmic-ray electrons in the nearby Galactic space. The best fit to the spectrum that we measure is given by a broken power-law, with the break located at 53±8 GeV. Such break, however, is not significant when all the systematic uncertainties are taken into account. Above 50 GeV our data are well described by a single power law with a spectral index of 3.07 ± 0.02 (stat + syst) ± 0.06 (energy scale). An exponential cutoff lower than 1.7 TeV is excluded at 95% CL.

Speaker: Mr Alberto Manfreda (Università di Pisa, INFN sezione di Pisa)

Slides Manfreda_Scineghe2016.pdf

9 DAMPE: a Gamma and Cosmic Ray Observatory in Space

DAMPE (DArk Matter Particle Explorer) is one of the five satellite missions in the framework of the Strategic Pioneer Research Program in Space Science of the Chinese Academy of Sciences (CAS). Launched on December 17th 2015 at 08:12 Beijing time, it is taking data into a sun-synchronous orbit, at the altitude of 500 km. The main scientific objective of DAMPE is to detect electrons and photons in the range of 5 GeV-10 TeV with unprecedented energy resolution, in order to identify possible Dark Matter signatures. It will also measure the flux of nuclei up to 100 TeV with excellent energy resolution. The satellite is equipped with a powerful space telescope for high energy gamma-ray, electron and cosmic rays detection. It consists of a plastic scintillator strips detector (PSD) that serves as anti-coincidence detector, a silicon-tungsten tracker (STK), a BGO imaging calorimeter of about 31 radiation lengths, and a neutron detector. With its excellent photon detection capability and its detector performances (at 100 GeV energy resolution ~1%, angular resolution ~0.1°), the DAMPE mission is well placed to make strong contributions to high energy gamma-ray observations: it covers the gap between space and ground observation; it will allow to detect a line signature in the gamma-ray spectrum, if present, in the sub-TeV to TeV region; it will allow a high precision gamma-ray astronomy. A report on the mission goals and status will be presented, together with in-orbit first data coming from space.

Speaker: Domenico D'Urso (ROMA2)

Paper durso.tar

Slides dampe_ddurso_schineghe2016.pdf

13:10 Lunch

Session Ib: High-Energy experiments: reports and connection with Gravitational Waves

Convener: Alessandro De Angelis (PD)

10 Recent Results from the HAWC Observatory

The High-Altitude Water Cherenkov Observatory (HAWC) is a TeV gamma-ray detector located at an altitude of 4,100 meters on the slope of the Sierra Negra volcano in Puebla, Mexico. Inaugurated in March 2015, HAWC observes 65% of the sky every day with more than 90% duty cycle and an excellent angular resolution. HAWC plays an important role as a survey instrument for multi-wavelength studies, and presently is the most sensitive instrument to detect transients and extended sources of gamma-rays at multi-TeV energies. In this talk I will present the recent results from the experiment and discuss the future goals of the collaboration.

Speaker: Dr Francisco Salesa Greus (IFN-PAN)

Slides Salesa_Pisa_final.pdf

11 Current status and recent results from H.E.S.S.

The High Energy Stereoscopic System (H.E.S.S.) is an array of Imaging Atmospheric Cherenkov Telescopes (IACTs) located in the Khomas Highland of Namibia. The array initially consisted of four 12 m telescopes, operating as a single stereoscopic system. A decade of H.E.S.S. observations yielded a vast array of discoveries which now form the heritage of the very-high-energy (VHE) gamma-ray astronomy. This includes the H.E.S.S. Galactic Plane Survey, which provided a systematic scan of the Galactic disk with a ∼ 2% Crab Nebula point-source sensitivity and a ~ 0.1 deg angular resolution, spectral and morphological studies of Supernova Remnants, Pulsar Wind Nebulae, observations of fast variability in blazars, gamma-ray binaries, constraints on the Extragalactic Background Light, and other important results. In 2012, a fifth telescope, with a 28 m mirror, was added in the center of the array, marking the start of H.E.S.S. Phase II. The new telescope, dubbed CT5, potentially extends the energy range covered by H.E.S.S. down to ∼ 30 GeV. Such an extension of the instrument's energy range is particularly beneficial for studies of transient phenomena and variable sources with soft spectra, such as Gamma-Ray Bursts (GRBs) and Active Galactic Nuclei (AGNs) located at high redshifts (> 0.5), as well as gamma-ray pulsars. The cameras of the 12 m telescopes are currently being upgraded to improve the data taking efficiency and optimize the array performance at low energies. We will present the current status of H.E.S.S. and its recent results, including the H.E.S.S. II observations of the Vela pulsar and several AGNs, as well as the famous discovery of the Galactic Centre "Pevatron", observations of the Large Magellanic Cloud, and new VHE source discoveries from the H.E.S.S. Galactic Plane Survey. We will also discuss the potential of H.E.S.S. to detect possible gamma-ray counterparts of gravitational waves.

Speaker: Dmitry Zaborov (LLR - Ecole Polytechnique)

Slides zaborov_SciNeGHE_2016.pdf

12 MAGIC highlights: An instrument for cosmic-ray and gamma-ray astroparticle physics at the TeV scale

MAGIC is an instrument composed of a pair of telescopes for gamma-ray and cosmic-ray astrophysics in the TeV range. It is operating for more than a decade now, and is one of the current best performing instruments in this field, specifically at low energies, where it achieves the largest sensitivity among current installations of this kind. MAGIC pursues a strong program in galactic and extragalactic gamma-ray science. Its catalog of blazar, radiogalaxy and galaxy clusters observations as well as supernovae, novae, pulsar wind nebulae, pulsars and binary systems has now increased to several tens of detected targets, and will be critically reviewed and discussed in this contribution. In addition, MAGIC has a strong fundamental physics program, with searches for particle dark matter, Lorentz Invariance violations, axion-like particles and primordial black hole evaporation, providing important recent constraints in some relevant cases. Finally, MAGIC is suited for cosmic ray searches, being sensitive to the signatures of earth-skimming tau-neutrinos, cosmic antiprotons, and others. The basic instrumental features and challenges will also be presented. A discussion about the future of the instrument will be made in the closing remarks.

