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4 Editorial 8 Foreword 13 Scientific Commission A Space Studies of the ’s Surface, Meteorology and Climate 21 Scientific Commission B Space Studies of the Earth- System, Planets, and Small Bodies of the 43 Scientific Commission C Space Studies of the Upper Atmospheres of the Earth and Planets Including Reference Atmospheres 55 Scientific Commission D Space Plasmas in the Solar System, Including Planetary 69 Scientific Commission E Research in from Space 115 Scientific Commission F Life Sciences as Related to Space 123 Scientific Commission H Fundamental Physics in Space 131 Acronyms 135 Sitography 141 Acknowledgments editorial

Italy is today deeply involved in space science with a multifaceted activity. A remarkable sequence of scientific results over the past years and a considerable number of projects driven by Italian scientists, engineers and technologists position as a frontrunner in space astrophysics and space physics. Since the launch of the on December 15, 1964 (a satellite under the management and total responsibility of Italian scientists) space research fostered in Italy during almost six decades. In mid- 1960s Italy was the third country, after USA and the Soviet Union, capable of developing and managing a space satellite. Today, tens of different space projects have Italy as an essential partner, if not the only player, for instrument development and for obtaining fundamental scientific results. Since 1988, ASI has the supervision of the Italian space program and of specific projects. This activity is performed in collaboration with all main research institutions and universities in Italy. Being the Italian research institution specifically focused on astrophysics 4 and , INAF is a major player in research related with observations and exploration of the Universe from space. INAF operates through 17 research Institutes across the country plus several major research infrastructures (the National Telescope TNG in the Canary Islands, the Large Binocular Telescope LBT in Arizona, the Radio Telescope SRT) supporting more than 1000 researchers and engineers.

INAF can then participate in investigations of space research with its own astrophysical infrastructures including radio-telescopes (the Medicina antenna and the Northern Cross, the Noto antenna, SRT), optical telescopes (the TNG, the LBT, and several telescopes in Italy and in Chile), and the -ray astrophysics AGILE satellite. Italian scientists very actively participate in international programs related with facilities and instruments of the European Southern Observatory (projected towards E-ELT). Programs and collaborations in space research involve an impressive string of Italy-led instruments in operated by programmatic partners: ESA, NASA, Jaxa, Roskosmos, CAS and others. The science range spans from space weather, and planetary science (, Bepi Colombo, Express, MRO, Osiris-Rex, , , Exomars-2016, and future Exomars-2022, Juice, Interceptor, MMX and SolarC) to optical astronomy (, Cheops, and future , Plato and Ariel) up to high-energy astrophysics (XMM-, INTEGRAL, , NuSTAR, Fermi, and future Ixpe, and eXTP). To these activities related with astrophysics and planetary science performed by INAF scientists with an increasing collaboration with INFN colleagues, we add space research in cosmic ray physics carried out mainly by INFN scientists (Pamela, AMS, Calet, Dampe, and Jem-Euso). A strong interest of the Italian astronomical community is for the Hubble observations, and a special attention will be devoted to the JWST program. and CMB studies 5 consolidated by the European mission are now done with spectrometry and experiments (Olimpo, Lspe). INAF will operate the ASTRI Mini-Array of Cherenkov telescopes in Tenerife to study sources in the TeV energy range, and is strongly involved in the development of CTA. Recent experience shows how the collection of multi-frequency spectral information from cosmic sources from radio to TeV energies is absolutely crucial for the understanding of the underlying physical processes. To complete the INAF participation in future major ground-based astrophysics projects a special mention is for the SKA radio observatory for which Italy is an important contributor. The birth of research witnessed during the last decade has major implications for the search of electromagnetic counterparts through ground-based and space observations. The Italian community is largely involved in these searches through the Virgo detector and a network of telescope and satellite follow-up programs. The space project LISA is in perspective a major endeavour with strong interests of the Italian community. Last but not least, Earth observations are an important part of the Italian space program involving remote sensing by the Cosmo- Skymed satellite constellation, the study of terrestrial gamma-ray flashes by the AGILE satellite, and the participation in the CSES program. The “philosophy” of the Italian engagement in space research is therefore based on clear and successful principles: creativity and focused involvement in instrument development and mission operations, pursuing scientific excellence of the results, a multi- frequency approach to astrophysics and space science with a combined use of ground-based and space instruments. The year 2020 marks the end of a decade and the beginning of a new one. Italy will continue to strengthen its scientific capability and will continue its participation in space science activities through national and international collaborations. Italy is more than ready to confront the challenges of space science and to contribute in a fundamental way to the scientific discoveries of the next decade. 6 7

Marco Tavani President of the Italian National Institute for Astrophysics foreword

The Italian Report to the 43rd COSPAR General Assembly, is edited by INAF, the formal Italian national body that by the law supports the COSPAR activities, with the collaboration of ASI and the other stakeholders playing a major role in the Italian scientific space programs (INFN, CNR, INGV, etc.). This Report summarizes the last two years of space science activity in Italy. In view of the appreciation received for the former editions, this year the Report has been formulated in a similar condensed form to give the relevant information in a snapshot, though providing a fully updated overview of the Italian research programs carried out from space, apologizing for any omission or misunderstanding. The Report is organized with the description of the scientific goals, technical requirements and actual realization of the space missions, enumerated following the COSPAR Scientific Commissions scheme:

Commission A: Space Studies of the Earth’s Surface, Meteorology and Climate; 8 Commission B: Space Studies of the Earth-Moon System, Planets, and Small Bodies of the Solar System; Commission C: Space Studies of the Upper Atmospheres of the Earth and Planets Including Reference Atmospheres; Commission D: Space Plasmas in the Solar System, Including Planetary Magnetospheres; Commission E: Research in Astrophysics from Space; Commission F: Life Sciences as Related to Space; Commission G: Materials Sciences in Space, and Commission H: Fundamental Physics in Space

The aim is to provide an overview of the main involvement or commitment of the Italian community in the space programs, mission by mission. We have limited the descriptions of the missions to those that are still on-going, approved or formally proposed for selection at national and international level, at our best level of knowledge at the time of this edition. The main research programs are in the field of observation of the Universe science including cosmology, planetary science, fundamental physics, Earth observation, climate and meteorology, life science in space, space related new technologies, and educational. ASI is delegated by the Italian Government to lead and support the Italian space science program, including the mandatory contribution to ESA. Other relevant contributions are provided by the national research bodies (INAF, CNR, INFN, etc.) proposing space programs, missions, satellites and observatories in different research . When the relevant peer committees approve a program, the above mentioned bodies provide staff scientists, engineers, technologists and management on contracts as well laboratories and dedicated financial support on ground and operations in space. The majority of the Italian scientific space programs are carried out in the framework of ESA funding, via the mandatory and optional programs. Italy has also a well-consolidated partnership with NASA. In addition, it has a history of on-going programs with , JAXA and other international space organizations via bilateral or multilateral agreements. More recently a broad range of programs have started with China in different scientific fields, materialized the 2nd of February 2018 with the successful launch of CSES, the China Seismo-Electromagnetic 9 Satellite, carrying on board the Italian HEPD, a High Energy Particle Detector, built under the lead of INFN, and the EFD, the Electric Field Detector, a Sino-Italian effort lead by INFN and INAF. Since the injection in the polar , CSES is successfully monitoring electromagnetic field and waves, and particles perturbations of the atmosphere, and induced by natural sources and anthropocentric emitters, and to study their suggested correlations with the occurrence of seismic events. A solid national program, including dual missions, complements these international endeavours. Italy is playing a major role in the ESA program, participating with PIs and Co-Is in the on going Large mission to : BepiColombo, Small mission for exoplanet search: CHEOPS, Medium size missions M1: Solar Orbiter, M2: Euclid, and M3: PLATO. The Italian community is also committed to the exploitation of the ESA first Large mission L1: JUICE, to the ’s icy , as well as L2: ATHENA, to study the hot and energetic Universe, and in the forthcoming L3: LISA, the Gravitational Wave Observatory to be realized with an important US participation. Among the ESA optional program, Italy participates to the ExoMars programs, with the first spacecraft already orbiting Mars and the second one, featuring a rover: a scientific exploration mission lead by ASI to bring a rover to Mars, a joint venture between Italy, ESA and . Italy has entered its 57th year of space scientific exploration: since 1964 (launch of the San Marco 1 satellite), the national scientific and industrial community has continued its path toward space science and exploration building up on the achieved record of success, investing in space programs and cooperation with other Space- Faring nations pushing to the extremes our frontier of knowledge.

Italy also has a relevant participation to the ISS with more than 40% of the habitable modules delivered by the Italian and an 10 important astronauts crew, committed to the success of the Italian and international manned space programs during the years to come. Finally, it is worth mentioning that in the last years the Italian scientific community has gained its leadership in the discoveries of Gravitation Waves (GW) from binary black holes mergers via the LIGO-VIRGO Collaboration, and of the first gamma-ray counterpart detected contemporary by INTEGRAL and FERMI in coincidence with the GW170817 signal from two coalescent neutron stars, starting the era of the “multi-” astronomy: a success of our ground and space community expected to continue in the future decades. 11

Pietro Ubertini Italian National Committee Delegate to COSPAR 12 a

SCIENTIFIC COMMISSION A Space Studies of the Earth’s Surface, Meteorology and Climate

13 Previous page: The Sentinel-2A satellite takes us over the very eastern part of the Sundarbans in Bangladesh, in this natural-colour on 18 March 2016. Contains modified Copernicus Sentinel data, processed by ESA. SCIENTIFIC COMMISSION A

cosmo-skymed

COSMO-SkyMed consists of a constellation of four The system is conceived mid-sized satellites still operating for to pursue a Multi-Mission approach thanks to its intrinsic Earth observation, funded and managed by the ASI interoperability with other and the Italian Ministry of Defense. Earth observation missions and expandability towards COSMO-SkyMed (COnstellation of small Satellites for Mediterranean other possible partners with basin Observation) represents the largest Italian investment in space different sensors typologies to systems for Earth observation. It is a dual-use (civilian and defence) end- implement an integrated space- to-end Earth observation system aimed at establishing a worldwide service based system providing Earth providing data, products and services compliant with well-established observation integrated services international standards and relevant to a wide range of applications, such to large user communities as emergency and risk management, scientific, commercial and defence and partner countries (IEM applications. The system consists of a constellation of four Low Earth Orbit capability). These features mid-sized satellites, each equipped with a multi-mode high-resolution SAR designate COSMO-SkyMed (Synthetic Aperture ) operating at X-band and fitted with particularly as a system capable to provide flexible and innovative data acquisition and transmission equipment “Institutional Awareness” in and a dedicated full featured ground infrastructures for managing the order to make proper decisions constellation and granting ad-hoc services for collection, archiving and in preventing and managing distribution of acquired remote sensing data. world-wide crisis. In particular 15 The first generation of the COSMO-SkyMed program is based on a primary mission objective is constellation of 4 medium-size satellites, each one equipped with a high- thus to meet customer’s needs, resolution SAR operating in X-band, having ~600 km single side access under economical, schedule and ground area, orbiting in a sun-synchronous orbit at ~620 km height over political constraints, for a space the Earth surface, with the capability to change attitude in order to acquire borne Earth Observation System images at both right and left side of the satellite ground track (nominal capable to provide: acquisition is right looking mode). - environmental risk and The Constellation started operations in September 2008, with the security management for both deployment of the first two satellites qualified in orbit. The deployment of civilian institutional and defence the complete constellation onto operations, with four satellites qualified in needs, through monitoring orbit, was completed in January 2011. and surveillance applications COSMO-SkyMed Mission offers today an efficient and well-established assessing exogenous, response to actual needs of Earth observation market providing an asset endogenous, and anthropogenic characterized by full global coverage, all weather, day/night acquisition risks; capability, higher resolution, higher accuracy (geo-location, radiometry, - commercial products and etc.), superior image quality, fast revisit/response time, interferometric/ services (e.g. for agriculture, polarimetric capabilities and quicker-and-easier ordering and delivery of territory management) to world- data, products and services. wide civilian user community. SCIENTIFIC COMMISSION A

cosmo-skymed second generation

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The second generation COSMO-SkyMed COSMO-SkyMed is funded by ASI in partnership with constellation is the improved version of the the Defense Ministry. It is the Italian system for Earth observation. product of the best practices among the ASI and the COSMO-SkyMed second generation (COnstellation of small Satellites national space industry, with for Mediterranean basin Observation SG) are satellites planned for Earth Leonardo S.P.A., Thales Alenia observation with state of art technologies. They will further improve the Space and also in Italian leadership in this area of strategic observations, also with the aim collaboration with several to expand strategic partnership at international level. PME. The new constellation will consist in two new technology satellites to be launched into a Sun-synchronous orbit at 619 km from the launch facility in French Guyana. The first of the two satellites was placed in orbit with a at the end of 2019, while the second is scheduled with a C. These two new satellites will be equipped with SAR (Synthetic Aperture Radar), in order to be able to provide detailed Earth observation in any meteorologic situation and illumination. 17

COSMO-SkyMed image of the summit of Mount Etna at 1 m spatial resolution. Credit: ASI. SCIENTIFIC COMMISSION A

PRISMA is an Earth Earth observation, both for scientific community and for end users, thanks to the capability to acquire worldwide a large amount of Observation System data with a very high spectral resolution and in a wide range of launched in 2019 spectral wavelengths. PRISMA provides the capability to acquire, with innovative, downlink and archive images of all Hyperspectral/Panchromatic electro-optical channels totaling 200,000 Km2 daily almost on the entire worldwide instrumentation area, acquiring square Earth tiles of 30 km by 30 km. The combined hyperspectral and panchromatic products enable the capabilities that combines of recognition of the geometric characteristics of a scene and may a hyperspectral provide detailed information about the chemical composition sensor with a of materials and objects on the Earth surface, giving enormous medium-resolution impacts to remote sensing applications. The PRISMA system panchromatic camera. includes ground and space segments. The PRISMA mission can operate in two modes, a primary mode and a secondary mode. The PRISMA (PRecursore primary mode of operation is the collection of hyperspectral and IperSpettrale della Missione panchromatic data from specific individual targets requested by the Applicativa - Hyperspectral users. In the secondary mode of operation, the mission will have an 18 Precursor of the Application established ongoing ‘background’ task that will acquire imagery to Mission) is an Earth fill up the entire system resources availability. Daily planning should observation satellite for always include the user acquisition requests and enough background monitoring of natural (systematic acquisitions) to guarantee the full usage of the entire resources and atmospheric system resources. characteristics (information The PRISMA payload consists in a hyperspectral/panchromatic on land cover and crop status, camera with VNIR (Visible and Near-) and SWIR pollution quality of inland (ShortWave InfraRed) detectors. This is able , status of coastal zones to acquire in a continuum of spectral bands ranging from 400 to and the Mediterranean Sea, 2505 nm (from 400 nm to 700 nm in VNIR and from 920 nm to soil mixture and carbon 2505 nm in SWIR) with 30 m of spatial resolution and a medium cycle). PRISMA has been resolution PAN (Panchromatic Camera, from 400 nm to 700 nm) launched on 22 March 2019 with 5 m resolution. The PRISMA Hyperspectral sensor utilizes on board a VEGA rocket. the prism to obtain the dispersion of incoming radiation on a PRISMA is a scientific and 2-D matrix detectors in order to acquire several spectral bands of demonstrative mission lead by the same ground strip. The “instantaneous” spectral and spatial ASI. It will play a significant dimensions (across track) of the spectral cube are given directly by role in the upcoming the 2-D detectors, while the “temporal” dimension (along track) is international scenario of given by the satellite motion (push broom scanning concept).

