The II National Workshop of SKA science and technology

Europe/Rome
Area della Ricerca di Bologna, via P. Gobetti, 101
Description

 The UTG-II Radioastronomia and the Italian SKA Board invite the astrophysical community to attend the “The II National Workshop of SKA science and technology”, that will be held in Bologna (Area della Ricerca - CNR) on 3-5 December 2018.


Workshop description and aims

The SKA (Square Kilometer Array), currently under design and development, is the next generation radio observatory, and one of the most ambitious astrophysical projects for the 2020s. In its first phase (SKA1) it will consist of two telescopes, one comprised of dishes operating at mid frequencies (350 MHz-15 GHz; SKA1-MID) and located in South-Africa, and the other comprised of Log-Periodic antennas operating at low radio frequencies (50-350 MHz; SKA1-LOW) which will be located in Australia. SKA will be equipped with advanced technologies for receivers, signal and data transport, science data processing and computational facilities. Its development and construction will have major impact on technological and HPC advances and a strong industrial return.

Italy is one of the founding countries of the SKA Organization (SKAO), an independent structure established in 2011 to organize and coordinate the design phase. Italy is currently coordinating the negotiations towards the establishment of an Intergovernmental Organization (IGO)– similar to CERN and ESO – that will lead towards the construction phase of the telescope.

Following the first SKA National Conference organized in 2012, this workshop will bring together the astrophysical community in a more mature phase of the SKA project. All Italy-based researchers who have interest in SKA-related science and technology (including HPC) are welcome to join, as well as all interested industrial players.

The main aim of the workshop is to review the scientific, technological and industrial activities in progress in Italy in the framework of the SKA project, and to involve the astrophysical community at large in tracing an Italian roadmap towards the SKA. Particular attention will be given to exploring possible synergies between SKA and other scientific and technological projects relevant to INAF, through a dedicated Session (organized in close collaboration with UTG-I and UTG-III).


Scientific Program

The program of the conference is now available. See 'Timetable' (on the left) for the schedule and 'Scientific Programme' for instructions to speakers and poster presenters.


Registration

The abstract submission call and the registration are now closed.


SOC: I. Prandoni (chair), G. Bernardi, G. Brunetti, R. Cassano, G. Comoretto, D. Fierro, F. Govoni, J. Monari, A. Navarrini, A. Possenti, R. Smareglia, C. Trigilio, G. Umana. In collaboration with Adriano Fontana (UTG-I) and Massimo Cappi (UTG-III)

LOC: R. Cassano (co-chair), I. Prandoni (co-chair), G. Bernardi, G. Brunetti, J. Monari, M. Nanni, M. Stagni


News: The Programme of the workshop is now available. See 'Timetable' (on the left) for the schedule and 'Scientific Programme' for instructions to speakers and poster presenters.

News: The Abstract Booklet is now available (see attachment below or menu on the left ).