Speaker: Michele Doro (PD)

Slides doro_2016_scineghe_web.pdf

13 Recent Highlights from VERITAS

VERITAS is an array of four 12-m imaging atmospheric-Cherenkov telescopes, sensitive to very-high-energy (VHE; >100 GeV) gamma rays. Ground-based VHE instruments like VERITAS provide powerful means to probe into astrophysics problems including the particle acceleration and radiative processes in both Galactic and extragalactic sources, cosmological problems such as the history of galaxy formation and primordial black hole evaporation, and fundamental physics topics such as potential decay/annihilation products from dark matter, or Lorentz-invariance violation. In this talk, I will review the status of VERITAS operations, our collaboration with multi-wavelength and multi-messenger partners, and some of our recent results.

Speaker: Qi Feng (McGill University)

Slides QF_VERITAS_Scineghe16.pdf

16:10 Coffee break

14 LATTES: a new window into very high energy gamma rays

The Large Array Telescope for Tracking Energetic Sources ( LATTES ) is a novel hybrid detector concept for the measurement of Extensive Air Showers (EAS) generated by Very High Energy Gamma rays. The aim of the detector is to have a good sensitivity at low energies (~100 GeV) extending into the TeV region, operating day and night with a wide field of view. The experiment is planned to be installed in South America at high altitude (~5.000m), such that it will be complementary to the Cherenkov detectors which are planned to be installed at that part of the world. LATTES will be a powerful tool to trigger further observations of variable sources and to detect transients phenomena.

Speaker: Dr Bernardo Tomé (LIP - Laboratório de Instrumentação e Física Experimental de Partículas)

Paper BernardoTome.tar

Slides LATTES

15 The Pierre Auger Observatory ultra-high energy neutrinos follow-up of the LIGO gravitational-waves events.

In early 2016 the LIGO and Virgo collaborations reported the breakthrough observation of the first gravitational-wave transient with the twin detectors of Advanced LIGO in September 2015 (event GW150914), followed three months later by the detection of GW151226. Both events are produced by the coalescence of black holes. Although no electromagnetic emission is generally expected from such events, in presence of magnetic fields and debris from the formation of black holes, radiation of ultra-high energy (UHE) neutrinos might be possible and, if detected, could help constraining the direction of the source of the events. The Pierre Auger Observatory is capable of identifying air-shower events initiated by ultra-high energy neutrinos, using the data from its 3,000 km^2 surface grid of water Cherenkov detectors. The emission of neutrinos with energy > 100 PeV can be detected from point-like sources contained in the equatorial declination band between -65 and +60 degrees, including a portion of the 90% CL inferred position for GW150914 and GW151226. A search for neutrinos in temporal proximity with the GW events (and for the GW candidate event LVT151012) was performed, with time windows of +/- 500 s around ("coincidence") and 1 day after ("afterglow") the gravitational-wave events. Constraints to the energy radiated in UHE neutrinos are derived from the detection of no neutrinos in the search windows.

Speaker: Carla Bleve (LE)

Paper carla_bleve.tar.zip

Slides Bleve_SchiNeGHE16.pdf

16 HARPO: 1.7 - 74 MeV gamma-ray beam validation of a high-angular-resolution high-polarisation-dilution gas telescope and polarimeter

A number of groups are developing pair-conversion detector technologies alternative to the tungsten-converter / thin-sensitive-layer stacks of the COS-B / EGRET / Fermi-LAT series, to improve the single-photon angular resolution. Presently observers are almost blind in the 1-100 MeV energy range, mainly due to the degradation of the angular resolution of e+e- pair telescopes at low energies: to a large extent, the sensitivity-gap problem is an angular-resolution issue. I will show that gas detectors such as TPCs (time projection chambers) can enable an improvement of up to one order of magnitude in the single-photon angular resolution (0.5° @ 100 MeV) with respect to the Fermi-LAT (5° @ 100 MeV), a factor of three better than what can be expected for Silicon detectors (1.0-1.5° @ 100 MeV). With such a good angular resolution, and despite a lower sensitive mass, a TPC can close the sensitivity gap at the level of 10^{-6} MeV/(cm2 s) between 3 and 300 MeV. In addition, the single-track angular resolution is so good that the linear polarisation fraction and angle of the incoming radiation can be measured. I will describe the fast-gas (low pile-up), cool-gas (low-diffusion), high pressure (0.5-4 bar) HARPO detector prototype and the results of its high-statistics characterisation in the 1.7-74 MeV fully-polarised or non-polarised gamma-ray beam provided by the BL01 line at NewSUBARU. The excellent value of the polarisation asymmetry dilution factor that we measured paves the way to the opening of the polarimetry window in the MeV-GeV energy range. I will end this talk with the presentation of the balloon-flight prototype ST3G (Self-triggered TPC for Space gamma-ray Telescope, pronounced STEG) the design of which is in progress, and of its expected performance.

Speaker: Dr Denis Bernard (LLR Ecole Polytechnique)

Paper DenisBernard.tar

Slides SciNeGHE_HARPO_DBernard.pdf

17 CHARACTERISATION AND COMPARISON OF EVENT GENERATORS FOR PAIR CONVERSION: A CRUCIAL STEP FOR FUTURE LOW ENERGY GAMMA TELESCOPE

Gamma ray astronomy suffers from a sensitivity gap between 0.1 and 100MeV. The lower end can be covered by improved Compton telescopes, while the higher end needs to use photon conversion to electron-positron pairs. With high angular resolution for the electrons, it will also be possible to probe the linear polarisation of the photons. There is a fierce competition to build high sensitivity pair telescopes for this energy range, with electron tracking technologies such as: silicon (e-ASTROGAM, Compair, PANGU), gas (HARPO, Adept), or nuclear emulsions (GRAINE). An accurate simulation is necessary to correctly design and compare these detectors. I will establish baseline distributions of key kinematic variables as simulated by a Bases/Spring-based, 5D, exact down to threshold, and polarised event generator. I will compare them to simulations with the low energy electromagnetic models available in Geant4 (in particular G4PenelopeGammaConversion, G4LivermoreGammaConversionModel, and G4LivermorePolarizedGammaConversionModel) and with EGS5. I will focus in particular on the effects of the recoil momentum of the nucleus, which is often neglected and becomes a dominant effect at low energies. I will show that different generators give a different picture of the optimal angular resolution of pair telescopes. I will also show that, of all the simulations we used, only the full 5D generator describes accurately the angular asymmetry in the case of polarised photons.