20 b

SCIENTIFIC COMMISSION B Space Studies of the Earth-Moon System, Planets, and Small Bodies of the Solar System

21 Previous page: fly free after leaving the CubeSat Deployer on the ISS. Seen here are the MinXSS and CADRE satellites. Credit: NASA Johnson. SCIENTIFIC COMMISSION B

abcs

automatic laboratory able to reagents, mixing of chemicals, ABCS is an Italian provide a highly integrated in- detection of emitted photons, mission situ multiparameter platform electronics, data storage and to be launched that uses immunoassay tests transmission) and the stability in 2020, hosting exploiting chemiluminescence of chemicals and biomolecules detection. The experiment employed in the experiment a mini laboratory will consist in a set of LFIA and necessary for performing payload for research (Lateral Flow ImmunoAssays) bioassays (e.g., immunoassays in , on nitrocellulose support exploiting chemiluminescence life sciences, where target biomolecules are detection) in space 23 biotechnology and immobilized in specific test conditions for astrobiological areas. Reagents are deposited investigations. pharmaceutics. in a non-permanent fashion In-orbit validation of the and in a dry form in the proposed technology would ABCS (AstroBio CubeSat) is a initial part (starting area) of represent a significant scientific 3U cubesat hosting the microfluidic path. When breakthrough for autonomous a mini laboratory payload the reagents-delivery-system execution of bio-analytical based on innovative lab-on provides a volume of liquid experiments in space with chip technology suitable for reagent to the starting pad, potential application in research in astrobiology, life capillary forces will guide the planetary exploration for sciences, biotechnology and reagents through the LFIA biomarkers detection, pharmaceutics. INAF/OAA microfluidic pathway. During astronauts’ healthcare, space with the collaboration of Roma the flow, liquid reagents will stations’ environmental Sapienza University have the solubilize and transport along monitoring and more. responsibility of the project, the path the deposited reagents, INAF/OAA has the that will be launched late 2020 triggering specific reactions. responsibility of the project from . The experiments will aim with the collaboration of The objective of ABCS is to at evaluating the functional Sapienza University, School of test in space environments an tests of the device (delivery of Aerospace Engineer in Roma. 24

Exploded view of the BepiColombo spacecraft components. From bottom to top these are: the Mercury Transfer Module, Mercury Planetary Orbiter, Sunshield and Interface Structure, and Mercury Magnetospheric Orbiter. Credit: ESA/ATG medialab. SCIENTIFIC COMMISSION B

BepiColombo is an ESA/JAXA mission devoted to The four sensors of the the and to fundamental SERENA (Search for Exosphere physics quests, with an important Italian Refilling and Emitted Neutral Abundances) instrument, contribution. Launched in 2018, it will arrive at with the responsibility of Mercury in 2025. INAF/IAPS, will monitor neutral energetic atoms and BepiColombo is the fifth ESA Cornerstone mission and its name is due ions of the planet exosphere. to prof. Giuseppe Colombo who discovered the spin-orbit resonance Finally the suite SIMBIO-SYS between Mercury and the Sun. (Spectrometers and Imagers for It is an ESA/JAXA mission devoted to the exploration of Mercury and MPO BepiColombo Integrated to fundamental physics quests. The BepiColombo mission is composed Observatory), with the of two modules: the MPO (Mercury Planetary Orbiter) and the MMO responsibility of INAF/OAPD (Mercury Magnetospheric Orbiter). In MPO, 11 European instruments in collaboration with INAF/ 25 are integrated. IAPS and the Parthenope BepiColombo has been launched in 2018 with an 5, and the two University (Napoli), composed modules will be inserted in orbit around Mercury at the end of 2025. of a camera, an high The main scientific objectives are related to the surface and composition resolution camera and a of Mercury, to its internal structure and environment and to the test hyperspectral Vis-NIR imager, of Einstein’s theory of . MMO includes 10 sensors will provide 50% of the data realized and integrated in Japan by JAXA. The main scientific objectives volume of the entire mission are related to the magnetosphere and exosphere of Mercury and to the through images and spectra of interplanetary medium. the entire surface of Mercury, The Italian contribution, coordinated by ASI, is very important, even in 3D. including four PI instruments on the MPO plus minor participation on other instruments on both modules. The ISA (Italian Spring Accelerometer), with the responsibility of INAF/IAPS, will measure with high accuracy non-gravitational accelerations. The MORE (Mercury Orbiter Radio science Experiment), with the responsibility of the Roma Sapienza University, will provide very accurate position of MPO with respect to the Earth and the Sun, in order to determine the parameters of the theory of General Relativity and the internal structure of Mercury. SCIENTIFIC COMMISSION B

Comet Interceptor was selected in 2019 by ESA simulation of the dusty-gas to be launched in 2028. The probe will be the environment of a possible target object are being first one to visit a dynamically new comet or developed. Since the exact possibly an interstellar body. target is not known in advance, the range of possible ESA selected Comet Interceptor in June 2019, the first ESA/F- parameters and their values class mission, which will be launched in 2028 together with Ariel, variation is very broad. The an exoplanet telescope. For the first time a will visit model is based on rather a dynamically new comet, i.e. never having approached the Sun general parameters and before, or possibly an interstellar body. Such objects are difficult to suitable for rough description target: they can only be discovered when entering the inner Solar of dusty-gas environment System. suitable for the preliminary 26 Comet Interceptor will likely be launched before its exact target planning. is even known and an observation strategy is being organized to generate the largest catalog of Solar System objects to date: the Vera As for the onboard payload, Rubin Observatory’s LSST (Legacy Survey of Space and Time). LSST Italy contributes to the is involving available ground based observational facilities and DFP (Dust, Field and pushing at the edge the technological capabilities. Plasma package) with the The LSST Solar System Science Collaboration will actively DISC (Dust Impact Sensor contribute to the identification of potential targets for Comet and Counter) and to the Interceptor. In fact, after the launch, the mission will wait at the all-sky multispectral and stable point L2 for about 2 years, waiting for the discovery polarimetric imager EnVisS from ground observations of a suitable target, which will be then (Entire Visible Sky). intercepted close to the ecliptic plane. To ensure a low-risk interdisciplinary scientific return via multi-point measurements, which will provide unprecedented 3D information on the target, Comet Interceptor consists of 3 spacecraft: after departure from L2 the main spacecraft will stay at safe distance from the target and the two small spacecraft will separate and proceed for a closer distance. In support to spacecraft operations safe planning, numerical 27

Neowise, a long period comet with a near-parabolic orbit discovered on 27 March 2020, by astronomers during the NEOWISE mission of the Wide-field Infrared Survey Explorer space telescope. Credit: Zixuan Lin. SCIENTIFIC COMMISSION B

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Ushas Mons, a 2-kilometer-high volcano in the southern hemisphere of . Credit: JPL/NASA. SCIENTIFIC COMMISSION B

The Italian contribution to EnVision is a candidate mission to explore 29 Venus with particular emphasis on geological EnVision is on the payload and consists in the Subsurface activity and its relationship with the Radar Sounder, which is a low atmosphere. frequency nadir looking radar for subsurface measurements. EnVision has been selected as one of the three candidate missions for downselection in the framework of the fifth call for Medium- class missions (M5) in ESA’s Cosmic vision 2015-2025 program. The mission, if finally selected, is planned for launch in 2032. It consists of an orbiter for Venus with three science payloads (Synthetic Aperture Radar, Subsurface Radar Sounder, IR mapper and IR and UV spectrometer suite) and a Radio Science investigation. EnVision will contribute to answer the crucial question on the reasons why Venus and Earth (the terrestrial planets) could have evolved so differently. It will determine the and current state of geological activity on Venus, and its relationship with the atmosphere. It will provide global image, topographic and subsurface data at a resolution rivalling those available from Earth and Mars, inspiring the next generation of European scientists and engineers. SCIENTIFIC COMMISSION B

ExoMars includes two missions to Mars: the first one was launched in 2016, consisting of an Orbiter plus an Entry, Descent and Landing Demonstrator Module. The second one, including a surface platform and a rover, will be launched in 2022.

ExoMars is an ESA/ROSCOSMOS program. Divided in two distinct missions, it will investigate the environment, its geochemical and geophysical characteristics, including traces of past and present and it will help gather information for future manned missions to the planet. The first mission in 2016 had two main elements, the TGO () and Schiaparelli, the EDM (Entry, Descent and Landing Module), that unfortunately crashed on the surface on September 19, 2016. The TGO, with the Italian INAF and ASI participation in 30 different instruments, including the Co-PI of NOMAD (Nadir and Occultation for MArs Discovery) and CASSIS (Colour And Stereo Surface Imaging System), is studying Mars. NOMAD is observing the gas composition of the , looking for possible biological and geological activities. The CaSSIS camera is providing stereo colour high resolution images of Martian regions. The second mission, expected for 2022, will have a European rover and a Russian surface platform. The rover combines the capacity of movement to that of drilling the surface up to 2 meters in depth. The main objective of the rover is to find evidence of past or present life, thanks to sample analysis drilled from the ground. The Russian surface platform, once the rover will be released, will study the surrounding environment with a suite of instruments, including an Italian instrument (MicroMed, INAF). The other Italian instrument is Ma_MISS (INAF), a spectrometer inside the rover’s ExoMars 2020 will investigate the drill, that will analyze the geological and biological evolution of the in search of traces of subsurface of Mars, providing the context necessary for the sample past and present life. The operation control center will be in , Italy. analysis. Italy is also responsible for the RROC in Turin, the center Credit: Altec. from which the rover will be operated. SCIENTIFIC COMMISSION B

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Didymos is a binary . The primary body has a diameter of around 780 meters. Credit: ESA. SCIENTIFIC COMMISSION AB

hera

Hera is an ESA moon of the NEO asteroid with some on-board autonomy. mission, planned Didymos to demonstrate the Mapping the shape of the for launch in 2024, ability of kinetic impactors to crater will provide unique change the orbit of an asteroid. information to validate the to rendezvous and A variation of its rotation numerical impact models study the binary period around the primary necessary to design asteroid near-Earth asteroid body is expected and will be deflection missions in future. Didymos four years measured with Earth-based In addition, it will shed light after the impact telescopes. However, a full also on the asteroid’s surface picture of the collision and properties and internal of NASA’s DART resulting momentum transfer structure thanks to the first spacecraft. will only become possible radar sounding of an asteroid. once Hera maps the mass of Hera will map Didymoon’s Hera, as currently designed, is Didymoon to a high level of entire surface down to a size planned to launch in October certainty. resolution of a few meters and 33 2024 and will rendezvous During the about six months also much of the surface of the with the binary near-Earth of Hera mission, the main primary Didymos, providing asteroid (65803) Didymos and spacecraft and its two crucial scientific data from two its little moon four years after companion CubeSats will in a single mission. the impact of NASA’s DART conduct detailed surveys of The payload consists of two (Double Asteroid Redirection both asteroids, with particular AFC (Asteroid Framing Test) spacecraft. focus on the crater left by Cameras), a PALT (Planetary Hera, named after the Greek DART’s collision and a precise Altimeter), a TIRI (Thermal goddess of marriage, is determination of the mass of Infrared Instrument) by ESA’s contribution to the Didymos B. Hera’s detailed JAXA and two CubeSats 6U international AIDA (Asteroid post-impact investigations (Juventas, with contribution Impact Deflection Assessment) will substantially enhance the from Bologna University cooperation, the first planetary planetary defense knowledge and the other one still to defense mission devoted to gained from DART’s asteroid be defined). Several Italian the deflection attempt of an deflection test. Hera will also scientists from INAF and hazardous near-Earth asteroid. demonstrate the ability to Italian universities are In 2022, the NASA’s DART will operate at close proximity members of the DART-Hera impact the 165 m diameter around a low-gravity asteroid Investigation Team. SCIENTIFIC COMMISSION B

juice

JUICE is a future ESA mission, planned for The Italian contribution to JUICE is relevant for the launch in 2022, to explore the Jupiter system payload, in particular for and the planet’s moons Ganymede, Callisto and the camera (Jovis, . Italy contribution is on four scientific Amorum ac Natorum instruments. Undique Scrutator), the imaging spectrometer JUICE (JUpiter ICy moons Explorer) is the first Large-class mission in MAJIS (Moons And Jupiter ESA’s Cosmic Vision 2015-2025 program and it is planned for launch Imaging Spectrometer), in 2022, with arrival at Jupiter in 2029. The total mission duration is the ice-penetrating radar 34 close to 11 years and with the currently envisaged launch , RIME (Radar for Icy Moons the nominal mission would end in June 2033. Exploration) and the radio It will spend at least three years making detailed observations of the science (3GM) experiments. biggest planet in the Solar System and three of its largest moons: The main Italian industrial Ganymede, Callisto and Europa. prime contractors are The moons are thought to harbour vast oceans beneath their icy Leonardo S.P.A. (for JANUS surfaces and JUICE will map their surfaces, sound their interiors and and MAJIS) and Thales Alenia assess their potential for hosting life in their oceans. The studies of the Space (for RIME and 3GM). Jovian atmosphere will be focused on the investigation of its structure, dynamics and composition. The focus on the Jovian magnetosphere will include an investigation of the three-dimensional properties of the magnetodisc and in-depth study of the coupling processes within the magnetosphere, ionosphere and thermosphere. Within the Jupiter’s satellite system, JUICE will also study the moons’ interactions with the magnetosphere, gravitational coupling and long-term tidal evolution of the Galilean satellites. JUICE will have a complement of instruments on board that includes cameras and spectrometers, a laser altimeter, an ice-penetrating radar, a , plasma and particle monitors, radio science hardware. 35

Artist’s impression of the JUICE spacecraft, as of July 2017. Credit: ESA/ATG medialab. liciacube

LICIACube is an LICIACube will be released ten Parthenope University of Italian CubeSat that days before the DART impact Napoli. The team is enriched and autonomously guided to by Bologna University, for orbit will be part of the perform a fly-by of the binary determination and satellite NASA DART mission. system after the DART impact. navigation, and Politecnico It will be launched LICIACube will collect several di Milano, for mission in 2021 to impact unique images of the effects analysis and guidance and an asteroid and of the DART impact on the optimization. asteroid and will downlink The , with demonstrate the them to Earth after the data archiving and processing, impactor method for Didymos fly-by. It will also will be managed by the ASI/ planetary defense. obtain multiple images of the SSDC. ejecta plume taken over a span of time and phase angle and LICIACube (Light Italian measure the evolution of the Cubesat for Imaging of dust distribution. Asteroids) is a 6U CubeSat LICIACube will be equipped mission that will be carried as a with two optical cameras: LEIA 36 piggyback by the NASA DART (LICIAcube Explorer Imaging (Double Asteroid Redirection for Asteroid), a catadioptric Test) mission, the first aimed to camera designed to work in demonstrate the applicability focus between 25 km and of the kinetic impactor method infinity, and LUKE (LICIAcube for planetary defense. After Unit Key Explorer), a RGB being launched in summer camera designed to work 2021, DART spacecraft will in focus between 400m and impact in autumn 2022 the infinity. secondary member of the LICIACube is being designed, (65803) Didymos binary integrated and tested by asteroid (provisionally named (Italian aerospace Didymos B). company, Torino). With a mass of 650 kg and The scientific team is led an impact velocity of about by INAF, with CoIs from 6.6 km/s, DART is expected INAF/OAR, INAF/IAPS, to change the binary orbital INAF/OAA, INAF/OAPD, period of the 160-m Didymos INAF/OATS, and with the B by about 10 minutes. support of CNR/IFAC and SCIENTIFIC COMMISSION B