Participants
  • Adriano Ingallinera
  • Alessandra Zanichelli
  • Alessandro Caccianiga
  • Alessandro Cortopassi
  • Alessandro Costa
  • Alessandro Navarrini
  • Alessandro Scalambra
  • Andrea Botteon
  • Andrea Ferrara
  • Andrea Girardi
  • Andrea Maccaferri
  • Andrea Mattana
  • Andrea Melis
  • Andrea Possenti
  • Andrei Mesinger
  • Anna Zoldan
  • Annalisa Bonafede
  • Antonio Garufi
  • Carlo Baffa
  • Carlo Burigana
  • Carlo Stanghellini
  • Carlotta Gruppioni
  • Carolina Belli
  • Caterina Boccato
  • Chiara Stuardi
  • Claudio Codella
  • Claudio Scafuri
  • Corrado Trigilio
  • Crescenzo Tortora
  • Cristina Knapic
  • Dane Kleiner
  • Daniel Molnar
  • Daniela Vergani
  • Daniele Dallacasa
  • Daria Guidetti
  • Davide Chinigo'
  • Davide Fierro
  • Diego Carraro
  • Elena Zucca
  • Eleonora Ferroni
  • Eliana Palazzi
  • Elisabetta Giani
  • Elisabetta Liuzzo
  • Enrico Lenzi
  • Enzo Brocato
  • Ettore Carretti
  • Evgeniya Kravchenko
  • Fabio Casini
  • Fabio Paonessa
  • Federica Govoni
  • Federico Abbate
  • Federico Di Giacomo
  • Federico Perini
  • Fiamma Capitanio
  • Filippo Maccagni
  • Filomena Bufano
  • Francesca Loi
  • Francesca Panessa
  • Francesco Cavallaro
  • Francesco Cuttaia
  • Francesco Paolo Bonetti
  • Francesco Rampini
  • Francesco Schilliro'
  • Franco FERRARESI
  • Franco Tinarelli
  • Franco Vazza
  • Franco Vivaldi
  • Gabriele Bruni
  • Gabriele Giovannini
  • Gabriella De Lucia
  • Gabriella Raimondo
  • Giampaolo Vettolani
  • Giancarlo Ghirlanda
  • Gianfranco Brunetti
  • Gianni Bernardi
  • Gianpietro Marchiori
  • Giorgio Lanzuisi
  • Giovanni Comoretto
  • Giovanni Naldi
  • Giovanni Piano
  • Giovanni Tartarini
  • Giuliano Taffoni
  • Giuseppe Pupillo
  • Grazia Umana
  • Graziano Todaro
  • Isabella Prandoni
  • Jader Monari
  • Kamlesh Rajpurohit
  • Laura Pentericci
  • Lauro Moscardini
  • Leonardo Testi
  • Linda Podio
  • Lorenzo Amati
  • Lorenzo Ciani
  • Lorenzo Mezzadrelli
  • Luca Moscadelli
  • Luca Olmi
  • Luca Stringhetti
  • Luciano Gramiccia
  • Luigi Fumagalli
  • Luigi Iavarone
  • Luigi Pierno
  • Luigina Feretti
  • Manuela Magliocchetti
  • Marcella Massardi
  • Marcello Giroletti
  • Marco Bondi
  • Marco Padovani
  • Marco Poloni
  • Marco Schiaffino
  • Marco Tavani
  • Maria Teresa Botticella
  • Mario Ballardini
  • Marisa Brienza
  • Marta Burgay
  • Marta Spinelli
  • Marzia Rivi
  • Massimiliano Tordi
  • Massimo Della Valle
  • Matteo Bonato
  • Matteo Canzari
  • Matteo Di Carlo
  • Matteo Viel
  • Mattia Vaccari
  • Maurizio Carraro
  • Maurizio Miccolis
  • Mauro Contursi
  • Mauro Dolci
  • Micol Bolzonella
  • Miles Deegan
  • Monica Alderighi
  • Mpati Ramatsoku
  • Myriam Gitti
  • Nunziato Sorrentino
  • Paola Di Ninni
  • PAOLO SARTINI
  • Paolo Serra
  • Pietro Bolli
  • Renato Aurigemma
  • Riccardo Cesaroni
  • Riccardo Smareglia
  • Robert Braun
  • Roberto Ambrosini
  • Roberto Gilli
  • Roberto Ricci
  • Roberto Russo
  • Roberto Scaramella
  • Roberto Singuaroli
  • Rosario Cimmino
  • Rosita Paladino
  • Rossella Cassano
  • Sandro Bardelli
  • Sandro Pastore
  • Sara Loru
  • Sara Ricciardi
  • Serena Pastore
  • Sergio Molinari
  • Sergio Poppi
  • Simone Bianchi
  • Simone Chiarucci
  • Simone Riggi
  • Simone Rusticelli
  • Stefania Grazioli
  • Stefania Matteoli
  • Stefania Varano
  • Stefano Camera
  • Stefano Losa
  • Stefano Vercellone
  • Tiziana Trombetti
  • Tiziana Venturi
  • Tommaso Marchiori
  • Ugo Becciani
  • Umberto Maio
  • Valentina Alberti
  • Valentina Vacca
  • Vincenzo Galluzzi
  • Viviana Casasola
  • Víctor M. Rivilla
LOC contact:
    • 09:30 10:55
      General: The SKA Project [chair: M. Tavani]
      • 09:30
        Welcome from host - 5' 5m
        Speaker: Tiziana Venturi
      • 09:35
        Welcome from INAF - 10' 10m
        Speaker: Marco Tavani
      • 09:45
        The SKA Project and its Science - 45' 45m

        The current status of the SKA Project will be summarised, highlighting progress toward a completed design, establishment of the Observatory and consolidation of a construction and comissioning plan. The many science areas in which the SKA is anticipated to make major contributions will be briefly reviewed, together with a discussion of the SKA Data Challenges that are now underway to maximise community engagement with SKA data products and the optimised science extraction from them.

        Speaker: Robert Braun
      • 10:30
        The SKA project from the SEAC perspective - 25' 25m
        Speaker: Andrea Ferrara
    • 11:00 11:30
      coffee break 30m
    • 13:00 14:00
      Lunch break 1h
    • 16:00 16:30
      coffee break 30m
    • 16:45 17:40
      Science with SKA Precursors and Pathfinders: HI [chair: G. Bernardi]
      • 16:45
        Extragalactic HI Science: ongoing activities towards the SKA - 25' 25m

        I will discuss SKA-related work in the field of extragalactic HI astronomy. I will focus on recent, ongoing and upcoming science projects with a variety of telescopes -- including SKA pathfinders and precursors -- that will pave the way for SKA1 programs. I will discuss a few technical challenges such as RFI rejection/nulling, data volume and source finding; and I will present some exciting new recent HI results. FInally, I will describe how the extragalactic HI community has organised its activities towards the SKA.

        Speaker: Paolo Serra
      • 17:10
        First results from MeerKAT Commissioning Observations - 15' 15m

        The MeerKAT Fornax Survey (MFS, PI Paolo Serra) is a dedicated large survey project planned by the MeerKAT telescope, the South-African precursor of the SKA. The MeerKAT telescope was inaugurated in July 2018. As of early 2019, MeerKAT will observe for 900 hours the Fornax cluster to study its assembly of new gas-rich galaxies and groups and the physics of gas accretion occurring in its environments. In this talk, I will outline the main scientific goals of the MeerKAT Fornax Survey and the main challenges that we will face in the analysis of high resolution (~25 kHz) and sensitivity (0.1 mJy) MeerKAT observations. I will show new results from high resolution (8’’) MeerKAT commissioning observations of the brightest cluster galaxy of Fornax (NGC 1399), of Fornax A, the extended radio source in the in-falling group of the cluster, and of the region connecting these two sources, where we detect neutral hydrogen gas (HI). I will focus on the challenges presented by the spatial extent of Fornax A (~1 degree in the sky) in correctly subtracting its continuum emission, and detecting the HI line with high signal to noise ratio. I will show how we solve these issues in the automated data reduction pipeline we developed for MeerKAT continuum and spectral line observations (MeerKATHI). The techniques for the reduction and analysis of MeerKAT observations will set an important starting point to plan and develop the SKA survey projects and data reduction strategies.