Speaker: Dr Philippe Gros (LLR, Ecole Polytechnique)

Paper SciNeGHE2016_Gros.tgz

Slides 2016-10-17_SciNeGHE_Generators_Gros.odp 2016-10-17_SciNeGHE_Generators_Gros.pdf

Wednesday, 19 October

08:15 Bus departure to EGO

Meeting point: Largo Bruno Pontecorvo, 3. In front of the Physics Department

Gravitational Waves and the other messengers

Conveners: Dr Barbara Patricelli (PI), Giancarlo Cella (PI)

18 Welcome to EGO

19 Status of Advanced LIGO

Speaker: Daniel Hoak (PI)

Slides Hoak.pdf

20 ADVANCED VIRGO FIRST LIGHT

Advanced Virgo, the project designed to make Virgo 10 times more sensitive, has finally been completed. The light is circulating in the arms and the detector is being commissioned, with the goal of joining the two LIGOs in the next observation run in early 2017. The story of the project, the main technology aspects and the short and mid-term perspectives are reviewed in this talk.

Speaker: Giovanni Losurdo (PI)

Slides Losurdo.pdf

21 The LVC EM follow-up program

Speaker: Maria Giuliana Stratta (FI)

Paper author_stratta.tar

Slides Stratta.pdf

22 A 3rd generation GW observatory: Einstein Telescope

The detection of the GW emitted by the coalescence of a two black hole binary system, disclosed the new era of the GW astronomy. Advanced detectors will allow the detection of several GW sources, but to evolve toward the precision astronomy and astrophysics are needed new observatories with improved sensitivities and challenging performances. In this talk the path toward the realisation of the 3rd generation of GW observatories and the details of the Einstein Telescope project will be described.

Speaker: Michele Punturo (PG)

Slides Punturo_ET-talk-Scineghe2016.pptx

11:00 Coffee Break

23 The first steps towards observing gravitational waves from space with LISA

The Laser Interferometer Space Antenna or LISA is a future ESA satellite mission to observe mill-Hertz gravitational waves originating from extreme events such as the merger of supermassive black holes. Gravitational waves will be measured as they pass through a million-km arm-length interferometer whose test masses are perfectly free-falling through space. The technology demonstration mission LISA Pathfinder was launched in December 2015 to demonstrate the unprecedented level free-fall required for such an observatory. I will present the results from the first months of LISA Pathfinder measurements and their consequences for the performance of LISA.

Speaker: Dr Peter Wass (Imperial College London)

Slides Wass_SciNeGHE2016.pptx

24 Modeling gravitational waves from compact-object binaries

The direct observation and characterization of gravitational waves from binary black-hole mergers by LIGO is a testament to the crucial role played by waveform modeling in these discoveries. I will review recent developments in the field, discussing both numerical and analytical approaches to the problem of compact-object binaries and their gravitational-wave emission.

Speaker: Mr Andrea Taracchini (Max Planck Institute for Gravitational Physics)

Paper Taracchini_Andrea.zip

Slides Taracchini_SciNeGHE.pdf

25 Sifting the Gravitational-Wave Universe via Multimessenger Astronomy: Forthcoming Prospects for Continuous-Wave detection

The upgrade of worldwide gravitational-wave network has led to the first transient gravitational-wave detection, which has started to hone the comprehension we have about our Universe, and some of its constituents. A broader picture would be however provided by the detection of continuous-wave signals, which could be more easily achieved by exploiting the synergy with multimessenger Astronomy. Thanks to electromagnetic observations we may indeed be able to know, with enough accuracy, the sky location, rotational and/or orbital parameters of a broad class of rapidly-rotating neutron stars. This would allows us to perform a multitude of targeted and directed continuous-wave searches, and would facilitate narrow-band searches for the same class of signals. I will describe the prospects for detecting continuous gravitational waves by especially employing novel strategies for neutron stars in binary systems directed to sources whose parameters have been electromagnetically estimated. Employing those methods to analize data from the ever-more-sensitive advanced detectors will remarkably increase the chances of a continuous wave detection.

Speaker: Paola Leaci (ROMA1)

Paper cimento_paper_PLeaci.zip

Slides Paola_Leaci_Scineghe_PI_2016.pdf

26 Strategy for signal classification to improve data quality for Advanced Detectors gravitational-wave searches

Noise of non-astrophysical origin contaminates science data taken by the Advanced Laser Interferometer Gravitational-wave Observatory and Advanced Virgo gravitational-wave detectors. Characterization of instrumental and environmental noise transients has proven critical in identifying false positives in the first aLIGO observing run O1. In this talk, we present three algorithms designed for the automatic classification of non-astrophysical transients in advanced detectors. Principal Component Analysis for Transients (PCAT) and an adaptation of LALInference Burst (PC-LIB) are based on Principal Component Analysis. The third algorithm is a combination of a glitch finder called Wavelet Detection Filter (WDF) and machine learning techniques for classification.