Mars Express is Italy participates in five out of to an altitude of about 50 seven scientific experiments: km. MARSIS identified the an ESA mission PFS (the Planetary Fourier presence of water-ice deposits launched in 2003 Spectrometer), the MARSIS underground and revealed and still exploring radar (Mars Advanced the internal structure of the planet Mars. Radar for Subsurface and polar deposits, detecting Italy participates Ionosphere Sounding), the liquid water at the bottom OMEGA (Observatoire pour of the South polar cap. The in five of the la Minéralogie, l’Eau, les radar has also been probing seven scientific Glaces et l’Activité) imaging the upper atmospheric layer experiments. spectrometer, the ASPERA (the ionosphere) detecting (Analyser of Space Plasmas structures associated with and Energetic Atoms) plasma localized magnetic fields in Mars Express is a space instrument and the HRSC the Martian crust, which exploration mission conducted (High-Resolution Stereo originates near the surface of by ESA. Launched in 2003 Camera). Mars. OMEGA has provided and still exploring the planet The first two experiments unprecedented maps of water Mars, it was the first ESA have been developed under and carbon dioxide-ice in mission to enter orbit around Italian leadership, OMEGA the polar regions. It also 37 another planet. In addition to and ASPERA see a significant determined that the presence global studies of the surface, Italian contribution both in of phyllosilicates in some subsurface and atmosphere hardware and science, while areas of the surface is a sign of Mars with unprecedented the participation in HRSC is that abundant liquid water spatial and spectral resolution, solely scientific. existed in the early history the unifying theme of the PFS has made the of Mars. ASPERA identified Mars Express mission is the complete map to date of the solar scavenging of the search for water in its various chemical composition of upper atmospheric layers as states, everywhere on the the atmosphere, revealing one of the main culprits of planet, using different remote the presence of . If atmospheric degassing and sensing techniques with each confirmed by the Exomars escape. HRSC has shown very of its seven instruments. The Trace Gas Orbiter mission, young ages for both glacial exploration of the Martian this could indicate geological and volcanic processes, from moons, and , processes that are still hundreds of thousands to a few is a secondary objective of the active today, or even active million years old, respectively, mission, achieved via multiple biochemical processes. PFS and provided evidence of a fly-bys of Phobos about every also produced temperature planet-wide groundwater five months. maps from the surface up system on Mars. 38

A circular depression on the surface of Mars acquired in 2015 by the HiRISE camera on NASA’s Mars Reconnaissance Orbiter. Credit: NASA/JPL-Caltech/. SCIENTIFIC COMMISSION B

mro

MRO is a NASA mission launched in 2005 and still cycles on Mars. It detected studying Mars. Italy participates with SHARAD, a low- debris-covered glaciers at 39 frequency radar that probes the Martian subsurface. mid latitudes, which will constitute a fundamental resource for future colonists. MRO (Mars Reconnaissance Orbiter) is a NASA planetary It also probed young lava mission that aims at determining whether life ever arose on Mars, flows and revealed retreating characterizing the climate and geology of the planet, and preparing ice sheets in parts of the for human exploration. northern plains of Mars. The probe was launched in August 2005 and began operations at Mars in early 2006. The mission has been extended well past its original intended lifetime and it is expected to continue at least until 2021. The payload consists of six scientific instruments for the study of the atmosphere, the surface and the subsurface from orbit. ASI provided the SHARAD (SHAllow RADar) facility instrument, a low-frequency radar that can probe the Martian subsurface to depths of up to 1 km to search for ice or water. SHARAD has studied the fine internal layering of the Martian polar caps with unprecedented detail, providing into its geological history and climate SCIENTIFIC COMMISSION B

osiris-rex

NASA launched in The objectives of the mission are: 2016 OSIRIS-REx, a - To map the global, chemical, and mineralogical properties of the mission to collect asteroid in order to characterize its geological and dynamic history a fragment of the and to provide the context for the collection of the sample. primitive carbon- - To document the structure, morphology, and spectroscopic properties of the regolith in the sampling area at the 40 rich asteroid Bennu millimeter scale. and return it to - To measure the Yarkovsky effect - the thermal force acting on the Earth in 2023. asteroid - on an asteroid potentially dangerous for the Earth and define the properties of the asteroid that contribute to this effect. OSIRIS-REx (Origins, - To characterize the integrated global properties of a carbon- Spectral Interpretations, rich primitive asteroid to allow a direct comparison with the Resource Identification, observations of the entire asteroid population from the ground. Security - regolith EXplorer) - To bring to the ground and analyze a sample of carbon-rich is a New Frontiers NASA primitive regolith in a quantity sufficient for the study of the mission that will travel to the nature, history and distribution of the minerals and the organic near-Earth asteroid Bennu material of which it is composed. 1999 RQ36 and bring back The group of INAF/OAA and INAF/OAR analyzed data of to Earth a small sample the OVIRS (OSIRIS-REx Visible and Infrared Spectrometer) (about 60 g) for study. The and the OTES (OSIRIS-REx Thermal Emission Spectrometer) mission launched Sept. 8, spectrometers on board of OSIRIS-REx, acquired spectroscopic 2016, from Cape Canaveral, data in laboratory and made comparison with laboratory reached Bennu in 2018 and measurements. The group of INAF/OAPD studied the global and will return a sample to Earth local distributions of the boulders present on the surface of the in 2023. asteroid Bennu, analyzing the sampling sites.

42 SCIENTIFIC COMMISSION C Space Studies of the Upper Atmospheres of the Earth and Planets Including Reference Atmospheres

43 Previous page: Some storms on Jupiter are quite complex. These one were captured by the NASA’s robotic Juno spacecraft. Credit: NASA/JPL-Caltech/SwRI/MSSS. SCIENTIFIC COMMISSION C

cses constellation

CSES Constellation, ionosphere, the magnetosphere 5-100 MeV for electrons and 15- and the Van Allen belts due to 300 MeV for protons. the first one launched electromagnetic phenomena The EFD-02 (Electric Field in 2018, are scientific of natural and anthropogenic Detectors) developed by INAF/ missions to monitor origin, and to study their IAPS and INFN has been perturbations in correlation with seismic events. specifically designed to monitor the ionosphere, the Furthermore, the CSES mission electromagnetic fields (from allows to study the physical DC to 3.5 MHz) for the study of magnetosphere properties of the ionospheric Space Weather and ionospheric and the Van Allen plasma at the satellite altitude, to disturbances possibly related to belts. CSES satellites characterize the ionosphere in seismic activity and earthquake operate in a Sun- quiet and disturbed conditions. preparation mechanisms. The synchronous circular The mission will cover other new design of the instrument relevant topics as the study of will allow the detection of orbit at an altitude of solar perturbations, namely environmental irregularities about 500 km. CMEs (Coronal Mass Ejections) in a wider range of plasma and SEPs (solar flares, solar density, thus including extreme CSES (China Seismo- energetic particles), the cosmic phenomena induced by transient Electromagnetic Satellites) is ray modulation and the X-ray electric fields. 45 a constellation program by variation. Italy participates The environmental plasma CNSA and ASI that cooperate with several universities and parameters, including ion for instruments development, research institutes. INAF and density, temperature, drift calibration and data analysis. INFN are directly involved in velocity, composition and density The satellites, 3-axis attitude instrumental development and fluctuation, are monitored by the stabilized, are based on the test respectively. The HEPD-01 CSES PA (Plasma Analyser) and Chinese CAST2000 platform and 02 (High-Energy Particle by two Lp (Langmuir probes) designed to operate in a 98° Sun- Detector), developed by INFN developed by NSSC. Their synchronous at an and several Italian Universities, functionalities are tested at the altitude of 500 km. CSES-01 has detects high energy electrons, Plasma Chamber at INAF/IAPS been successfully launched from protons and light nuclei. Their in order to check their sensitivity Jiuquan Satellite Launch Center main objective is to measure in detecting the ionospheric on 2 February 2018, and its the increase of the electron plasma parameters. Italian expected lifetime is 5 years, while and flux due to short- collaboration will be renewed the launch of CSES-02 is foreseen time perturbations of Earth’s for instrumental development for March 2022. The main environment caused by cosmic, and calibration, and for the data objectives of the missions are solar, and terrestrial phenomena. analysis. to monitor perturbations in the The energy range explored is 46 47

The satellite Zhangheng 1 launched on 2 February 2018. Credit: Wang Jiangbo/Xinhua. duster

The DUSTER project is aimed at uncontaminated in-situ collection, retrieval and laboratory analysis of stratospheric solid particles from the upper stratosphere.

48 DUSTER (Dust in the Upper Stratosphere Tracking Experiment and Retrieval) is a multinational project aimed at collecting and retrieving solid micron-submicron dust from upper stratosphere (altitude >30km). Dust particles are collected and analyzed in laboratory by state of the art analytical techniques for a physico-chemical characterization and disentanglement of the terrestrial and extra-terrestrial component. DUSTER results are related with planetology, astrophysics and atmospheric physics. Solid and condensed sub-micrometre particles present in the stratosphere are a mix of terrestrial and extra-terrestrial dust. The extra-terrestrial component is highly represented in the upper stratosphere while volcanic ejected residues are more prevalent in lower stratosphere. The main and most ambitious goal is the collection and characterization of Solar System debris particles <3 microns not sampled by the stratospheric aircraft/NASA collection facility. In addition, no other instrument/ facility does currently sample the upper stratosphere. DUSTER provides a record of the amount of solid , their size distribution, shapes and chemical properties in the upper stratosphere, for particles down to about 0.5 micron in size. SCIENTIFIC COMMISSION C

Two fully successful DUSTER flights were performed from the Stratospheric Base in Svalbard Islands, Norway in June 2008 and July 2009, supported by ASI and a third flight was performed in 2011 from Kiruna, Sweden, thanks to CNES. The PNRA funded a DUSTER launch campaign from Antarctica, which took place at the end of 2016. Compositions, morphologies and structure of the analyzed particles, which were randomly collected in the upper stratosphere during the 2008 and 2011 49 flights, are consistent with ultra-rapid, non-equilibrium processes and fragmentation of extra-terrestrial entering the Earth atmosphere. In the frame of the HEMERA H2020 program, a flight was performed in September 2019 from the SSC launch facility. These campaigns collected about 200 stratospheric particles and analysis to understand the origin are on going. Thanks to DUSTER for the first time extraterrestrial dust from these sources has been intercepted while settling in the Earth’s Stratosphere. The project has been supported by ASI, PNRA, CNES, the Italian Ministry of the Environment, the Italian Ministry of Instruction, Research and University, the Foreign Ministry and Regione Campania. DUSTER could become a permanent facility for extraterrestrial dust collection in the upper stratosphere. The Italian man power contribution is assured by INAF/IAPS and Parthenope University, Science and Technology Department (Napoli). SCIENTIFIC COMMISSION C

juno

NASA’s Juno mission spacecraft entered the orbit footprints of the moons; a new to Jupiter, launched of Jupiter on 4 July 2016 and, understanding of the structure in 2011, is devoted based on the current mission of the “core” of Jupiter. to study the planet’s plan, will extend its nominal Italy participates to Juno with interior, atmosphere phase to mid-2021. The current two scientific instruments: the 50 mission profile includes 33 KaT (Ka band Transponder) and magnetosphere elliptical lasting 53.5 and JIRAM (Jovian InfraRed with the goal of days each. The passages above Auroral Mapper). understanding its the planet are at an altitude The radio science Ka-band origin, formation and of about 5000-8000 km; as frequency translator KaT evolution. of 1/3/2020, 24 orbits were is the core element of the performed. gravity experiment on Juno Juno is a NASA New Frontiers Among the main scientific for mapping the gravitational mission devoted to an in-depth results: the discovery of field of the planet. It was study of Jupiter, launched regular cyclone polygons developed by Thales Alenia in 2011. Juno scientific in the Jupiter poles; the Space and ASI, under the objectives are the study of the structure of the below scientific responsibility of the planet’s magnetosphere, its the visible surface of Jupiter; Roma Sapienza University. radiation environment and the presence of the “blue dot” It has a frequency stability the electromagnetic fields, in its magnetic field; new of a few parts in 10-16 at the auroras, the atmospheric volcanoes and hot spots on the an integration time of 1000 composition and structure, moon Io; the fine morphology seconds, corresponding to a the gravitational field and of the auroral restrictions in range rate accuracy of about the planet interior. The Juno the correspondence of the 0.0001 mm/s. The end-to- end radio system, including of the thermal emission of to observe the moons of Jupiter the media and ground station the planet near the 5 micron Io, Europa, Ganymede and contributions, has attained spectral window and of Callisto, providing information range rate accuracies of 0.0015 the characterization of the about the temperature and mm/s after all calibrations planetary emission with a surface composition and, in have been applied. Coherent resolution of 9 nm. The spatial the case of Io, the position and 51 X-and Ka-band links will resolution of the instrument morphology of the “hot spots”. enable precise measurement of at 1 bar can vary from 10 km JIRAM was built according to spacecraft motion during close to 300 km depending on the the specifications provided by polar orbits to determine the position of the spacecraft INAF/IAPS. The JOC (JIRAM gravity field, distribution of with respect to the planet. Operative Center) team is at mass, core characteristics, and The primary objectives of INAF/IAPS and follows the perhaps convective motion in JIRAM are the study of the entire operational phase of the the deep atmosphere. polar auroras and the Jovian mission from planning of the JIRAM has been manufactured atmosphere up to the depths observations, to generation by Leonardo S.P.A. and it’s (depending on the presence of the operating sequences of activity is under the scientific of clouds and atmospheric remote controls, to collection responsibility of INAF/IAPS. opacity) of 3-5 bars in terms and calibration of data up to JIRAM includes a spectrometer of chemical composition delivery (as foreseen for the and a camera in the infrared related to some minority mission) to the “Planetary wavelength range between 2 gases (water, ammonia and Atmospheric Node” of NASA’s and 5 µm. JIRAM provides phosphine), microphysics “Planetary Data System”. maps and spectra of the (clouds) and atmospheric auroras generated by H3+, dynamics. JIRAM is also used 52

A Junocam view of Earth taken during Juno’s close flyby on 9 October 2013. The image includes a view of the Argentinean coastline with reflections, or specular highlights, off the Rio Negro north of Golfo San Matias, as well as cloud formations over Antarctica. Credit: NASA/JPL-Caltech/MSSS.

54 SCIENTIFIC COMMISSION D Space Plasmas in the Solar System, Including Planetary Magnetospheres

55 Previous page: The Sun photographed by the Atmospheric Imaging Assembly of NASA’s Solar Dynamics Observatory. Credit: NASA/SDO. SCIENTIFIC COMMISSION D

aspiics

The ASPIICS Proba-3 technological mission, which is devoted to prove coronagraph is the high-precision formation-flight guest payload of technologies. 57 the ESA’s Proba-3 A pair of satellites will fly technological together maintaining a fixed mission. It includes configuration as a large rigid structure in space. The two two spacecrafts in satellites will form a 150-m long flight formation and solar coronagraph to study the is developed by a Sun’s faint corona closer to the European consortium solar limb than has ever been including ASI. achieved before from space invisible light. ASPIICS (Association of ASI and INAF, as part of a Spacecraft for Polarimetric large European consortium, are and Imaging Investigation of responsible for coronagraphic the Corona of the Sun) is a calibrations, optimization of coronagraph imaging the solar the occulter and for formation- corona out to 3 solar radii. With flying metrology system and a launch foreseen in 2022, it for contributing to the spectral is under development for ESA filter. SCIENTIFIC COMMISSION D

Cluster is a fleet of formation, which carry an four spacecrafts identical set of instruments for the in situ measurements of launched in 2000, 58 charged particle and fields. which provided in Italy, in the framework of an situ tridimensional international collaboration, measurements contributed to the development allowing significant of the mechanics and the onboard software of the CIS advance in the (Cluster Ion Spectrometry) knowledge of experiment. Cluster scientific fundamental space data analysis in Italy pertains plasma processes. to the study of fundamental plasma processes as magnetic reconnection and turbulence Cluster is an ESA Horizon 2000 occurring in the key regions of cornerstone mission launched the magnetosphere. in 2000, extended until 31 December 2020, with indicative extensions for an additional two years, up to 2022. Cluster The explosive realignment of comprises four spacecrafts, magnetic fields. Credit: NASA flying in a tetrahedral Goddard/SWRC/CCMC/SWMF 59 60 61

Bright threads of solar materials visible over the sunspots. Credit: NASA/JAXA.