        Speaker: Filippo Maccagni (INAF)
      • 17:25
        ASKAP HI Imaging of a nearby spiral galaxy - 15' 15m

        The Australia Square Kilometre Array Pathfinder (ASKAP) is a new radio interferometer that is pioneering revolutionary Phased Array Feed (PAF) receivers, which are under consideration for future SKA instrumentation. I will give an update on ASKAP status, rollout and commissioning, and present the first results from WALLABY, the main extragalactic ASKAP HI survey that has been using an ASKAP sub-array for early science. We have produced the highest resolution HI images of the nearby, gas-rich, spiral galaxy IC 5201 that has also revealed 3 gas-rich dwarf satellite galaxies. An additional 5 galaxies and 2 tidal features are detected in the same HI images due to the instantaneous wide-filed imaging capabilities of ASKAP. I will discuss the physical properties of these systems, focusing on the ratios of available HI gas, star formation rate and stellar mass in order to describe the galaxies and their environments.

        Speaker: Dane Kleiner (INAF)
    • 17:40 18:05
      Synergies between SKA and other facilities: [chair: G. Bernardi]
    • 11:00 11:30
      coffee break 30m
    • 12:05 12:30
      Synergies between SKA and other facilities: [chair: C. Trigilio]
      • 12:05
        Synergies between SKA and other cosmological probes - 25' 25m
        Speaker: Stefano Camera (on behalf of Matteo Viel)
    • 12:30 13:10
      Science with SKA Precursors and Pathfinders: Our Galaxy [chair: C. Trigilio]
      • 12:30
        The SCORPIO project: the first ASKAP glimpse in the Galactic plane - 25' 25m

        SKA precursors are going to revolutionize our view of the Milky Way. ASKAP is entering its regime phase and one of its large program, EMU, is the largest radio survey ever designed at the planned depth of 10 μJy/beam. In the wide context of the preparation for EMU and ASKAP we present the SCORPIO project, an ATCA survey of a patch of the Galactic plane, originally covering a ∼5-square-degree. SCORPIO has recently been extended to ∼40-square-degree thanks to the first ASKAP early science data, being the first Galactic field ever imaged at this frequency by an SKA precursor. In this talk we show the major scientific results we are obtaining on point and extended sources in the general context of stellar evolution. We present also the first ASKAP early science observation of SCORPIO, carried out in January 2018 at a central frequency of 912 MHz. We highlight the surprising capability of ASKAP to image wide fields toward the Galactic plane also in view of EMU.

        Speaker: G. Umana / F. Bufano (INAF - OA Catania)
      • 12:55
        New methodologies for Galactic data reduction and analysis - 15' 15m

        SKA precursors have just started to collect data, whose amount is so huge that is somehow overwhelming scientists. And the data stream is going to blow up once the precursors will be fully operational, not to mention SKA itself. How are we preparing for this? Automation in data reduction and analysis is mandatory but it is still far to be complete with respect to all the cases the radio astronomy community is going to encounter in the very next future. Data reduction pipelines and newly developed analysis tools are representing an intriguing challenge for scientists and a formidable test bench for super-computing facility. In this talk we present the use case of data reduction and analysis of ASKAP Galactic observations of the SCORPIO field, as representative of a series of issues for radio mapping. We first discuss how we fitted the ASKAP data reduction pipeline to the "Galactic needs". Then we present some algorithms we developed or are developing to analyse Galactic maps, in particular for source extraction and characterization. We finally propose and summarise some practical solutions to help shaping the ASKAP Galactic data processing strategy.

        Speaker: Francesco Cavallaro (INAF-OA Catania)
    • 13:10 14:00
      Lunch break 50m
    • 14:00 14:40
      Science with SKA Precursors and Pathfinders: the Cradle of Life [chair G. Umana]
      • 14:00
        From protostellar disks to planetary atmospheres with SKA: Back to cm-wavelengths with new perspectives - 25' 25m

        The ingredients for the recipe to make a “habitable” planet like our own Earth are: a relatively small rocky planet, at the right distance from the host star, with a not too thick atmosphere rich in volatiles and capable of developing interstellar complex organic molecules (iCOMs) chemistry. Searches for exoplanets have shown a large degree of diversity in the planetary systems, and as yet is unclear how common a System like our own is. Understanding the formation of planetary systems and the chemical processing of the volatiles that will form their atmospheres is key to understand the origins of the Solar System and how common the “habitable” planet outcome may be. More specifically key questions still to be addressed are: how chemically complex are the volatiles delivered on the pristine planetary atmospheres? What molecules are passed from the large-scale envelope to the disk in which planets, comets, and asteroids form?

        These are questions addressed by the INAF funded project GENESIS-SKA. The GENESIS-SKA approach is: to fully exploit the capabilities of the telescopes working in the mm- and sub-mm wavelengths to prepare pilot projects in the cm-domain and consequently plan science goals for SKA. We will present and discuss what obtained so far by GENESIS-SKA:
        (1) the large program ALMA FAUST, the first and so far unique ALMA large program on astrochemistry (iCOMs and light C-chains at 220-260 GHz);
        (2) a pilot project for the preparation of a VLA large program (iCOMs, at 23-24 GHz);
        (3) a pilot project for the preparation of a Green Bank single-dish large program (iCOMs and heavy C-chains, at 13-15 GHz).

