LXVII Congresso Annuale della Società Astronomica Italiana

4 mag 2026, 09:00 → 8 mag 2026, 18:30 Europe/Rome

L'Aquila

ATTENZIONE!!! SCADENZA PER L'INVIO DI ABSTRACT PROROGATA AL 21 APRILE!

 

LXVII Congresso Annuale della Società Astronomica Italiana
I dieci anni delle onde gravitazionali
e le sfide astrofisiche del prossimo decennio
L’AQUILA – Sala Ipogea del Consiglio Regionale d’Abruzzo
4 – 8 maggio 2026

 

Il decennio appena trascorso è stato caratterizzato da progressi decisivi (si pensi all’entrata in fase operativa di JWST ed EUCLID, alla prima luce di Rubin LSST e alle varie release della missione Gaia, solo per fare qualche esempio) e da scoperte rivoluzionarie, prima fra tutte quella delle onde gravitazionali, che ha aperto una nuova finestra sullo studio del Cosmo e della sua storia.

D’altro canto, partendo da queste conquiste e con la prossima entrata in funzione di nuove grandi facilities (come SKAO, CTAO, ELT, ET…), nonché di tecniche di osservazione e analisi la cui potenza cresce a velocità vertiginosa, il nuovo decennio appare altrettanto florido, se non ancor più ricco di conquiste scientifiche e di grandi, nuove sfide.

L’intero panorama dell’astrofisica è destinato ad esserne coinvolto: dalla formazione ed evoluzione delle strutture nelle varie epoche cosmiche alla fisica degli oggetti compatti e dei processi di accrescimento e feedback nelle galassie; dallo studio degli esopianeti e delle loro condizioni di abitabilità alla ricerca di biosignatures intorno ad altre stelle o già in altri corpi del sistema solare; dall'archeologia galattica allo studio delle prime stelle, dalla natura della materia oscura e dell’energia oscura alla storia dell’espansione dell’Universo e a test sempre più raffinati della Relatività Generale.
Nella cornice della città de L’Aquila, Capitale Italiana della Cultura 2026, il LXVII Congresso Annuale della Società Astronomica Italiana vuole essere l’occasione per avviare una discussione sulle prospettive della ricerca astrofisica, e di quella italiana in particolare, da qui alla metà degli anni Trenta.
Con l’avvento dell’astronomia multi-messaggera, come stanno evolvendo le nostre capacità di osservare e capire l’Universo sempre più in dettaglio e sempre più in profondità ? Con le nuove facilities che stanno iniziando o inizieranno ad operare e a fare scoperte nei prossimi anni, come cambieranno le grandi domande della moderna astrofisica? Quali nuove sfide ci attendono?

Il congresso prevede contributi scientifici sotto forma di presentazioni orali e poster; la lingua ufficiale del congresso è l’italiano, anche se le slide delle presentazioni possono essere in inglese.
Durante il Congresso si terrà anche l’Assemblea annuale dei Soci, fondamentale punto di scambio di idee e di confronto tra le diverse realtà che contraddistinguono l'associazione, e avrà luogo l’assegnazione dei  premi SAIT. Al congresso sarà dedicato un volume delle Video Memorie della SAIt a cura della Redazione.  

Il LXVII Congresso Annuale della Società Astronomica Italiana (SAIt) è organizzato in collaborazione con l'Osservatorio Astronomico d’Abruzzo dell’Istituto Nazionale di Astrofisica (INAF), con il supporto del Gran Sasso Science Institute (GSSI) e dei Laboratori Nazionali del Gran Sasso dell’Istituto Nazionale di Fisica Nucleare (INFN).
L’evento ha ottenuto il patrocinio della Presidenza del Consiglio Regionale d’Abruzzo e del Comune dell’Aquila - Capitale Italiana della Cultura 2026.
Si ringraziano:
COSPAR 2026 - comitato organizzatore per Firenze 2026
Club Alpino Italiano - Sezione dell'Aquila, La Lampara Eventi

 

 

--------- [English version] --------------

 

LXVII Annual Congress of the Italian Astronomical Society
Ten Years of Gravitational Waves and the 

astrophysical challenges of the next decade

L'AQUILA – Sala Ipogea del Consiglio Regionale d'Abruzzo
May  4 – 8, 2026

The past decade has been marked by decisive progress (consider, for example, the operational start of JWST and EUCLID, the first light of Rubin LSST and the various releases of the Gaia mission) and by revolutionary discoveries, foremost among them the detection of gravitational waves, which has opened a new window onto the study of the Cosmos and its history.
On the other hand, building on these achievements and with the upcoming commissioning of new major facilities (such as SKAO, CTAO, ELT, ET…), as well as observational and analytical techniques whose power is growing at a staggering rate, the new decade appears equally flourishing, if not even richer in scientific achievements and major new challenges.
The entire field of astrophysics is set to be involved: from the formation and evolution of structures across different cosmic epochs to the physics of compact objects and the processes of accretion and feedback in galaxies; from the study of exoplanets and their habitability conditions to the search for biosignatures around other stars or even on other bodies within the Solar System; from galactic archaeology to the study of the first stars, from the nature of dark matter and dark energy to the history of the expansion of the Universe and increasingly refined tests of General Relativity.
In the context of the city of L'Aquila, Italian Capital of Culture 2026, the LXVII Annual Congress of the Italian Astronomical Society aims to be an opportunity to initiate a discussion on the prospects of astrophysical research, and Italian research in particular, between now and the mid-2030s.

With the advent of multi-messenger astronomy, how are our capabilities to observe and understand the Universe evolving in ever greater detail and depth? With the new facilities that are beginning, or will soon begin, operations and making discoveries in the coming years, how will the major questions of modern astrophysics change? What new challenges await us?

The conference will include scientific contributions in the form of oral presentations and posters; the official language of the conference is Italian, although presentation slides may be in English.

The Annual Members' Meeting will also be held during the Congress, a key opportunity for exchanging ideas and discussion among the association's stakeholders. The SAIT awards ceremony will also take place.

A volume of SAIt Video Memories, edited by the Editorial Staff, will be dedicated to the Congress.

The LXVII Annual Congress of the Italian Astronomical Society (SAIt) is organized in collaboration with the Astronomical Observatory of Abruzzo of the National Institute for Astrophysics (INAF), with the support of the Gran Sasso Science Institute (GSSI) and the Gran Sasso National Laboratories of the National Institute for Nuclear Physics (INFN).
The event has received the patronage of the Presidency of the Regional Council of Abruzzo and of the Municipality of L’Aquila – Italian Capital of Culture 2026.
Special thanks to:
COSPAR 2026 - Organizing Committee for Florence 2026
CAI Italian Alpine Club – L’Aquila Section, La Lampara Eventi

 

 

Sessioni

• Onde Gravitazionali e astronomia multimessaggera
• La Galassia e il Gruppo Locale
• Cosmologia
• Evoluzione delle galassie
• Oggetti variabili e transienti in astrofisica
• Sistema Solare e astrobiologia
• Eliofisica e Space Weather
• Pianeti extrasolari e astrobiologia
• Oggetti compatti
• Grandi facilities osservative da terra e dallo spazio
• Valorizzazione della Conoscenza
• Calcolo, Archivi e Intelligenza Artificiale

 

Sessions

• Gravitational Waves and Multi-Messenger Astronomy
• The Galaxy and the Local Group
• Cosmology
• Galaxy Evolution
• Variable and Transient Objects in Astrophysics
• The Solar System and Astrobiology
• Heliophysics and Space Weather
• Exoplanets and Astrobiology
• Compact Objects
• Major Ground- and Space-Based Observational Facilities
• Knowledge valorisation
• Computing, Archives, and Artificial Intelligence

 

lun 4 maggio

14:00 → 14:30 Saluti istituzionali

14:30 → 16:00 La Galassia e il Gruppo Locale

14:30 Decoding the Galaxy’s history with high-resolution stellar spectroscopy

High-resolution stellar spectroscopy, combined with precise astrometry from Gaia, has revolutionized our understanding of both the formation and evolution of the Milky Way and stellar nucleosynthesis. In this talk, I will present recent progress in mapping the Galaxy’s large-scale chemical structure over time, including radial metallicity gradients and spiral patterns, and explore how stellar chemical compositions relate to planetary system architectures. I will also discuss detailed abundance measurements of heavy elements and their isotopes, providing key insights into nucleosynthetic processes from the lightest to the heaviest elements. Finally, I will outline future perspectives, with particular emphasis on the proposed ESO high-resolution multi-object spectrograph HRMOS, and its potential to advance studies ranging from exoplanet populations and precise stellar age determinations to the detailed chemical history of the Galaxy and its satellites.

Relatore: Magrini, Laura (Istituto Nazionale di Astrofisica (INAF))

14:55 Unveiling the ultra-faint dwarf galaxies: exploring the low-luminosity end of the galaxy population

The faint end of the galaxy luminosity function represents one of the most powerful yet observationally challenging windows onto galaxy formation and evolution. Ultra-faint dwarf (UFD) galaxies — the least luminous, most dark matter-dominated, and chemically most primitive stellar systems known — are fossil relics of the early universe, offering unique constraints on cosmological models, feedback mechanisms, and the nature of dark matter. In the past two decades, wide-field deep photometric surveys with new-generation telescopes have revolutionized the census of Milky Way satellites, pushing the exploration well below the classical dwarf galaxy regime. In this talk, I will review our current understanding of UFD galaxies, discussing the techniques employed for their detection and characterization. I will also highlight how the study of their stellar populations can shed light on the physical processes governing the formation and evolution of these extreme systems. Finally, I will outline the exciting prospects offered by upcoming facilities and surveys, which promise to dramatically advance our knowledge of the low-luminosity end of the galaxy population in the near future.

Relatore: Gatto, Massimiliano (Istituto Nazionale di Astrofisica (INAF))

15:15 The unexpected stellar populations of the Milky Way's satellite Fornax dSph

Building upon the seminal work of Searle & Zinn (1978) and within the framework of the Λ-CDM paradigm, the Milky Way (MW) halo is understood to have formed through the progressive and ongoing accretion of smaller sub-galactic fragments. This hierarchical assembly can be empirically tested via Near-Field Cosmology, specifically by comparing theoretical structural predictions with star-by-star observations of extant MW satellites.

Among these satellites, the Fornax dwarf Spheroidal (dSph) is particularly significant; its substantial mass allows it to host its own system of globular clusters and complex, multi-modal stellar populations. While Fornax is known for its diverse metallicity and age distributions, it presents a striking anomaly for a dSph: an intermediate-age population (~1.5 Gyr) and a potential young component (~200 Myr). Recent KiDS (Kilo-Degree Survey) catalogues derived from VST imaging further suggest an even younger stellar population of approximately 100 Myr. To validate this, we have initiated an observational campaign to identify these extremely young stars and characterize their associated variable star populations, providing a definitive temporal record of Fornax's recent star-formation history.