Speaker: Elena Cuoco (EGO and INFN PI)

Paper elena_cuoco.tgz

Slides Cuoco.pdf

12:50 Lunch

Other messangers: neutrinos

Convener: Antonio Marinelli (PI)

27 Potential candidates for the astrophysical neutrino signal measured by IceCube experiment and the role of GRBs

During the last years the IceCube collaboration has detected the largest astrophysical neutrino sample ever obtained up to few PeV energies. The origin of these events encourage the astroparticle community and several hypotheses are now under debate. Based on temporal and spatial correlations, we explore some potential TeV gamma-ray (galactic and extragalactic) sources to explain some events. In addition, we show a possible theoretical scenario to explain the observed astrophysical neutrino events in the gamma-ray bursts (GRB) scenario

Speaker: Dr Nissim Fraija (IA-UNAM)

Slides Talkpisa_Nfraija.pdf

28 Results from IceCube

Speaker: Thorsten Glüsenkamp (DESY)

Slides pisa_scinighe_oct19_2016_gluesenkamp.pdf

29 High-energy neutrino searches in the Mediterranean Sea: ANTARES results and KM3NeT/ARCA perspectives

A primary goal of neutrino telescopes is the search for astrophysical neutrinos in the TeV-PeV range. This covers generic searches for any diffuse cosmic neutrino flux as well as more specific searches for astrophysical sources such as AGN and GRBs or close-by Galactic sources. The first generation, ANTARES, has been running in its final configuration since 2008. It is today the largest neutrino telescope in the Northern hemisphere. After the discovery of a cosmic neutrino diffuse flux by the IceCube, the understanding of its origin has become a key mission in high-energy astrophysics. ANTARES makes a valuable contribution thanks to its excellent angular resolution in both the muon channel and the cascade channel (induced by all neutrino flavors). The ANTARES sensitivity is sufficient to constrain the origin of the IceCube excess from regions extended up to 0.2 sr in the Southern sky. Assuming various spectral indexes for the energy spectrum of neutrino emitters, the Southern sky and in particular central regions of our Galaxy are studied searching for point-like objects and for extended regions of emission. By adopting a multi-messenger approach, based on time and/or space coincidences with other cosmic probes, the sensitivity of such searches can be considerably augmented. As an example of the various multi-messenger searches, ANTARES has participated, with IceCube, to a high-energy neutrino follow-up of the gravitational wave signal GW150914, providing the first constraint on high-energy neutrino emission from a binary black hole coalescence. ANTARES has also performed indirect searches for Dark Matter, yielding limits for the spin-dependent WIMP-nucleon cross-section that improve upon those of current direct-detection experiments. The successor of ANTARES in the Mediterranean abysses is KM3NeT. KM3NeT is a distributed research infrastructure hosting a km-scale neutrino telescope for high-energy neutrino astronomy, ARCA, offshore Capo Passero in Italy and a megaton scale detector for the determination of the neutrino mass hierarchy with atmospheric neutrinos, ORCA, offshore Toulon in France. Recently, the first ARCA detection strings have been deployed and preliminary results will be presented. The latitude of KM3NeT-ARCA will allow for a wide coverage of the sky with optimal sensitivity to the region of the Galactic Centre. The expected sensitivity of the complete KM3NeT/ARCA detector will allow the observation of the IceCube flux in less than a year, providing new information on its origin, energy spectrum and flavor composition. After five years, KM3NeT/ARCA could also give indications at more than 3-sigma level on some Galactic sources.

Speaker: Maurizio Spurio (BO)

Paper Spurio-ANTARES.zip

Slides SciNeGhe-Spurio-2016-ANTARES.pptx

30 Galactic diffuse neutrino component in the astrophysical excess measured by the IceCube experiment

The Galaxy is a guaranteed source of neutrinos produced by the interaction of cosmic rays (CR) with the interstellar gas. According to conventional CR propagation models, however, this emission may be too weak to be detected even by Km^3 scale neutrino telescopes. This belief has been questioned by recent Fermi-LAT results which showed that the CR spectrum in the inner Galactic plane is significantly harder than that inferred from local CR measurements. I will show that a phenomenological model adopting a spatial dependent CR diffusion coefficient, which accounts for that feature and reproduces the gamma-ray excess found by Milagro at 15 TeV, predicts a significantly larger Galactic neutrino emission. I will compare the prediction of this models with ANTARES and IceCube results and discuss the perspectives of KM3NeT.

Speaker: Dario Grasso (PI)

Paper Grasso_neutrino.tar.gz

Slides Grasso_Scineghe16.pdf

31 Astroparticle and neutrino oscillation research with KM3NeT

KM3NeT, located in the abysses of the Mediterranean Sea, is a distributed research infrastructure that will host a km3-scale neutrino telescope (ARCA), offshore from Capo Passero in Italy, for high-energy neutrino astronomy, and a megaton scale detector (ORCA), offshore from Toulon in France, for the determination of the neutrino mass hierarchy. The ORCA array is optimised for the study of atmospheric neutrinos in the energy range 3-30 GeV. Physics studies demonstrate that the neutrino mass ordering can be determined with a significance of 3-7 sigma (depending on the true value of the hierarchy and the value of mixing angle sinθ23) after three years of operation. The ARCA detector is aimed for the high energy neutrino astronomy. It should provide a measurement of the diffuse neutrino cosmic flux recently discovered by IceCube in a complementary part of the sky and test several possible origins. ARCA's location allows for surveying most of the Galactic Plane, including the Galactic Centre and the most promising source candidates (SNR RJ1713, Vela X) as well as the Fermi Bubbles. The future KM3NeT participation in multi-messenger programs will exploit the high connection between neutrinos and other cosmic messengers: electromagnetic signals, from X-rays to high energy gamma-rays, charged cosmic rays, gravitational waves. Moreover, both KM3NeT detectors are sensitive to the lower energy neutrinos from the supernova explosions by observing the global light rate increase in the detector. Finally, they both can also look for neutrinos produced by the co-annihilation of Dark Matter particles; in the case of spin-dependent WIMP-nucleon cross section, the expected ORCA sensitivity is one of the best in the WIMP mass range of 10-100 GeV.

Speaker: Mr Vladimir Kulikovskiy (CPPM/CNRS)

Paper km3net_kulikovskiy.tar.gz

Slides KM3NeT_CONF_WD2016_008_ScinNeGHE_Kulikovskiy_v7.pdf

16:30 Visit to the Virgo interferometer

Thursday, 20 October

Gamma-ray sources and connections with Gravitational Waves

Convener: Dr Nicola Omodei (Stanford University/KIPAC)

32 Gravitational waves transients : Sources and Searches

Gravitational waves transient signals can be classified broadly as compact binary coalescence (CBC) and generic short and long duration transients (bursts), the search techniques/algorithms for them differs on various levels and hence the background and sensitivity for both these searches are quite different, however even when they target different sources, they are not completely mutually exclusive of each other, this means the same source can be captured by both CBC and bursts searches but not always. In the present talk I will present a broad overview of these searches and discuss the expectations and prospects of these searches in the era of advanced interferometers. Moreover VIRGO detector in Italy is expected to join soon the LIGO detectors in the U.S. improving the sky localisation of the further observed signals, so coming time is exciting for multi-messenger astronomy with gravitational waves.

