ASTRONOMY, ASTROPHYSICS AND SPACE SCIENCE

Seminari

Il Dottorato in Astronomy, Astrophysics and Space Science incoraggia gli studenti a seguire in grande numero di seminari organizzati dagli istituti che organizzano il corso:
- Sapienza Università di Roma, dipartimento di Fisica
- Università degli studi di Roma "Tor Vergata", dipartimento di Fisica
- INAF, Istituto Nazionale di AstroFisica

Segue lista di seminari

2026

Cosmic Microwave Background Experiments as a Laboratory for Fundamental Physics
09/07/2026
Building on over a decade of rapid gains in cosmic microwave background (CMB) sensitivity, CMB surveys are now poised to map the millimeter sky with unprecedented depth at arcminute resolution. In this talk, I will discuss how the Simons Observatory (SO) is leading this charge, specifically through the Large Aperture Telescope and its currently observing receiver upgrade, Advanced SO. The SO survey, intends to observe the fine details in the CMB with increased sensitivity, probing the initial conditions of the early universe as well as the formation of structure due to the presence of gas and dark matter. I will highlight how these instrumental leaps enable two distinct searches for new physics: using the pairwise kinematic Sunyaev-Zeldovich (kSZ) effect as a model-independent probe of the gravitational force law, and searching for parity-violating signatures of new particles through cosmic birefringence, the rotation of the CMB polarization as it travels from the surface of last scattering to us throughout the universe.

The Atacama Large Aperture Submillimeter Telescope (AtLAST): enabling large-scale sub-mm science beyond 2030
02/07/2026
Astronomical observations at (sub-)millimeter ((sub-)mm) wavelengths are uniquely suited for studying regions of the Universe that are too cold, too dusty, too distant, or too hot and tenuous to be probed in the visible and at other wavelengths. Current (sub-)mm telescopes have achieved major breakthroughs, beyond what is possible with optical and infrared observations. However, many emerging science goals now exceed the capabilities of existing telescopes. Achieving the next transformational leap in discovery requires a new, large-aperture (50-meter), multi-purpose single-dish telescope with a wide field of view (FoV, >=1 deg) and a fast mapping speed across the full (sub-)mm band (30-950 GHz). These requirements cannot be met through upgrades of existing facilities, but demand a fundamentally new approach to telescope and instrument design. In parallel, climate change and fuel price volatility are challenging many fields, including astronomy, to become more sustainable and responsibly use energy resources. Because they require clear skies, dry atmospheric conditions, and a pristine radio environment, major astronomical observatories are often located in remote areas, sometimes near communities with limited access to reliable power. Telescope operations are power intensive, and, particularly in the (sub-)mm/radio bands, they may continue up to 24 hours per day requiring a continuous year-round power supply. Historically, sustainability has not been a primary driver in observatory design and operations, leading to continuous dependence on fossil fuels. Active research in the field of renewable energy, tailored to the needs of astronomical facilities, is therefore a necessary first step towards a meaningful transition. The dual ambition to pursue transformational science in the (sub-)mm and make astronomy sustainable has motivated the Atacama Large Aperture Submillimeter Telescope (AtLAST (https://www.atlast.uio.no). In this seminar, I will summarise the current status of AtLAST development, showing the results of the EU-funded Design Study (AtLAST, 2021-2024 https://cordis.europa.eu/project/id/951815), and preliminary results from the ongoing EU-funded design consolidation project (AtLAST2, 2025-2028, https://cordis.europa.eu/project/id/101188037).

Probing binaries with wide binaries
11/06/2026
Wide binaries (WBs) offer a unique opportunity to test gravity in the low-acceleration regime. Because they experience gravitational accelerations comparable to those in the outer regions of galaxies, yet are unaffected by dark matter, and their dynamics are well understood. Furthermore, they can be treated as isolated systems because the differential acceleration exerted by the Galaxy on the two stars is negligible. Thanks to exceptional astrometry from Gaia, it has been possible in recent years to construct large samples of WBs with precise projected separations and transverse velocities (2D analyses). However, these studies have reached conflicting conclusions on whether Newtonian gravity best reproduces observations for systems in the low-acceleration regime (e.g., <~10-9 msec-2 ). We focused instead on the study of 3D solutions by adding precise and accurate radial velocities to the Gaia data. High-quality radial velocities are essential for identifying and removing multiple systems; when combined with Gaia DR3 parallaxes and proper motions, they allow the orbits of binaries to be tightly constrained. We first analyzed ESO 3.6m/HARPS spectra for 32 WBs, finding that 31 of them could be represented with a viable, bound Newtonian solution. From a second sample of 12 wide binaries with very large separations (greater than 13,000 AU) observed with ESPRESSO@VLT, we found that for three of the systems, no bound Newtonian orbits were possible. However, these binaries have very large separations and are expected to be disrupted by interactions with the Galaxy or encounters with other stars. Finally, we added a sample of 26 low-mass WBs, because these binaries experience low accelerations at much smaller separations, thereby minimising the probability of disruption by Galactic tides or third bodies. Performing a Monte Carlo analysis on the entire sample, we find bound Newtonian solutions for 65 out of the 70 WBs; we map the orbital parameter solutions and find that their distribution behaves as expected. This agreement holds even when dividing the data into low- and high-acceleration samples, with the possible exception of the orbital phase. Considering that the unbound systems are likely disrupted binaries, we conclude that Einstein-Newtonian gravity provides a coherent view of wide binaries, and no evidence for new physics is required. Looking ahead, Gaia DR4 and a new, large sample of WBs currently being observed with ESPRESSO@VLT will provide new insights into this fascinating test.