Hinode is a Japanese and dynamic corona. INAF has been directly involved in mission with USA the calibration of the XRT 62 and UK contributions, telescope, with its XACT/ launched in 2006, OAPA laboratories in Palermo. observing the Sun in Hinode scientific data analysis the optical, EUV and in Italy pertains to the study of the fine magnetic dynamics X-ray bands. and structure of the active Hinode is a JAXA solar mission photosphere (SOT), of the (Japan) launched in 2006, eruptions and holes, the hot devoted to the study of solar intermittent components and activity. A set of instruments the fine thermal structure of the in the optical (SOT, Solar corona (EIS, XRT). The Optical Telescope), EUV (EIS, of Venus observed also with the Extreme Imaging XRT has been used to probe the Spectrometer) and X-ray bands upper planetary atmosphere. (XRT, X-Ray Telescope) are on-board Hinode. Italy has worked on the instrument calibration and studied the magnetic photosphere, the hot SCIENTIFIC COMMISSION D

score

Prototype of the is part of the HERSCHEL program approved by Solar Orbiter NASA and led by the Naval coronagraph Research Laboratory, US. Its 63 Metis, SCORE second flight in 2021 is in was successfully preparation. SCORE is the launched in 2009 first multi-band coronagraph obtaining simultaneous as part of the NASA images of the solar corona in suborbital flight polarized visible light, in the program HERSCHEL, UV and EUV Ly alpha lines with a second flight of H and He, respectively. foreseen in 2021. In the 2009 flight, the first maps in Helium emission and SCORE (Sounding Rocket abundance of the solar corona Coronagraphic Experiment), have been obtained. prototype of the Solar SCORE, an INAF-ASI Orbiter coronagraph Metis, instrument, has been was successfully launched developed by INAF/OATO in a suborbital flight in and by the Forenze University. 2009 from the White Sands Missile Range, US. SCORE 64

Artist impression of ESA’s Solar Orbiter spacecraft. Credit: ESA/ATG medialab. SCIENTIFIC COMMISSION D

solar orbiter

Solar Orbiter is ESA’s exceeding 30°, towards the end corona in the range from 1.6 of the mission, which will allow to 3.0 solar radii at minimum primary contribution to observe the polar regions perihelion (0.28 AU), and to the ILWS from above. These observations from 2.8 to 5.5 solar radii at (International Living from remote, together with 0.5 AU. With a Star) program. the measurements provided The scientific payload of Solar Launched in 2020, by the in-situ instruments, Orbiter also includes SWA will represent the necessary ( Analyser), a it will contribute to ingredients to unravel the plasma analyser suite with 4 reveal how the Sun mechanisms at the basis of sensors and a single, common creates and drives the generation and heating of the DPU (Detector Processing heliosphere. solar corona. Unit). The DPU has an Italian The scientific payload includes Co-PIship (INAF) and has Solar Orbiter is an ESA Cosmic the Metis coronagraph, been realized in Italy with 65 Vision M1 mission launched consisting in a coronal imager the ASI support. SWA will on 9 February 2020 with a working in both polarized VL measure particle velocity nominal science phase due to and UV light. This coronagraph distribution functions of begin in December 2021. Solar has an Italian PIship (Firenze protons, helium, minor ions Orbiter will provide the unique University) and is realized and electrons of the solar wind opportunity to discover the in Italy under ASI contract, with unprecedented sampling fundamental links between the exploiting the legacy of UVCS/ time resolution, of the order of magnetized solar atmosphere SOHO. (MPS) and the proton scales. There is also and the dynamics of the solar (CAS) provide a participation of the group wind that, ultimately, is the a hardware contribution. Metis of Genova (University, CNR/ source of space weather. can simultaneously image the SPIN) to the Spectrometer The Solar Orbiter unique visible and ultraviolet emission Telescope for Imaging X-rays mission profile allows the of the solar corona and (also supported by ASI). The investigation of the Sun at very diagnose, with unprecedented Italian contribution (CoIship) high spatial resolution by taking temporal coverage and spatial consists in the flight software advantage of a close-by vantage sampling element (down to for flare detection and real- point at a perihelion of 0.28 AU about 2000 km), the structure time science data analysis. and of an and dynamics of the full SCIENTIFIC COMMISSION D

stereo

(Solar Terrestrial Probes) program. It consists of two space-based 66 STEREO consists of observatories, one ahead of Earth in its orbit, the other trailing two space-based behind. They separate from Earth in opposite directions at a rate observatories, one of 22° per year, in order to obtain a stereoscopic view of the solar ahead of Earth in atmosphere. The two spacecrafts are equipped with the same set of its orbit, the other instruments for remote sensing and in-situ observations of the Sun trailing behind. and of the heliosphere. The Italian solar physics community is involved in the analysis of Launched in 2006 data from the instruments SWAVES (STEREO/Waves), IMPACT by NASA, its goal (In-situ Measurements of Particles And Cme Transients) and is to study the PLASTIC (PLAsma and SupraThermal Ion Composition), finalized structure and to the investigation of turbulence in the solar wind and particle evolution of solar acceleration, and from the instruments COR2 (Outer Coronagraph) and Secchi HI (Heliospheric Imager), designed storms. to study the solar wind acceleration with correlation tracking techniques and the physics of coronal mass ejections. STEREO (Solar TErrestrial RElations Observatory) has been launched in 2006 as the third mission in NASA’s STP

68 SCIENTIFIC COMMISSION E Research in Astrophysics from Space

69 Previous page: The AGILE satellite ready for launch. Credit: ASI. SCIENTIFIC COMMISSION E

AGILE is an X-ray and gamma-ray astronomical satellite by ASI, launched in 2007.

AGILE (Astro rivelatore Gamma a Immagini LEggero) is an ASI space mission dedicated to high-energy astrophysics. The main 71 goal is the simultaneous detection of hard X-ray and gamma-ray radiations in the 18-60 keV and 30 MeV-30 GeV energy bands, with optimal imaging and timing capability. The AGILE satellite was launched on 23 April 2007 from Sriharikota () in an equatorial orbit. Since then, AGILE contributed very significantly to the study of Galactic and extragalactic cosmic sources. The main scientific results are the surprising discovery of transient gamma-ray emission and extreme particle acceleration in the Crab Nebula; the direct evidence for hadronic cosmic-ray acceleration in Supernova Remnants; the detection of intense gamma-ray flares from blazars (e.g., 3C 454.3 and 3C 279); the observations of and wind nebulae; the discovery of transient gamma-ray emission from the Cygnus X-3 and Cygnus X-1; the observations of GRBs; the detection at the highest energies of TGFs (Terrestrial Gamma-Ray Flashes). Particular care is devoted to multi-frequency programs in synergy with radio, optical, X-ray and TeV observations. AGILE has also a great capability for the detection of counterparts of gravitational wave sources. SCIENTIFIC COMMISSION E

72

A hot planet transits in front of its parent star in this artist impression. Credit: ESA/ATG. SCIENTIFIC COMMISSION E

Selected as ESA M4 mission to be launched in The Italian contribution to ARIEL is relevant, with two Co-PIs 2028, ARIEL will study the atmospheres of a of the mission and important large and diverse sample of exoplanets across contributions for the hardware the optical and infrared bands. of the telescope, including the telescope responsibility and the ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) realization of an innovative 1-m 73 was selected as ESA M4 mission for launch in mid-2028, to observe a large primary mirror, entirely built in number (~1000) of warm and hot transiting gas giants, Neptunes and aluminum, electronics, software, super- orbiting a range of host star types using transit and ground segment, with the in the ~1-8 μm spectral range and broadband photometry in the optical. responsibility of the coordination Because of their high temperatures, the well-mixed atmospheres of the of the science ground segment. majority of ARIEL’s planets will show limited or minimal condensation In addition, Italian researchers and sequestration of less volatile materials and will reveal their bulk and chair some of the scientific elemental composition (especially C, O, N, S, Si). Observations of the working groups built within the exo-atmospheres will allow to explore the link between the planets and international consortium for the their formation environments in circumstellar discs, and to understand scientific consolidation of the the earliest stages of planetary and atmospheric formation and their mission. Several Italian scientific subsequent evolution. ARIEL will thus provide a truly representative picture institutes, laboratories and of the chemical nature of the exoplanets, contributing to put our own universities participate to ARIEL’s Solar System in context, and relate this directly to the characteristics and scientific and technological chemical environment of their host stars, exploring the interaction of stars activities. with their planets in a large range of star-planet configurations. To address this ambitious scientific program, ARIEL is designed as a dedicated survey mission for transit and eclipse spectroscopy, capable of observing a large and representative planetary sample within its 4-year mission lifetime. SCIENTIFIC COMMISSION E

AstroSat is an Indian keV, 8000 cm2 @ 10 keV, only one of them is operating since mission launched 2019), a soft X-ray telescope in 2015 to study (0.3-8 keV, 120 cm2 @ 1 keV), celestial sources in a CZTI (Cadmium-Zinc- X-ray, optical and Telluride Imager) coded-mask UV spectral bands imager (10-150 keV, 480 cm2) and an All-Sky monitor. It is simultaneously. It 74 operated as an observatory. opens a window An open AO for 10% of onto X-ray fast observing time has been timing, with an released in 2017, increased to interactive software 20% in 2018. Since 2019, all observing time is open to the developed by INAF. world through annual calls of AstroSat is the first dedicated opportunity. Indian astronomy mission The Italian participation is aimed at studying celestial through the software for sources in X-ray, optical timing analysis GHATS, and UV spectral bands developed at INAF/OAB, for simultaneously. the analysis of bright X-ray It was launched on 28 sources. One Italian scientist is September 2015 into a LEO part of an instrument team and (Low Earth Orbit). It carries currently collaboration projects on board two 38-cm optical/ with INAF/OAB scientists are UV telescopes, an array of 3 ongoing. proportional counters (3-80 75

Hoisting of PSLV-C30 (AstroSat mission) second stage during vehicle integration. Credit: Indian Space Research Organisation. SCIENTIFIC COMMISSION E

athena

ATHENA is a observatories inaugurated by Chandra and XMM-Newton, offering transformational capabilities in several key areas. It is conceived to large ESA X-ray answer some of the most pressing questions in astrophysics for the early observatory with 2030s that can uniquely be addressed with X-ray observations. 76 a launch planned ATHENA will transform our understanding of two major components for 2031 that will of the Cosmos. The hot Universe: the bulk of visible matter in the address the most Universe comprises hot gas which can only be accessed via space-based facilities operating in the X-ray band. Revealing this gas and relating pressing questions in its physical properties and evolution to the cosmological large-scale astrophysics for the structure and to the cool components in galaxies and stars, is essential early 2030s. if we want to have a complete picture of our Universe. The energetic Universe: accretion onto black holes is one of the major astrophysical ATHENA (Advanced energy generation processes, and its influence via cosmic feedback Telescope for High-Energy is profound and widespread. X-ray observations provide unique Astrophysics) is a large X-ray information about the physics of growth, the causes and observatory and the second effects of the subsequent energy output, as well as revealing where in large-class ESA mission (L2), the Universe black hole accretion is occurring and how it evolves to the with a launch planned for 2031 highest redshifts. and currently in B phase. Its The Italian community has a key role as regards both the scientific part adoption is planned at the end and the instruments of the mission, supported by ASI. of 2021 with C phase starting in 2022. It will continue the series of large X-ray calet

CALET is an experiment that reached the ISS in elements up to Z=40 will be studied. To date, CALET 2015 to search for possible signatures of dark has contributed to several matter in the spectra of electrons and gamma gamma-ray transients rays. detections by mean of the 77 dedicated GBM (Gamma-ray Burst Monitor) as well to the CALET (CALorimetric Electron Telescope) is a mission by JAXA in interpretation of the cosmic collaboration with ASI and NASA, that reached the ISS in August ray e+/e− spectrum from 2015 starting an initial 5 year period of data taking on the JEM-EF 10 GeV to 3 TeV and other exposure facility. Thanks to its success, CALET experiment operative cosmic ray studies. life has been extended up to March 2021 with a further extension up to 2024. CALET main science objective is the exploration of the electron spectrum above 1 TeV whose shape might reveal the presence of nearby acceleration sources at kpc distance from Earth. With excellent energy resolution, proton rejection capability and low background contamination, CALET is searching for possible signatures of dark matter in the spectra of electrons and gamma rays. Deviation from a simple power-law in proton and He spectra will be studied with high precision in the region of a few hundred GeV and extended to the multi-TeV region and to heavier nuclei. Energy spectra, relative abundances and secondary-to-primary ratios of cosmic nuclei from proton to iron will be measured. Heavier chandra

Chandra is a high beam surveys in order to a Gravitational Wave event. angular resolution disentangle the origin of the Chandra combines the X-ray telescope X-ray background. Moreover, mirrors with four science Chandra allowed to separate instruments to capture launched in 1999 close-by double AGN in and probe the X-rays from 78 to detect emission merging galaxies and to astronomical sources. The from very hot detail AGN eclipses due to incoming X-rays are focused regions of the gas and dust clouds inclose by the mirrors to a tiny Universe such as AGN. Chandra was also used spot (about half as wide as to study clusters and a human hair) on the exploded stars, in particular the interactions plane, about 30 feet away. clusters of galaxies between the central giant The focal plane science and matter around galaxy and the intra-cluster instruments, ACIS (Advanced black holes. medium. Chandra was, and CCD Imaging Spectrometer) actually is, fundamental to and HRC (High Resolution The Chandra X-ray study celestial objects in Camera), are well matched observatory has been the crowded fields of the to capture the sharp images launched on 23 July 1999. Milky Way. In particular, formed by the mirrors and Since the launch, scientists Chandra gave a fundamental to provide information about all over the world took contribution in the study of the incoming X-rays: their advantage of the excellent the present and past activity number, position, energy and imaging capabilities of the of the nucleus of our own time of arrival. ACIS is one of observatory. These were Galaxy, and the discovery of two focal plane instruments used to perform deep pencil the first X-ray counterpart to and it is an array of CCDs, SCIENTIFIC COMMISSION E

which are sophisticated (1/8 the thickness of a human behind the mirrors, where versions of the crude CCD’s hair) and 1.2 millimeters they redirect (diffract) the used in camcorders. This long. HRC is especially useful X-rays according to their instrument is especially for imaging hot matter in energy. The X-ray position is useful because it can make remnants of exploded stars, measured by HRC or ACIS, X-ray images, and at the and in distant galaxies and so that the exact energy 79 same time, measures the clusters of galaxies, and for can be determined. The energy of each incoming identifying very faint sources. science instruments have X-ray. ACIS is the instrument Two additional science complementary capabilities of choice for studying instruments provide detailed to record and analyze temperature variations information about the X-ray X-ray images of celestial across X-ray sources such energy, the LETG (Low objects and probe their as vast clouds of hot gas Energy Transmission Grating physical conditions with in intergalactic space, or Spectrometer) and HETG unprecedented accuracy. chemical variations across (High Energy Transmission The INAF/OAPA has been clouds left by supernova Grating Spectrometer) involved in the instrumental explosions. The primary spectrometers. The LETG development and calibration components of the HRC are gratings are designed to cover of the filters of the High two MCP (Micro-Channel an energy range of 0.08 to 2 Resolution Camera on board Plates). They each consist keV, while the HETG gratings Chandra. of a 10 cm square cluster of a 0.4 to 10 keV energy range. 69 million tiny lead-oxide These are grating arrays glass tubes that are about which can be flipped into 10 micrometers in diameter the path of the X-rays just 80