        Speaker: Claudio Codella (INAF - Osservatorio Astrofisico di Arcetri)
      • 14:25
        Searching for exoplanets with SKA - 15' 15m

        The improvement in sensitivity of radio telescopes is disclosing a brand new method for searching and characterizing extrasolar planets. Mutual magnetic interaction between an exoplanet and its parent star (or even one of its satellites) can give rise to a electron cyclotron maser emission (ECME), known as auroral radio emission. The radio emission has a peculiar signature in time and in polarization. There are two scenarios: in one case the planet orbiting the star can trigger this emission leading to a ECME in the stellar magnetosphere; in tho other one the stellar wind can trigger the auroral radio emission directly above the planet. Information like the presence of a planetary magnetosphere or of different satellites can be inferred. Current observations of are however heavily hampered by the limited sensitivity, and we expect that a major step forward will be possible only with SKA. Despite this limitation we present two cases we recently studied: the ultra-cool dwarf TVLM 513-46546 and α Centauri. For the first star we used VLA observations at 4.9 and 8.4 GHz to constrain an auroral radio emission model and reproduce the cyclic circularly-polarized pulses of the star. Our model explains the observed radio emission, and in particular its anomalies at 8.4 GHz, as a possible interaction of the star with an external body (Leto et al. 2017). For α Cen, we successfully detected both the stars at 17 GHz, being the first detection ever at these frequencies. We used 2-GHz data to search for time-variable coherent emission as a signature of the claimed Earth-sized planet in close orbit to α Cen B, finding no results (Trigilio et al. 2018). We finally discuss the implication of this early pioneering study in planning and proposing observations with SKA and its precursor, when the unprecedented sensitivity could be unveiling hundreds of these cases.

        Speaker: Adriano Ingallinera (INAF - OA Catania)
    • 14:40 15:45
      Synergies between SKA and other facilities: [chair: G. Umana]
      • 14:40
        Infrared-Radio synergies in Galactic Interstellar medium and star formation - 25' 25m

        I will illustrate recent developments in Galactic star formation and ISM studies from large panoramic surveys in the infrared and submillimeter. The amount and the quality of data now available over our entire Galaxy call for renewed efforts also in the radio. SKA allows a new leap in sensitivity and mapping capabilities at high spatial resolution both in continuum and spectroscopy to unveil new perspectives in the study of the atomic and ionised phases of the diffuse ISM and the initial stages in intermediate and massive star formation.

        Speaker: Sergio Molinari
      • 15:05
        Synergies between SKA and LSST: the transient sky - 25' 25m

        The LSST will be a wide-field 8m class telescope designed to obtain multi-band images over a substantial fraction of the sky every few nights. Multiple goals are expected in many relevant astrophysical areas, such as : (i) taking an inventory of the Solar System; (ii) mapping the Milky Way; (iii) exploring the transient universe; and (iv) probing dark energy and dark matter. The SKA and LSST offer significant synergies, in particular in time-domain astrophysics. Simultaneous observations of the transient sky carried out with SKA and LSST will allow us to study "known" and yet "unknown" classes of transient phenomena with unprecedented accuracy. The optical counterparts of a broad range of radio transients will be imaged by LSST in different bands and the spectroscopic follow-up of the most exciting candidates will be carried out with SOXS.

        Speaker: Maria Teresa Botticella
      • 15:30
        Definitive characterization of the ISM in the Local Universe: SKA and other facilities - 15' 15m

        Understanding the interplay between the various components of the interstellar medium (ISM: dust, atomic and molecular gas) in galaxies of the Local Universe is of fundamental importance for studies of galactic formation and evolution. In the last decade, thanks in particular to Herschel, we made a considerable effort in the study of one of these components, the dust. In this framework, the DustPedia project has been devised aimed at performing a complete characterization of dust in the Local Universe. However, we need information on all the phases of the ISM, including the gas, to draw definitive conclusions on it.

        Exploring the cosmic evolution of the gas content of galaxies is a key science driver for SKA, and DustPedia is supporting this providing a first important step in understanding how the cold ISM related to the dust content, and to galaxy ability to form stars. We present the main scaling relations between uniformly homogenized data of molecular and atomic gas, and dust for a sample of ~450 nearby (z<0.01), late-type galaxies extracted from the DustPedia sample. Only such a large and coherent dataset of all phases of the ISM can provide a definitive view of the ISM in the Local Universe and permit to link it with that at high redshift, tracing its evolution.

        ALMA is revealing the molecular gas component through several tracers, as e.g. CO, detectable at millimeter wavelengths, while telescopes as JVLA and, in future, SKA detect the atomic gas component (21cm-HI). Our approach therefore represents a clear example of synergy between SKA pathfinder/precursors, ALMA, and Herschel, in addition to put us in a favored position for the forthcoming use of SKA.

        Speaker: Viviana Casasola (Istituto Nazionale di Astrofisica (INAF))
    • 15:45 16:15
      coffee break 30m
    • 16:15 17:15
      Science with SKA Precursors and Pathfinders: Transients [chair: A. Possenti]
      • 16:15
        Pulsars and FRBs: ongoing activities towards the SKA - 25' 25m

        I will present an overview of the ongoing and planned activities of the italian radioastronomical community related to pulsar and Fast Radio Burst science, in view of the SKA.