Data-driven constraints on the coevolution of supermassive black holes and their host galaxies
09/06/2026
Most, if not all, massive galaxies host a supermassive black hole (SMBH) in their nucleus. Yet the formation and evolution of these SMBHs remains one of the key open questions in astrophysics. This has gained renewed attention as, at low redshift, PTAs have recently detected a gravitational wave background, however this may be in tension with the demography of local SMBHs. While at high redshift, JWST has significantly extended the observable parameter space, revealing a diverse population of active galactic nuclei (AGN) which, at face value, appear both more massive and more numerous than the pre-JWST expectations. Motivated by these findings, we present a data-driven investigation of the coevolution of SMBHs and their host galaxies across cosmic time (z = 10 - 0) using the semi-empirical model DECODE. In this model, the growth of galaxies is associated to that of its host halo via abundance matching between the star-formation rate and halo-accretion rate, whereas BHs are grown via the observed accretion rate distribution, with mergers included in accordance with the dark matter merger trees. Thereby offering physical insights, while minimising the number of assumptions and free parameters. At high z, we demonstrate that current estimates of the AGN luminosity function can reproduce the most massive AGN observed by JWST at z ~ 6 – 8 and predicts a mean SMBH mass – stellar mass relation at z = 6 that lies below the AGN observed by JWST, but is consistent with them being the tail of the underlying distribution. At intermediate z, we find that the BH-galaxy scaling relations are near constant with redshift, but that the intrinsic scatter decreases with both cosmic time and mass. Furthermore, this evolution of the intrinsic scatter is driven primarily by accretion, with mergers playing a minor role. At low z, we find that local SMBH mass function is primarily driven by accretion, with mergers only meaningfully contributing at high masses, and that this lies below the mass function claimed to be consistent with the PTA measurements. Thus, corroborating the tension previously identified within a distinct data-driven framework. In the near future, we will further extend DECODE to predict the gravitational wave signal in both the PTA and LISA bands.

Probing the Universe with cross-correlation of Large-Scale Structure observables
04/06/2026
Cross-correlation analyses between tracers of the large-scale structure (LSS) of the Universe have become one of the most powerful tools in modern astrophysics and cosmology. By combining independent observables, we can map the distribution of both dark and luminous matter across different cosmic epochs while better handling the instrumental and observational systematics that often affect single surveys. Moreover, this approach allows us to effectively break degeneracies between nuisance and cosmological parameters, providing competitive constraints on both. In this talk, I will discuss the cross-correlation of Cosmic Microwave Background (CMB) lensing with radio galaxy maps and with the Quaia quasar sample, showing how these tracers map the growth of cosmic structures up to high redshifts. I will then focus on state-of-the-art results obtained from the newly released Euclid Quick Release 1 (QR1) data, presenting their high-significance cross-correlation with both CMB lensing and the EMU radio survey. Ultimately, this overview highlights how synergies approaches between LSS observables can be a unique tool for testing our description of the Universe.

Velocity-Resolved Fine Structure Line Observations and Star Formation: New Results and New Capabilities
27/05/2026
What controls star formation?" is a key question in astrophysics, and one very important aspect of this is the interaction of newly-formed stars with their surroundings. The radiative and mechanical feedback from young, massive stars can be dramatic. The altered composition and increased temperature that result make atomic and ionic fine structure lines ideal probes of stellar feedback. The value of such observations is dramatically increased if the spectral lines are velocity-resolved so that the momentum and energy impact on the stars’surroundings can be determined. But such observations must be carried out from suborbital or space observatories due to absorption in the Earth’s atmosphere. The fine structure lines of ionized carbon, and atomic oxygen are the most important and have been widely observed with high spectral resolution starting with the Herschel HIFI instrument and continuing with upGREAT on SOFIA. In this talk I will discuss some recent fine structure line observations focusing on the effects of star formation on the surrounding interstellar medium and possible problems with measuring the rate of star formation. I will conclude by presenting two fine structure line spectroscopic balloon missions. GUSTO was launched on 31 December 2023, and until 27 February 2024 surveyed the 205 μm line of [NII] and 158 μm line of [CII] in the central portion of the Milky Way and the Large Magellanic Cloud. ASTHROS, which is to follow at the end of 2027, has a much larger 2.5m diameter telescope, and will observe both [NII] fine structure lines to derive the electron density in selected regions.

The steady-state population of Earth's co-orbitals of lunar provenance
12/05/2026
When we talk of coorbital motion, we assume a three-body problem where two of the three bodies orbit the central one in approximately the same amount of time. In other words, the coorbital motion is a 1:1 mean motion resonance. Different asteroids and moons in the solar system exhibit this behavior with respect to a given planet and are of particular interest because they usually show a quite stable evolution. Given the recent hypothesis that the asteroid Kamo‘oalewa, in coorbital motion with the Earth, could have a lunar provenance, in this work we deepen this possibility, by estimating the steady-state number of Earth’s coorbitals coming from lunar ejecta, originated by a high enough energetic impact. The results show that the Moon can provide small Earth’s co-orbitals, characterized by a low eccentricity and inclination, but the main belt (mainly the inner region) can explain the known Earth’s co-orbital population. From the same main belt model, we get a high percentage of tadpole objects, not yet discovered. The work also indicates the possibility that spectroscopic and orbital characterization can constrain impact processes scaling laws.

Space science and technology
29/04/2026
Ongoing and upcoming cosmological surveys—including the Simons Observatory, LiteBIRD, Rubin LSST, Euclid, DESI, PSF, SPHEREx, and the Roman Space Telescope—will deliver observations of unprecedented precision. Joint analyses across these surveys will be essential for uncovering fundamental physics, including the nature of inflation, dark energy, dark matter, neutrino mass, and more. In this talk, I will discuss the opportunities, challenges, and strategies for simulating our universe across multiple wavelengths to realize these goals.

Neutrino astronomy in the era of the Global Neutrino Network
22/04/2026
In recent years, neutrino astronomy has emerged as a new window into the extreme and hidden universe. Current-generation experiments have detected high-energy neutrinos of astrophysical origin and identified the first sources, opening the field to discovery. The Global Neutrino Network program will focus on the very and ultra-high energy neutrino sky and can be crucial for the future multi-messenger prospects. In this talk, a special focus will be dedicated to the KM3NeT/ARCA telescope, under construction in the Mediterranean Sea, to its scientific goals and the observation of KM3-230213A with the possible associated origins. Moreover, some of the most recent questions linked to different very-high-energy astrophysical accelerators will be reviewed.