Speaker: Shubhanshu Tiwari (TIFP)

Slides Scinghe_16.pdf

33 GRBs as multimessenger sources

Speaker: Giacomo Vianello

Slides Vianello.pdf

34 Exploring the Gravitational-Waves Universe with THESEUS

The Transient High Energy Sky and Early Universe Surveyor (THESEUS) is a mission concept under development by a large international collaboration aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and monitoring the X-ray sky with an unprecedented combination of deep sensitivity and large field of view. These goals will be achieved through a unique combination of instruments allowing GRBs and X-ray transients detection and arcmin localization over a broad FOV (more than 1sr) and an energy band extending from several MeVs down to 0.3 keV with unprecedented sensitivity, as well as on-board prompt (few minutes) follow-up with a 0.6m class IR telescope with both imaging and spectroscopic capabilities. THESEUS is thus perfectely suited for detecting, locating and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late ‘20s / early ‘30s by next generation facilities like aLIGO/aVirgo, eLISA, KAGRA, ILIGO, Einstein Telescope, Cosmic Explorer. If selected within the ESA/M5 programme, the launch of THESEUS will coincide with a golden era of multi-messenger astronomy, to which this mission will provide a fundamental contribution. The detection of EM counterparts of GW (or possibly neutrino) signals will enable a multitude of science programmes (e.g. Bloom et al. 2009; Phinney 2009) by allowing for parameter constraints that the GW/neutrino observations alone cannot fully provide. For example, finding a GW/neutrino source EM counterpart in X-rays with THESEUS/SXI, will allow to localize the source with an accuracy good enough for optical follow-up and hence to possibly measure its redshift and luminosity. On the other hand, not finding an EM counterpart will constrain merger types (such as BH-BH mergers), emission mechanisms, astrophysical conditions at the time of merger, and total energetics.

Speaker: Dr Lorenzo Amati (INAF - IASF Bologna)

Slides amati_scineghe16.pdf

35 Prospects for joint GW and high-energy EM observations of BNS mergers

With the recent detection of two transient gravitational wave (GW) signals by the Advanced LIGO interferometers the era of GW astronomy has begun. The two events, labeled GW150914 and GW151226, are both consistent with the inspiral and the merger of a binary system of black holes (BBH). In the next years the 2nd generation interferometers will increase their sensitivity: many other GW events are expected to be detected, expanding the frontiers of the multimessenger investigations of the universe. Besides the merger of BBH systems, one of the most promising candidates for the direct GW detection is the coalescence of binary neutron stars (BNS) and black holes (NSBH). These mergers are thought to be connected with short Gamma Ray Bursts (GRBs), that are among the most energetic events in the universe, but a definitive probe of this association is still missing. Combined observations of gravitational and electromagnetic (EM) signals from these events will provide an unique opportunity to unveil the progenitors of short GRBs and study the physics of compact objects. In particular, large field-of-view instruments such as Fermi will be crucial to observe the high-energy electromagnetic counterparts of transient gravitational wave signals and provide a robust identification based on a precise sky localization. We will present the prospects for joint GW and high-energy EM observations of merging binary systems with Advanced LIGO and Virgo and with Fermi, focusing on BNS.

Speaker: Dr Barbara Patricelli (PI)

Slides Patricelli-SciNeGHE2016.pdf

36 Prospects for Gamma-Ray Bursts detection by the Cherenkov Telescope Array

The Large Area Telescope (LAT) on the Fermi satellite is expected to publish a catalogue with more than 100 Gamma-Ray Bursts (GRBs) detected above 100 MeV thanks to a new detection algorithm and a new event reconstruction. This work aims at revising the prospects for GRB alerts with the Cherenkov Telescope Array (CTA) based on the new LAT results. We start considering the simulation of the observations with the full CTA of two extremely bright events, the long GRB 130427A and the short GRB 090510, then we investigate how these GRBs would be observed by different subsamples of the array pointing to different directions, namely adopting the CTA "coupled divergent" mode.

Speaker: Elisabetta Bissaldi (BA)

Paper BISSALDI_PROCEEDINGS_Scineghe_Talk_GRB.zip ProcSciNeGHE_POSTER_BISSALDI.zip

Slides Bissaldi_CTAGRB_Scineghe_161020_v4.pdf

10:50 Coffee break

Gamma-ray sources and connections with Gravitational Waves

Conveners: Dr Barbara Patricelli (PI), Francesco Longo (TS), Massimiliano Razzano (PI)

37 The search for continuous gravitational waves in LIGO and Virgo data

The detection of continuous gravitational waves is among the main targets of the LIGO and Virgo detectors. Such kind of signals, emitted e.g. by spinning neutron stars asymmetric with respect to the rotation axis, are very weak and their search poses challenging data analysis problems. In this talk I will discuss the main issues regarding the search of continuous gravitational waves in the data of current interferometric detectors, some recently published results, and what are the future prospects.

Speaker: Cristiano Palomba (ROMA1)

Paper palomba_scineghe2016.zip

Slides cw_palomba_scineghe2016.pdf

38 Latest results on gamma-ray pulsars

The Fermi Large Area Telescope (LAT) has been scanning the gamma-ray sky since 2008. The number of pulsars detected by the LAT now exceeds 200, making them by far the largest class of Galactic gamma-ray emitters. I will present some of the latest pulsar discoveries made by the LAT, describe the properties that make some of these systems unique and discuss them in the context of current pulsar emission models.