        Speaker: Marta Burgay (Istituto Nazionale di Astrofisica (INAF))
      • 16:40
        Probing the properties of globular clusters using pulsars with MeerKAT - 15' 15m

        Globular clusters contain a large number of millisecond pulsars. Besides being extremely interesting by themselves, these pulsars are an invaluable tool to probe the cluster environment and dynamics. They can be used to search for the presence of an intermediate mass black hole in the center, ionized gas and its magnetic field. The SKA precursor MeerKAT is in a unique position as it is capable of observing all of the Milky Way globular clusters. Thanks to its large collecting area and wide bandwidth, MeerKAT will be able to time the pulsars in globular clusters with higher precision than now possible and to constrain better the structural parameters of the clusters. This will also lead to tighter limits on the mass of central black holes.

        Speaker: Federico Abbate (Istituto Nazionale di Astrofisica (INAF))
      • 16:55
        Deciphering the puzzle of GRB170817 and the SKA studies of Gamma Ray Bursts - 20' 20m

        Radio observations of the first gravitational wave event with an electromagnetic counterpart (GRB170817) has shown unexpected features. The long lived, slowly rising, non--thermal radio emission (together with optical and X--ray observations), between 10 and 200 days after the BNS merger, is consistent with being produced by either a narrowly collimated or an isotropic outflow with geometrical and/or dynamical structure. Global-VLBI observations, owing to the exquisite angular resolution, hold the key to distinguish between these two models answering the question weather a relativistic jet emerged from the merger. Implications for the event rate and jet physics will be discussed.

        Speaker: Giancarlo Ghirlanda (Istituto Nazionale di Astrofisica (INAF))
    • 17:15 18:20
      Synergies between SKA and other facilities: [chair: A. Possenti]
      • 17:15
        GRAWITA: the role of SKA - 25' 25m

        The first joint gravitational wave (GW) and electromagnetic (EM) signals detection in August 2017 marked the dawn of GW+EM multi-messenger astronomy. The GRAWITA collaboration has been at the forefront of this new era providing the most impressive spectro-photometric optical/near-infrared data set on the EM source. These observations secured the first compelling evidence for the existence of kilonovae.
        The GRAWITA team has been awarded time at several observing facilities and the project is representing an efficient operational framework capable of fast reaction on large error box GW triggers and direct identification and characterization of detected EM counterpart candidates. I will describe the GRAWITA collaboration and its activities and the contribution that the Square Kilometre Array (SKA) will provide to the discovery and understanding of transient EM sources associated to GW signals.

        Speaker: Eliana Palazzi
      • 17:40
        Synergies between SKA and CTA - 25' 25m

        The Cherenkov Telescope Array (CTA) will be the next generation gamma-ray observatory, open to the scientific community, to investigate the very high-energy emission from
        a large variety of celestial sources in the 20 GeV - 300 TeV energy range. The full array, distributed over two sites, one in the northern and one in the southern hemisphere, will provide whole-sky coverage and will improve the sensitivity with respect
        to the current major arrays such as H.E.S.S., MAGIC and VERITAS by a factor of five to twenty, depending on the energy.
        CTA will investigate a much higher number of already known classes of sources, going to much larger distances in the Universe, performing population studies, accurate variability and spatially-resolved studies. We review the current status of the CTA project and discuss the main CTA Key Science Projects,
        which will focus on major scientific cases, allowing us to provide legacy data-sets of high value to a wider community in a context of synergies with other major multi-wavelength facilities.

        Speaker: Stefano Vercellone
      • 18:05
        The THESEUS space mission and its sinergy with SKA - 15' 15m

        The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) is a space mission concept under study by ESA as candidate M5 mission aiming at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. THESEUS will address main open issues in cosmology such as, e.g., star formation rate and metallicity evolution up to redshift 10-12, Pop III stars, re-ionization. In addition, it will provide a fundamental contribution to time-domain and multi-messenger astrophysics by identifying the electromagnetic counterparts to sources of gravitational radiation, which will be routinely detected in the late '20s / early '30s by next generation facilities like aLIGO/aVirgo, LISA,
        KAGRA, and Einstein Telescope and studying most classes of transient sources, thus providing an ideal sinergy also with the large observatories of the near future like LSST, ELT, TMT, SKA, CTA, ATHENA. In particular, the perspective sinergy between THESEUS and SKA is apparent. First of all, the two observing facilities will address fundamental open issues in cosmology through complementary measurements and methods, whose combination will allow to increase substantially the accuracy and reliability in the determination of, e.g., star formation rate evolution up to the very early Universe, physics and evolution of cosmic re-ionization, detection and characterization of pop III stars and first galaxies. In addition, THESEUS will be a wonderful machine for the detection, characterization and redhsift measurement of any kind of GRBs and many classes of X-ray transients. The combination of THESEUS data with those from simultaneous and follow-up observations of these phenomena with SKA will provide unique clues to their physics, progenitors and, more in general, will be a cornerstone contribution to the time domain and multi-messenger astrophysics of
        the future.

        Speaker: Lorenzo Amati (INAF - OAS Bologna)
    • 09:10 09:50
      Science with SKA Precursors and Pathfinders: Active Galactic Nuclei [chair: F. Govoni]
      • 09:10
        AGN Science with the SKA - 25' 25m

        In this talk I will overview the current open and hot questions in the area of radio emission from active galactic nuclei, and will address the impact the SKA and its precursors and pathfinders will play/are playing. I will further highlight the relevance of the SKA-VLBI in this field.