Relatore: Dall'Ora, Massimo (Istituto Nazionale di Astrofisica (INAF))

15:30 Challenging the i-process paradigm in CEMP-rs stars: new insights from TYC 6044-714-1

Carbon-Enhanced Metal-Poor (CEMP) stars are fundamental tracers for Galactic archaeology, providing a unique window into the nucleosynthetic processes that shaped the early Milky Way. A key challenge in this field is the interpretation of CEMP-rs stars, whose chemical patterns are often attributed to the intermediate ($i$-) process. However, distinguishing between an $i$-process origin and a combined $s+r$ enrichment requires high-precision abundance determinations and advanced spectral modelling. Here we present a comprehensive re-analysis of the benchmark CEMP-rs star TYC 6044-714-1, using new high-resolution, high-S/N UVES spectra. These observational results were compared with the latest AGB nucleosynthesis predictions to investigate the physical consistency of the proposed enrichment scenarios. Our results indicate that TYC 6044-714-1 is an in-situ halo star, likely pre-enriched by a standard $r$-process event. We find that a pure $s+r$ model provides the best overall reproduction of the heavy-element distribution and Ba isotopic ratios. While models incorporating the $i$-process can improve the fit for specific elements, they require physically extreme conditions and yield Ba isotopic fractions that are inconsistent with the 4934 Å resonance line. We conclude that the $s+r$ scenario remains the most robust explanation for this star, highlighting the critical role of high-precision spectroscopy in refining our understanding of early Galactic chemical evolution.

Relatore: Vescovi, Diego (Istituto Nazionale di Astrofisica (INAF))

15:45 Probing the Milky Way's Assembly History using RR Lyrae Stars

The dual role of RR Lyrae (RRL) stars as tracers of ancient merging events and high-precision distance indicators is fundamental to investigating the evolutionary history of the Milky Way (MW). Their distribution in the Galactic Halo and Globular Clusters provides a unique opportunity to trace interactions with satellite galaxies. This study investigates the origin of the Oosterhoff dichotomy, specifically focusing on whether it is an intrinsic feature of the Galaxy or was "imported" through merging events with dwarf galaxies, such as Gaia-Enceladus and Sagittarius. To test this hypothesis, we apply chemo-dynamic classifications to a large sample of RRLs, analyzing their distribution in the space of integrals of motion to distinguish between in situ and accreted populations. Accurate orbital analysis is ensured by the derivation of a new Period-Wesenheit-Metallicity (PWZ) relation, using a robust Bayesian MCMC (Markov Chain Monte Carlo) framework combined with Gaia astrometric data. Preliminary results show that the PWZ coefficients are consistent with current literature. This framework sets the stage for a detailed characterization of the pulsational properties (including Fourier parameters) for each identified dynamical component, aiming to reconstruct the early assembly of our Galaxy with high precision.

Relatore: Luongo, Emanuela (Istituto Nazionale di Astrofisica (INAF))

16:00 → 16:30 Coffee Break

16:30 → 18:20 Oggetti variabili e transienti in astrofisica

16:30 L’Universo transiente nell’era multi-messaggera

L’astrofisica del dominio temporale e multi-messaggera rappresenta oggi una delle frontiere prioritarie della ricerca, come evidenziato dalle principali roadmap internazionali. I fenomeni transienti, che si manifestano su un’ampia gamma di energie e scale temporali, coinvolgono molteplici processi fisici la cui comprensione richiede un approccio integrato che combina le informazioni trasportate dai fotoni lungo l’intero spettro elettromagnetico con quelle provenienti da onde gravitazionali e neutrini, all’interno di un quadro osservativo coordinato e sinergico.
Nel prossimo decennio assisteremo a una convergenza senza precedenti di nuove infrastrutture osservative, che aprirà opportunità uniche. Queste consentiranno non solo di affrontare alcune delle principali questioni ancora aperte sull’Universo transiente, ma anche di studiare in modo sistematico le popolazioni di transienti, esplorando regioni finora inesplorate dello spazio dei parametri. Ciò permetterà di scoprire nuove classi di fenomeni e di caratterizzare in modo più completo le controparti elettromagnetiche associate a segnali ad alte energie e multi-messaggeri.
Questo intervento si propone di offrire una sintesi aggiornata dello stato dell’arte e di delineare le prospettive future dell’astrofisica del dominio temporale.

Relatore: Dr. Botticella, Maria Teresa (Istituto Nazionale di Astrofisica (INAF))

16:55 Pulsating variable stars as tracers of galaxy evolution

Resolved stellar populations in Local Group galaxies provide fundamental information to understand galaxy formation and evolution, which can be constrained using their photometric, spectroscopic, and dynamical properties. Pulsating variable stars such cepheids and RR Lyrae star add extra constraints, as they trace the age and metallicity of the parent population.

In this talk I will show how combining different approaches such as the star formation history derivation from the deep colour-magnitude diagrams together with the properties of variable stars can provide quantitative insights on the host galaxy evolution, chemical evolution, and accretion history. In the era of large photometric and spectroscopic surveys, pulsating stars will thus be crucial to investigate all the Galactic structures, from the obscured bulge and disk to the most remote parts of the halo, as well as nearby dwarf systems to the outskirts of the Local Group.

Relatore: Dr. Monelli, Matteo (INAF - Osservatorio d'Abruzzo)

17:15 LSST e Gaia: una sinergia per la scala delle distanze basata su stelle variabili

Nei prossimi dieci anni la Legacy Survey of Space and Time e le prossime Data Release di Gaia (DR4 e DR5) offriranno una sinergia irripetibile per lo studio delle variabili pulsanti nella Via Lattea e nel Gruppo Locale. La profondità e la copertura multi-banda (in sei filtri) di LSST, insieme alla precisione astrometrica di Gaia, rappresentano gli elementi chiave di questo filone di ricerca. Gaia fornisce una calibrazione geometrica delle relazioni periodo–luminosità (PL, utilizzate come indicatori di distanza) tramite parallassi ad alta precisione, mentre LSST estende tali relazioni a distanze extragalattiche grazie ad una combinazione di profondità, copertura temporale e angolare senza precedenti, consentendo anche la cross-calibrazione con altri indicatori di distanza, quali il TRGB e il JAGB. Tra le variabili pulsanti, le Cefeidi Classiche e le RR Lyrae ricoprono un ruolo fondamentale come candele standard, rispettivamente per le popolazioni giovani e antiche.

Nell’era della tensione di Hubble (la crescente discrepanza che si osserva da quasi 10 anni, oggi a livello di $\sim$5–6$\sigma$, tra le misure locali di $H_0$ e quelle ottenute dalla radiazione cosmica di fondo), migliorare la calibrazione delle PL, sia in termini di dipendenza dalla metallicità sia di zero-point geometrico, è cruciale per valutare possibili bias sistematici o eventuali tensioni con il modello cosmologico standard. In questo contributo presentiamo una rassegna delle principali opportunità e criticità della sinergia Gaia–LSST, delineando le prospettive per una determinazione più robusta e precisa della scala delle distanze extragalattiche.

Relatore: Braga, Vittorio Francesco (Istituto Nazionale di Astrofisica (INAF))

17:35 Ultra-long MeV transient from a relativistic jet: a tidal disruption event candidate

Gamma-ray bursts (GRBs) are extragalactic MeV transients lasting from fractions of a second to several minutes, typically associated with mergers of compact objects or the collapse of massive stars. On 2 July 2025, the Gamma-ray Burst Monitor onboard the Fermi Gamma-ray Space Telescope detected three emission episodes with overlapping sky localizations, occurring 1-2 hours apart, collectively designated GRB 250702B. Taken together, the emission lasted more than 3 hours, making it the longest MeV transient ever observed. Follow-up observations with the Neil Gehrels Swift Observatory and the Nuclear Spectroscopic Telescope Array revealed a rapidly decaying soft X-ray counterpart over the subsequent ten days.

Our time-resolved spectral analysis of the prompt emission phase shows that the gamma-ray spectra are harder than those of long GRBs. The spectra are well described by a single power law extending from 10 keV to 40 MeV, with evidence for a spectral break above 50 MeV.

The extreme duration, broadband spectral properties, and X-ray evolution suggest GRB 250702B likely originates from a relativistic jet launched during the tidal disruption of a star by a compact object. From $\gamma\gamma$ opacity constraints, we derive a lower limit on the jet bulk Lorentz factor of $\Gamma$ > 10. The inferred luminosity and energetics are consistent with those of previously reported relativistic tidal disruption events. The MeV spectra disfavour inverse Compton scenarios and are naturally explained by synchrotron emission from sub-TeV electrons.

Relatore: Ierardi, Annarita (Gran Sasso Science Institute)

17:50 High resolution spectroscopy of Classical Cepheids in the NIR

Classical Cepheids (DCEPs) are the primary indicators for the extra-galactic distance scale. Establishing precise zero points for their Period-Luminosity and Period-Wesenheit (PLZ/PWZ) relations is crucial for resolving the 5σ H0 tension, yet current calibrations lack statistics for low-metallicity ([Fe/H] < -0.4 dex) and long-period (P > 10 days) pulsators. While metal-poor DCEPs exist at large Galactocentric radii, they are often obscured in optical bands by dust.
GIANO-B high-resolution spectra for DCEPs at large radii or with long periods ensures a comprehensive coverage of the parameter space. By shifting the observational focus to the Near-Infrared (NIR), it is possible to mitigate interstellar extinction, reduce intrinsic scatter, and include the distant metal-poor objects necessary for a homogeneous metallicity sampling. These data, along with forthcoming Gaia DR4 parallaxes, allow to put firm constraints on the PLZ/PWZ for MW DCEPs and, in turn, provide a more stringent test of the extra-galactic distance scale. Within this framework, I will present the first preliminary results from the analysis of these infrared spectra.

Relatore: Salmeri, Laura (Istituto Nazionale di Astrofisica (INAF))

18:05 The identity card of Cepheids and RR Lyrae through the modeling of light and radial velocity curves

Classical Cepheids and RR Lyrae stars represent fundamental laboratories for testing stellar evolution and pulsation theories. Cepheids are young, intermediate-mass stars and primary standard candles for the extragalactic distance scale, while RR Lyrae stars are low-mass objects tracing old stellar populations. Both classes are characterized by radial pulsations, producing periodic variations in luminosity, effective temperature, and radial velocity.
In this contribution, we present results obtained by comparing predictions from non-linear convective pulsation models with multi-epoch photometric and radial velocity data, primarily from the Gaia mission, showing that the models accurately reproduce the observed morphology of light and radial velocity curves. Our model-fitting approach enables a precise determination of their intrinsic structural parameters, including mass, effective temperature, and luminosity.
For both Classical Cepheids and RR Lyrae stars, the derived parameters provide individual distance estimates, offering an independent check of Gaia parallaxes, and constrain their internal structure and convective efficiency. For Classical Cepheids, the results also place constraints on the mass–luminosity relation.

Relatore: Molinaro, Roberto (Istituto Nazionale di Astrofisica (INAF))

18:20 → 18:40 Discussione

19:00 → 21:00 Welcome Cocktail

Al termine della prima giornata di lavori, tutti i partecipanti al Congresso sono invitati al welcome cocktail di ice breaking, previsto nei pressi del porticato del Palazzo dell'Emiciclo che ospita l'evento scientifico.

mar 5 maggio

09:00 → 10:45 Evoluzione delle galassie

09:00 L’evoluzione delle galassie svelata dal JWST: tra scoperte e nuovi interrogativi

L’entrata in funzione del James Webb Space Telescope (JWST) ha aperto una nuova finestra sull’universo primordiale, permettendoci di osservare galassie fino all’epoca della reionizzazione, quando le prime strutture cosmiche erano ancora in fase di formazione. Grazie alla sua straordinaria sensibilità nell’infrarosso, il JWST ha portato a numerose scoperte, rivelando una popolazione di galassie più luminose, massicce e ricche di metalli di quanto previsto dai modelli teorici. Questi risultati hanno anche sollevato nuovi interrogativi fondamentali sulla rapidità dei processi di formazione galattici, sull’assemblaggio delle strutture e dei primi buchi neri e sulla comparsa delle prime regioni ioizzate nel mezzo intergalattico. In questo scenario, le nuove osservazioni spingono a rivedere e affinare i modelli esistenti, aprendo prospettive inedite sulla comprensione dell’evoluzione cosmica.