2025

Non-Gaussianity in Planck, LiteBIRD and component separation
18/12/2025
Non-Gaussianity in cosmology is the study of deviations from a Gaussian distribution in cosmological observables, commonly probed through the 3-point correlator, the bispectrum. Primordial non-Gaussianity (PNG), i.e. the bispectrum of the primordial fluctuations, provides a powerful means of constraining inflationary models. I will present how our analysis of the Planck Release 4 (PR4) data has yielded the most stringent constraints to date on scalar PNG, and how future missions such as LiteBIRD will further enhance these measurements by accessing the tensor sector. I will then introduce a new formalism for the Spectral Matching Independent Component Analysis (SMICA) method that incorporates higher-order statistical information from foregrounds. This framework enables direct bispectrum estimation using frequency-channel maps, allowing simultaneous recovery of the bispectra of multiple components. By shifting non-Gaussianity estimation from the cleaned-map stage to the component-separation step, the method more effectively propagates and manages foreground uncertainties. This approach optimally combines the data by jointly accounting for both the power spectrum and bispectrum of all components—an improvement over standard analyses.

The hot Neptune desert: Neptunian planet demographics, validation, and PLATO prospects
17/12/2025
ABSTRACT: Hot Neptunian planets, that is Neptune-size planets at short orbital periods, occupy a scarcely populated region in the radius–period plane. The origin of this so-called hot Neptune desert is a key puzzle for theories of planetary formation. I will present recent results on the demographics of Neptunian planets in and around the desert, showing how revised stellar properties and homogeneous vetting of TESS candidates modify the inferred occurrence rates and the desert's structure. I will summarise the validation of short-period Neptunes and the construction of homogeneous catalogues, and outline how irradiation and mass-loss processes sculpt the hot Neptune desert. Finally, I will briefly discuss the prospect for the ESA PLATO mission to obtain new data and deeper insight into this riddle, and our recent work related to PLATO's broader goal of detecting and characterising potentially habitable planets.

Ground-based scientific perspectives for the next decades
16/12/2025
A variety of ground-based facilities and surveys are broadening our understanding in different astrophysical domains by relying on complementary techniques and tools. These observations on one side help clarify several contentious issues, on the other introduce new key questions. The situation will become even more intricate with the contribution of upcoming ground-based instruments (such as the Rubin-LSST, ELT, SKA, and CTA), as well as the next generation of gravitational wave detectors (including LISA and the Einstein Telescope). New discoveries and new debates are expected in the next 10-20 years. Some of the current open problems will have been at least partially answered, others will still be open and new questions will arise. This complex landscape needs to be taken into account when thinking of the next ESO big facility after ELT, a process called Expanding Horizon, that ESO started some months ago. On this basis, and in the context of current and upcoming projects, as well as of the ESO Expanding Horizons initiative, the scientific perspectives for the next decades will be presented and discussed.

NinjaSat: Astronomical X-ray CubeSat Observatory
11/12/2025
NinjaSat is a 6U X-ray CubeSat that was funded at RIKEN in April 2020 and launched into a 530-km Sun-synchronous orbit on November 11, 2023. The mission is dedicated to pointed observations of X-ray sources, aiming to monitor newly emerging bright X-ray transients as well as conduct long-term observations of known objects. The satellite carries two non-imaging gas proportional counters (Gas Multiplier Counters; GMCs) with a total effective area of 32 cm^2 at 6 keV, providing photon-event time tags with a resolution of 61 microseconds. To monitor the space radiation environment, NinjaSat is also equipped with two Si-PIN radiation belt monitors (RBMs). [Ref.1] Scientific operations began on February 23, 2024, and continued until re-entry on September 18, 2025, during which NinjaSat successfully observed 32 X-ray targets. In this talk, I will describe the mission design, instrumentation, operations, and scientific results obtained with NinjaSat. In addition to its primary astronomical objectives, NinjaSat produced valuable byproducts, including demonstrations of X-ray pulsar navigation and atmospheric density measurements. I will also introduce the follow-up mission, NinjaSat2, currently planned for launch in 2028.

VLBI and Gaia Astrometry in the Service of AGN Astrophysics
05/12/2025
We are living in a golden age of astrometry when sub-milliarcsecond positional accuracies for a large number of extragalactic objects can be achieved in both the optical and radio wavebands. For many decades, very long baseline interferometry (VLBI) in the radio was the only method capable of providing such high-precision astrometric data for certain extragalactic objects, radio-loud active galactic nuclei (AGN). Recently, the European Space Agency's Gaia space mission has delivered massive amounts of accurate astrometric data for optically bright extragalactic sources. The synergy between these two techniques is unlocking new insights into AGN, allowing us to explore astrophysical phenomena such as jet physics, binary and dual supermassive black hole systems, and peculiar types of AGN. At the same time, it also contributes to improving the accuracy of celestial reference frames essential for most fields of astronomy, as well as spacecraft navigation and geodesy. In this talk, I will review some of the key results in this field, with an obvious bias towards studies I myself was involved in.

Revealing the Extreme Universe with CTAO: A New Piece of the Cosmic Puzzle
02/12/2025
Imaging Atmospheric Cherenkov Telescopes (IACTs) have transformed ground-based gamma-ray astronomy, enabling the detection and detailed study of very-high-energy (VHE) gamma rays from cosmic sources. Pioneering arrays such as H.E.S.S., MAGIC, and VERITAS demonstrated the power of stereoscopic observations, achieving arcminute-scale angular resolution, enhanced background suppression, and sensitivities on the order of 10⁻¹³ photons cm⁻² s⁻¹. Building on this legacy, the Cherenkov Telescope Array Observatory (CTAO) is the next-generation VHE gamma-ray facility, with two sites located in La Palma (Spain) and the Paranal desert (Chile), designed to operate for 30 years as an open, proposal-driven observatory. CTAO will cover a broad energy range from 20 GeV to 300 TeV, offering unprecedented sensitivity, improved angular and energy resolution, and a significantly wider field of view. Currently under construction, CTAO is approaching a pivotal milestone: the first intermediate array configurations are expected to deliver data within the next three years. Even at this early stage, these arrays will surpass existing facilities, enabling transformative studies of cosmic accelerators, transient phenomena, and fundamental physics. The early science program will emphasize short-duration events, positioning CTAO as a key player in multi-messenger and multi-wavelength astronomy. This talk will provide a construction update and highlight the scientific potential of the first arrays, showcasing CTAO’s role in unraveling the most extreme phenomena in the Universe and adding a crucial piece to the cosmic puzzle.