        Speaker: Tiziana Venturi (INAF, Istituto di Radioastronomia)
      • 09:35
        Search and modelling of remnant radio galaxies at 150 MHz with LOFAR - 15' 15m

        Low frequency observations have finally opened the way to the search and study of remnant radio galaxies. These sources represent the last evolutionary stage of radio galaxies when the jets have switched off, and have remained elusive and poorly understood so far. For a long time there have been claims that new sensitive surveys would lead to the discovery of many more remnant radio galaxies, especially at low frequency, and LOFAR now gives us the opportunity to investigate whether this is the case.
        In this talk I present an extensive search for remnant radio galaxies at 150 MHz in the Lockman Hole, a well-studied extragalactic field, and JVLA follow-up observations of the candidate sources. In addition to this, I will show the results from Monte-Carlo simulations that we have performed to predict the fraction of remnants that should be found in radio flux limited samples, to be compared with observations.
        This study puts the basis for a statistical investigation of remnant radio galaxies over larger sky areas using new generation surveys performed with SKA precursors, such as the LOFAR Two-metre Sky Survey, The MeerKAT International GHz Tiered Extragalactic Exploration and GAMA Legacy ATCA Southern Survey.

        Speaker: Marisa Brienza (Istituto Nazionale di Astrofisica (INAF))
    • 09:50 10:05
      Synergies between SKA and other facilities: [chair: F. Govoni]
      • 09:50
        The latest Fermi catalogs and SKA prospects for high energy studies - 15' 15m

        The Fermi-LAT Fourth Source Catalog (4FGL), based on 8 years of E>50 MeV photon data, will comprise about 5500 sources. This number corresponds to a 60% increase relative to 3FGL. The talk will describe the analysis improvements over 3FGL and the new catalog features. About 66% of the sources will have high-confidence counterparts detected at other wavelengths, both extragalactic (mainly blazars) and galactic (mainly pulsars). The nature and properties of the newly detected sources will be discussed, in particular with a description of the accompanying Fourth LAT AGN catalog (4LAC), which will comprise about 3000 sources, essentially doubling the number of sources published in 3LAC, and of the first Fermi-LAT low energy catalog (1FLE) of sources detected in the 30 MeV - 100 MeV range. Multiwavelength observations are key for the characterisation of the physical properties of the identified objects, as well as for the classification of the so-far unassociated gamma-ray sources. The SKA and its precursor can have a prominent role in this area, as I will point out in this presentation with some case studies.

        Speaker: Marcello Giroletti (Istituto Nazionale di Astrofisica (INAF))
    • 10:05 11:00
      Science with SKA Precursors and Pathfinders: Magnetism and Galaxy Clusters [chair F. Govoni]
      • 10:05
        Magnetism and Galaxy Clusters: ongoing activities towards the SKA - 25' 25m

        Galaxy clusters are the host of complicated non-thermal phenomena, that are best visible at radio wavelengths. The current generation of radio instruments, such as the uGMRT, LOFAR, and the JVLA, are showing in these years new and interesting features regarding both the cluster magnetic fields and the non-thermal emission associated with the intra-cluster medium. In this talk, I will review the main milestones that the community has achieved in the last years, and show the main advances that we expect to obtain with the SKA.

        Speaker: Annalisa Bonafede
      • 10:30
        Observation of a nearby filament of galaxy clusters - 15' 15m

        During this talk I intend to present radio observations with the Sardinia Radio Telescope (SRT) of a region of the sky of 8°x8°, likely associated with an over-density traced by nine massive galaxy clusters at z≈0.1. The combination of the SRT data with observations from the NRAO VLA Sky Survey revealed the presence of 28 new diffuse synchrotron radio sources with radio emissivity and X-ray luminosity 10-100 fainter than known diffuse synchrotron cluster sources (radio halos and relics). The comparison with magneto-hydro-dynamical simulations suggests that this population is potentially the tip of the iceberg of a class of diffuse large-scale synchroton sources associated with the filaments of the cosmic web and corresponding to magnetic field strengths of ~20-50 nG.

        Speaker: Valentina Vacca (Istituto Nazionale di Astrofisica (INAF))
      • 10:45
        Cosmic magnetism with the SKA: expectations on the study of intracluster magnetic fields - 15' 15m

        In the next years, thanks to the advent of the SKA we expect a revolution of our knowledge about cosmic magnetism. Its precursors and pathfinders are already pushing the current limits of sensitivity and resolution and they will allow us to study large scale magnetic fields with unprecedented details. In this talk, I will present a computational tool which can produce realistic synthetic full-Stokes images that we expect to detect with the SKA1-MID. The simulated data are used as a framework to investigate how we can constrain large scale magnetic fields hosted by galaxy clusters with this next generation instrument.

        Speaker: Francesca Loi (Università di Bologna & INAF)
    • 11:00 11:30
      coffee break 30m
    • 11:30 12:00
      Synergies between SKA and other facilities: [chair: R. Cassano]
      • 11:30
        Synergies between SKA and Athena - 30' 30m