Relatore: Calabro, Antonello (Istituto Nazionale di Astrofisica (INAF))

09:25 Chemical enrichment of high-z galaxies: latest results from JWST and future perspectives

The James Webb Space Telescope has fulfilled its long-awaited promises, opening an entirely new window to constrain star-formation, metal and dust enrichment, and feedback processes in some of the earliest galaxies ever formed. A key driver of this progress is the JWST capability to deliver auroral-line detections out to high redshift, enabling increasingly robust, physically motivated electron-temperature (Te)-based metallicity measurements beyond the local Universe.
Yet the emerging picture remains complex. Several studies point to rapid chemical enrichment and an increased scatter in metallicity scaling relations--potentially reflecting more stochastic star-formation and feedback--while compelling candidates for (nearly) pristine, extremely metal-poor systems have also been reported.
In parallel, growing evidence for non-solar abundance patterns (e.g. elevated N/O at low O/H) suggests variations in star-formation efficiency and/or short-timescale enrichment channels, possibly linked to very massive stars.
I will present some recent developments in the study of detailed chemical abundances in high-z galaxies that leverage deep, both MSA and IFS NIRSpec spectroscopy in combination with novel, multi-cloud photoionisation modeling. I will also discuss how the evolution in the metallicity-dependence of star-formation and the prevalence of non-solar abundance patterns across the cosmic history can influence our understanding of stellar evolution and the predicted rates of phenomena linked to metal-poor progenitors.
Finally, I will discuss future prospects in light of forthcoming large spectroscopic surveys (e.g. MOONS, 4MOST) and next-generation ground-based (ELT) and space-based (e.g. PRIMA) facilities.

Relatore: Curti, Mirko (Istituto Nazionale di Astrofisica (INAF))

09:45 Stellar kinematics of ultra-diffuse galaxies as probes of dark matter physics

Ultra-diffuse galaxies offer a powerful laboratory to probe the nature of dark matter in low-density regimes. In this talk, I present a kinematic analysis of two galaxies from the "Looking into the faintEst WIth MUSE" project. By using integral-field spectroscopy of stellar tracers, we derived two-dimensional velocity fields and modeled these systems as rotating systems embedded in spherical dark matter halo. Our analysis is performed within a Bayesian framework, allowing us to connect the observed stellar kinematics to the underlying mass distribution. We considered the standard cold dark matter paradigm alongside alternative scenarios, including fuzzy, self-interacting, and non-minimally coupled dark matter. Our results demonstrate the power of extremely low-surface brightness galaxies as stringent and independent tests of dark matter physics on galactic scales.

Relatore: Buttitta, Chiara (Istituto Nazionale di Astrofisica (INAF))

10:00 Effects of the velocity anisotropy and typical size on the orbital decay of galactic satellites

The original formulation of dynamical friction (DF), developed for a particle moving in a infinite and media, delivers accurate predictions of sinking time scales for a test mass in a broad class of models, while failing in several other cases. $N-$body simulations hint at a breakdown of the original formalism for massive satellites sinking in the host galaxy, or compact objects in cores. Semi-analytical treatment of DF have softened this discrepancy, even though a comparison with simulations is still missing, due to the interplay between DF and the tidal effects on extended systems. We performed $N-$body simulations of a satellite orbiting in spherical galaxy model, for different values of the initial orbital eccentricity, satellite mass, scale radius and velocity anisotropy of the host. We adopt a scheme where the self-consistent interaction among the particles representing the galaxy can be substituted with the effect of a static smooth potential and a semi-analytical DF to disentangle the contributions to the friction due the trailing wake from that of the tidal tails. The satellite can be modeled either with $N_{\rm sat}$ particles or represented by a particle with an effective extension parametrized by the form of the force exchanged with the other simulation particles. We find that, at fixed galaxy model and satellite mass, the more extended is the satellite the weaker is the effect of DF in particular for orbital eccentricities $\gtrsim0.6$. Independently on the satellite mass or size, DF is less efficient in systems dominated by low angular momentum orbits.

Relatore: Di Cintio, Pierfrancesco (Consiglio Nazionale delle Ricerche (CNR) & INAF OAA)

10:15 Svelare le galassie ultra-diffuse: verso una nuova comprensione dell’Universo alle basse brillanze superficiali.

Il modello ΛCDM descrive con successo la formazione degli aloni di materia oscura che nel tempo si aggregano in strutture più massicce attraverso fenomeni di fusione. In questo scenario bottom-up, la materia barionica segue il collasso gravitazionale degli aloni di DM: per questo ci si potrebbe aspettare una corrispondenza diretta tra le funzioni di massa degli aloni di DM (HMF) e la funzione di massa stellare (GSMF). Tuttavia, nello scenario del downsizing dedotto dalle osservazioni, le galassie più massicce si sono formate prevalentemente a redshift elevati in apparente contrasto con il modello bottom-up, dove le strutture a massa minore si formano per prime. Per affrontare queste discrepanze, è cruciale concentrarsi sullo studio delle galassie a bassa luminosità superficiale (LSBg), in particolare sulle UDG, che dominano l’estremità debole della funzione di luminosità delle galassie: infatti le differenze tra osservazioni e previsioni teoriche potrebbero derivare da un censimento incompleto di queste galassie. Con l’obiettivo di automatizzare la rilevazione e l’analisi delle LSB è stato progettato un nuovo strumento in linguaggio Python, ATTILA, che mira a fornire il campione statisticamente più ampio di galassie LSB e UDG in diversi ambienti e a determinarne i parametri strutturali. In questa fase iniziale del progetto si è scelto di testare ATTILA sull’ammasso HydraI, ampliando i risultati della survey VEGAS e identificando 22 nuove UDG e 77 LSB.

Relatore: Fonzo, Francesca (Istituto Nazionale di Astrofisica (INAF))

10:30 A New Perspective on Galactic Evolution: Studying the Outskirts of the Abell S1063 Galaxy Cluster

Galaxy clusters are key environments for studying galaxy evolution. While environmental effects on galaxy properties are evident, the mechanisms behind quenching and structural transformations remain debated.
In this talk, I will present the study of the cluster Abell S1063 at z = 0.346 using optical and near-infrared data from VST-GAME and VISTA surveys, respectively. The unique grasp of VST and VISTA, together with the availability of about 1500 cluster members, allow to performe an
unprecedented investigation of physical processes responsible for galaxy evolution across different
environments, from the dense cluster core to the periphery, out to about 5Rvir (~10Mpc). We compared cluster member properties across regions with different local densities, ranging from the cluster center to filaments.
We also analyse JWST data from the GLIMPSE program (P.I. Atek H.), in which Abell S1063 was observed in nine bands. These data represent a goldmine to estimate the stellar evolution parameters (mass, age, and star formation) of the galaxies in the cluster.

Relatore: Sig.na Pecoraro, Luisa (Università di Salerno)

10:45 → 11:15 Coffee Break

11:15 → 13:00 Valorizzazione della Conoscenza

11:15 Didattica dell'Astronomia (panel discussion)

Chair: Caterina Boccato

Angela Misiano
Società Astronomica Italiana

Settimio Mobilio
Università degli Studi di Roma Tre

Fabrizio Floris
Ministero dell'Istruzione e del Merito - Ufficio Scolastico Regionale per la Sardegna

Relatori: Boccato, Caterina (Istituto Nazionale di Astrofisica (INAF)), Floris, Fabrizio (Ministero dell'Istruzione e del Merito - Ufficio Scolastico Regionale per la Sardegna), Misiano, Angela (Società Astronomica Italiana), Settimio, Mobilio (Università degli Studi di Roma Tre)

11:55 Il bicentenario della morte di Giuseppe Piazzi (1746-1826): un'opportunità?

Nel corrente anno ricade il bicentenario della morte dell'astronomo Giuseppe Piazzi (1746-1826), fondatore dell'Osservatorio di Palermo, scopritore del primo asteroide Cerere (ora classificato come pianeta nano) e direttore generale degli osservatori di Palermo e Capodimonte, di cui ultimò i lavori di costruzione, per conto del governo borbonico.
All'approssimarsi del bicentenario, si è ritenuto opportuno istituire un Comitato Nazionale per redigere un programma di manifestazioni di carattere sia scientifico, sia storico, sia divulgativo, nella convinzione che il bicentenario potesse costituire un'opportunità per la comunità astronomica per parlare di scienza a più livelli. In realtà, il programma iniziale - molto ambizioso - è stato ridimensionato dal finanziamento concesso dal Ministero.
In questo intervento saranno quindi brevemente illustrate le iniziative in programma a Napoli e Palermo, realizzate con il supporto del Comitato, della Direzione Scientifica di INAF, e di risorse locali. Attraverso questa presentazione si intende sensibilizzare la comunità astronomica, nelle sue varie componenti, a valorizzare l'eredità scientifica del passato e a mantenerne la memoria, con uno sguardo che non sia semplicemente retrospettivo, ma diventi l'occasione per riflettere sul presente e sul futuro dell'astronomia, contribuendo allo sviluppo della cultura astronomica nella comunità scientifica e nella società.

Relatore: Chinnici, Ileana (Istituto Nazionale di Astrofisica (INAF))

12:10 L'astronomia nella formazione dei docenti: ruolo e prospettive

La formazione dei docenti rappresenta un canale strategico di connessione tra ricerca e scuola, con un impatto moltiplicativo sulla diffusione della conoscenza scientifica. In questo contesto, l’astronomia e l’astrofisica offrono un terreno privilegiato per sviluppare percorsi didattici interdisciplinari, capaci di integrare fisica, matematica, tecnologia e cultura scientifica in una prospettiva STEAM.

Negli anni l’Istituto Nazionale di Astrofisica (INAF) e la Società Astronomica Italiana (SAIt) hanno promosso numerose iniziative di formazione e aggiornamento rivolte ai docenti, che comprendono corsi strutturati, scuole estive, laboratori didattici e attività in collaborazione con realtà accademiche e istituzionali a livello nazionale e internazionale. Si osserva una crescente convergenza verso modelli formativi orientati all’integrazione tra contenuti disciplinari e pratiche didattiche, con particolare attenzione alla trasferibilità in ambito scolastico.

Il contributo presenta una panoramica delle principali attività sviluppate in ambito INAF e SAIt, evidenziandone complementarità, punti di forza e sinergie. Verrà discusso il ruolo della formazione docenti come strumento per sostenere la presenza dell’astronomia nei percorsi scolastici, pur in assenza di un suo inquadramento esplicito nei curricula.

Saranno inoltre illustrate le recenti azioni intraprese da INAF per il coordinamento dell’offerta formativa, finalizzate a favorire una maggiore integrazione tra iniziative, promuovere la condivisione di buone pratiche e rafforzare lo sviluppo di strategie comuni nel lungo periodo.