Exploring the Martian Ionosphere using Photochemical Model and Observations
27/11/2025
The Martian ionosphere has been a subject of study since the first mission to the red planet. It is the gateway of many atmospheric loss processes and therefore plays an important role in determining the evolution of the climate and habitability of Mars over geological time. The chemistry, dynamics and energetics of the ionosphere of Mars have spatial and temporal variations due to wide variations in solar forcing, atmospheric dynamics and composition, and the magnetic field. Understanding how competing physical processes produce the observed state of the ionosphere is a major unifying theme that underpins the science of the Martian ionosphere and its variability. There have been several space missions for studying Martian atmosphere/ionosphere. These missions have revolutionized our understanding on Martian environment. While observations are the key stone in our knowledge, they have inherent limitations in their temporal and geographical coverage. Computational models can help to overcome these limitations and in addition provide further insight into the physical processes that produce the observed structures. The need to determine how the ionospheric peak varies on spatial and temporal scales is the motivation behind developing a photochemical model for Martian ionosphere. Using the observations from NASA’s MAVEN spacecraft as model inputs, we investigate the behaviour of Martian electron and ion density profiles. The sensitivity of the modeled plasma profiles to the variations in parameters such as neutral atmospheres, plasma temperatures, etc are explored and used to interpret observed features in Martian ionosphere.

Processing of Gas in Galaxies within the Cosmic Web
26//11/2025
Galaxies are distributed in a complex filamentary network of matter called the cosmic web. It remains debated which is the overall impact of the cosmic web in processing cold gas of galaxies, as they move through large-scale filaments around the clusters down to the densest regions of the cluster cores. I will present the results of a large observational campaign, mainly exploiting IRAM millimeter facilities, with the goal of quantifying the processing of galaxies' gas in the cosmic web and with cosmic time. I will discuss the degree of such processing in a variety of dense megaparsec-scale environments. Finally, I will discuss the potential of such studies for next generation multi-wavelength facilities. Thousands of distant clusters and BCGs will be detected with Euclid, enabling an unprecedented leverage to constrain galaxy evolution in cluster.

Chasing Shocks with Solar Orbiter: Insights into Particle Acceleration During Solar Cycle 25
19/11/2025
Interplanetary (IP) shock waves propagate through the heliosphere as a result of solar activity. These shocks are key sites of energy conversion and particle acceleration and can be observed in situ through spacecraft measurements, providing a unique link to remote astrophysical environments and an excellent “natural laboratory” for testing still-debated acceleration mechanisms. The current fleet of heliospheric observers offers an unprecedented opportunity to study IP shocks, marking a “new golden era” for understanding their role in heliospheric energetics. In particular, Solar Orbiter provides high-resolution measurements in the suprathermal (above ~50 keV) range, opening a new observational window on how particles are accelerated out of the thermal population. In addition to presenting the statistical properties and trends of Solar Orbiter IP shocks up to the solar maximum of cycle 25, I will showcase specific events that uncovered new aspects of energetic particle production. I will show how leveraging state-of-the-art numerical simulations alongside multi-spacecraft observations makes it possible to probe the fundamental physics driving these acceleration processes in unprecedented detail. Together, these results offer fresh insights into how shocks energize particles across both heliospheric and astrophysical environments.

The population of infant black holes in the early Universe revealed by the James Webb Space Telescope
13/11/2025
The James Webb Space Telescope is revolutionising most areas of astrophysics. One of the most exciting and puzzling findings has been the discovery of a large population of accreting massive black holes within the first few billion years after the Big Bang. Their properties are remarkably different from Active Galactic Nuclei at lower redshift or when compared with the population of much more luminous quasars at similar cosmic epochs. Their large number and physical properties are difficult to reconcile with the standard black hole formation scenarios, and have required the development of new models, which are being tested against the additional constraints that are being provided by JWST. JWST has also revealed that the interplay between these early black holes with their host galaxies was probably quite different than what observed at later cosmic epochs, with important implications for the early formation of galaxies and their stellar populations. JWST is also finding an intriguing, significant population of dual black holes, which might be in the process of merging, indicating that this might be an additional route for their early growth and also an early source of gravitational waves. The seminar will give an overview of these various findings, highlighting the impressive progress made so far and also the exciting new questions that have been opened, as well as the prospects of tackling them in the coming years.

2024

Robust constraints on tensor perturbations from cosmological data: A comparative analysis from Bayesian and frequentist perspectives
20/12/2024
One of the central challenges in modern Cosmology is the precise characterization of the primordial tensor power spectrum, a cornerstone prediction of numerous cosmological models, particularly inflationary scenarios. These tensor perturbations carry distinctive imprints that can reveal their physical origins, making the robust reconstruction of their spectrum a pivotal goal for contemporary research. In this talk, I will present methods for constraining key parameters of the tensor power spectrum, such as the tensor-to-scalar ratio and the spectral tilt, with a particular emphasis on the statistical methodologies underpinning these inferences. I will critically examine the strengths and limitations of the standard Bayesian framework commonly employed in this context. Furthermore, I will demonstrate how complementary insights from a frequentist approach can deepen our understanding of the Bayesian results, offering a more nuanced perspective on the interplay between these statistical paradigms.

Wave dark matter
17/12/2024
We will explore the possibility that dark matter is composed of sufficiently light particles that it effectively behaves as a collection of waves. We will review the particle physics motivations and the rich wave phenomenology, and discuss the implications for astronomical observations and experimental detection.

Galaxy Clusters from adolescence to maturity: challenges for simulations
12/12/2024
In my talk I will review our understanding, through cosmological simulations, of the evolution of galaxy clusters from redshift z~2-3, to the recent cosmic epoch. Through a comparison with observational data at different wavelengths I will assess the capability of simulations to trace the fast evolution of such cosmic structures from their proto-cluster stage, characterized by a strongly star forming galaxy population embedded in a dynamically disturbed inter-galactic medium, to their relaxed stage at low redshift, characterized by a passive galaxy population immersed in a relatively relaxed intra-cluster medium. In this context, I will highlight successes of simulations, and critically assess their limitations and what we should learn from them.

Lighting up Blazar Physics at the Spectrum’s Edge: VHE and VLBI Synergies
12/12/2024
Blazars, a class of active galactic nuclei with jets aligned towards Earth, offer a unique opportunity to study extreme astrophysical processes. Their powerful jets emit across the entire electromagnetic spectrum, providing data at all wavelengths for investigation. This presentation focuses on the synergy between Very High Energy (VHE) gamma-ray observatories and VLBI arrays—two distinct facilities operating at opposite ends of the spectrum—used to uncover the mechanisms driving the non-thermal emission of blazars. VHE observations probe the highest energy emissions from these objects, while VLBI provides high-resolution imaging of their jet structures. Together, they enable the study of particle acceleration processes, jet kinematics, and emission variability across multiple scales. I will introduce the basics of VHE observations and the tools employed at the two extremes of the spectrum. Finally, I will present studies showing how this combined approach deepens our understanding of blazar physics, from the origins of high-energy photons to the dynamic behaviour of jets in their most compact regions.