        In this talk we will highlight the existing synergies between SKA and Athena in the framework of two major research fields: AGN physics and cosmic web studies.
        AGN physics:
        A rich phenomenology of jets, winds, and accretion states has been observed in both active galactic nuclei (AGN) and X+ray binaries (XRBs), suggesting a connection between the accretion and ejection flows at different black hole masses, from supermassive down to stellar mass. In AGN, the radiation field from the disk and the outflows, both of winds and jets, are thought to play a fundamental role in the feedback invoked in galaxy formation and evolution. Notwithstanding their importance, our knowledge of the accretion and ejection phenomena and their interplay is still very limited. Single+object and population studies can explore the accretion/ejection mechanism in XRBs and AGN. 
The Athena X+ray observatory will be launched when the complete SKA array will be fully operative. The combination of these two facilities will provide fundamental improvements on several topics, revolutionizing our comprehension of the accretion/ejection phenomena at all scales (spatial, mass, radio power). The Athena+SKA synergy will allow us to disentangle the jet/disk flows based on their different contributions to the overall spectral energy distribution, expected to be different in ADAF, ADAF+jet and standard disk/corona models. The superbe SKA and Athena sensitivities will lead to high temporal resolution, allowing to test the coronal emission models where reconnection events produce relativistic electrons, which may produce both the radio and the X+ray emission, leading to correlated variability. Given the large number of AGN that SKA will observe/detect, it will be possible to reconstruct all the AGN accretion phases in the local Universe, from pure ADAF, to ADAF+jet dominated, to accretion efficient regimes.
        Cosmic Web:
        The SKA promises to detect the synchrotron emission from shocked plasmas on scales beyond what is currently observed in galaxy clusters, finally imaging the location of the “missing baryons” of the cosmic web. This will have deep implications also for our understanding of how the magnetisation of cosmic structures has proceeded across cosmic epochs. By joining forces with the SKA, Athena should map the missing baryons in several regions: by observing with long exposures regions previously selected in the radio band, Athena will be able to collect enough X-ray photons to attempt first emission spectra from the missing baryons around galaxy clusters and in filaments. In particular, based on our ongoing campaign of simulations, we can predict that the interaction region of close pairs of galaxy clusters should emit enough radio waves to be detectable by the SKA, as well as enough X-ray photons to allow detections using the XIFU, which will allow us to capture these elusive baryons for the first time, and study their thermodynamical properties in detail.

        Speaker: F. Panessa / F. Vazza (Istituto Nazionale di Astrofisica (INAF))
    • 12:00 12:55
      Science with SKA Precursors and Pathfinders: The Epoch of Reionization [chair: R. Cassano]
      • 12:00
        Reionization and the Cosmic Dawn: ongoing activities towards the SKA” 25m

        The birth of the first stars, black holes and galaxies heralded the end of the cosmic Dark Ages and the beginning of the Cosmic Dawn. The light from these objects heated and ionized almost every atom in existence, culminating in the Epoch of Reionization: the final major phase change of the Universe. This final frontier of astrophysical cosmology is undergoing a transition from an observationally-starved epoch to a "Big Data" field. This process is set to culminate with upcoming Square Kilometre Array observations of the redshifted 21-cm line: providing a 3D map of the first billion years of our Universe. Currently, we are starting to get a handle on the timing of reionization. However with the SKA, we will be able to actually study the UV and X-ray properties of the first galaxies, which are encoded in the large-scale structure of the H I signal. I will discuss the innovative modeling techniques we are developing to tap into this bounty, allowing us to constrain astrophysical parameters in a fully Bayesian framework. With this framework, we can infer the star formation inside galaxies too faint to be seen even with JWST. Moreover, we can study high-energy processes in the early Universe, through their heating signature of the IGM before reionization. With SKA, the Italian astronomical community is in the position to become a world leader in the study of Reionization and the Cosmic Dawn.

        Speaker: Andrei Mesinger
      • 12:25
        Observing the cosmic dawn and epoch of reionization with the 21-cm line - 15' 15m

        The quest for the 21-cm signal from the Cosmic Dawn and subsequent Epoch of Reionization has taken an unexpected turn with the reported detection of a sky-average absorption trough centred at 78 MHz (z~17, Bowman et al., 2018) whose explanation challenges any current theoretical model. In this talk I will present competing observations aimed to confirm the reported detection. I will also review the current status of the Hydrogen Epoch of Reionization Array (HERA), the most sensitive SKA precursor for observations of the 21-cm line from the Cosmic Dawn and subsequent Epoch of Reionization.

        Speaker: Gianni Bernardi (Istituto Nazionale di Astrofisica (INAF))
      • 12:40
        Simulations of Galactic polarized synchrotron emission for Epoch of Reionization observations - 15' 15m

        Observations of the Epoch of Reionization (EoR) through the redshifted 21 cm line represent a new frontier in observational cosmology and have motivated the construction of several low frequency radio arrays.
        Detection of the redshifted 21 cm line emission is complicated by the contamination from foreground sources that are brighter by several orders of magnitude.
        The dominant foreground is Galactic synchrotron emission caused by cosmic ray electrons interacting with the galactic magnetic field. Synchrotron emission can also be polarized.
        Every EoR experiment with an instrumentally polarized response, may have to face a leakage of polarization into intensity. In this case, the polarized synchrotron becomes a potentially problematic foreground emission with its complex frequency dependent structure. Dedicated simulations are needed in order to estimate the level of contamination of this foreground emission.
        In this talk I will discuss how we tackle the issue of Galactic polarized emission, present our simulations and some applications to EoR studies down to Cosmic Dawn.

        Speaker: Marta Spinelli (Istituto Nazionale di Astrofisica (INAF))
    • 13:00 14:00
      Lunch break 1h
    • 14:00 14:15
      Synergies between SKA and other facilities: [chair: I. Prandoni]
      • 14:00
        Complementarity and synergy with CMB projects - 15' 15m

        The synergy between current and future cosmic microwave background (CMB) projects and the extreme sensitivity and resolution of the Square Kilometre Array (SKA) will be crucial for a wide set of themes relevant for cosmology and astrophysics at different cosmic epochs, including cosmological parameter estimation, integrated Sachs-Wolfe effect and constraints on dark energy, primordial non-Gaussianity and magnetic fields, CMB spectrum and cosmological reionization. I discuss the instrumental requirements and the observational/data analysis approaches relevant for performing these scientific investigations.