Relatore: Dr. Di Carlo, Elisa (INAF - OAAb)

12:25 Conservare, studiare, condividere: sinergie SISFA e INAF per una storia viva dell’astronomia

Da alcuni anni la SISFA – Società Italiana degli Storici della Fisica e dell’Astronomia e l’INAF hanno avviato un dialogo istituzionale, nel quadro delle loro condivise finalità scientifiche, formative e di diffusione culturale.
Il protocollo d’intesa, rinnovato nel 2025, permette di operare in sinergia negli ambiti della ricerca storica, della valorizzazione del patrimonio scientifico e della disseminazione della memoria storica dell’astronomia. Particolarmente significativa è la collaborazione che la SISFA ha instaurato con l’area MAB dell’INAF, recentemente riorganizzata all’interno della USC E – Valorizzazione della conoscenza della Direzione Scientifica.
L’intervento intende illustrare come la cooperazione tra SISFA e INAF rappresenti un’opportunità concreta per sviluppare iniziative comuni di ricerca, formazione e disseminazione della conoscenza, rafforzando il legame tra storia dell’astronomia, patrimonio culturale e comunità scientifica.

Relatore: Zanini, Valeria (Istituto Nazionale di Astrofisica (INAF))

12:40 PLAY INAF, la piattaforma di didattica innovativa dell’Istituto Nazionale di Astrofisica

La presentazione illustra le potenzialità educative di PLAY INAF, la piattaforma di didattica innovativa dell’Istituto Nazionale di Astrofisica rivolta a docenti e studenti dei diversi ordini scolastici. Nata nel 2020 in risposta all’emergenza pandemica da COVID-19, si è affermata come punto di riferimento per la progettazione e la diffusione di risorse digitali per la didattica dell’astronomia, in Italia e all’estero (le attività sono disponibili anche in inglese, francese e tedesco). Ha vinto il CLASSified Award 2023 come uno dei migliori prodotti del 2022 nel settore dell’innovazione tecnologica e digitale.
La piattaforma raccoglie risorse gratuite di coding, robotica educativa, tinkering, attività hands-on, making, realtà aumentata, realtà virtuale e giochi, con l’obiettivo di promuovere lo sviluppo del pensiero computazionale e delle competenze digitali. Le risorse sono sviluppate in modo continuativo da un team di circa trenta ricercatori e tecnologi. Le attività di punta, più strutturate, vengono presentate in occasione di eventi di divulgazione scientifica come il Festival della Scienza di Genova, la Notte dei Ricercatori e la Europe Code Week. Il gruppo di lavoro realizza inoltre webinar (fruibili anche on-demand), corsi di formazione per insegnanti su tutto il territorio nazionale e un concorso per le scuole, “C’è posta per E.T.”, che – insieme al concorso “Giovani astronomi al Telescopio Nazionale Galileo” – è disponibile su Edu INAF.
La piattaforma rappresenta uno strumento efficace per la valorizzazione della conoscenza e per il rafforzamento del dialogo tra scuola e comunità scientifica, contribuendo alla formazione di cittadini consapevoli e competenti.

Relatore: Dr. Sandri, Maura (Istituto Nazionale di Astrofisica (INAF))

13:00 → 14:15 Pranzo

14:15 → 14:30 3-minutes poster presentations

14:15 Perdere il cielo buio

L’inquinamento luminoso è la dispersione di luce artificiale
nell’ambiente oltre le aree che necessitano di essere illuminate. Negli
ultimi decenni il fenomeno è cresciuto rapidamente a scala globale, con
un aumento stimato della luminosità del cielo notturno di circa il 10%
all’anno. L'intervento discute possibili strategie di mitigazione, tra
cui l’uso di apparecchi schermati, la regolazione intelligente del
flusso luminoso e la riduzione delle componenti spettrali blu delle
sorgenti LED. Viene infine presentato il caso della Stazione Astronomica
di Loiano, sede del telescopio Cassini da 1.52 m, dove l’aumento della
brillanza del cielo negli ultimi anni rappresenta un limite crescente
per le osservazioni astronomiche e per le attività tecnologiche di
monitoraggio di satelliti e detriti spaziali.

Relatore: Galleti, Silvia (Istituto Nazionale di Astrofisica (INAF))

14:18 Early X-ray emission of short gamma-ray bursts: insights into physics and multi-messenger prospects

Accurate modeling of the early X-ray emission in short gamma-ray bursts (GRBs) is essential for probing the GRB engine, understanding jet physics, and improving electromagnetic follow-up of gravitational wave signals from binary neutron star mergers in the context of multi-messenger astronomy.

Thanks to the operation of the Swift satellite over the last 20 years, we now have access to an extensive archive of GRB X-ray observations. The early X-ray light curves often exhibit a bright and steep decay phase, whose physical origin remains poorly understood. In short GRBs, this phase is particularly prominent, as their fainter forward-shock emission makes the steep decay detectable for up to 15 minutes.

In this talk, I will present our systematic analysis of the early X-ray emission of short GRBs, including both the temporal and spectral evolution. We introduce a new modeling technique that accounts for both the curvature and the intrinsic evolution of the GRB spectrum in Swift/XRT and Swift/BAT data. This approach enables us to track the evolution of spectral peak energy and the bolometric flux during the steep decay phase. Our study reveals a tight correlation between the peak energy and the isotropic equivalent luminosity. This relation enables us to infer the intrinsic properties of short GRBs and assess the detectability of their early X-ray emission with wide-field X-ray cameras. In particular, our work can help to interpret the nature of some fast X-ray transients detected by Einstein Probe and suggest observational multi-messenger strategies.

Relatore: Ierardi, Annarita (Gran Sasso Science Institute)

14:21 L’Osservatorio di Campo Imperatore: Innovazione Strumentale e Attività Scientifiche

La Stazione Osservativa di Campo Imperatore (INAF-OAAb), situata sul Gran Sasso a circa 2150 m s.l.m., è l’infrastruttura professionale più elevata in Italia per l’astronomia nel Visibile e nel vicino infrarosso (NIR), con condizioni atmosferiche caratterizzate da alta trasparenza, bassa umidità e bassa luminosità di fondo. Da alcuni anni, il sito è oggetto di un complesso programma di ammodernamento finalizzato alla gestione in modalità remota e robotica.
La Stazione ospita due strumenti: il Visible-Infrared Telescope (VIT) da 1.1 m e il Wide-field Optical Telescope (WOT), uno Schmidt da 0.9 m. Al fuoco del VIT sono in fase di installazione il nuovo imager NIR "CI²RCE" che, tramite un correttore Tip-Tilt, garantirà un significativo enhancement della PSF (fino a 1.4 arcsec FWHM, con un seeing di 2.5 arcsec) su un campo di vista maggiore di 50 arcmin², e uno spettrografo ottico a bassa risoluzione. Il WOT è invece ottimizzato per l’imaging a grande campo nel Visibile, offrendo capacità di monitoraggio ad alta efficienza.
Le attività scientifiche spaziano dalla ricerca e follow-up di controparti di Onde Gravitazionali e transienti quali Supernovae, TDE e GRB - grazie soprattutto alle caratteristiche del WOT - fino allo studio, usando entrambi i telescopi in sinergia, di stelle variabili, corpi del Sistema Solare (in particolare corpi minori) e detriti spaziali. Lo spettrografo installato al VIT supporterà la classificazione spettroscopica delle sorgenti. Grazie all'accesso simultaneo alle bande del Visibile e del NIR, la Stazione offre una facility unica nel panorama nazionale per tali progetti.

Relatore: De Luise, Fiore (INAF-Osservatorio Astronomico d'Abruzzo)

14:24 Multi-messenger astrophysics and cosmology with the THESEUS space mission

The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) is a mission concept developed by a large European collaboration under study by ESA since 2018 and currently one of the three candidate M7 mission for a launch in the late '30s. THESEUS aims at fully exploiting Gamma-Ray Bursts for investigating the Cosmic Dawn and as key phenomena for multi-messenger astrophysics. By providing an unprecedented combination of X-/gamma-ray monitors, on-board IR telescope and spacecraft autonomous fast slewing capabilities, THESEUS will be a wonderful machine for the detection, multi-wavelength characterization and redshift measurement of any kind of GRBs and many classes of X-ray transients, including high-redshift GRBs for cosmology (primordial low-mass/luminosity galaxies, first stars, cosmic re-ionization) and electromagnetic counterparts to sources of gravitational waves. Moreover, THESEUS will enable extreme and fundamental physics through unprecedented breakthrough measurements of GRB prompt and afterglow
emission, as well as the detection and multi-eavelength characterization of many classes of high-energy transients. In all these respects, THESEUS will thus provide an ideal synergy with the very large astronomical facilitiesof the future working in the e.m. (e.g., ELT, CTA, SKA, Athena) and multi-messenger (e.g., Einstein Telescope, Cosmic Explorer, km3NET).

Relatore: Amati, Lorenzo (Istituto Nazionale di Astrofisica (INAF))

14:27 Cosmology with Gamma-Ray Bursts

The huge luminosity, the redshift distribution extending up to z > 9 and the association with the explosive death of very massive stars make long Gamma-Ray Bursts (GRB) extremely powerful probes for the exploration of the Cosmic Dawn. Indeed, the NIR afterglow emission of GRBs allows the direct detection of exploding stars up to very high redshift and, at teh same timne, acts as a uniquely powerful cosmic beacon which enable the identification, accurate localization, redshift measurement and absorption spectroscopy of primordial galaxies independently on their mass and luminosity. Thus, very high-z GRBs are a unique tool for directly detecting first population of stars, unveiling and characterizing (metallicity, gast to dust ration, neutral hydrogen fraction) the bulk population of low mass / luminosity primordial galaxies and exploring the evolution and sources of cosmic re-ionization. At the same time, the correlation between radiated energy and spectral photon peak energy ("Amati relation" enables the use of GRBs for measuring cosmological parameters, investigating the nature and evolution of ”dark energy” and testing non-standard cosmological models. Finally, short GRBs, produced by the merging of NS-NS and NS-BH systems, sources of Gravitational Wave signals, are a key phenomenon for enabling multi-messenger cosmology. Space mission concepts like THESEUS, under study by ESA, aim at fully exploiting these breakthorugh potentialities of the GRB phenomenon for cosmology, also in synergy with the large e.m. (e.g., JWST. ELT, TMT, SKA, CTA, NewATHENA) and multi-messenger (e.g., ET, CE, Km3NET) facilities of the future.

Relatore: Amati, Lorenzo (Istituto Nazionale di Astrofisica (INAF))

14:27 Nuove fonti su Mentore Maggini per l’Archivio Storico dell’Osservatorio d’Abruzzo

Nel corso del 2025 alcuni preziosi documenti sono stati donati dalla famiglia Maggini all'INAF-Osservatorio d'Abruzzo, già Specola di Collurania che Mentore Maggini diresse dal 1926 (esattamente cento anni fa) fino alla sua prematura scomparsa, l'8 maggio 1941.

Fra questi, il manoscritto originale del libro "Il pianeta Marte" ed una copia a stampa con copertina disegnata dall'autore, unitamente a due diversi provini, originali, della stessa; alcuni volumi, conservati da Maggini, donati a Cerulli da Schiaparelli con dedica autografa di quest'ultimo; e corrispondenza, finora inedita, con Cerulli e con Alfani.