Breaking the distance-duality relation to address cosmic tensions
11/12/2024
Persistent cosmic tensions arise from discrepancies in the cosmological distance ladder constructed from different distance observables, such as BAO and SnIa, which are calibrated using measurements from either the early or late Universe. These tensions are typically evaluated under the assumption that the distance-duality relation (DDR) holds, allowing for a direct comparison between measurements of the luminosity and angular diameter distances. In this talk, we will examine the implications of relaxing this assumption and considering more general relations. We will discuss how this approach impacts the interpretation of current cosmic tensions and its potential to clarify whether new physics is needed to address these discrepancies.

Extended AGN jets as a direct test to the ΛCDM model
03/12/2024
Current small-scale cosmological controversies are coming down to the precision level of observations. The key point is whether a better understanding of baryonic physics, dark matter physics, or both is required to address these challenges. In this talk, I will describe how very long baseline interferometric observations of extended AGN jets (sometimes gravitationally lensed) are contributing to understanding some of these small-scale cosmological issues while simultaneously providing insights on the jet physics up to the earliest epochs (z>6).

The nature and fate of the most obscured high-z massive galaxies
28/11/2024
The early assembly of the most massive galaxies, and their contribution to the SFR density of the universe is currently one of the main challenges for galaxy formation models. Recently, a population of massive red sources already in place at z>2-3 have been discovered, and called HST-dark, because they are missed by optical/UV search but detected at MIR and often in the mm. Their characterisation remains uncertain, due to limited information available, and to different selection techniques. JWST is now allowing us to investigate the nature of HST-dark galaxies, and to reveal new populations of early massive galaxies. I will discuss the main properties of HST-dark galaxies, compared to those of JWST NIR-dark. For those ALMA detected, the molecular gas mass and depletion times show that they are likely on the way to quenching their SF. For ALMA HST-dark, there is a consensus on the presence of large amounts of dust, posing the problem of high-z dust production. To constrain dust properties and obscured SF at high-z we need to observe in the FIR. I will present the recently selected NASA PRobe far-Infrared Mission for Astrophysics (PRIMA), a FIR (25-235 μm) observatory operating in the 2030s in spectroscopy and imaging, that will allow us a leap forward in our knowledge of the high-z obscured universe.

Gamma-Ray Burst Polarimetry: History and Future Prospects
25/11/2024
Gamma-Ray Bursts (GRB) are the brightest electromagnetic events in the Universe since the Big Bang. As such they have intrigued the astrophysical community since their accidental discovery in 1967. Despite almost 60 years of intense research, resulting in over 10000 GRB detections, very little remains known about these violent events. While we know that these events are related to the death of massive stars or the merger of compact objects, we still lack an understanding of how, and where, the gamma-rays which give these events their name, are produced. Attempts to understand this have thus far focussed primarily on measurements of the time of arrival, the direction and energy of the gamma-ray emission. Measurements of the 4th parameter, the polarization, are rare, despite their significant potential to resolve theoretical models. In this talk I will discuss this potential in detail, while in parallel addressing the reasons for the lack of polarization measurements. Finally, I will present an overview of past missions as well as the missions which aim to provide the first detailed measurements in the coming decade.

Recent observations of the near-Earth radiation environment: a plethora of galactic, solar and magnetospheric particles
22/11/2024
The near-Earth radiation space is a unique environment where particle populations of different origins coexist and evolve dynamically over time and space, spanning a wide energy range. Galactic cosmic rays – entering the heliosphere – are continuously modulated by the change in the solar wind and the associated heliospheric magnetic field. Moreover, changes in galactic particle fluxes show a very clear time-dependence, which is directly related to the periodical activity of the Sun. However, the Sun acts as both a modulator and a source of space radiation – especially during maxima of solar activity – with powerful emissions of the so-called solar energetic particles (SEPs). Despite notable improvements in the latest decades, the complex mechanisms underlying their origin and transport still challenge the development of a comprehensive picture of SEP events. Many efforts have also been directed at modelling the Earth’s trapped charged particle environment, as in the case of the South Atlantic Anomaly (SAA). Observations of the SAA radiation environment are crucial to validate these models (e.g., the NASA AE9/AP9 models), as well as to investigate the temporal evolution of the geomagnetic field, to study perturbations generated by space weather events (such as geomagnetic storms), and, last but not least, to safeguard spacecraft systems and human crew health. After the foundational results of successful past (PAMELA) and present (AMS-02) spaceborne missions, the CSES (China Seismo-Electromagnetic Satellite) mission aims to continue the study of the near-Earth radiation environment, through a constellation of low-Earth orbit satellites. This presentation will review the main results achieved by the High-Energy Particle Detector (HEPD-01) on board the CSES-01 satellite, which will be followed by the launch of the improved HEPD-02 detector on the CSES-02 satellite in December 2024.

Magnetic field amplification in neutron star mergers and the role of the MRI
21/11/2024
The first detection of a binary neutron star merger has made sharp reality the long-standing paradigm that these cosmic fireworks are exciting laboratories for extreme physics. To get the most out of present and future observations, however, we require accurate models of the merger dynamics, which can only be achieved through numerical relativity simulations. One of the key factors in these simulations is the magnetic field, which plays a crucial role in shaping the dynamics of the system. It is also instrumental in the launching of relativistic jets and the associated gamma-ray bursts. In this seminar I will discuss the main mechanisms responsible for the amplification of the magnetic field, with a particular focus on the magneto-rotational instability and its potential role in binary neutron star mergers."