Speaker: Dr Pablo Saz Parkinson (The University of Hong Kong)

Paper Saz_Parkinson_scineghe16.tar.gz

Slides Saz_Parkinson_Scineghe_161020.pdf

39 Prospects of continuous gravitational waves searches from Fermi-LAT sources

Non-axisymmetric spinning Neutron Stars are expected to be sources of continuous gravitational waves. Only a small fraction of the total number of neutron stars believed to exist in the Galaxy is observed through their electromagnetic emission. This number steadily increasing recently, thanks to the Fermi-Large Area Telescope and to radio surveys. The Fermi-Large Area Telescope catalogue contains several potentially interesting sources for gravitational wave searches, such as supernova remnants and the "unassociated" sources. In order to look for continuous gravitational signals a knowledge of the NS parameters, i.e rotational frequency and position, is needed. Depending on the degree of accuracy with which these parameters are known, several types of search can be performed. In this talk I will discuss the perspectives and considerations of continuous gravitational wave searches for Fermi-LAT sources, including the astrophysical information that we can derive from a detection or even from upper limits.

Speaker: Simone Mastrogiovanni (R)

Paper simone_mastrogiovanni.zip

Slides Mastrogiovanni_scineghe.pdf

40 The black hole binary model of OJ 287 as witness of the validity of the General Relativity

A peculiar and controversial phenomenology is the periodicity of AGN. This can be related to the indirect search for close supermassive black holes (SMBHs) at sub-parsec separation. A representative case study with multifrequency radio-optical and X-ray data, for example by XMM-Newton, Kepler, and Swift, is presented; namely the X-ray and gamma-ray BL Lac object OJ 287. This is one of the best monitored blazars since about 20 years, with historical optical data dating back to more than 100 years. The last two observing multifrequency campaigns of 2004-2007, organized as the campaign manager, and of 2015-2016, co-organized, allowed to put some indirect tests of the General Relativity (GR), using calculations with three-body problem theory and Post-Newtonian expansion in strong gravitational fields and the timing and clocking given by the light curves and variability of the observed flux. These tests are made under the, debated, assumption that the driving physical model for OJ 287 is an inspiralling binary SMBH system with masses of the order of 10^10 M_sun and 10^8 M_sun and <0.1pc separation, under the action of low frequency gravitational radiation.

Speaker: Dr Stefano Ciprini (ROMA2)

Slides SCiprini_OJ287binarySMBHs_PisaOct2016_V3.pdf

41 The empirical grounds of SN-GRB connection

I will review the status of the SN-GRB connection. Present data suggest that SNe associated with GRBs form a heterogeneous class of objects including both bright and faint Hypernovae. Finally I’ll discuss the empirical estimate of the ratio GRB/SNe-Ibc, to be in the range ∼0.4%-3%.

Speaker: Prof. Massimo Della Valle (Capodimonte Astronomical Observatory, INAF-Naples)

Slides DellaValle.pdf

13:10 Lunch

Gamma-ray sources and connections with Gravitational Waves

Convener: Francesco LONGO

42 GW stochastic background

Speaker: Giancarlo Cella (PI)

Paper proceeding.tar.gz

Slides Cella.pptx

43 High and very-high energy gamma-ray observations of the Milky Way

Observations of the gamma-ray emission from the Milky Way have significantly improved in recent years thanks to the current space instruments such as Fermi-LAT and AGILE, and to the ground-based telescopes such as H.E.S.S., VERITAS, Milagro at higher energies. While high-quality data are providing crucial information on Galactic sources, interstellar emissions and high-energy particles, they are challenging our understanding. I will discuss the state of the art, recent results, and prospects for future instruments.

Speaker: Dr Elena Orlando (Stanford University)

Paper orlando.zip

Slides Scineghe2016_Orlando_def.pdf

44 Gamma-ray catalogs and unidentified sources

The Fermi Large Area Telescope (LAT) has been surveying the full sky since August 2008. The third LAT source catalog (3FGL, about 3000 sources) is still the largest general gamma-ray catalog, but it is based on only 4 years of data. Going deeper over the full energy band (down to 100 MeV) requires more robust methods. The analysis is much simpler at high energies due to the good spatial resolution and low confusion. The third high-energy catalog (3FHL above 10 GeV) reaches much deeper in that energy range (yielding about 1700 sources) thanks to the longer data set (7 years) and the improved effective area and point-spread function (from the Pass 8 event reconstruction and classification). It provides a large reservoir of extragalactic targets for pointed TeV instruments. The fraction of unassociated sources (1/3 in 3FGL at the time of its publication, 1/5 in 3FHL) reflects the balance between the depth of counterpart catalogs and that of the LAT catalogs, as well as the localization precision. Most of those unassociated sources should be of the same types as the major known contributors (BL Lacs above 10 GeV, flat-spectrum radio quasars and pulsars below 10 GeV) but surprises probably hide there. In terms of numbers of sources and sky coverage, the TeV catalogs are still far from the GeV ones. However, their description of sources in the Galactic plane (particularly extended sources) is often better, thanks to their better spatial resolution. The next-generation ground-based gamma-ray observatory (CTA) will provide an even deeper, more precise and broader view of the Galactic sources.

Speaker: Dr Jean Ballet (AIM/SAp, CEA Saclay)

Slides jballet_scineghe_1016_final.pdf

45 Electromagnetic Cascades and Intergalactic Magnetic Fields

The strength and structure of intergalactic magnetic fields (IGMFs) are an open problem in cosmology. Gamma-ray-induced electromagnetic cascades can be used to probe IGMFs as their charged components are sensitive to the underlying structure of the fields. For a complete Monte Carlo treatment of the effects of IGMFs on the development of electromagnetic cascades, GRPropa was developed. This novel tool enables the propagation of gamma rays and secondary electrons and photons in arbitrary magnetic field configurations, accounting for all relevant energy loss processes such as synchrotron emission and adiabatic losses due to the expansion of the universe, as well as interactions with pervasive photon fields including the cosmic microwave background and the extragalactic background light. Using simulations obtained with GRPropa the formation of blazar pair halos in the presence of intervening helical magnetic fields is studied. Combined, this and other studies can potentially be used to constrain the mechanisms whereby IGMFs originated.