La donazione va ad arricchire il Fondo Maggini dell'Archivio Storico dell'Osservatorio d'Abruzzo, già oggetto nell'ultimo triennio di un importante lavoro di riordino e catalogazione.

Relatore: Dr. Dolci, Mauro (Istituto Nazionale di Astrofisica (INAF))

14:30 → 15:00 Valorizzazione della Conoscenza

14:30 Progetto AstroSardegna_21-24apr26

Vedasi allegato.
Grazie

Relatore: Prof. Floris, Fabrizio (Agatino Rifatto e-mail: agatino.rifatto@inaf.it)

14:45 Dalla Ricerca alla Scuola: il Modello Nazionale INAF per i percorsi PCTO

L'INAF è da tempo fortemente impegnato in attività rivolte alle scuole per i Percorsi per le Competenze Trasversali e l'Orientamento (PCTO). Si intende illustrare i risultati conseguiti in questo settore per l'anno scolastico 2024-2025. Attraverso l'analisi dei dati raccolti nelle 12 sedi coinvolte, viene presentato un bilancio complessivo che vede la partecipazione di oltre 1.100 studenti e l'erogazione di migliaia di ore di formazione. Si approfondirà la nuova struttura di governance del Gruppo Nazionale PCTO, evidenziando il passaggio strategico verso un'autonomia finanziaria e una programmazione infrastrutturale centralizzata (2025-2026). Vengono inoltre analizzati i profili scientifici dei progetti, l'impatto del bilancio di genere e l'efficacia del modello di coordinamento tra sede nazionale e referenti locali testimoniando il valore della "Terza Missione" dell'Ente nel panorama educativo italiano.

Relatore: D'Alessio, Francesco (Istituto Nazionale di Astrofisica (INAF))

15:00 → 16:10 Cosmologia

15:00 Precision measurements of the cosmic microwave background: extreme physics and cosmology

The Cosmic Microwave Background (CMB) is our most profound window into the primordial universe. While temperature maps established the $\Lambda$CDM model, the next frontier lies in polarization and spectral distortions. These signals provide a high-precision laboratory for "extreme physics" at energy scales far beyond Earth-bound accelerators. Searching for primordial B-modes offers a direct test of the inflationary paradigm and a measurement of the energy scale of the early universe via gravitational waves. Minute deviations from the blackbody spectrum act as a fossil record of energy injection, probing dark matter decay and the damping of primordial fluctuations. Together, these observables allow us to investigate the universe's earliest moments at the highest conceivable energy. In this talk, I will review the potential of these signatures and provide an overview of current experimental efforts and upcoming missions.

Relatore: Prof. de Bernardis, Paolo (Dipartimento di Fisica, Sapienza Università di Roma)

15:25 Testing the Cosmological Model in the Next Decade: Gravitational Waves, Large-Scale Structure, and the CMB

The coming decade will be decisive for Cosmology because, for the first time, several largely independent probes of the Universe will become simultaneously mature. On the large-scale-structure side, DESI is already delivering high-precision BAO constraints, while Euclid, Rubin/LSST and Roman will map the expansion history and the growth of structure with unprecedented reach. On the CMB side, ACT DR6 has provided a new post-Planck benchmark, Simons Observatory is entering operations, and LiteBIRD is expected to sharpen tests of primordial physics and inflation. At the same time, gravitational-wave astronomy is evolving from proof of concept to an actual cosmological tool, through standard sirens, propagation tests, and stochastic backgrounds, with PTAs now in a characterisation era and LISA offering the prospect of direct access to cosmological gravitational-wave backgrounds. In this talk I will discuss how gravitational waves, large-scale structure, and the CMB can be combined to test the expansion history, the growth of cosmic structure, dark energy, neutrino physics, primordial fluctuations, and possible departures from General Relativity. The key question is whether these probes will converge on a coherent extension of the standard cosmological framework, or instead reveal statistically significant cracks in ΛCDM.

Relatore: Dr. Carbone, Carmelita (INAF IASF-MI)

15:45 Generation of gravitational waves in warm inflation via Bogoliubov coefficients

We investigate the gravitational-wave background predicted by a two-scalar-field cosmological model that aims to unify primordial inflation with the dark sector, namely late-time dark energy and dark matter, in a single and self-consistent theoretical framework. In this context, we derive the gravitational-wave energy spectrum over wavelengths ranging from today’s Hubble horizon to those at the end of inflation.
We employ the continuous Bogoliubov coefficient formalism, originally introduced to describe particle creation in an expanding Universe,in analogy to the well-established mechanism of gravitational particle production and, in particular, generalized to gravitons. Using this method, which enables an accurate description of graviton creation across all cosmological epochs, we find that inflation provides the dominant gravitational wave contribution, while subdominant features arise at the inflation-radiation, radiation-matter, and matter-dark energy transitions, i.e., epochs naturally encoded inside our scalar field picture.
Specifically, we explore how the dissipation regime of warm inflation, plays a crucial role in the production of gravitational waves.
The resulting energy density spectrum is thus compared with the sensitivity curves of the planned next generation ground- and space-based gravitational-wave observatories. The comparison identifies frequency bands where the predicted signal could be probed, providing those windows associated with potentially detectable signals, bounded by our analyses.

Relatore: Mengoni, Tommaso (Istituto Nazionale di Astrofisica (INAF), University of Camerino)

15:58 The EXPANSION CENTER of the UNIVERSE as a NEW SCIENTIFIC PARADIGM for a REVOLUTION IN COSMOLOGY

According to Thomas Kuhn (1962), the recognition of the Expansion Center of the Universe has to be considered as a new scientific PARADIGM for a revolution in Cosmology (Lorenzi 2009, p.5). Indeed, the discovery by Bahcall & Soneira (1982) of a Huge Void of Rich Clusters didn’t recognize its Center 𝑽𝑪(𝜶 ≈ 𝟗𝒉, 𝜹 ≈ +𝟑𝟎°) as the Cosmic Expansion Cente, but the Expansion Center Model (ECM: Lorenzi 1999ab) has proven it (compare also Dirac's LNH results: 1937-1938)! Now we present a series of 23 DIPOLES of the Expansion Center Hubble ratio of the Universe (Lorenzi 1991, 1999b, 2004ab, 2012b) at the mean redshifts 〈z〉≪0.1,〈z〉≅0.5,〈z〉=1.00.
Figures 1-2-3 show the first five 𝒓̇/𝒓 Hubble Ratio DIPOLES of ECU1 (Lorenzi–Ferrari–Masani 1991), while in Fig.5 the two DIPOLES of Fig. 4 have a minimum of the 𝒔 standard deviation of the least square fitting at 𝑹 ≈ 𝟐𝟔𝟎 𝑴𝒑𝒄. The listed Figures 1-2-3-4-5-6-7 of ECM paper II (Lorenzi 1999b) represent seven DIPOLES of the 𝒓̇/𝒓 Hubble ratio versus − 𝐜𝐨𝐬 𝜸 of the nearby Universe, with the result H_0≅(70±3) H.u.. In 4x2 Figures at 〈𝒛〉 ≈ 𝟎.𝟓 of SCP SNe Ia (Lorenzi 2004ab) and in the 3 Figures 1-2-3 (Lorenzi 2012b: ECM paper XV or ECU20), at 〈𝒛〉 = 𝟏.𝟎𝟎 of SCP SNe Ia, we have a series of DIPOLES, or NORMAL COSMIC DIPOLES CD accoding to the eq. cz/D=H_0 〖- a〗^ cos⁡γ. The final result at 〈z〉=1.00 is an angular coefficient 〈a^ 〉=(5.47±0.25) H.u. as an average of 33 values of a^*.

Relatore: Lorenzi, Luciano (SAIt & SIF)

16:10 → 16:40 Coffee Break

16:40 → 17:55 Sistema Solare e astrobiologia

16:40 Icy worlds habitability and the objectives of MAJIS on board the ESA JUICE mission to the Jupiter system

JUICE - JUpiter ICy moons Explorer - is the first large mission in the ESA Cosmic Vision 2015-2025 program. The mission was launched on April 14th 2023, with arrival at Jupiter in July 2031. It will make detailed observations of Jupiter and three of its largest moons: Ganymede, Callisto, and Europa. MAJIS (Moons And Jupiter Imaging Spectrometer), the visible-IR imaging spectrometer on board JUICE, will investigate the spectral characteristics of Jupiter, the Galilean satellites, rings, small satellites, and exospheres with two channels: the VIS-NIR channel in the spectral range from 0.5 to 2.35 μm, and the IR channel from 2.28 to 5.56 μm. The IFOV is 150 µrad, with 400 pixels across the 60 mrad FOV and 508 spectels. The spectral sampling is about 3.6 nm/band and 6.5 nm/band for VIS-NIR and IR channels respectively. The Jupiter icy satellites, Ganymede, Europa, and Callisto, have as many similarities as differences. Their surface is at the interface between the interior and space, and as such records endogenous processes tied to the geological activity and exogenous processes due to their surrounding environments. These processes, responsible for the morphology and composition of their surface, are not yet well understood. Studying their composition would thus provide new insight into the geochemical state of the subsurface as well as the space environment. Finally, JUICE made an Earth-Moon flyby, and a long distance observation of the 3I/Atlas comet, resulting in an extremely important opportunity to verify the calibration and performance in flight with real extended targets.

Relatore: Dr. Piccioni, Giuseppe (Istituto Nazionale di Astrofisica (INAF))

17:05 Io's Volcanic Interior Revealed: Interconnected Magma Systems and Lava Lake Thermal Budgets

Recent observations by the JIRAM instrument onboard NASA's Juno mission have fundamentally revised our understanding of Io's interior structure and global thermal budget. We present two major results from JIRAM infrared imaging of Io's hot spots.
On 27 December 2024, JIRAM captured a multi-hotspot eruption in Io's southern hemisphere covering approximately 65,000 km². The event produced 140–260 TW, more than three orders of magnitude above prior estimates and likely exceeding the brightest eruption ever recorded on Io. Three adjacent hot spots brightened simultaneously, and temperature analysis demonstrates a synchronous onset, implying a single eruptive event propagating laterally beneath the surface across hundreds of kilometers. This is the first time such behavior has been observed on Io, pointing to a system of massive interconnected subsurface magma reservoirs whose topology may resemble a large-scale sponge, with reservoirs connected through a largely solid outer shell.
A systematic analysis of thirty lava lakes identified by JIRAM reveals that the dominant thermal contribution comes from their low-temperature central crusts rather than from the hotter peripheral rings, implying that previous power estimates were underestimated by up to a factor of ten. Io's paterae undergo stochastic resurfacing on timescales of roughly a decade, with crust temperature serving as a proxy for the evolutionary state of each lake. Together, these results indicate that current assessments of Io's global heat flux are significant underestimates, and that only full-surface high-resolution infrared observation can yield a realistic value for the moon's total thermal output, with direct implications for tidal dissipation models.

Relatore: Mura, Alessandro (Istituto Nazionale di Astrofisica (INAF))

17:25 CONVERGE: un ponte tra la scienza di Venere e degli esopianeti terrestri

Venere occupa una posizione centrale tra la scienza del Sistema solare e la caratterizzazione degli esopianeti terrestri. Da un lato, resta un pianeta chiave per comprendere vulcanismo, evoluzione geologica, interazioni atmosfera-superficie ed evoluzione climatica dei pianeti rocciosi; dall'altro, costituisce il riferimento più vicino per interpretare i potenziali analoghi venusiani già individuati tra gli esopianeti terrestri e quelli che future osservazioni potranno caratterizzare. L'arrivo di missioni dedicate a Venere e delle missioni per lo studio degli esopianeti terrestri rende sempre più necessario un quadro comparativo condiviso.