2023

Towards the geology of exoplanets
20 Aprile, 2023, ore 16:30 CEST
Hot rocky exoplanets offer exciting opportunities to place terrestrial geology into Galactic context, through composition measurements with JWST and Ariel. To capitalise on these opportunities we must identify the very best targets for spectroscopic characterisation. The catastrophically disintegrating exoplanets (CDEs) are the most dramatic examples of mass loss from an ablating rocky surface. They were discovered by Kepler through the variable transits of dust co-existing with metal-rich vapour, and are particularly suitable for transmission spectroscopy because the ablated material is spread over a large scale-height. But the Kepler CDEs are too faint for transmission spectroscopy. The Dispersed Matter Planet Project (DMPP) is discovering the nearby analogues and progenitors of the Kepler CDEs. DMPP uses archival stellar spectra to identify stars we view through shrouds of diffuse, metal-rich, circumstellar gas. The underlying hypothesis is that the gas is ablated from hot, close-orbiting planets. DMPP searches for the putative planets with high-precision, high cadence radial velocity measurements. The approach has been extremely successful and efficient, with planet discoveries whenever 60 RV measurements have been collected. DMPP-1 is a compact multiplanet system orbiting a star brighter than V=8. A possible CDE transit has been discovered in TESS data. DMPP-2 b is the joint-first RV planet discovery orbiting a strongly pulsating star. DMPP-3 is an eccentric binary star system with the secondary at the mass threshold for sustaining hydrogen fusion. A 2.6 Earth mass planet orbits the K0V primary star in a 6.7 day orbit, with a second Earth-mass circumprimary planet marginally detected. DMPP-3AB is in a hitherto unpopulated parameter space for binary star planetary systems. I will include updates on our latest discoveries of around 20 short period planets, including planets orbiting a star of magnitude 6, and planets orbiting a young star. We may have caught the latter system in the act of evolving out of the Neptune desert through planetary ablation. DMPP planets are likely to be viewed edge-on as ablated material will remain concentrated near the planets’ orbital planes. Thus they have high transit probability. The subset of DMPP planets which transit are thus amenable to direct empirical determinations of mass, radius and composition.

2022

Annalisa Pillepich, Max Planck Institute for Astronomy, Heidelberg: The many diverse manifestations of supermassive black-hole feedback: from simulations to observations, and back
26 ottobre 2022
Large-volume cosmological galaxy simulations, such as IllustrisTNG, provide a holistic view on galaxies and on how their evolution depends on the interplay of internal and external physical phenomena. Among the internal mechanisms, feedback from super massive black holes (SMBHs) is commonly invoked in such numerical models to halt star formation in massive galaxies. In fact, no other mechanism so far has been shown to be capable of returning entire populations of simulated massive quenched galaxies that are consistent with the observed galaxy red sequence and quenched fractions. With simulations like IllustrisTNG we are putting together ever more quantitative and plausible evidences as to the role that feedback from SMBH can have, not only in shaping galaxy structural properties and galaxy populations across 90 per cent of the Universe’s history, but also in regulating the thermodynamical, ionization, and metal enrichment properties of the cosmic gas across halo scales and beyond. In this talk, I will use the outcome of the IllustrisTNG and other simulations in combination with current and future observational data, chiefly SDSS galaxy data and eROSITA X-ray observations, to further our understanding of the tight interconnections between SMBHs, star-formation quenching, and the physical state of the circumgalactic medium.

Pascal Oesch, University of Geneva: Galaxy Build-up During the Cosmic Reionization Epoch
4 luglio 2022
Speaker: Pascal Oesch (University of Geneva) Title: Our Panchromatic View of Galaxy Build-up at Cosmic Dawn into the JWST Era Abstract: The first deep images with the Hubble Space Telescope (HST) have transformed our view of the Universe. Over the following more than two decades, HST continued to extend our cosmic horizon reaching to only ~400 Myr after the Big Bang at z~11. In combination with other observations across the electromagnetic spectrum, from the rest-frame optical with Spitzer/IRAC, and now all the way to (sub)mm wavelengths with ALMA/NOEMA, we are gaining a more and more complete census and understanding of galaxy build-up across 97% of cosmic history. Yet some critical gaps remain, mainly because (1) our galaxy samples are still mostly rest-UV selected at z>3, and (2) we still only have highly-incomplete spectroscopic information at z>6. In this talk, I will present an overview of our current understanding of star-forming galaxies at z>3 based on our panchromatic view from HST+Spitzer+ALMA/NOEMA data. This will be completely revolutionized over the next months, however, as the first observations with the JWST are being taken. In particular, JWST will provide deep rest-frame optical data out to z=10, both in imaging and spectroscopy, which is truly unprecedented. JWST will thus finally allow us to probe the physics of the first generations of galaxies that ended the cosmic Dark Ages and started the reionization of the Universe. Join Zoom Meeting https://uniroma1.zoom.us/j/81122901013?pwd=M1hnRHRXZkEyeW1QMFlPQ2FXa0dNZz09 ID riunione: 811 2290 1013 Passcode: 686688

Elena Maria Rossi, Leiden Observatory: A multi-tracer study of the Local Group of galaxies
8 giugno 2022
The Local Group, and the Milky Way in particular is a unique laboratory to study the process of galaxy assembly because of our vantage point. This is especially true in this era of current and up-coming (all sky) surveys like e.g. Gaia, WEAVE, 4MOST, DASI, LSST, and Euclid, that are delivering an unprecedented astrometric, spectroscopic and photometric view of the Galactic stellar population. In this talk, I will review my group's work --both theoretical and observational -- towards the understanding of the mass distribution and other properties of the Milky Way using different dynamical tracers such as stellar streams and hypervelocity stars. Looking at the future, I will also show my vision for Galactic studies in the LISA era, when gravitational waves will deliver complementary information with respect to electromagnetic waves.