Speaker: Rafael Alves Batista (University of Oxford)

Paper RafaelAlvesBatista.zip

Slides RAB-20161020-SciNeGHE.pdf

16:25 Social program: Pisa guided tour

20:00 Social dinner

Friday, 21 October

Gamma-ray sources

Convener: Aldo Morselli (ROMA2)

46 The Sun and Solar System

Speaker: Rachele Desiante (TO)

Slides desiante_Solar_Scineghe_v2.pdf

47 Observations of Galactic cosmic ray accelerators in the gamma-ray sky with Fermi-LAT

The Fermi Large Area Telescope (LAT) has been exploring the gamma-ray sky for more than eight years, observing many powerful events happening in our Galaxy, in a range of energies from less than one hundred MeV up to few TeV. It provides essential information on the physical processes occurring at the source, involving both leptons and hadrons, in order to understand the mechanisms responsible for the acceleration of these particle populations. I will give a review of the latest results from Fermi-LAT observations of Galactic objects, in particular about Supernova Remnants (SNRs) and Pulsar Wind Nebulae (PWNe).

Speaker: Francesco De Palma (BA)

Slides fdepalma_scineghe_2016_v0.3_pub.pdf

48 Is there need for axions to explain the signal from blazars? Where do we stand?

Axions and axion-like particles (ALPs) are a generic prediction of many extensions of the Standard Model. They are attracting growing interest as they are good candidates for cold dark matter, and -- in the case of ALPs -- they also give rise to very interesting effects in high -energy astrophysics for suitable values of the parameters. In the first place, photon-ALP oscillations considerably enlarge the gamma-ray horizon for E > 100 GeV. Besides, for the same choice of the parameters they also solve two open problems: the very-high-energy spectral anomaly of blazars (to be explained in the talk) and why flat spectrum radio quasars (FSRQs) emit up to 400 GeV (conventional physics prevents any emission above 20 GeV). Combining these two results -- one occurring in extragalactic space while the other inside a FSRQ -- we get a strong hint of the existence of an ALP with mass of about 10^{- 9} GeV. Remarkably, this issue will be settled in the near future not only by the CTA but also the laboratory experiment ALPSII at DESY. Finally, for a different choice of the parameters, ALPs would change the polarization of the light emitted by some sources in the ranges (2 -- 10) keV and (0.3 -- 10) MeV, an effect that could be detected by the XIPE and e-ASTROMAM missions, respectively.

Speaker: Marco Roncadelli (PV)

Slides Roncadelli__Talk_Scineghe_-.pdf

49 SEARCH FOR GAMMA-RAY SIGNALS FROM DWARF SPHEROIDAL GALAXIES WITH THE CHERENKOV TELESCOPE ARRAY

Cosmological observations indicate that approximately 27% of the energy density of the universe is in the form of dark matter which is non-baryonic. The nature of dark matter is an open question in modern physics. A well motivated candidate constituent is a weakly interacting massive particle (WIMP) with mass in the range between O(10)GeV and O(100)TeV. The annihilation radiation from such particles can be searched for with imaging atmospheric Cherenkov telescopes (IACTs) such as the planned Cherenkov Telescope Array. Dwarf spheroidal galaxies (dSphs) of the Milky Way are among the most promising targets since these are dynamically dominated by dark matter and have no intrinsic (astrophysical) gamma-ray emission. In this contribution we will review the status of such searches and give prospects for future observations with the Cherenkov Telescope Array.

Speaker: Gonzalo Rodriguez Fernandez (ROMA2)

Paper DM.Gonzalo.Rodriguez.tar.gz gonzalo_DM.pdf

Slides Gonzalo.Rodriguez_SCINEGHE2016_Dark.Matter__TalkVersion.pdf

10:40 Coffee break

50 Statistical Measurement of the Gamma-ray Source Count Distribution as a Function of Energy

Statistical properties of photon count maps have recently been proven to provide a sensitive observable for characterizing gamma-ray source populations and for measuring the composition of the gamma-ray sky with high accuracy. In this contribution, we generalize the use of the standard 1-point probability distribution function (1pPDF) to decompose the high-latitude gamma-ray emission observed with Fermi-LAT into: (i) point-source contributions, (ii) the Galactic foreground contribution, and (iii) a diffuse isotropic background contribution. To that aim, we analyze the gamma-ray data in five adjacent energy bands between 1 GeV and 171 GeV. We measure the source-count distribution dN/dS as a function of energy, and we demonstrate that our results extend current measurements from point-source catalogs to the regime of so far undetected sources. Our method improves the sensitivity for resolving point-source populations by about one order of magnitude in flux. The dN/dS distribution as a function of flux is found to be compatible with a broken power law. We derive upper limits on further possible breaks as well as the angular power of unresolved sources. We discuss the composition of the gamma-ray sky and future prospects and capabilities of the 1pPDF method.

Speaker: Dr Hannes-S. Zechlin (University of Torino, Italy)

Slides 1pPDF_dNdS_scineghe_zechlin.pdf

The other messengers: Cosmic rays

Convener: Ivan De Mitri (LE)

51 Cosmic Ray Physics: sources and fundamental physics

The physics of Ultra High Energy Cosmic Rays (UHECR) will be reviewed with a particular focus on the (possible) experimental tests of new theories. We will discuss: top-down models for the production of these extreme energetic particles and tests of the Lorentz invariance.

Speaker: Roberto Aloisio (INFN)

Paper Aloisio.zip

Slides Aloisio-SciNeGHE2016.pdf

52 Space-based cosmic ray experiments:results and perspectives

In the last decade a wealth of direct CR measurements has been performed by space based experiments leading to unexpected results and bringing this field of research in the "precision era" up to the TeV energy scale. New missions have just started their operation, or are close to launch, and will extend of 1-2 decades in energy the study of the CR composition and energy spectra. Current measurements and what can be expected from existing programs will be reviewed in this contributions, as well as the requirements for future missions to further advance in this field.