Previous page: Lorem ipsum Artist’sdolor sit impression amet lorem of ipsumthe CHEOPS dolor sit satellite.amet lorem Previous ipsum page: dolor The sit ametPerseus Clusterlorem ipsum Waves. dolor Credit: sit ESA/NASA.amet SCIENTIFIC COMMISSION E

CHEOPS is the first small mission in ESA members of the Core Science Team are leading the studies Cosmic Vision 2015-2025 program. It was of multiplanetary systems 81 launched in 2019 to study the internal via the TTV technique, structure of small-size transiting planets. and the CHEOPS Ancillary Science. CHEOPS in Italy CHEOPS (CHaracterising ExOPlanet Satellite) is mainly dedicated is made by a collaborative to the determination of the internal structure of small-size efforts of INAF (INAF/OACT transiting planets by means of ultrahigh precision photometry of and INAF/OAPD), Padova their parent stars. It is the first small mission in ESA Cosmic Vision University, and ASI. 2015-2025 program. Launched in 2019, it will provide the targets to the future ground (e.g. E-ELT) and space-based (e.g. JWST, Ariel) facilities, that will be used to characterize the exoplanet atmospheres. CHEOPS is a joint ESA-Switzerland mission, with important contributions from Italy and other ESA member states. Funded by ASI, the Italian contribution to the payload was the integration and testing of its 32 cm telescope, whose optical parts were designed by INAF and produced by the TJV made by Leonardo S.P.A., and Media Lario SrL. INAF and ASI contributed before launch to the preparation of the scientific program and the realization of the mirror archive for the scientific data. Italian SCIENTIFIC COMMISSION E

dampe

82 DAMPE is a Chinese space telescope for high energy gamma-rays, electrons and cosmic rays detection, in a sun-synchronous orbit at the altitude of 500 km since 2015.

DAMPE (Dark Matter Particle Explorer, also known as Wukong), is a Chinese CAS satellite launched on 17 December 2015, with main scientific objective to measure electrons and photons with much higher energy resolution than currently achievable, in order to identify possible Dark Matter signatures. DAMPE is composed by a double layer plastic scintillator, a STK (silicon-tungsten tracker-converter), made of 6 tracking double layers of silicon strip detectors with three layers of Tungsten plates for photon conversion, and an imaging calorimeter (BGO, Bismuth Germanium Oxide) of about 31 radiation lengths thickness, made up of 14 layers of Bismuth Germanium Oxide bars in a hodoscopic arrangement. The Italian contribution, under the leadership of INFN - Perugia, has been in the design and construction of the STK, and is currently focused on the detector calibration and data analysis. 83

First data from DAMPE space mission. Credit: Paolo Bernardini. euclid

Euclid, to be Oscillations and redshift-space distortions, derived from the spatial distribution of galaxies as a function of redshift (i.e. of Universe time launched in 2022, evolution), will be used to study Universe expansion rate. This is will investigate the supposed to be governed by Dark Energy, which represents almost 75% distance-redshift of the matter-energy content of the Universe today. relationship and the Two cryogenic instruments detect radiation collected simultaneously evolution of cosmic over more than 0.5 sq deg on the sky by a 1.2 m diameter telescope made of SiC: VIS (visible panoramic camera) and NISP (Near-IR structures, galaxies Spectro-Photometer). VIS, with its 36 4Kx4K CCDs (0.1 arcsec/ and clusters of pixel) will be able to measure the shape of 1.5 billion galaxies down to 84 galaxies. magnitude 24.5. NISP will provide photometric redshift (Y, J, H) for the imaged sources and more than 30 million accurate redshifts from Euclid, to be launched in 2022 slitless spectroscopy using H-alpha emission lines. to an L2 orbit, will observe The Euclid Consortium is composed of more than 250 institutes from more than 15000 square 16 European countries, with the participation of NASA. Italy is leading degrees of extragalactic sky in the Science Ground Segment and delivered the Detector Control and a 6 year long mission. Euclid Data Processing Units, along with their On-Board softwares, for both will investigate the evolution instruments, and the NISP Grism Wheel. Italian scientists have key of the Universe during the last roles in all scientific areas in the consortium and in the ESA Euclid 10 billion years, by accurately Science Team. tracking gravitational effects on expansion rate and cosmic structure growth. Tiny distortions, induced on galaxies shape by the presence of Dark Matter along the line of sight, will allow gravitational field to be reconstructed with 3D maps. Baryonic Acoustic SCIENTIFIC COMMISSION E

fermi

Launched in 2008, Fermi observes the cosmos we now know 50 Geminga-like neutron stars. using the highest-energy form of light, providing The Italian participation an important window into the most extreme encompasses several phenomena of the Universe and playing a contributions starting with crucial role in the newly born multi messenger the design, construction astronomy. and calibration of the LAT tracker, performed by INFN under ASI responsibility, and The Fermi Gamma-ray Space Telescope mission was launched on the exploitation of the data 11 June 2008 by a Delta II rocket. Fermi is a NASA mission with a by INAF, INFN and Italian 85 wide international collaboration from Italy, Japan, , Germany universities. Additional tasks and Sweden. Thanks to the detection of gamma-rays from a neutrino such as software development, emitting AGN and from a Gravitational Waves event produced by a management of the Italian NS-NS merger, in the summer of 2017 Fermi contributed to the birth data archive mirror as well of multi-messenger astronomy. Thanks to its capabilities, Fermi has as scientific data analysis are collected 4 Bruno Rossi prizes, the most prestigious acknowledgment in jointly performed by INFN and the high energy astrophysics. ASI/SSDC. The scientific payload is composed of the LAT (Large Area Telescope), The first astrophysical operating in the 20 MeV-300 GeV energy range, and the GBM counterpart of a Gravitational (Gamma-ray Burst Monitor), operating in the 10 keV-25 MeV energy Wave was detected on 17 range. Fermi is operating in sky survey mode and the LAT observes the August 2017. After a long quest, entire sky every 3 hours, providing uniform exposure on the timescale Fermi and INTEGRAL detected of days. The high sensitivity and nearly uniform sky coverage of the LAT a short γ-ray burst caused by make it a powerful tool to investigate the properties of all high-energy the merger of two neutron astrophysical sources. After more than 11 years of successful operations, stars: it was the start of the the Fermi LAT fourth Source Catalog exceeds 5,000 entries. While more Multimessenger Astrophysics. than 3,000 sources have been identified or associated with active galactic nuclei, pulsars are the second most numerous source class with about 250 objects a third of which were not known before Fermi LAT; notably SCIENTIFIC COMMISSION E

gaia

revolutionizing our view of data, yielding quality Launched in 2013, the Galaxy, with a precise and radial velocities and ESA mission Gaia detailed entire-sky survey multi-band photometry is providing a of all detectable celestial for the determination of 86 whole-sky census objects down to the G(aia) astrophysical properties magnitude 20.7 (close to R). (luminosity, surface gravity, of over 1.5 billion Gaia, launched in December temperature and chemical objects, mostly 2013, commenced science composition). The predicted stars in our Galaxy operations in the Summer end-of-mission parallax and its immediate of 2014. Data taking will standard errors, i.e. after surroundings, continue through the end global processing the of 2020, thanks to the totality of data acquired unraveling the 1.5-yr extension granted over the mission lifetime, is chemical and by ESA to the initial 5-yr anticipated at 9-25 μas at R dynamical history of operational life. Gaia’s high- =15 depending on star color, the Milky Way and, accuracy global astrometry providing a 10% error up to therefore, of its place measures the 3D position individual distances of 10 kpc. of a star and its movement The GDR2 (Gaia Data in cosmology. across the sky. In addition, Release 2) catalog was thanks to its multi- released in 2018 with the Gaia is a major project for function focal plane, Gaia astrometry for more than 1.5 the European astronomical gathers also spectroscopic billions sources and partial community that is and spectrophotometric . GDR2 processed together the first spectrophotometric data largest in Italy ever dedicated 22 months of satellite data. reduction and absolute to astronomy, and a direct Two more data releases are calibration, variable and connection to the Italian anticipated: GDR3 (34 months special object treatment (with supercomputing center at of data), will be in two issues, primary responsibility on CINECA to operate its global 87 e(arly)DR3 for the late-Fall Cepheids, RR-Lyrae, moving astrometric pipeline. Italy 2020, and GDR3 in 2021; objects, e.g. known and new also provides one of the four at least one full release will asteroids, and extrasolar partner data centers (the follow. planets), source classification ASI/SSDC at ASI Hq) for The scientific data processing and cross-match to external the access and distribution is the responsibility of the catalogs. To support the of Gaia’s released catalogs, DPAC (Gaia Data Processing astrometric verifications, Italy thus supporting the National and Analysis Consortium), a has contributed a dedicated scientific data exploitation. pan-European effort of ~450 data processing center, the scientists. DPCT (jointly participated by Italy’s strategic involvement ASI and INAF with ALTEC in DPAC activities, the Inc as industrial contractor), second largest, includes: one of the six across . Gaia Initial Catalog, the The DPCT receives all catalog of SPSS (Spectro- of the Gaia observations Photometric Standard Stars), including the raw pixels of daily and cyclic pipeline the astrometric focal plane, astrometric verification, requiring a 1.5 PBy DBMS, the gaps

GAPS is stratospheric anti-helium nuclei have of the features of the decay Antarctic balloon never been detected in of exotic atoms produced mission to be cosmic rays, and their after capture of anti-nuclei 88 operated in identification would provide by the atoms of the detector 2021/2022 for the unprecedented information materials. A plastic time on the understanding of the of flight system tags the study and search of Universe, revealing unique particle and measures its the rare antimatter details on the nature of Dark velocity and energy deposits. components in Matter and on the origin The particle then slows cosmic rays. of cosmic rays. The GAPS down and form an excited detector is now starting its exotic atom in the Si(Li) integration phase and will be tracker which de-excites and GAPS (the General operating on a stratospheric releases X-rays and a “star” AntiParticle Spectrometer) long duration (30 days) of pion and protons from the is an experiment designed balloon flight in Antarctica nuclear annihilation. The to study the rare antimatter from the McMurdo base simultaneous measurements component in cosmic rays during austral summer of the X-ray energy deposits, with a specific focus on 2021/2022. with 4 keV energy resolution low energy (<0.25 GeV/n) The GAPS antiparticle of the Si(Li) detector, the pion anti-proton, anti-deuteron identification approach is and proton multiplicities, and and low-energy anti-helium an innovative technique the stopping depth, velocity nuclei. Anti-deuteron and based on the measurement and energy deposition of the SCIENTIFIC COMMISSION E

primary precisely determine researchers from INFN the type of primary particle. departments and Firenze, This provides the required Pavia, Bergamo, Napoli, rejection of protons and Torino, Roma Tor Vergata and 89 other nuclei for an anti-nuclei Trieste Universities participate search, and discrimination to GAPS since 2017 and with between the different anti- support from ASI since 2018. nuclei species. The data The Italian contribution collected during the first flight concentrates on the will provide enough statistics development and construction to investigate the properties of electronics components of low energy anti-protons, of the detector and on the while two additional flights development of data analysis will be required to achieve pipelines and simulations and the scientific objectives for data interpretation models. anti-deuteron and anti-helium physics. GAPS is a mission sponsored by NASA with participation of scientists from American, Japanese and Italian institutions. Italian SCIENTIFIC COMMISSION E

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The Eagle Nebula’s Pillars of Creation as seen in visible light, capturing the multi-coloured glow of gas clouds, wispy tendrils of dark cosmic dust, and the rust-coloured elephants’ trunks of the nebula’s famous pillars. Credit: NASA/ESA/Hubble and the Hubble Heritage Team. hubble

HST is the most popular NASA/ESA joint mission. The three interferometers It was launched in 1990 and since then, it has aboard Hubble are the FGS made some of the most dramatic discoveries in (Fine Guidance Sensors). The FGSs measure the relative the history of astronomy. positions and brightnesses of stars and are very sensitive Launched in 1990, HST () has provided the instruments. They seek out most spectacular images of the Universe. With its spectroscopic and stable point sources of light imaging instruments that cover from the Ultraviolet through the (known as “guide stars”) and Infrared bands, it has provided unprecedented insight into many then lock onto them to keep astrophysical questions, from the Solar System to the early stages of the telescope pointing steadily. 91 the Universe. After having been serviced several times by the Space Italy has contributed to Shuttle, allowing repair and substitution of its instruments, it is still the development of its first working at its best. It is expected to continue operation for several instruments. Italians are more years, with significant overlap with the JWST mission. among the major users of HST has three types of instruments that analyze light from the HST. universe: cameras, spectrographs and interferometers. It has two primary camera systems to capture images of the cosmos. Called the ACS (Advanced Camera for Surveys) and the WFC3 (Wide Field Camera 3), these two systems work together to provide superb wide-field imaging over a broad range of wavelengths. While ACS is primarily used for visible-light imaging, WFC3 probes deeper into infrared and ultraviolet wavelengths, providing a more complete view of the cosmos. The current two spectrographs are: the COS (Cosmic Origins Spectrograph) and the STIS (Space Telescope Imaging Spectrograph). COS and STIS are complementary instruments that provide scientists with detailed spectral data for a variety of celestial objects. Working together, the two spectrographs provide a full set of spectroscopic tools for astrophysical research. 92

On 17 August 2017, a burst of gamma rays lit up in space for almost two seconds. It was promptly recorded by INTEGRAL and NASA’s Fermi satellite. The detectors of the LIGO experiment, in the USA, recorded the passage of gravitational waves: a groundbreaking discovery, revealing for the first time gravitational waves and highly energetic light released by the same cosmic source.Crediti: Aurore Simonnet, LIGO/Caltech/MIT. SCIENTIFIC COMMISSION E

INTEGRAL is an ESA gamma ray observatory It still continues to contribute launched in 2002 that played a crucial role in to this key topic linking the new non-electromagnetic discovering the first prompt electromagnetic astronomies with the high- radiation in coincidence with a Gravitational energy electromagnetic Wave event, opening the multi-messenger Universe in the poorly-covered astrophysics era. 10 keV to 10 MeV domain. This is mainly due to the unique capabilities: highly efficient The INTEGRAL (INTernational Gamma-Ray Astrophysics Laboratory) coverage of the whole sky and mission was approved as the 2nd medium size ESA project of the rapid reaction for Target of Horizon 2000 Scientific Program in April 1993 and successfully Opportunity observations. No launched from Baikonur () on 17 October, 2002. INTEGRAL mission, neither in operation, is an observatory type mission and its science payload is designed nor planned in the coming for the imaging and spectroscopy of persistent and transient cosmic years, offers INTEGRAL’s sources in the 10-10000 keV band. There are two main instruments combination of capabilities in detecting gamma rays: the imager IBIS (Imager on Board of the the hard X/γ-ray parts of the INTEGRAL Satellite) giving the sharpest gamma-ray images yet seen 93 . from astronomical targets; and the spectrometer SPI (SPectrometer on The program is led by INTEGRAL) which precisely measures Gamma-ray energies. ESA, with the instrument Besides the two main instruments, INTEGRAL offers substantial complement and the Scientific monitoring capability in the X-ray range, from 3 to 30 keV, and in the Data Centre (based in Geneva) optical V band at 550 nm. In view of the impossibility of focusing high provided by five different energy X-rays and soft Gamma-rays, the three high energy instruments European consortia with a large are operated with a coded mask to provide good imaging capability contribution from ASI and over a wide field of view. This technique is a key feature of INTEGRAL INAF Institutes (INAF/IAPS, to provide simultaneous images of the whole field observed, detection INAF/IASF, INAF/OAPA and and location of all the sources. After almost 18 years of operation, INAF/OAS) especially for IBIS INTEGRAL has detected more than 1000 high-energy emitters of all and to a minor extent for SPI types, most of which are new detections including many transient and Jem-X. Contributions were sources that shine once in a while in the sky. Because of the high also provided by Russia, for the quality scientific results, the operative life of the mission has been Proton launcher, and by the extended up to the end of 2020, with an ongoing extension request till USA which made available a 2023. INTEGRAL, together with Fermi/GBM, played a crucial role in NASA ground station. discovering the γ-ray Burst (GRB 170817A) linked to Gravitational Waves as result of the collision of two neutron stars.