In questo contesto presentiamo CONVERGE (COordinated Network for Venus and Exoplanet Research and GEoscience), una rete internazionale che mette in dialogo la comunità venusiana, le geoscienze planetarie e la ricerca sugli esopianeti. L'obiettivo è duplice: usare Venere per rafforzare l'interpretazione di atmosfere e superfici dei pianeti terrestri extrasolari, e usare le domande emergenti dalla scienza degli esopianeti per definire nuove priorità nello studio di Venere. CONVERGE promuove un approccio interdisciplinare basato su dati di missione, analoghi terrestri, esperimenti di laboratorio e prodotti scientifici condivisi, per costruire un linguaggio comune tra comunità finora solo in parte in dialogo.

In questa prospettiva, Venere non è soltanto un obiettivo dell'esplorazione planetaria, ma anche un banco di prova essenziale per vincolare la diversità evolutiva dei pianeti rocciosi e i limiti dell'abitabilità. CONVERGE si propone come una piattaforma di coordinamento scientifico interdisciplinare e orientata alla collaborazione, pensata per favorire uno scambio bidirezionale tra la comunità venusiana e quella esoplanetaria in vista delle sfide osservative del prossimo decennio.

Relatore: D'Incecco, Piero (Istituto Nazionale di Astrofisica (INAF))

17:40 Aspettando BepiColombo: grandi bacini da impatto dell'emisfero meridionale di Mercurio e implicazioni per le stime di contrazione globale del pianeta

La conoscenza del record dei crateri di Mercurio si è evoluta significativamente nell’ultimo decennio grazie alla missione NASA MESSENGER, che ha permesso l’implementazione di cataloghi globali aggiornati e l’identificazione di una grande quantità di strutture da impatto precedentemente sconosciute. Un recente riesame dei dati di MESSENGER ha portato all’identificazione di decine di grandi bacini da impatto (D > 150 km) precedentemente non segnalati. Questi grandi bacini non sono ancora stati studiati in dettaglio, nonostante la loro notevole importanza geologica e geofisica.
Qui presentiamo indagini geologiche, topografiche, strutturali, composizionali e geofisiche di un bacino con diametro superiore ai 1500 chilometri, le cui strutture più esterne si estendono ben oltre i 2000 km dal centro, suggerendo un diametro equivalente, se non maggiore, al bacino Caloris, noto come il più grande bacino di Mercurio.
I nostri risultati evidenziano un fondo anulare terrazzato del bacino, suggerendo che questo possa essersi formato come una struttura di tipo peak ring o multiring. Il fondo della struttura mostra un’anomalia gravitazionale e uno spessore crostale ridotto rispetto alle aree circostanti. Diverse evidenze suggeriscono che l’impatto abbia innescato attività vulcanica analoga a quella dei maria lunari.
I nostri risultati mostrano che la tettonica associata a questo bacino, potrebbe aver avuto un significato regionale e globale, finora trascurato. Infatti, queste strutture legate agli impatti sono state finora incluse nelle attuali stime della contrazione di Mercurio, probabilmente portando a delle sovrastime. Proponiamo questa regione come target ad alta priorita' per la missione ESA BepiColombo in arrivo in orbita a fine anno.

Relatore: Di Achille, Gaetano (Istituto Nazionale di Astrofisica (INAF))

17:55 → 18:15 Discussione

19:30 → 20:30 Concerto - Coro del CAI Club Alpino Italiano dell'Aquila

SAIT 2026 Concerto.pdf

mer 6 maggio

09:00 → 10:15 Pianeti extrasolari e astrobiologia

09:00 Caratterizzazione delle atmosfere degli esopianeti: metodi, risultati e prospettive future

A trent’anni dalla scoperta del primo pianeta attorno a una stella simile al Sole, l’esoplanetologia è passata da una fase pionieristica di scoperta a una scienza di caratterizzazione. Con oltre 6000 esopianeti attualmente confermati, è emersa un’inaspettata varietà di architetture planetarie, spesso prive di analoghi nel Sistema Solare. In questo contesto, lo studio delle atmosfere esoplanetarie rappresenta la chiave di volta per risolvere il complesso puzzle di questa diversità: nella sua composizione chimica sono infatti codificate informazioni cruciali sulla storia di formazione e di migrazione.
In questo contributo verranno presentate le principali tecniche osservative impiegate per sondare le atmosfere esoplanetarie, con particolare attenzione ai pianeti di breve periodo studiati tramite spettroscopia di trasmissione ed emissione. Discuterò i risultati più significativi ottenuti finora, principalmente su giganti gassosi, e illustrerò come il campo stia progredendo verso la caratterizzazione di pianeti sempre più piccoli.
Infine, saranno delineate le prospettive future del campo, dalle osservazioni attuali con il telescopio spaziale James Webb alle prossime missioni e survey, sia da terra sia dallo spazio, come Ariel, con l’obiettivo di identificare per la prima volta possibili biomarcatori atmosferici e avanzare nella ricerca di ambienti potenzialmente abitabili.

Relatore: Guilluy, Gloria (Istituto Nazionale di Astrofisica (INAF))

09:25 Spin-orbit alignment in planetary systems

Measuring spin-orbit obliquities via the Rossiter-McLaughlin effect is crucial for understanding how planets form and migrate. Different mechanisms are expected to leave different signatures in the obliquity; scattering encounters tend to randomise orbital alignments, whereas disc-planet interactions tend to preserve orbital coplanarity. In this talk, I will present hot topics in exoplanet research involving spin-orbit obliquities, such as the leading formation mechanism of hot-Jupiters, the role of migration in shaping the Neptune desert, ridge and savanna, and the role of obliquity excitation in the early stages of planet formation.

Relatore: Dr. Mantovan, Giacomo (Università degli studi di Padova (UniPd); Istituto Nazionale di Astrofisica (INAF))

09:45 KELT‑9b as a preview of the ELT era: probing 3D dynamics and thermochemical regimes with GIARPS

High-resolution spectroscopy has evolved over the past decade into a key technique for exoplanet atmospheric characterization, enabling detailed constraints on chemical composition, thermal structure, and atmospheric dynamics. Ultra-Hot Jupiters (UHJs), with their extreme irradiation and temperatures, offer unique laboratories for exploring atmospheric physics under conditions far beyond those found in the Solar System.
In this talk, I will present a new analysis of the hottest known UHJ, KELT‑9b (equilibrium temperature ~4000 K), observed in transmission with the GIARPS facility at the Telescopio Nazionale Galileo, combining simultaneous near‑infrared (GIANO‑B) and optical (HARPS‑N) spectroscopy. Through this case study, I will illustrate how high‑resolution observations are increasingly sensitive to both the underlying thermochemical assumptions, such as the choice between LTE and NLTE treatments, and the inherently three‑dimensional nature of UHJ atmospheres. Features such as strong day-night temperature contrasts, vertical thermal gradients, and high‑velocity winds can imprint detectable signatures on the spectra, influencing both the strength and interpretation of atmospheric signals.
These results highlight the broader need for atmospheric frameworks that jointly account for realistic chemistry, radiative processes, and multidimensional dynamics when interpreting high‑resolution datasets. Looking ahead, next‑generation instruments such as ANDES at the ELT will provide the sensitivity required to probe complex 3D atmospheric processes, chemical stratification, and dynamical regimes with unprecedented detail.

Relatore: di Paola, Alessia (Istituto Nazionale di Astrofisica (INAF) - OATo)

10:00 From Neptunes to Earths: Implications from Multi-Resolution Atmospheric Characterization of WASP-107b for Future ELT Observations of Terrestrial Exoplanet

The atmospheric characterization of Neptune-mass exoplanets serves as a crucial stepping stone toward understanding smaller, potentially habitable worlds. This study presents a comprehensive multi-resolution analysis of WASP-107b, a warm super-Neptune with an extended atmosphere ideal for transmission spectroscopy, using the novel GUIBRUSH® framework that combines high-resolution ground-based observations (GIANO-B, IGRINS) with low-resolution space-based data (HST/WFC3, JWST/NIRCam, JWST/MIRI). Our analysis successfully detected seven molecular species (H₂O, CO₂, CO, CH₄, NH₃, SO₂, H₂S) through low-resolution spectroscopy while revealing significant challenges in high-resolution observations, particularly regarding telluric and stellar contamination that limited reliable detections to H₂O and CO. A critical finding is that when planetary and telluric signals overlap in velocity space, disentangling atmospheric absorption features becomes significantly more challenging, particularly for planets with low Kp values. This velocity overlap analysis serves as a critical planning step to optimize observational strategies and ensure the detectability of planetary atmospheric signatures.
While the upcoming Extremely Large Telescopes (ELTs) will improve high-resolution exoplanet spectroscopy by providing increased collecting power and better signal-to-noise ratios, this fundamental disentangling challenge will persist for Earth and super-Earth planets. Despite enhanced sensitivity from ELTs, the velocity overlap between planetary and telluric features represents a systematic limitation that will require sophisticated mitigation strategies for reliable atmospheric characterization of terrestrial exoplanets.

Relatore: Amadori, Francesco (Istituto Nazionale di Astrofisica (INAF))

10:15 → 10:20 3-minutes poster presentation

10:15 GUIBRUSHR - A comprehensive tool to characterize exoplanet atmospheres at different spectroscopic resolutions and with a multi-instrument approach

Exoplanetary atmospheres reveal key information about planet formation, evolution, and habitability. Spectroscopy at different orbital phases probes chemical composition, thermal structure, and physical processes. Ground-based high-resolution (HR; GIANO-B, HARPS-N, IGRINS, CRIRES+) and space-based low-resolution (LR; JWST, HST) observations probe complementary depths. However, characterization requires separate tools: telluric and stellar contamination removal, radiative transfer, and Bayesian inference. We present GUIBRUSHR (Graphic User Interface for Bayesian Retrieval Using Spectroscopy at High Resolution), a comprehensive Python 3.10+ package that unifies these capabilities into a single framework with an intuitive tkinter-based GUI. The tool integrates a local SQLite3 database for organized operation tracking and covers the complete atmospheric characterization workflow through dedicated modular tabs: unified parameter configuration, telluric removal via PCA with customizable settings, cross-correlation analysis for HR datasets, forward model generation, Bayesian retrieval analysis using parallelized differential evolution Markov chain Monte Carlo (DE-MCMC), and synthetic HR dataset generation. GUIBRUSHR enables simultaneous analysis of multi-resolution and multi-instrument datasets, combining HR ground-based observations with LR space-based data to leverage their complementary strengths. The retrieval framework and the forward model module use petitRADTRANS v3.0 as the radiative transfer engine. The user-friendly interface removes the burden of managing multiple configuration files, offering one-click workflows for complex multi-step analyses with clear diagnostic visualizations. Results, retrieval settings, and system parameters are automatically organized in a structured directory tree and database, ensuring easy data access and reproducibility. GUIBRUSHR is built to handle today's large datasets and scale to future instruments (ANDES@ELT, ARIEL), while remaining flexible for new techniques and methodologies.