        Speaker: Carlo Burigana (Istituto Nazionale di Astrofisica (INAF))
    • 14:15 15:10
      Science with SKA Precursors and Pathfinders: Galaxy Formation and Evolution [chair: I. Prandoni]
      • 14:15
        Galaxy/AGN Evolution: ongoing activities towards the SKA - 25' 25m

        Nowadays deep radio surveys reach micro-Jy level flux densities detecting mainly star-forming galaxies and radio-quiet AGN. These are the classes of objects which have been studied for decades in the infrared, optical and X-ray bands. Moreover, radio observations are unaffected by absorption and therefore are sensitive to all kinds of AGN indipendently of orientation (e.g. Type 1s and Type 2s) and provide a dust-unobscured view on star formation achieving a better resolution than that obtained in current deep far-IR surveys. For these reasons radio observations provide a complementary and important tool to investigate the galaxy/AGN co-evolution throughout cosmic time. In this presentation I will summarize some recent results obtained from the VLA-COSMOS 3 GHz Large Project.

        Speaker: Marco Bondi
      • 14:40
        Theoretical Models of Galaxy Formation including HI - 15' 15m

        In my talk, I will present results obtained using the state-of-the-art galaxy formation model GAEA, and its most recent version including prescriptions to partition the cold gas into its atomic and molecular components (Xie et al. 2017 - X17).

        I will first discuss how the most recent observational measurements available for HI selected galaxies in the local Universe compare with prescriptions from six independently developed semi-analytic models (all run on the same cosmological N-body simulation, with X17 being the only one including an explicit treatment for the partition of cold gas in HI and H2).
        I will show that the specific treatment adopted for satellite galaxies strongly affects the final HI content at low masses but that, contrary to naive expectations, instantaneous stripping of hot gas from infalling galaxies does not translate necessarily in lower HI masses.
        In fact, I will demonstrate that stellar feedback and star formation can influence significantly the gas content of satellites.
        Finally, I will discuss the origin of the correlation between HI content of model galaxies and the spin of the parent halos.

        In the second part of my talk, I will focus on X17 and on its specific predictions for the sizes and specific angular momenta (j_*) of galaxies.
        Our model includes an explicit treatment for specific angular momentum exchange between galactic components, and the scale radii of the gaseous and stellar disks depend directly on their specific angular momenta.
        I will discuss how model predictions compare with recent observational estimates, and how they are affected by different prescriptions for cold gas accretion and stellar feedback.

        The results I will present show that the X17 model is able to reproduce both the HI content and the dynamical properties of simulated galaxies, representing an ideal tool to create dedicated mock catalogues for the interpretation of existing surveys and the preparation of future ones.
        We have developed a dedicated software to this aim.
        A first preliminary all sky mock catalog has already been made available to the SKA cosmology group working on intensity mapping.
        We plan to expand this work by extending this catalog up to higher redshift and including the 21 cm line emission of model galaxies.
        We plan to make the catalogues available to the larger SKA community.

        The results I will present have been published in Zoldan et al. (2017) and Zoldan et al. (2018).

        Speaker: Anna Zoldan (OATS - INAF)
      • 14:55
        Hosts and environments of radio-active AGN - 15' 15m

        Investigations of the population of radio-active AGN up to z=3.5 not only show that these sources are hosted by galaxies of very large, M*>10^10.5 Msun, stellar masses, but also that at all redshifts they reside in very massive dark matter halos, comparable to those associated with groups-to-clusters of galaxies. This result is found both via clustering studies and by directly pinpointing such sources to the cosmological structures they belong to. We also show how intense star-forming activity is encountered in the overwhelming majority of z>1 (massive) galaxies hosts of radio-active AGN, and how this activity is only halted by nuclear feedbacks in the relatively local universe. What emerges from our work is a scenario whereby physical processes at sub-pc/pc (e.g. AGN emission) and kpc scales strongly influence the large-scale structure behavior of the AGN and its host. Within this context, wider and deeper radio surveys are strongly foreseen in order to beat the uncertainties associated to studies confined to small regions of the sky, so to provide the ultimate answer on how these sources evolve with cosmic epoch.

        Speaker: Manuela Magliocchetti (IAPS-INAF)
    • 15:10 15:25
      Synergies between SKA and other facilities: [chair: I. Prandoni]
      • 15:10
        The IDIA Cloud and the HIPPO Project - 15' 15m

        The IDIA cloud is a cloud computing system being developed at the Institute for Data Intensive Astronomy (IDIA). The IDIA cloud is a data intensive research facility whose main aim is to facilitate the reduction and the scientific exploitation of MeerKAT data. Building on the IDIA cloud, the HELP-IDIA Panchromatic Project (HIPPO) is developing an environment for the effective multi-wavelength characterization of radio sources detected by MeerKAT. In my talk I will introduce the IDIA cloud, detail the aims and the status of the HIPPO project and demonstrate some IDIA and HIPPO use cases in a Jupyter Notebook.

        Speaker: Mattia Vaccari (Istituto Nazionale di Astrofisica (INAF))
    • 15:25 15:45
      General: The SKA Project [chair I. Prandoni]
    • 15:45 16:15
      coffee break 30m
    • 16:15 17:15
      General Discussion: [chaired by SKA Italy Board]
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