IXPE is a NASA ASI and three X-ray optics in some cases, represents mission with a large developed at NASA/MSFC. the only way to have The main contractor for the knowledge of the geometry 94 participation by ASI, spacecraft is Ball Aerospace. of the systems at angular to be launched in IXPE reaches a focal length scales much smaller than 2021. It will provide of 4 meters by means of an those of Chandra (less than imaging X-ray extendable boom provided by 1 arcsec) and to determine polarimetry resolved ATK-Orbital. The launcher is the physical processes at , but, as a matter of work. IXPE, in addition to in energy and time of fact, IXPE has been designed the detailed study of isolated celestial sources. to be included in the fairing celestial point sources, of the Pegasus launcher to be allows meaningful studies IXPE (Imaging X-ray compliance with the proposal of much larger classes of Polarimetry Explorer) is a requirement for this SMEX sources thanks to: a reduced SMEX (Small Explorers) mission. and controlled background mission to be launched in X-ray polarimetry allows and the consequent smaller 2021. The mission, led by to study black holes and measurable flux down to those NASA/MSFC is devoted to neutron stars binaries in of AGNs and dim , time-spectrally-spatially their variable physical the capability to resolve resolved X-ray polarimetry. It conditions for the unstable multiple sources in crowded comprises three GPDs (Gas presence of jets, coronae and regions, the provision Pixel Detectors) provided by accretion disks. Polarimetry, of angularly resolved SCIENTIFIC COMMISSION E

polarimetry for extended accomplished at INAF/ sources (such as shell-like IAPS such as the electrical Supernova Remnants and and functional integration for and test of the instrument. 95 mapping magnetic fields, INAF/IAPS also performed determining its uniformity the Thermo-Vacuum test for studying the acceleration and designed the on-board mechanisms at the emission calibration system to monitor site). the performance of the The Italian contribution instrument during flight. ASI (INAF, INFN and OHB-I) will also provide the Malindi comprises the whole primary IXPE Ground focalplane: the Detector Unit Station and contributes to with the Gas Pixel Detectors, the development of the flight the Back-End Electronics, pipeline with ASI/SSDC. including the High Voltage Power Supplies, the Filter and Calibration Wheel and the housing. Moreover, Italy provides the Detector Service Unit developed by OHB-I. The calibrations have been SCIENTIFIC COMMISSION E

jem-euso

JEM-EUSO is a unsolved in contemporary astroparticle physics. Give an answer to program that these questions is rather challenging because of the extremely low flux at extreme energies (i.e. E > 5x1019 eV). The main objective includes several of JEM-EUSO is the realization of an ambitious space-based missions to explore mission devoted to UHECR science. The JEM-EUSO program the origin of the includes several missions: on ground, EUSO-TA, in operation at extreme energy the Telescope Array site in Utah since 2013; on board stratospheric cosmic rays and balloon, EUSO-Balloon, that flew in August 2014, EUSO-SPB1, launched in April 2017 on a super pressure balloon, EUSO-SPB2, cosmogenic in construction phase for a long duration flight in 2022; in space, neutrinos. 96 TUS, a Russian mission that has been flying for a year on board the Lomonosov Satellite since April 2016; MINI-EUSO, in operation JEM-EUSO (Joint since August 2019 inside the ISS, looking down the atmosphere Experiment Missions for from the UV transparent window in the Russian Module; and the Extreme Universe Space large size mission K-EUSO, in phase of realization, to be installed Observatory) is a program outside the ISS. The final goal of the JEM-EUSO program is to send that aims at exploring in orbit a super-wide-field telescope that will look down from space the origin of the extreme onto the night sky to detect UV photons emitted from air showers energy cosmic rays and generated by UHECRs in the atmosphere, with a year time exposure cosmogenic neutrinos by more than one order of magnitude of Auger. This is the context looking downward at Earth of the POEMMA mission (Probe Of Extreme Multi-Messenger from space, and detecting Astrophysics) approved by NASA for a study phase. 16 countries the fluorescence light of and about 300 researchers are collaborating in JEM-EUSO. extensive air-showers that JEM-EUSO in Italy is presently funded by INFN within the they generate in the Earth’s Astroparticle and Neutrino Committee; funds have also been atmosphere. provided for several years by ASI. The full commitment of ASI is The origin and nature depending on the final approval of the mission. of UHECRs (Ultra-High Energy Cosmic Rays) and cosmogenic neutrinos remain 97

The Japanese Experiment Module of the ISS in 2017. Credit: JEM-EUSO. SCIENTIFIC COMMISSION E

jwst

sunshield that attenuates heat its 5 year mission and it is JWST is an infrared from the Sun more than a designed to observe 100 objects telescope to be million times. It will be equipped simultaneously. The NIRSpec launched in 2021. It with 4 instruments: the NIRCam will be the first spectrograph in will be the premier (Near-InfraRed Camera), built space that has this remarkable by the Arizona University, multi-object capability. MIRI observatory of NIRSpec (Near InfraRed has both a camera and a the next decade, Spectrograph), provided by ESA spectrograph that sees light in serving thousands with components by NASA/ the mid-infrared region of the of astronomers GSFC, MIRI (Mid-InfraRed electromagnetic spectrum, with worldwide. Instrument), provided by a wavelengths in the 5-28 microns European Consortium including range. Its sensitive detectors will ESA and by NASA/JPL and allow it to see the redshifted JWST (James Webb Space FGS/NIRISS (Fine Guidance light of distant galaxies, newly Telescope) is an infrared Sensor/Near InfraRed Imager forming stars, and faintly visible telescope with a 6.5-meter and Slitless Spectrograph), as well as objects in the primary mirror, currently provided by CSA. Kuiper Belt. FGS allows JWST 98 scheduled for launch in October NIRCam is JWST’s primary to point precisely, so that it can 2021. imager and it will cover the obtain high-quality images. With its four main science infrared wavelength renge of The Near Infrared Imager and themes, 1) first light and 0.6-5 microns. NIRCam will Slitless Spectrograph part of reionization, 2) assembly of detect light from: the earliest the FGS/NIRISS will be used galaxies, 3) birth of stars and stars and galaxies in the process to investigate, in a wavelength proto-planetary systems, 4) of formation, the population range of 0.8-5.0 microns, the planets and origins of life, JWST of stars in nearby galaxies, as following science objectives: will study every phase in the well as young stars in the Milky first light detection, exoplanet history of our Universe. Way and Kuiper Belt objects. detection and characterization, Several innovative technologies NIRCam is equipped with and exoplanet transit have been developed for JWST coronagraphs, instruments spectroscopy. which include a primary mirror that allow astronomers to take Italians are participating to the made of 18 separate segments pictures of very faint objects mission, either as ESA members that unfold and adjust to shape around a central bright object, or because of their individual after launch. The mirrors are like stellar systems. NIRSpec role in international consortia made of ultra-lightweight will operate over a wavelength and committees. beryllium. JWST’s biggest feature range of 0.6-5 microns to study is a tennis court sized five-layer thousands of galaxies during 99

The engineering design unit primary mirror segment (flight spare) coated in gold. Credit: Drew Noel. SCIENTIFIC COMMISSION E

100

The LISA Pathfinder mission. A technology testing mission for the LISA mission. Credit: DLR . SCIENTIFIC COMMISSION E

lisa

LISA is a Gravitational Waves observatory made of a constellation of 3 spacecrafts millions of km apart, to be launched by ESA in 2034. 101 The gravitational Universe is the theme of the ESA L3 Mission (third Large mission of the ESA Cosmic Vision program) scheduled for 2034. ESA has selected LISA (Laser Interferometer Space Antenna) observatory for L3. LISA will consist of a constellation of three spacecrafts, millions of km apart, each containing Test Masses in free fall, whose relative motions are measured by laser interferometry. LISA will detect and measure Gravitational Waves in the 20 microHz to 100 mHz band, performing precision observations of astrophysical phenomena like coalescing massive black holes in the aftermath of galaxy collisions virtually at any distance in the Universe, stellar black holes skimming the horizon of massive black holes (the so called Extreme Mass Ratio Inspirals) in galaxies out to redshift z~3, ultra compact binaries in the Milky Way and possibly signatures of a primordial Gravitational Wave background from the infant Universe providing the closest reach to the Big Bang. Most of the “enabling technologies” have been tested by LISA Pathfinder. Based on its role in LISA Pathfinder, Italy leads the development of the free-falling test-masses. SCIENTIFIC COMMISSION E

lspe

Wave Plates), and the STRIP LSPE is an ASI and Gravitational Waves produced (Survey TeneRIfe Polarimeter) INFN stratospheric during cosmic inflation, ground-based polarimeter balloon mission that a split-second after the with low-frequency coherent big-bang, induce linear will measure the radiometers, aimed at 102 polarization in the CMB (with polarization of the foreground monitoring. The both gradient modes E-modes 40-250 GHz frequency range CMB radiation at and curl modes B-modes). is covered with 5 channels, large angular scales. The signal from B-modes with an angular resolution The first flight is is extremely small, <0.1 of 0.5-1.3 deg FWHM and microK rms, and is mainly planned for 2021. a combined sensitivity of 20 at large angular scales. LSPE microK arcmin. LSPE (Large Scale Polarization targets are the reionization Explorer) is a stratospheric and recombination bumps balloon mission funded by in the angular power ASI and INFN, with a first spectrum of B-modes. The flight planned for 2021. LSPE LSPE program features two will measure the polarization polarimeters: the SWIPE of the CMB (Cosmic (Short Wavelength Instrument Microwave Background) for the Polarization Explorer) radiation at large angular balloon-borne polarimeter, scales, during a long duration with cryogenic multi-mode stratospheric flight in the bolometers and a spinning Arctic Winter. HWP modulator (Half neil gehrels swift observatory

Neil Gehrels Swift Observatory average, more than four ToOs The Neil Gehrels is a collaborative MIDEX per day are performed. Thanks Swift Observatory (Medium-Class Explorers) to its fast and autonomous (previously named NASA Mission with a strong repointing capability and contribution from Italy and UK good sensitivity in the X-ray Swift) is a NASA for the observation of the GRB and optical/UV bands, Swift 103 mission with a strong (Gamma Ray Bursts). It has is also heavily involved in the contribution from onboard three instruments: the search of the electromagnetic BAT (Burst Alert Telescope), counterparts of Gravitational Italy and UK. It was the XRT (X-Ray Telescope) Waves and neutrino sources. launched in 2004 to and the UVOT (Ultraviolet/ Italy provides the ASI ground solve the mystery of Optical Telescope). Swift station in Malindi for the detects ~90 GRBs per year uplink/downlink of the data, the origin of Gamma and since its launch it the Mirror Module of the XRT Ray Bursts. revolutionized our knowledge developed by the INAF/OAB of the field. The observing plan under an ASI contract, the The Neil Gehrels Swift has evolved with time and now, XRT data analysis software Observatory was launched although Swift continues to developed by the ASI/SSDC. on November 2004. It was hunt for GRBs, the majority Furthermore, the Italian team previously named Swift and of the time is spent on participates to the scientific renamed in memory of Neil target of opportunity (ToO) management of the mission, Gehrels, who served as its observations, covering all funded by ASI. principal investigator until his kind of sources, from comets death on 6 February 2017. The to high redshift . On

The NuSTAR mission the radioactive debris of the is a NASA Explorer CasA ; the study of the Galactic launched in 2012: it Center with unprecedented 104 is the first hard X-ray resolution at hard X-rays and focusing satellite. the properties of ultraluminous sources with the discovery of an NuSTAR (Nuclear ultraluminous pulsar. NuSTAR Spectroscopic Telescope Array) works efficiently in coordinated mission is a NASA Explorer programs with other X/ launched in 2012: it is the Gamma-ray missions. first orbiting telescopes to The Italian contribution focus light in the high energy includes: the provision of ASI X-ray (6-79 keV) region of the ground station in Malindi electromagnetic spectrum. (), data reduction Main results include a census of software support and archival black holes and stellar compact storage at the ASI/SSDC, objects at different scales; contribution to the project with the measurements of their a team of INAF scientists that spins and of the properties of collaborates to the primary their outflows; shedding light scientific mission goals. Artist’s concept of NuSTAR on orbit. Credit: NASA/JPL-Caltech. Previous on acceleration processes in page: Omega Centauri, also known various sites; the mapping of as NGC 5139. Credit: NASA/Swift. SCIENTIFIC COMMISSION E

olimpo

OLIMPO is a balloon high efficiency, extracting tiny mm-wave telescope spectral anisotropies from an overwhelming instrumental and for spectroscopic atmospheric background. In the measurements of the first long-duration flight from 105 Sunyaev-Zeldovich Svalbard islands, in July 2018, the effect in clusters of instrument and its new kinetic galaxies. It was flown inductance detector arrays were successfully validated. in a first flight in 2018, The instrument has been with a long duration recovered and is being prepared Arctic flight. for a second circumpolar flight, aimed at obtaining data-cubes from about hundred deep OLIMPO is a balloon-borne 2.6 sky areas, including Sunyaev- m aperture mm-wave telescope Zeldovich targets, as well as blank coupled to a DFTS (Differential reference areas, to measure the Fourier Transform Spectrometer) spectral-spatial anisotropy of the with 4 cryogenic detector arrays, diffuse mm and sub-mm cosmic covering spectroscopically 4 wide background. The experiment is bands centered at 140, 220, 340 funded by ASI. and 480 GHz. The DFTS rejects the common-mode signal with 106

Artist’s impression of ESA’s PLATO spacecraft. This top view highlights the unique payload that comprises 26 cameras. Credit: ESA/ATG medialab. SCIENTIFIC COMMISSION E