Relatore: Amadori, Francesco (Istituto Nazionale di Astrofisica (INAF))

10:20 → 11:05 Oggetti compatti

10:20 Magnetic Fields Matter: The role of Strong Fields in Compact Objects

Magnetic fields play a fundamental role in shaping the observational properties and evolution of compact objects across multiple scales. I will review some advances highlighting the impact of strong magnetic fields in neutron stars and white dwarfs, with particular emphasis on new observational results.

Magnetars represent the most extreme case, where ultra-strong magnetic fields (≳10¹⁴ G) dominate the emission physics. Recent X-ray polarimetric observations with IXPE have provided the first direct measurements of high degrees of polarization, offering crucial constraints on emission geometries, radiative transfer in strongly magnetized plasmas, and quantum electrodynamics effects.

Then, the emerging class of Long Period Radio Transients (LPRTs), initially interpreted as the long-period tail of the pulsar or magnetar population. However, accumulating evidence now suggests that at least a fraction of these sources are highly magnetized white dwarfs, challenging our understanding of coherent radio emission mechanisms and expanding the landscape of magnetically powered transients.

Next, I will address ultraluminous X-ray sources (ULXs), where strong magnetic fields in accreting neutron stars might be responsible for enabling super-Eddington luminosities. These systems provide key laboratories to study extreme accretion regimes regulated by magnetic fields.

Finally, I will briefly explore compact double white dwarf ultra compact binaries, such as HM Cnc, where magnetic coupling may enforce spin–orbit synchronization, potentially powering the observed emission, similar to the Io-Jupiter interaction.

Together, these examples illustrate how magnetic fields are a unifying ingredient in compact object astrophysics, driving diverse and often extreme observational regimes.

Relatore: Israel, GianLuca (Istituto Nazionale di Astrofisica (INAF))

10:45 Pulsars in the SKA era: using the best celestial clocks to study fundamental physics and astrophysics

The clock-like precision of pulsar signals allows us to use these rapidly-rotating, radio-emitting compact objects as superb laboratories in space: we can employ them collectively as probes of the magnetised interstellar medium of our Galaxy, or as beacons in a space-time distorted by long gravitational waves such as those emitted by supermassive black-hole binaries. When we find them orbiting around compact companion stars - potentially also around the central black hole of our own Milky Way - we can exploit them to precisely test relativistic gravity in extreme environments. When found in Globular Clusters - breeding grounds of large number of exotic pulsar binaries - they can be used to probe the clusters themselves. The most massive or fastest spinning pulsars, finally, can also be used to put limits on the nature of nuclear matter, constraining its equation of state.

The imminent advent of the SKA telescopes, with their large instantaneous sensitivity, wide frequency coverage and flexible observation modes, will immensely benefit (pulsar) science and will allow us to make great progress in all these science cases, and many more, in particular bringing us in the era of multi-messenger gravitational wave astronomy in the nano-hertz regime.

Relatore: Burgay, Marta (Istituto Nazionale di Astrofisica (INAF))

11:05 → 11:30 Coffee Break

11:30 → 13:05 Oggetti compatti

11:30 Accretion and jet formation in black hole X-ray binaries

The inflow of matter onto astronomical objects is connected to the generation of outflows throughout the Universe on a variety of scales, from proto-planetary disks, to merging neutron star systems and gamma ray bursts, to stellar mass and supermassive black holes.

The matter inflow/outflow processes scale predictably with mass, and proceeds according to the same basic principles around all collapsed objects, slower around supermassive black holes and much faster near stellar mass compact objects.
Low-mass X-ray binaries hosting either stellar mass black holes or neutron stars are the most common type of transient in the Galaxy, and constitute ideal laboratories where to study the accretion/jet connection at work in real time.
I will focus on black hole X-ray binaries, and I will give an overview on accretion states and how they are associated with jets. I will review some of the most important science that has been done recently, especially with the MeerKAT telescope, precursor of the SKA.

Relatore: Motta, Sara Elisa (Istituto Nazionale di Astrofisica (INAF))

11:50 HIghlights from observations of radio pulsars in globular clusters with MeerKAT

Observations with the MeerKAT radio telescope, located in South Africa, has lead to significant advances in several fields of radio astronomy, including the field of radio pulsars. In this talk will be reported about some recent discoveries and follow up results obtained through observations of millisecond pulsars in globular clusters.

Relatore: Corongiu, Alessandro (Istituto Nazionale di Astrofisica (INAF) - Osservatorio Astronomico di Cagliari)

12:05 Ultraluminous X-ray sources in the time domain

Ultraluminous X-ray sources (ULXs) are off-nuclear point sources radiating above the Eddington limit for a typical stellar remnant black hole.
Some ULXs might be sub-Eddington intermediate-mass black holes, but the bulk of this class is now widely believed to be powered by super-Eddington accretion onto compact objects.
In a handful of cases, this was proven by the detection of pulsations, which unequivocably identify the accretor as a neutron star. In a few other cases, the luminosity is so high that the leading interpretation remains sub-Eddington X-ray binaries powered by IMBH.
In this talk, I will review the information these remarkable sources have given us on extreme accretion over the years, and present some recent results exploiting time domain information to investigate them.

Relatore: Dr. Bachetti, Matteo (Istituto Nazionale di Astrofisica (INAF))

12:20 Tracing r-process nucleosynthesis in neutron star mergers with long-lived remnants: results from M1 neutrino transport simulations

Binary neutron star (BNS) mergers eject neutron-rich matter, providing ideal conditions for the nucleosynthesis of heavy elements via the r-process. The radioactive decay of these elements powers a quasi-thermal electromagnetic transient known as kilonova (KN). Despite significant progress since the detection of GW170817, many open questions about KNe remain, such as the interpretation of the spectral features observed in AT2017gfo. On the one hand, accurate predictions of r-process yields are crucial for modeling and interpreting KN signals. On the other hand, precise modeling of microphysics in BNS merger simulations is essential to determine the properties of the merger ejecta, which provide the starting point for nucleosynthesis calculations. In my talk, I will present the results of the nucleosynthesis from BNS merger ejecta, computed for the first time using tracer particles from numerical relativity simulations performed with the M1 neutrino transport scheme. These simulations predict long-lived remnants and account for three distinct ejecta channels: dynamical ejecta, neutrino-driven wind, and spiral wave wind.

Relatore: Loffredo, Eleonora (Istituto Nazionale di Astrofisica (INAF))

12:35 Constraints on Hadronic Emission from Microquasars Detected by LHAASO

Recently, the Large High-Altitude Air Shower Observatory (LHAASO) collaboration reported ultra-high-energy gamma-rays from six microquasar systems.
For five of these sources, the emission exceeds $100$ TeV, making microquasars promising Galactic PeVatrons.
In this work, we investigate whether gamma-rays around $100$ TeV can originate from hadronic interactions of accelerated cosmic rays with the ambient medium and estimate the contribution of these sources to the CR proton knee.
Two transport scenarios are considered: one in which particle transport around the source is dominated by advection with the velocity of the jet, and another in which it is dominated by diffusion, with the diffusion coefficient reduced with respect to the Galactic value. In both scenarios, the diffusion coefficient matches the Galactic value at large distances from the source.
We find that in both advection and diffusion scenarios, hadrons alone cannot fully explain the observed emission in most sources, allowing us to place upper limits on the hadronic contribution to the observed gamma-ray flux.
Finally, we estimate the contribution of these sources to the Galactic cosmic-ray spectrum; this quantity strongly depends on source age and injection history.

Relatore: Vecchiotti, Vittoria (Istituto Nazionale di Astrofisica (INAF))

12:50 Quasi-periodic oscillations as probes of new physics: spin-curvature coupling in neutron star binaries

Quasi-periodic oscillations (QPOs) observed in the X-ray emission of accreting compact objects are among the most promising astrophysical messengers of strong-field gravity. Yet, despite decades of observations, their physical origin remains debated, and the most established framework to interpret them, the relativistic precession model (RPM), shows persistent observational tensions, including a systematic preference for Schwarzschild-de Sitter (SdS) geometries over standard Schwarzschild or Reissner-Nordström solutions, with no clear justification for the role of a cosmological constant at such scales.

We argue that this tension points to missing physics in the RPM rather than to exotic spacetime geometries. Treating accreting matter as a collection of structureless test particles is a severe oversimplification: real accretion disks carry macroscopic angular momentum and internal structure. We incorporate this ingredient into a macroscopic precession model (MPM), based on the Mathisson-Papapetrou-Dixon equations on a Schwarzschild background, which introduces a spin-curvature coupling that modifies both the Keplerian and radial epicyclic frequencies. This correction naturally reproduces a SdS-like behavior, offering a physical explanation for what was attributed to an effective cosmological constant.

We apply the MPM to eight neutron star low-mass X-ray binaries via MCMC fits to twin kHz QPOs, finding statistically competitive or superior results with respect to the SdS framework, with consistent neutron star masses, disk boundary radii in physically plausible ranges, and a natural emergence of the observed 3:2 frequency clustering. These results suggest that QPOs carry information about the internal structure of orbiting matter, opening a new observational window on spin-curvature effects in strong-field regimes.

Relatore: BIANCHINI, GABRIELE (University of Camerino)

13:05 → 14:05 Pranzo

14:05 → 15:05 Grandi Facilities da terra e dallo spazio: stato attuale e prospettive tecnico/scientifiche future (panel discussion)

Pietro Bolli
INAF - Osservatorio Astrofisico di Arcetri

Giulia Rodighiero
INAF - Osservatorio Astronomico di Padova

Marcella Marconi
INAF - Osservatorio Astronomico di Capodimonte
Optical-Infrared Ground-based scientific perspectives for the next decades
A variety of Optical-Infrared 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 and the next instrumentation for VLT and ELT).
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 about 1 year ago.

Adriano Fontana
INAF - Osservatorio Astronomico di Roma

Massimo Cappi
INAF - Osservatorio di Astrofisica e Scienze dello Spazio

Paolo Soffitta
INAF - IAPS Roma
Alte energie dallo spazio
Nel mio contributo al panel illustrerò brevemente le facilities dallo spazio delle principali agenzie spaziali internazionali che consentono osservazioni astrofisiche nei raggi X e gamma, soffermandomi in particolare su quelle in cui il contributo italiano è più rilevante.

Chair: Simone Esposito / Mauro Dolci

15:05 → 15:50 Grandi facilities osservative da terra e dallo spazio

15:05 Il progetto NUVOLA: osservare nel vicino UltraVioletto da terra

Lo scopo del progetto NUVOLA (Near UltraViolet Observation with a Light Assembly), recentemente proposto alla call INAF “Astrofisica di Frontiera 2025” tra i progetti tecnologici esplorativi a basso TRL, è di realizzare un piccolo strumento ottimizzato per osservazioni da terra nel vicino Ultravioletto (NUV).
Effettueremo osservazioni nel vicino ultravioletto dalla Stazione Osservativa di Campo Imperatore, usando strumentazione ottimizzata per l’UV, con il progetto a lungo termine di installare nell’entroterra antartico uno strumento con diametro maggiore ed equipaggiato con uno spettrografo per compiere osservazioni al di sotto dei 300 nm durante il periodo di apertura del buco dell’ozono. L’apertura di una finestra osservativa in NUV in Antartide sarebbe importante non solo dal punto di vista astrofisico ma anche ambientale, dato che permetterebbe il monitoraggio dello strato d’ozono stratosferico.
Per quanto riguarda la progettazione dello strumento, l’attenzione maggiore è stata rivolta al coating degli specchi, che verrà rimosso e sostituito con un coating con efficienza superiore al 90% tra i 250 nm e i 550 nm: il lavoro verrà svolto da Officina Stellare. Il telescopio Ritchey-Chrétien F8 da 40 cm verrà usato con una camera commerciale con sensore CMOS caratterizzato da una buona QE in NUV, equipaggiata sia con dei filtri fotometrici UBVRI standard sia con dei filtri passabanda scelti per la loro elevata trasmissività nella regione tra 200 e 400 nm. Il telescopio, la camera e i filtri verranno testati al laboratorio SPRINT del CNR-IOM di Trieste prima dell’installazione dello strumento a Campo Imperatore e dell’inizio del programma osservativo.