Samaya Nissanke, University of Amsterdam: Gravitational waves and multi-messenger astrophysics
26 maggio 2022
Abstract: Since the revolutionary discovery of gravitational wave (GW) emission from a binary black hole merger in 2015, the exquisite GW detectors LIGO, Virgo and KAGRA have detected more than 90 compact object mergers. Most notably, one of these mergers corresponds to the first binary neutron star merger, dubbed GW170817. This event has been transformative because it was observed in both gravitational and electromagnetic radiation, thus opening up a new era in multimessenger astrophysics. The multi-messenger characterisation of such an event has enabled major advances into diverse fields of modern physics from gravity, high-energy and extragalactic astrophysics, nuclear physics, to cosmology. In this talk, I will discuss work in strong-field gravity astrophysics and how combining observations, theory and experiment is key to make progress in this field. I will present the opportunities and challenges that have emerged in multi-messenger astrophysics, and what the future holds in this new era. Join Zoom Meeting https://uniroma1.zoom.us/j/81122901013?pwd=M1hnRHRXZkEyeW1QMFlPQ2FXa0dNZz09 ID riunione: 811 2290 1013 Passcode: 686688

Rachel Somerville, Center for Computational Astrophysics Flatiron Institute: Developing new galaxy formation models that will help us Learn the Universe
5 maggio 2022
Understanding and simulating galaxy formation from first principles is a huge computational challenge because of the vast range of scales and rich array of physics involved. Upcoming experiments will map galaxies and gas across unprecedented volumes and probe further back into cosmic time than ever before. These experiments have the potential to probe fundamental physics questions such as the nature of dark matter and dark energy, and the initial conditions of the Universe. But in order to extract the full scientific potential from these data, we need to understand how luminous tracers (stars and gas) are related to the underlying matter density field, and we must develop techniques that can accurately forward model the galaxy formation process with a computational efficiency that is orders of magnitude higher than standard numerical hydro/N-body techniques. I will describe the philosophy and status of the SMAUG (Simulating Multiscale Astrophysics to Understand Galaxies) project, and how it will form a pillar in the new Simons Collaboration "Learning the Universe", which will combine new galaxy formation models, new machine learning techniques, and simulation based inference to obtain constraints on cosmology and astrophysics.

Georges Meynet, University of Geneva: Stars at the Extreme: First Stars, Spinstars and Supermassive Stars
6 aprile 2022
The presentation will focus on stars at some extreme either from the point of view of their mass (supermassive stars), rotation (spinstars) or initial composition (Pop III stars). The talk will begin by a general overview of the main challenges faced by the modeling of massive stars with a special focus on the transport processes in convective and radiative zones. Then the presentation will continue discussing recent results about the binary statistics of Pop III populations, the chemical and radiative feedback of Pop III stars, the evolution of very massive stars i.e. stars with masses between 150 and 300 solar masses at different metallicities addressing the question of the progenitor of Pair Instability supernovae and the limits of the mass domain for the black hole mass gap. Finally, new models for the formation of supermassive stars that are candidates as seeds for the formation of supermassive black holes at high redshift will be presented

Felix Aharonian, Dublin Institute for Advanced Studies and Max-Planck-Institute for Nuclear Physics (MPIK), Heidelberg, Germany: PeVatrons and the "Century-old-Mistery" of Galactic Cosmic Rays
2 marzo 2022
Despite the recent advances in Cosmic Ray studies, the origin of Galactic Cosmic Rays (CRs) is still considered a "century-old mystery" - we do not know yet which sources contribute to CR fluxes measured in the Earth's vicinity. Identifying the major CR contributors with astronomical source populations is one of the highest priorities of the field. The best carriers of information about CR factories are gamma-rays and neutrinos - the only stable and neutral secondary products of CR interactions pointing to the CR production sites. The recent years' outstanding achievement of gamma-ray astronomy was the discovery of TeV gamma-radiation from SNRs generally supporting the SNR paradigm of the origin of Galactic CRs. On the other hand, the lack of the extension of gamma-ray spectra of young SNRs well beyond 10 TeV raises doubts about their ability to contribute to the highest energy galactic CR spectrum in the so-called "knee" region above 1 PeV. Meanwhile, the ultra-high-energy (UHE; E> 100 TeV) gamma-ray observations of the clusters of young massive stars demonstrate mounting evidence of these objects (and related superbubbles) being prime contributors to Galactic CRs at PeV energies. I will discuss these observations in the context of the concept of "Young Stars versus Dead Stars". The hunt for CR PeVatrons cannot be reduced merely to the identification of the sources contributing to the local "CR fog". The term 'cosmic rays' has broader implications; after matter, radiation and magnetic fields, the relativistic nonthermal plasma constitutes the fourth substance of the observable Universe. The localisation and exploration of physical conditions and processes in these extreme CR factories, independent of their relative contributions to the 'CR fog', is a fundamental issue in its own right. I will highlight the recent exciting achievements of UHE gamma-ray astronomy in elucidating the cites of extreme CR accelerators in the Milky Way and discuss the implications of the discovery of a large number of CR PeVatrons by the LHAASO collaboration.

Volker Bromm, University of Texas at Austin: What do we know about the first stars and galaxies?
8 febbraio 2022
I will review the emerging theoretical framework for how stars, galaxies, and black holes transformed the early universe. Predictions for the enrichment of the intergalactic medium with heavy chemical elements, the rate of supernova explosions and gamma-ray bursts, as well as the number density and properties of the first galaxies, sensitively depend on the particle-physics nature of dark matter. To constrain the elusive first generation of stars, we can bring to bear a powerful combination of probes at high redshifts and in our local neighborhood. The latter approach, known as “stellar archaeology” holds particular promise in light of ongoing and planned large surveys of metal-poor stars, both in the Milky Way and its dwarf satellites. It is exciting to contemplate the decade ahead, when the James Webb Space Telescope (JWST) will allow us to confront theory with observations at the edge of time.

2021

Licia Verde, ICREA and Institute of Cosmological Sciences, University of Barcelona: "The future beyond precision cosmology"
14/12/2021
The standard cosmological model (the LCDM model) has been established and its parameters are now measured with unprecedented precision. This model successfully describes observations from widely different epochs of the Universe, from the first few minutes, all the way to the present day. However, there is a big difference between modelling and understanding. The next decade will see the era of large surveys; a large coordinated effort of the scientific community in the field is on-going to map the cosmos producing an exponentially growing amount of data. But precision is not enough: accuracy is also crucial. The "unreasonable effectiveness” of the LCDM model offers challenges and opportunities. I will present some of the lines of enquiry explored by my group in this direction.

Samaya Nissanke, University of Amsterdam: "Gravitational waves and multi-messenger astrophysics"
30/11/2021

Giovanna Tinetti, Department of Physics and Astronomy, University College London: "Decoding the light from other worlds"
09/11/2021
Thousands of planets orbiting stars other than our own are being discovered (extrasolar planets). Since their discovery in the 1990s this field of astronomy and planetary science has exploded, being today one of the most exciting and dynamic. Even within the limits of our current observational capabilities, studies of extrasolar planets have provided a unique contribution to improving our view of the place that the Solar System and the Earth occupy in the galactic context. The arrival of more performing and dedicated facilities from space and the ground in the coming decade, will provide an unprecedented opportunity to study these worlds in great detail. In this talk, I will review highlights and pitfalls of our current knowledge of this topic and discuss the scientific and technical steps to be taken in this fascinating journey of remote exploration of the planets in our Galaxy.