PLATO, to be launched in 2026 by ESA, Lario SrL. Italy, through ASI, is also will catalog transiting planets of closeby providing the Instrument stars, including earth like planets, providing Control Unit (made in measurements with unprecedented accuracy of collaboration with IWF, Graz, planetary density and age. Austria, designed at INAF, produced, tested and delivered PLATO (PLAnet Transit and stellar Oscillations) is the next generation by Kayser Italia), the segment 107 exoplanet finder, the third medium-class mission in ESA’s Cosmic of the ground center devoted Vision program, to be launched in 2026. It will obtain light curves of up to the handling of the PLATO to one million bright dwarfs and subgiants, covering up to half of the Input Catalog (ASI/SSDC). sky, with almost continuous coverage for up to 3 years. Main purpose is Moreover, ASI and INAF are the search for exoplanets, including rocky Earths and SuperEarths, and leading the coordination of obtain seismic measurement of radii (~3% error), masses (~10% error), the PLATO Camera System, and ages (10% error) of hosting stars. PLATO will set the basis for the and together with Paodva statistical study of exoplanet and exoplanet system bulk properties, their University, the preparation of dependence on the environment, and how they evolve with age. the PLATO Input Catalog. The Made by a set of 24 telescopes, mounted on the satellite in 4 slightly preparation of the PLATO misaligned groups, it provides a field of view of almost 2400 square scientific program involves degrees and an equivalent aperture comparable to a 0.9 m telescope. researchers from INAF and Two more telescopes are optimized to observe very bright stars universities spread overall Italy. (magnitude 4-8), each of which specializes in blue and red light, respectively. Italy, through ASI, is providing the 26 Telescope Optical Units, made in collaboration with Bern University, based on an optical design by INAF, tested and delivered by Leonardo S.P.A., Thales Alenia Space and Media SCIENTIFIC COMMISSION E

SPICA is a joint a spectroscopic sensitivity the SRON, which coordinates, European-Japanese hundred times better than together with ESA and JAXA, both Spitzer and Herschel, a consortium of international candidate mission to SPICA will enable a physical institutes. The Italian unveil the formation exploration of the hidden participation is led by INAF/ and evolution of Universe and provide a three IAPS and funded by ASI and it structures, galaxies, dimensional (3-D) view of includes both technology and stars and planets galaxy evolution in the rest- science: the development of frame mid-IR. the Instrument Control Units through mid and far- SPICA is an infrared space and On-Board Software for IR spectroscopy and observatory with a 2.5 m the two European instruments polarimetric imaging. primary mirror cooled to SAFARI and B-BOP, as well as 108 below 8 K and three focal plane the coordination of the SPICA SPICA (SPace Infrared instruments: SAFARI, a 35-230 Galaxy Evolution Working telescope for Cosmology and μm spectrometer with a grating Group and the participation to Astrophysics) was selected module at low (R~300) and the ISM and Star Formation, in 2018 as one of the three an FTS module at medium Planetary Disks and Solar candidate missions for the (R=3000-11000) spectral System Working Groups. 5th Medium Size Mission of resolution; SMI, a 17-36 μm the ESA Cosmic Vision. The spectrometer with a large selection of one of the three field (12’ x 10’) low-resolution candidates is expected in 2021. spectrophotometric camera, a SPICA is a joint European- medium resolution (R~2000) Japanese project with world- grating module and a high- wide participation on the focal resolution 12-18 μm echelle plane instruments. SPICA will module (R~28000); B-BOP, be a unique facility, designed a large field (2’.6 x 2’.6), three for deep and wide surveys channel, (70 μm, 220 μm and to unprecedented depths in 350 μm) polarimetric camera. spectroscopy, photometry The European participation in and polarimetry. Reaching the SPICA mission is led by

THESEUS is a mission is to fully exploit the contributions from other candidate ESA great potential of the GRBs European countries like, e.g. for cosmology purposes, Slovenia. mission to open a especially in the study of The Italian participation is new window on the the primordial Universe. led by INAF/OAS and funded early Universe and THESEUS will provide a by ASI and it includes the the multi-messenger fundamental contribution development of one of the transient sky. to the time-domain and three instruments on board, multi-messenger astrophysics the XGIS (X/Gamma-ray and to several fields of Imaging Spectrometer), the THESEUS (Transient astrophysics, cosmology and development of the TBU High-Energy Sky and Early fundamental physics. It will (Trigger Broadcast Unit), Universe Surveyor) is one of operate in beautiful synergy the contribution to ground 109 the three mission concepts with the large worldwide segment (Malindi Antenna) selected by ESA in 2018 for facilities planned for the next and the general coordination a 3-years Phase A study as decade devoted to the study of the international candidate M5 mission, with a of the Cosmos, such as LSST, consortium. planned launch date in 2032. ELT/ TMT, Ska, CTA, Athena, THESEUS aims at exploring Ligo, aVirgo, Kagra, Et and the early (first billion years) Km3NeT. Universe through high- The THESEUS mission redshift GRBs (Gamma-Ray concept was proposed and is Bursts), the most extreme supported by an European explosions in the cosmos, and consortium led by Italy and providing detection, accurate with main contributions by location and redshift of the UK, France, Germany and electromagnetic counterparts Switzerland. Further relevant of gravitational waves and contribution come from neutrino sources, as well as of , Denmark, , many other transient celestial , Czech Republic, sources. The main aim of the with additional minor xmm-newton

Since 1999, XMM- AGN taxonomy and EPIC CCDs are designed Newton is detailing population across cosmic to exploit the full design the physical time has been studied using range of the X-ray mirrors, XMM-Newton to survey 0.1-15 keV. They provide conditions in portions of the sky. It was also energy resolution at 6.5 the star forming fundamental to study galaxy keV of E/dE~50, and their regions and the clusters and in particular to positional resolution is mechanisms acting study their physics and the sufficient to resolve the for the production effects induced by the “Dark mirror performance of 6 Matter”. Finally, XMM- arc seconds FWHM (15 arc of X-rays in the Newton has been successfully seconds HEW). The MOS 110 magnetosphere of operated to detail the physical CCDs are front illuminated planets. conditions in the star forming 600 x 600 pixel devices. The regions and the mechanisms physical size of each pixel XMM-Newton was the second acting for the production of is 40µm, corresponding to cornerstone of the ESA X-rays in the magnetosphere 1.1 arc seconds on the sky. Horizon 2000 program. It was of planets. There are seven CCD chips launched on 10 December The XMM-Newton spacecraft with one in the center of the 1999 and it is still operating is carrying a set of three field of view with the other perfectly. The mission shall X-ray CCD cameras, six surrounding it. The CCDs operate up to at least 2022 comprising the EPIC camera are offset from one another with possible extension to (European Photon Imaging to match the curvature of the 2025. Camera). Two of the cameras focal plane. RGS consists of Taking advantage of its are MOS (Metal Oxide Semi- RGAs (Reflection Grating high throughput, spectral conductor) CCD arrays. Assemblies) and RFCs and timing capabilities, They are installed behind (RGS Focal Cameras). The XMM-Newton allowed to the X-ray telescopes that are RGS provides high spectral collect probes of the theory equipped with the gratings resolution (E/dE from 200 of relativity in AGN and of the RGS (Reflection to 800) X-ray spectroscopy compact Galactic objects. Grating Spectrometers). The over the energy range 0.35- SCIENTIFIC COMMISSION E

2.5 keV (5-35 Å). The RGAs (European Photon Imaging intercept about 50% of the Camera) cameras. Moreover, X-rays passing through the INAF/OAB did significantly mirrors. The reflected X-rays contribute, together with are directed onto linear arrays the Media Lario SrL, to the of 9 MOS chips forming realization of the large area the RFC. The OM (Optical mirror modules. The INAF/ Monitor) is co-aligned OAPA has been involved with the X-ray telescopes, in the development and providing simultaneous UV/ calibration of the EPIC optical/X-ray observations. optical filters. The instrument consists of 111 a 30 cm -Chretien telescope feeding a compact image-intensified photon- counting detector. The detector operates in the UV and blue region of the optical spectrum. Since the majority of X-ray sources are variable, the optical monitor allows the observer to know the optical state of the X-ray object they are viewing. Thanks to the coordinated involvement of its research structures INAF/IASF, INAF/ OAS and INAF/OAPD, INAF is contributing to the realization of the three EPIC 112

Conformal Cyclic Cosmology predicts that much of the Universe will be pulled into enormous black holes that will then boil away. Credit: NASA/JPL-Caltech.

114 SCIENTIFIC COMMISSION F Life Sciences as Related to Space

115 Previous page: During the Beyond mission the ESA astronaut supported more than 50 European and over 200 international experiments and gained the European record for longest cumulative spacewalking time. Credit: Francesco Algeri. SCIENTIFIC COMMISSION F

the missions vita and beyond and the asi experiments

VITA and BEYOND are two Italian missions the event that signed the conducted onboard the ISS by astronauts Paolo successful completion of the ESA mission BEYOND. One Nespoli and Luca Parmitano including a large of the mission goals was to number of experiments in different research carry out six experiments fields. sponsored by ASI. Three investigations (Acoustic Diagnostics, Amyloid Thanks to the agreement with NASA signed in 1997 (Memorandum Aggregation and NutrISS) of Understanding between NASA and ASI - MoU), ASI has a were integrated on board privileged access to the ISS. In fact, according to the MoU, in and operated via a specific exchange for the supply of the three MPLMs (Multi Purpose Logistic agreement between ESA 117 Module), ASI is entitled - among other things - to long-lasting and ASI, two (XenoGRISS astronaut flights every 5 years and to the exploitation of part of and LIDAL) were launched NASA’s on-board resources (0.85% of NASA ISS resources, which through the ASI-NASA corresponds to 0.6% of the total station resources). MoU for the MPLM/PMM In 2017, ESA and ASI jointly selected the astronaut modules, one (Mini-EUSO) for the long-lasting flight mission called VITA. In order to stemmed by an international complement the VITA mission, ASI coordinated a pool of scientists, cooperation led by Italy and industry leaders in innovative technological fields and academic Russia, which required a researchers who worked on the design and implementation of specific agreement between payloads, experiments and scientific protocols in the fields of ASI and ROSCOSMOS. human physiology, cell biology, countermeasures, physical sciences, Based on the resources technological demonstrations and educational activities. available from the start Following a call for research opportunities, as well as promoting of the program until the public-private partnership, ASI appointed for the VITA mission completion of the mission a total of 11 investigations, involving 29 different institutions and BEYOND, ASI has conducted about 40 investigators. 73 experiments, in all the The return of the ESA astronaut with Italian passport Luca different research fields Parmitano on board the Soyuz MS-13, on 6 February 2020, is foreseen for the ISS science. in situ bioanalysis

The IN SITU was conducted during the complex and expensive, Bioanalysis project VITA mission on board and it also significantly the ISS, without the need lengthens response times. allows to perform to send samples to Earth, Furthermore, this scenario on board the ISS offering the astronaut the is not conceivable for long- chemical-clinical opportunity to monitor range future missions. The his health in real time. The peculiarity of the IN SITU analysis of biological system is based on the LFIA Bioanalysis is that the samples obtained in (Lateral Flow Immunoassay) chemical-clinical analysis is a non-invasive way. technique, widely known carried out directly within in the diagnostic field (e.g. the ISS, allowing a timely 118 pregnancy test), which diagnosis and therefore a The scientific objective of exploits the high specificity rapid intervention in case the IN SITU Bioanalysis of antibodies to recognize of problematic situations. project was the design and the biomarker of interest This device, designed for development of a portable and the capillary forces to space, can then also be used analytical device, suitable for promote the movement of in other critical situations the quantitative measurement reagents; the coupling with on Earth, for example of biomarkers of interest in the chemiluminescence for POCT (point-of-care the oral fluid of astronauts detection (CL-LFIA) testing) applications at the during their mission onboard allows to obtain accurate patient’s bed, in the doctor’s the ISS. In particular, the quantitative information. office or in an ambulance, project was focused on the Currently, biological samples in emergency medicine, in measurement of salivary taken by crewmembers on cases of bioterrorism or for levels of cortisol, as a stress board the ISS are normally diagnostics in developing biomarker, but in the future, frozen and kept on board countries or in remote or it can be easily adapted for the until they can be sent to isolated communities. analysis of other biomarkers of Earth and analyzed in the interest in different biological laboratory. This makes samples. The entire analysis the operation extremely SCIENTIFIC COMMISSION F

acoustic diagnostics

The Acoustic performed on the astronauts recording the OAE response. Diagnostics before and after their Periodic DPOAE mission, and by performing measurement session experiment aims at accurate OAE (OtoAcoustic were performed on two evaluating possible Emission) tests on a monthly astronauts during the mission hearing damage base while on board the ISS. BEYOND on board the ISS. OAEs are acoustic signals The astronauts set up and on astronauts by generated in the hearing operated the experiment, performing tests sensory organ (the cochlea), guided by a user-friendly before and after as a response to acoustic acquisition software. Both stimuli, and measured in the ears were tested in each their missions and ear canal. Their amplitude is session. 119 on board the ISS strictly correlated to hearing The test results will allow us with an innovative sensitivity, so they represent to demonstrate or to exclude an objective, fast, non- hearing damage, even mild system. invasive hearing diagnostic or transitory, statistically tool. An innovative system associated to residence on Microgravity and for measuring DPOAE board the ISS in conditions of environmental noise are (Distortion Product of OAE) noise and microgravity, with potential risk factors for was designed, guaranteeing obvious implications for the the astronauts’ hearing, high reproducibility of the design of future longer-term particularly in case of very test results, exploiting a missions, dedicated, e.g. to long-term missions that are particular technique for the . foreseen for the exploration the stimulus calibration in Such a compact and of the Solar System. The the ear canal, and a high performing device will find Acoustic Diagnostics frequency-resolution. A interesting applications in experiment aims at evaluating customized probe, inserted clinical audiology and health possible hearing damage by in the ear canal, houses the at work, allowing performing comparing the outcome of loudspeakers delivering the accurate audiological tests in several audiological tests stimulus and the microphone a noisy environment. SCIENTIFIC COMMISSION F

mini-euso

Mini-EUSO is a next- The optics is based on Fresnel lenses with 25 cm diameter. generation telescope The thin and compact construction of the lenses is particularly suitable for space-borne detectors. The field of view on the ground for the study is 40 degrees, corresponding to 260 x 260 km2 on the surface of and monitoring our planet. With the continuous acquisition of data, for the first of terrestrial, time we can therefore create a dynamic map of nocturnal emissions atmospheric and of ultraviolet in the Earth. A Near Infrared and a visible camera cosmic emissions in complete these measurements. Scientific objectives include: realization of the first UV night map Ultraviolet (UV) that of the Earth with a resolution of a few km; detection and study of operates in the ISS ; search for quark strange matter; monitoring and tracking since 2019. of for the realization of future laser-based removal methods; search for ultra-high-energy cosmic rays; study of marine 120 Mini-EUSO (Multiwavelength bioluminescence and of the ‘milky sea’ phenomenon, generated by Imaging New Instrument plankton. for the Extreme Universe Technological goals include the first use of a refractive telescope Space Observatory) is a based on Fresnel lenses in space and the first use of a high telescope designed to perform sensitivity focal surface, capable of detecting a single photon, and observations from the ISS, of related electronics resistant to the space environment. This type UV light emission in Earth of technologies have applications ranging from the creation of atmosphere. new and larger spatial telescopes such as EUSO, for the study of In 2019 it was located in the fundamental physics phenomena in space to practical applications ISS in the Zvezda Russian related to the new type of optics and detectors in space (solar energy module, looking at Earth in concentrators, removal of space debris, monitoring of land and nadir position. Mini-EUSO’s pollution and so on). ultra-fast video camera (400 Mini-EUSO was developed under an agreement between ASI and thousand frames per second, ROSCOSMOS with a wide international collaboration led by the 2.5 microsecond/frame), Italian INFN and the Japanese Riken. The Italian contribution also is capable of single photon involved other scientific realities and Italian academics. detection on each of the 2304 pixels composing the focal surface.