Speaker: Bruna Bertucci (PG)

Slides 2016-BERTUCCI-SciNeGHE_upload.pdf

53 Ground-based cosmic ray experiments : results and perspectives

This report aims at giving a brief summary of the most recent results from air shower observations and discussing their relevance in the understanding of the origin, acceleration and propagation of the high energy cosmic rays. The shape and composition of the primary spectrum as well as the large-scale anisotropy in the arrival direction of cosmic rays are key elements to understand their transition from a Galactic to an extra-Galactic origin, while at the highest energy the flux suppression may not be dominated by the GZK-effect but by the limiting energy of the sources. The physics case for multimessenger observations and the observational results and challenges will be discussed. We shall discuss the experimental progress in the field and its prospects for the very near future.

Speaker: Antonella Castellina (TO)

Paper Castellina_Antonella.tar.gz

Slides Castellina_Scineghe.pdf

54 Scineghe Awards

Speaker: Angelo Scribano (PI)

Slides Scineghe2016_Awards.pdf

13:00 Lunch

55 Multimessenger connections: Crs, neutrinos, and Gws

Speaker: Paolo Lipari (ROMA1)

Slides lipari_scineghe.pdf

56 Future cosmic ray detectors (ground and space)

In this talk an overview of the future experiments devoted to the cosmic ray detection both in space and on ground will be given, with particular emphasis on the charged cosmic ray component.

Speaker: Elena Vannuccini (FI)

Slides Vannuccini-SciNeGHE-final.pdf

The future

Conveners: Gloria Spandre (PI), PAOLO DA VELA (PI)

57 Prospects for Gamma-Ray Astrophysics in Space

After a brief review of the past and current X-ray and gamma-ray space missions, I will discuss the challenging astrophysics and physics issues that lead to the next generation of space experiments focused in the MeV-GeV range. I will summarize the scientific goals and technical features of the main proposed experiments in the context of the new Astronomy of the mid-2020's.

Speaker: Marco Tavani (ROMA2)

Slides Tavani_0280_Future_Gamma-Ray_Astrophysics_in_Space_SCINEGHE_Pisa_2016.ppt

58 ComPair and future perspectives in MeV Gamma-ray astronomy

The gamma-ray energy range from a few hundred keV to a few hundred MeV has remained largely unexplored since the pioneering but limited observations by COMPTEL on the CGRO (1991-2000). Fundamental astrophysics questions can be addressed by a discovery mission in the MeV range, from astrophysical jets and extreme physics of compact objects to a large population of unidentified objects. We will briefly go through the science drivers for such a mission. We will present the concept of the wide-aperture instrument ComPair (Compton-Pair Production Space Telescope) being developed by NASA/Goddard Space Flight Center in collaboration with Navy Research Laboratory, Clemson University, Washington University and University of California at Santa Cruz, to investigate the energy range from 200 keV to > 500 MeV with high energy and angular resolution and with sensitivity approaching a factor of 20-50 better than COMPTEL. We will also present extended science requirements to include nuclear gamma-ray spectrometry, gamma-ray polarization and precise mapping of the gamma radiation from the Galactic Center. A possible concept for a large-scale instrument to meet these requirements will be discussed

Speaker: Dr Alexander Moiseev (CRESST/NASA/GSFC and UMCP)

Slides Moiseev_talk.pdf

59 How Polarimetry will complete the role of X-rays as e.m. messenger of High Energy phenomena

X-rays have been for half a century one of the messengers driving the study of High Energy Phenomena. Our knowledge and understanding of these is in a phase of fast evolution, thanks to the outstanding crops of data from High Energy and Very High Energy Gamma-Rays, the systematic increase data from UHE CR and neutrinos and to the sudden show-up of the gravitational wave phenomena. But X-rays can still play a fundamental role because they are the highest energy where a high angular resolution, a high energy resolution and a high timing capability can be achieved. For sure, beside what they report by themselves, in a multi-messenger approach, will have for long time a privileged role in correlating the dramatic phenomena detected in other bands with the objects studied by astrophysics. The instrumentation for X-ray imaging, spectroscopy and timing has arrived a high level of sophistication and will further improve with the new planned or proposed missions. It seems that, at last, good chances are there that also polarimetry, namely the missing subtopic of X-ray astronomy, will be exploited in the next decade so opening this undisclosed window in sky. I show the status of instrumentation, the concept of missions and how we can realistically expect to study up to 100-200 sources, belonging to most of classes of X-ray astronomy, with a sensitivity of relevant interest according to a theoretical literature that, fed by the expectation of these new data, is systematically growing in the last years. A few topic cases are discussed.

Speaker: Enrico Costa (IASF Roma/INAF)

Slides COSTA_SCINEGHE_2016.ppt

60 Status and Perspectives of CTA

The very-high energy gamma-ray astrophysics in the few tens of GeV to 100 TeV domain experienced a real boost in the last decade from detecting just a few sources in 2003 to more than 150 galactic and extragalactic sources in 2016. Several outstanding discoveries were made during that time thanks to the excellent performance of the H.E.S.S., MAGIC and VERITAS arrays of imaging atmospheric Cherenkov telescopes. Their success paved the way to the next generation instruments, combined together in the Cherenkov Telescope Array (CTA) project, aiming to extend the accessible energy range and to improve the flux sensitivity by an order of magnitude compared with the existing installations. In this talk I will present the status and perspectives of the CTA project. In particular I will review the key elements of CTA instruments and the way the CTA observatory will be operating as well as I will highlight Key Science Projects targeted by the CTA consortium. I will also give an update on the schedule of CTA and the early science prospects.

Speaker: Daniel Mazin (MPI for physics, Munich and ICRR, University of Tokyo)

Paper mazin_CTA.tgz

Slides MAZIN-CTA.pdf

61 The future of gamma-ray astronomy with LHAASO

I'll firstly review the history of high altitude cosmic rays research in China and our pursuit for a high sensitivity gamma rays telescope in very high energy region. Then I'll talk about the status and prospect of LHAASO.

Speaker: Prof. HU HONGBO (Institute of High Energy Physics, CAS, Cina)

Slides hu.pptx

Concluding Remarks