Pavel Kroupa, University of Bonn and Charles University of Prague: How observations of stellar populations constrain cosmological models
19/10/2021
Quasars are found to appear a few hundred Myr after the Big Bang, but pressing matter together into super-massive black holes (SMBHs) so quickly appears to be impossible. At a later stage, the spheroidal component of a galaxy (its bulge if it is not an elliptical galaxy) is observed to show a correlation between its mass and that of the central SMBH it harbours, although spheroids with a mass lower than a few 1E9 Msun appear to only host a nuclear star cluster. I will discuss a theory for the formation of SMBHs which accounts for these observations using standard, non-exotic physics.

Ralf Klessen, Institute for Theoretical Astrophysics, University of Heidelberg: Star formation through space and time
23/09/2021
Stars and star clusters are the fundamental visible building blocks of galaxies at present days as well as in the early universe. They form by gravitational collapse in regions of high density in the complex multi-phase interstellar medium. The process of stellar birth is controlled by the intricate interplay between the self-gravity of the star-forming gas and various opposing agents, such as supersonic turbulence, magnetic fields, radiative feedback, gas pressure, and cosmic rays. Turbulence plays a dual role. On global scales it provides support, while at the same time it can promote local collapse. This process is modified by the thermodynamic response of the gas, which is determined by the balance between various heating and cooling processes, which in turn depend on the chemical composition of the material. In this talk I will try to give an overview of the our understanding of the star-formation process, discuss some examples of the recent progress in the field, and speculate about the implications for stellar birth in the high-redshift universe.

Piero Madau, Department of Astronomy and Astrophysics, University of California Santa Cruz: The dark and luminous side of structure formation
22/06/2021
The beaded filamentary network of intergalactic gas in which galaxies form and evolve, and which gives origin to a “forest” of hydrogen Lyman-alpha absorption lines in the spectra of distant quasars, encodes information on the physics of structure formation, the nature of the dark matter, the temperature and ionization state of baryons in the Universe. The potential of the Lyman-alpha forest for constraining with percent accuracy the matter density distribution on medium to small cosmological scales has motivated the construction of the Dark Energy Spectroscopic Instrument (DESI), which will measure absorption line spectra backlit by nearly a million high-redshift (z >2) quasars. In this talk I will describe the multiple steps needed to connect flux fluctuations in quasar spectra to physical parameters, present an unprecedented suite of hundreds of high-resolution hydrodynamical simulations of structure formation with different thermal histories, and use it to perform a statistical comparison of mock spectra with the observed 1D flux power spectrum and other data. A likelihood analysis shows that, over the last 13 billion years, gas in the cosmic web experienced four main heating and cooling epochs.

Debora Sijacki, Institute of Astronomy, University of Cambridge, UK: The evolution of massive black holes through cosmic times
01/06/2021
In this talk I will review current theoretical efforts in understanding supermassive black hole formation, accretion and feedback throughout cosmic time. Specifically, I will discuss possible links between large scale cosmological environments and supermassive black hole assembly and outline several possible interaction channels between active black holes and their host galaxies. In the second part of the talk I will focus on novel computational methods that allow us to follow black hole physics on much smaller scales in full galaxy formation simulations to unravel how black hole mass and spin evolve during the binary hardening stages or during launching of powerful jets.

Roberto Maiolino, Cavendish Laboratory, University of Cambridge, UK: Quenching star formation in galaxies
18/05/2021
In the local universe stars only make up about 7% of all baryons, indicating that star formation has been extremely inefficient across the cosmic epochs. Within this context, even more impressive is the fact that in a significant fraction of galaxies star formation has been totally “quenched”, resulting into the population of passive and quiescent local galaxies. Understanding what are the mechanisms responsible for suppressing or even quenching star formation in galaxies has been one of the main challenges of astrophysics in recent years and it is one of the research areas in which most of the efforts have been directed, both in terms of cosmological simulations and in terms of observing campaigns. I will give an overview of the potential causes and physical processes that might be responsible for regulating or even leading to the complete suppression of star formation in galaxies. I will illustrate that there are a variety of possible culprits. Among these I will show that supernova explosions can play a role, but the energy injected in the insterstellar and intergalactic medium by accreting supermassive black holes can have a truly dramatic effect on their host galaxies. The environment in which galaxies live (e.g. galaxy groups or clusters) can also play an important role, by suppressing star formation especially in satellite galaxies. I will discuss observational evidence for these various effects by using results from extensive multi-wavelength datasets. I will conclude by emphasizing open, outstanding problems and the possibility of tackling them with the next generation of observing facilities.

Joseph Silk, Institut d’Astrophysique de Paris, The Johns Hopkins University, University of Oxford: The future of cosmology
16/04/2021
One of the greatest challenges in cosmology is understanding the origin of the structure of the universe. The cosmic microwave background and large-scale surveys of galaxies have provided unique windows for probing cosmology and its inflationary origin. But where do we go next? Future experiments are planned with the next generation of observatories that will increase the current precision of cosmological measurements by an order of magnitude. However we need to do far better if there is to be a guaranteed science return that will definitively probe our cosmic origins. I shall argue that the ultimate goal for our future strategy must be astronomy from lunar-based telescopes.

Benedetta Ciardi, Max Planck Institute for Astrophysics: Exploring cosmic reionization with 21cm telescopes
09/03/2021
Cosmic reionization is the last major phase transition undergone by our Universe. Although most studies agree on the general characteristics of H reionization (for example that is driven by stars and it is mostly if not fully complete by z ≈ 6), its details are still largely unknown, among which the contribution from and role played by more energetic sources. In this talk, I will discuss the ingredients needed for a correct modeling of cosmic reionization and present results from recent radiative transfer simulations accounting for a variety of source types (such as stars, quasars, X-ray binaries). I will then discuss the observability of reionization in terms of various diagnostics associated to the 21cm signal from neutral hydrogen and present the latest results from the LOFAR radio telescope. Join Zoom Meeting https://uniroma1.zoom.us/j/89931306878?pwd=WG5RYlYyZzRSMzJsOFpSRHczWEFCZz09