SCIENTIFIC COMMISSION H Fundamental Physics in Space

123 Previous page: The second Alpha Magnetic Spectrometer (AMS-02) on the ISS. Credit: NASA. SCIENTIFIC COMMISSION H

ams-02

AMS-02 is a particle spectrometer, separating mechanisms of cosmic ray physics detector matter from antimatter cosmic origin, acceleration and rays. Additional sub-detectors propagation, and the origin of operating as external provide complimentary and the rare components of cosmic module on the ISS redundant information on the rays and of solar physics. since 2011, searching particle charge, velocity and AMS is an international for antimatter and energy to precisely identify collaboration of 44 institutions Dark Matter in the nature and properties of from America, Europe and each cosmic ray crossing the Asia. cosmic rays. detector. In Italy, the contribution to AMS-02 was launched on AMS is funded by INFN and AMS-02 (Alpha Magnetic ISS with the Space Shuttle ASI. Scientists from INFN 125 Spectrometer) is a particle Endeavour in 2011 and has departments and Bologna, physics spectrometer operating been operating on the ISS Milano, Perugia, Pisa, Roma as an external module on ever since. The recent upgrade Sapienza, Roma Tor Vergata, the ISS. It uses the unique of the AMS-02 Tracker Trento Universities and from environment of space to study Thermal Control System, ASI contribute to the detector the Universe and its origin which required four successful operations and data analysis. by searching for the rare extravehicular activities The ASI/SSDC also hosts the antimatter components and completed in January 2020, CRDB (Cosmic Ray Database) for Dark Matter signatures in have extended the expected that provides access to the cosmic rays while performing AMS-02 lifetime up to at AMS published data. precision measurements of least 2028. After more than cosmic ray composition, fluxes 8 years of operations, AMS- and time dependencies. 02 has collected more than AMS-02 is the unique 150 billion cosmic rays. The spectrometer operating results from the analysis of on the ISS. It measures the the AMS-02 data are proving particle rigidity and sign of unprecedented advances in the charge with its magnetic the understanding of the SCIENTIFIC COMMISSION H

LARES is an ASI position provided by SLR analysis of the laser-ranging laser-ranged (Satellite Laser Ranging). data combined with the satellite launched The satellite is covered ones given by the LAGEOS with 92 (NASA) and LAGEOS-2 (ASI- in 2012 aimed at distributed on its spherical NASA) satellites, the LARES performing tests of surface for precise satellite mission provided in 2019 General Relativity laser-ranging. It is aimed a measurement of frame- and measurements at testing Einstein’s theory dragging with approximately of space-geodesy of General Relativity and 2% accuracy. The LARES in particular at performing data are exploited also for and Earth science. an accurate test of frame- other tests of fundamental 126 dragging. Frame-dragging is physics, such as a test of the LARES (LAser RElativity an intriguing phenomenon weak equivalence principle, Satellite) is an ASI laser- of General Relativity: in or uniqueness of free fall, and ranged satellite launched Einstein’s gravitational theory for determinations of space in 2012 with VEGA. The the inertial frames, which geodesy and Earth science. spherical satellite is made can only be defined locally The LARES science mission of a single high-density according to the equivalence is a collaboration between Tungsten alloy to minimize principle, have no fixed ASI, Lecce, Roma Sapienza its non-gravitational direction with respect to the University, Maryland, Texas at orbital perturbations. Its distant stars but are instead Austin, Yerevan State, Oxford surface-to-mass ratio is by dragged by the currents of Universities and Helmholtz far the smallest among all mass-energy such as the Centre-GFZ of Potsdam. artificial satellites, making rotation of a body, e.g., the LARES the densest known rotation of the Earth (the orbiting object in the Solar axes of the local inertial System. The high precision frames are determined in measurements of its orbit are General Relativity by local achieved thanks to the very test-gyroscopes). precise measurements of its Through the scientific SCIENTIFIC COMMISSION H

127

The LARES laser relativity satellite from Italy’s ASI space agency undergoes preparations at Europe’s in . Credit: ESA, S. Corvaja. SCIENTIFIC COMMISSION H

lares-2

LARES-2 is an ASI has intriguing astrophysical science. The LARES-2 science new generation implications around spinning mission is a collaboration high-altitude laser- black holes, in active galactic between ASI, Lecce, Roma nuclei and quasars. The 2015- Sapienza, Maryland, Texas at ranged satellite to be 2018 detections of Gravitational Austin, Yerevan State, Oxford launched in 2020, Waves by the LIGO detectors Universities and Helmholtz aimed at highly have been based on computer Centre-GFZ of Potsdam. accurate testing simulations of the collision General Relativity and of spinning black holes and spinning neutron stars to form fundamental physics a spinning black hole. In such 128 and other improved astrophysical processes, frame- determinations of dragging plays a key role. Earth Science. LARES-2 is made of high- density material to minimize its non-gravitational orbital LARES-2 (LAser RElativity perturbation. The high Satellite-2) is an ASI new precision measurements of its generation high-altitude orbit are achieved thanks to laser-ranged satellite to be the very precise measurements launched with VEGA C in of its position provided 2020 at about 12270 km of by the ILRS (International altitude. It is aimed at highly Laser Ranging Service). The accurate testing General satellite is endowed with 303 Relativity and fundamental retroreflectors for laser-ranging physics, and in particular at distributed on the surface of highly accurate testing frame- the spacecraft. The LARES data dragging with an accuracy of will also be exploited for other approximately 2 parts in one tests of fundamental physics, thousand. Frame-dragging space geodesy and Earth

130 ACRONYMS

131

acronyms

ASI - ASI/SSDC - ASI Space Science Data Center CAS - Czech Academy of Science CNES - Centre National d’études Spatiales CNR/IFAC - CNR Nello Carrara” Institute of Applied Physics CNR/SPIN - SuPerconducting and other INnovative materials and devices institute CNSA - China National Space Administration CSA - ESA - INAF - National Institute for Astrophysics INAF/IASF - INAF Institute for Space Astrophysics and cosmic Physics of Milano INAF/IAPS - INAF Institute for Space Astrophysics and Planetology INAF/OAA - INAF Astronomical Observatory of Firenze INAF/OAB - INAF Astronomical Observatory of Brera INAF/OACT - INAF Astronomical Observatory of Catania INAF/OATO - INAF Astronomical Observatory of Torino INAF/OAPA - INAF Astronomical Observatory of Palermo INAF/OAPD - INAF Astronomical Observatory of Padova 133 INAF/OAR - INAF Astronomical Observatory of Roma INAF/OAS - INAF Astrophysics and Space Science Observatory of Bologna INAF/OATS - INAF Astronomical Observatory of Trieste INFN - Italian National Institute for Nuclear Physics ISS - International IWF - Institut für WeltraumForschung JAXA - Japan Aerospace Exploration Agency MPS - Max Planck Society NASA - National Aeronautics and Space Administration NASA/GSFC - NASA Goddard Space Flight Center NASA/JPL - NASA Jet Propulsion Laboratory NASA/MSFC - NASA Marshall Space Flight Center NSSC - National Space Science Center, CAS PNRA - National Antarctic Research Program ROSCOSMOS - Russian State Space Corporation SRON - Netherlands Institute for Space Research SSC - Swedish Space Corporation XACT/OAPA - X-ray Astronomy Calibration and Testing laboratory in INAF/OAPA 134 SITOGRAPHY

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sitography

For further www.the-athena-x-ray- www.esa.int/Science_ observatory.eu Exploration/Space_Science/ information please Cheops visit our websites. ASTROSAT http://astrosat.iucaa.in CLUSTER ABCS www.esa.int/Science_ www.nanosats.eu/sat/astrobio- BEPICOLOMBO Exploration/Space_Science/ cubesat www.cosmos.esa.int/web/ Cluster_overview2 bepicolombo ACOUSTIC DIAGNOSTICS www.asi.it/esplorazione/ COMET INTERCEPTOR www.asi.it/esperimenti/ sistema-solare/bepi-colombo/ www.cometinterceptor.space acoustic-diagnostics/ bepicolombo.iaps.inaf.it sci.esa.int/web/cosmic-vision/- www.oapd.inaf.it/index.php/ /61417-comet-interceptor- AGILE en/technology/technology-2/ concept www.asi.it/esplorazione/alte- simbiosys-for-bepicolombo. energie/agile/ html COSMO-SKYMED agile.rm.iasf.cnr.it FIRST GENERATION BEYOND https://www.asi.it/scienze-della- 137 AMS-02 www.asi.it/vita-nello-spazio/ /cosmo-skymed/ ams02.space missioni/expedition-60-61- https://www.e-geos.it/#/ http://www.roma1.infn.it/exp/ beyond/ satellite-hub/general/satellite- ams/ detail/csk www.asi.it/esplorazione/alte- CALET energie/ams-02/ calet.pi.infn.it COSMO-SKYMED SECOND GENERATION ARIEL CHANDRA https://www.asi.it/scienze-della- sci.esa.int/web/ariel https://www.nasa.gov/mission_ terra/cosmo-skymed-seconda- pages/chandra/astronomy/ generazione/ ASPIICS index.html www.esa.int/Enabling_ http://cerere.astropa.unipa.it/ CSES Constellation Support/Space_Engineering_ progetti_ricerca/indiceprog. www.asi.it/scienze-della-terra/ Technology/Proba_Missions/ html missione-cses-contributo- About_Proba-3 italiano-limadou/ CHEOPS ATHENA www.oact.inaf.it/cheops-italia/ DAMPE sci.esa.int/web/athena Home.html dpnc.unige.ch/dampe/ SITOGRAPHY

DUSTER HERA JWST www.oacn.inaf.it/oacweb/ www.esa.int/Safety_Security/ www.jwst..gov oacweb_ricerca/cosmici/ Hera/Hera_mission_images sci.esa.int/web/jwst sistema_solare www.stsci.edu/jwst/ HINODE ENVISION hinode.nao.ac.jp/en/ LARES envisionvenus.eu/envision/ www.asi.it/scienze-della-terra/ HUBBLE lares/ EUCLID hubblesite.org sci.esa.int/web/euclid www.nasa.gov/mission_pages/ LARES-2 www.nasa.gov/mission_pages/ hubble/about www.asi.it/scienze-della-terra/ euclid/main/index.html www.spacetelescope.org lares-2/

EXOMARS IN-SITU LICIACube exploration.esa.int/web/mars/- www.asi.it/en/esperimenti/in- nssdc.gsfc.nasa.gov/ /46048-programme-overview situ/ nmc/spacecraft/display. www.asi.it/esplorazione/ action?id=DART 138 sistema-solare/exomars/ INTEGRAL https://sci.esa.int/web/integral LISA FERMI https://www.asi.it/esplorazione/ sci.esa.int/web/lisa fermi.gsfc.nasa.gov alte-energie/integral/ www.asi.it/esplorazione/ www.asi.it/esplorazione/alte- cosmologia/lisa-pathfinder/ energie/fermi/ IXPE ixpe.msfc.nasa.gov LSPE GAIA lspe.roma1.infn.it sci.esa.int/web/gaia JEM-EUSO bandiasi.almaviva.it/it/attivita/ www.asi.it/esplorazione/ jem-euso.roma2.infn.it esplorare-lo-spazio/cosmologia- cosmologia/gaia/ e-fisica-fondamentale/lspe www.cosmos.esa.int/web/gaia/dr2 JUICE www.cosmos.esa.int/web/gaia/ sci.esa.int/web/juice MARS EXPRESS release sci.esa.int/web/mars-express JUNO www.asi.it/esplorazione/ GAPS www.nasa.gov/mission_pages/ sistema-solare/mars-express/ gaps1.astro.ucla.edu/gaps/ juno/overview/index.html www.asi.it/esplorazione/alte- www.asi.it/esplorazione/ MINI-EUSO energie/gaps/ sistema-solare/juno/ jem-euso.roma2.infn.it/?page_id=818 MRO SCORE www.nasa.gov/mission_ metis.oato.inaf.it/score.html pages/MRO/mission/index. html SOLAR ORBITER www.asi.it/esplorazione/ ci.esa.int/web/solar-orbiter sistema-solare/mio-/ metis.oato.inaf.it

NEIL GEHRELS SWIFT SPICA OBSERVATORY https://www.ir.isas.jaxa.jp/ swift.gsfc.nasa.gov SPICA/SPICA_HP/index-en. www.asi.it/esplorazione/alte- html energie/swift/ sci.esa.int/web/cosmic-vision/- www.swift.ac.uk /53635-spica

NUSTAR STEREO www.nasa.gov/mission_pages/ stereo.gsfc.nasa.gov nustar/overview/index.html nustar.ssdc.asi.it THESEUS 139 www.isdc.unige.ch/theseus/ OLIMPO www.esa.int/ESA_Multimedia/ olimpo.roma1.infn.it/index. Images/2019/03/Theseus_ html mission_concept

OSIRIS-REX VITA www.nasa.gov/osiris-rex www.esa.int/Space_in_ Member_States/Italy/ PLATO Missione_VITA_Paolo_ sci.esa.int/web/plato Nespoli www.asi.it/esplorazione/ www.asi.it/vita-nello-spazio/ sistema-solare/plato/ missioni/expedition-52-53- www.oact.inaf.it/plato/Plato- vita/ Italia/Home.html XMM-NEWTON PRISMA www.cosmos.esa.int/web/ www.asi.it/scienze-della-terra/ xmm-newton prisma/ sci.esa.int/web/xmm-newton 140 ACKNOWLEDGMENTS

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acknowledgments

Editors The editors Roberto Orosei Isabella Pagano acknowledge the Giuseppe Piccioni Teresa Capria contribution of the Piergiorgio Picozza Federica Duras following people as Giampaolo Piotto Livia Giacomini contributors. Luigi Piro Giulia Mantovani Roberto Ragazzoni Pietro Ubertini Sofia Randich Lorenzo Amati Fabio Reale Giovanni Ambrosi Paolo Soffitta Angela Bazzano Daniele Spadaro Tomaso Belloni Luigi Spinoglio Graphics Valentina Braito Gianpiero Tagliaferri John Robert Brucato Marco Tavani Patrizia Caraveo Elisabetta Tommasi Davide Coero Borga Elisabetta Cavazzuti Monica Tosi Ginevra Trinchieri 143 Alessandro Coletta Diego Turrini Marino Crisconio Valerio Vagelli Paolo de Bernardis Giovanni Valentini Maria Cristina De Sanctis Luca Valenziano Roberto Della Ceca Stefano Vitale Vincenzo Della Corte Angela Volpe Piero Diego Elisabetta Dotto Silvano Fineschi Mario G. Lattanzi Monica Lazzarin Ettore Lopinto Maria Federica Marcucci Silvia Masi Gabriele Mascetti Giusi Micela Alessandro Mura Lorenzo Natalucci 144

Aa.Vv. Italian Report to the 43rd COSPAR Scientific Assembly

Editors: Maria Teresa Capria, Federica Duras, Livia Giacomini, Giulia Mantovani and Pietro Ubertini.

Graphic design & layout: Davide Coero Borga © 2020 All rights reserved

Cover credit: NASA/Bill Ingalls. 3 Italy is more than ready to confront the challenges of space science and to contribute in a fundamental way 4 to the scientific discoveries of the next decade.