Relatore: Gasparetto, Thomas (Istituto Nazionale di Astrofisica (INAF))

15:20 INAF contribution to ELT

In this contribution I will summarise INAF’s involvement in ELT, with
particular emphasis on MORFEO, the adaptive module for ELT.
I will review the progress of the project and the key role played by INAF, both from a technical and scientific perspective and from a financial perspective.

Over the past three years, INAF has secured substantial European funding under the National Recovery and Resilience Plan (PNRR) to enhance MORFEO’s capabilities. These funds have enabled the purchase of a second deformable mirror for MORFEO, helping to boost its scientific performance.

Relatore: Dr. Ciliegi, Paolo (Istituto Nazionale di Astrofisica (INAF))

15:35 The Transient High-Energy Sky and Early Universe Surveyor (THESEUS)

The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) is a mission concept developed by a large European collaboration under study by ESA since 2018 and currently one of the three candidate M7 mission for a launch in the late '30s. THESEUS aims at fully exploiting Gamma-Ray Bursts for investigating the Cosmic Dawn and as key phenomena for multi-messenger astrophysics. By providing an unprecedented combination of X-/gamma-ray monitors, on-board IR telescope and spacecraft autonomous fast slewing capabilities, THESEUS will be a wonderful machine for the detection, multi-wavelength characterization and redshift measurement of any kind of GRBs and many classes of X-ray transients, including high-redshift GRBs for cosmology (primordial low-mass/luminosity galaxies, first stars, cosmic re-ionization) and electromagnetic counterparts to sources of gravitational waves. Moreover, THESEUS will enable extreme and fundamental physics through unprecedented breakthrough measurements of GRB prompt and afterglow
emission, as well as the detection and multi-eavelength characterization of many classes of high-energy transients. In all these respects, THESEUS will thus provide an ideal synergy with the very large astronomical facilitiesof the future working in the e.m. (e.g., ELT, CTA, SKA, Athena) and multi-messenger (e.g., Einstein Telescope, Cosmic Explorer, km3NET).

Relatore: Amati, Lorenzo (Istituto Nazionale di Astrofisica (INAF))

15:50 → 16:20 Coffee Break

16:20 → 18:35 Onde Gravitazionali e astronomia multimessaggera

16:20 Multi-Messenger astronomy with gravitational waves and light: status and perspectives

The detection of GW170817 and its electromagnetic counterparts—a short gamma-ray burst (sGRB) and a kilonova—pioneered the era of multi-messenger astrophysics. This event confirmed binary neutron star (BNS) mergers as progenitors of sGRBs and primary sites for r-process nucleosynthesis. By combining gravitational and electromagnetic data, it was possible to constrain the speed of gravity, the neutron star equation of state, and the Hubble constant. Furthermore, the observation of a structured jet emerging from the merger remnant explained most of the observational properties of the associated sGRB prompt and afterglow emission. Despite the absence of subsequent joint detections, GW170817 remains a transformative baseline for the field. Current challenges include the elusive search for EM counterparts to black hole-neutron star (BH-NS) mergers and the detection of expected emission components (e.g. early-UV and late-time X-ray/radio). As we transition toward third-generation observatories like the Einstein Telescope, multi-messenger astronomy will evolve from individual event analysis to large-scale population demographics, provided a robust global network of observational infrastructure and a coordinated scientific community are maintained.

Relatore: Dr. Ghirlanda, Giancarlo (Istituto Nazionale di Astrofisica (INAF))

16:45 The dawn of gravitational-wave cosmology

The multi-messenger detection of the binary neutron star merger GW170817 on August 17, 2017, marks the birth of gravitational-wave (GW) cosmology. GW sources are self-calibrating standard sirens; from their detection, it is possible to directly estimate the luminosity distance of the source. If provided with a redshift estimate, as in the case of GW170817 through spectroscopy of its host galaxy, GWs can be used to probe cosmic expansion. After four observing runs and almost 10 years later, GW170817 remains the only GW source with an identified host galaxy, thanks to its electromagnetic counterpart. In contrast, a few hundred dark sirens, mostly binary black holes, have been observed. In analogy with standard candles, we have recently learned how to calibrate the redshift of dark sirens using galaxy surveys, as well as astrophysical knowledge of the possible formation channels of binary black holes.

In this talk, I will present what we have achieved in GW cosmology over the last ten years. I will review the impact of the only bright siren, GW170817, as well as the continuous efforts to calibrate the population of dark sirens currently observed by ground-based GW detectors.

Relatore: Mastrogiovanni, Simone (INFN Roma)

17:05 More Than a Sidekick: Secondary Black Holes in Hierarchical Mergers

Stellar clusters are efficient factories of dynamical interactions that shape the black hole (BH) mass distribution observed by gravitational-wave (GW) detectors. Their ability to pair and retain BHs enables the formation of remnants more massive than those produced through isolated binary evolution. This is a crucial difference among binary BH formation channels, as highlighted by events such as GW231123, possibly the first detected merger involving an intermediate-mass black hole (IMBH; mass above 100 solar masses).
We investigate the hierarchical assembly of binary BHs, focusing on the formation and evolution of secondary branches within BH merger trees. We introduce a new formalism implemented in the semi-analytical population-synthesis code BPOP, which tracks the growth of structured hierarchical chains. We define secondary hierarchical mergers as events in which the secondary component is itself a merger remnant, and show that this sub-population, while rare, preferentially populates the high-mass tail of the remnant distribution and contributes significantly to IMBH formation beyond the pair-instability mass gap. Their merger products also carry a distinct spin signature, providing an additional observable handle on their origin.
We show that the multiplicity, and generational depth of secondary merger chains leave characteristic imprints on the remnant mass and spin spectra. Tracking the full hierarchical structure of secondary mergers is essential for correctly interpreting the origin of the most massive BHs observed in GW events.

Relatore: Ugolini, Cristiano (GSSI)

17:20 Collisioni stellari come canale di formazione per stelle molto massicce

I buchi neri di massa intermedia (IMBH), con masse comprese tra $10^2$ e $10^5$ M$_{\odot}$, rappresentano un anello mancante cruciale tra i buchi neri stellari e quelli supermassicci. La loro esistenza è ancora oggetto di dibattito osservativo, ma numerosi scenari teorici suggeriscono che possano formarsi in ambienti stellari densi attraverso interazioni dinamiche. Ammassi giovani e compatti offrono condizioni ideali per fusioni ripetute tra stelle massicce e sistemi binari, favorendo una crescita runaway che può portare alla formazione di stelle molto massicce (VMS), potenziali progenitrici di IMBH. Comprendere i meccanismi e le condizioni che rendono efficienti questi processi è fondamentale per chiarire l’origine di tali oggetti.

In questo contributo. mostrerò quali ambienti siano più favorevoli alla formazione di VMS e IMBH con masse $\gtrsim 10^3$ M$_{\odot}$. I risultati sono ottenuti con STARfall, un nuovo codice semi-analitico pensato per modellare la co-evoluzione di sistemi binari e dell’ammasso ospite. Il codice combina prescrizioni di evoluzione stellare e dinamica, con particolare attenzione a incontri ripetuti e collisioni.

Il focus è posto su binarie massicce in ammassi densi, dove interazioni frequenti possono innescare fusioni runaway, episodi di ringiovanimento stellare e la formazione di oggetti estremamente massicci. In questo regime, le interazioni non si limitano a modificare le proprietà di singole stelle, ma possono rimodellare l’intera popolazione stellare dell’ammasso. Presenterò, infine, le implicazioni per ammassi giovani e compatti osservati ad alto redshift, come quelli identificati nel Cosmic Gems Arc, e per sistemi compatibili con i progenitori degli ammassi globulari osservati.

Relatore: Simonato, Filippo (Istituto Nazionale di Astrofisica (INAF))

17:35 Constraining BNS Models with sGRB Data and Forecasting Next-Generation Synergies

The landmark multi-messenger observations of the binary neutron star (BNS) merger GW170817 provided firm evidence that such mergers can produce short gamma-ray bursts (sGRBs). However, the scarcity of BNS detections in recent gravitational-wave (GW) observing runs raises a critical question: are BNS merger rates high enough to account for the full population of observed sGRBs?

We address this question by analyzing 64 BNS population synthesis models against 16 years of Fermi-GBM data. By simulating synthetic sGRB catalogs under various jet scenarios, including GW170817-like structured jets and non-universal geometries, we constrain viable BNS properties.

We show that population models predicting low local rates $R_{\text{BNS}}(0) \lesssim 50 \text{ Gpc}^{-3} \text{ yr}^{-1}$ fail to reproduce the observed sGRB population unless they assume large jet opening angles ($\theta_c \geq 15^\circ$) that contradict the narrow cores ($\theta_c \approx 6^\circ$) inferred from afterglow observations. We find that models with local rates $R_{\text{BNS}}(0) \approx 100 \text{ Gpc}^{-3} \text{ yr}^{-1}$ successfully reconcile sGRB observations with realistic jet physics.

Within these constraints, we leverage our framework to forecast multi-messenger opportunities of the coming decades. Using our physics-informed BNS catalogues, we will show specific event rate predictions in the MeV and afterglow regimes for upcoming missions (THESEUS, Crystal Eye, GRINTA). We will discuss the joint detection capabilities of these electromagnetic facilities when paired with the Advanced LIGO, Cosmic Explorer, and Einstein Telescope GW networks. Ultimately, in this talk we will highlight how an end-to-end interface between theoretical population modeling and observational strategies enables consistent, physics-informed multi-messenger predictions for future facilities.

Relatore: De Santis, Alessio Ludovico (GSSI)

17:50 Testing the Buoyancy of the Vacuum: the Archimedes experiment

The Cosmological Constant problem is one of the most persistent unresolved issues in theoretical physics, arising from the fundamental incompatibility between Quantum Field Theory and General Relativity. Addressing this challenge, the Archimedes experiment investigates the potential coupling between zero-point quantum fluctuations of the electromagnetic field and gravitational interactions. The experiment employs an ultra-sensitive, custom-designed beam-balance to detect gravitational forces acting on suspended samples. These samples undergo vacuum energy modulation via a superconducting phase transition, effectively forming a series of Casimir cavities that exclude specific electromagnetic modes. Should vacuum energy gravitate, the expelled modes would generate an upward force on the samples, analogous to Archimedes’ buoyancy principle in fluids, and measurable as a variation in effective weight.

The expected torque signal from this modulation is on the order of 10^−13 Nm/√Hz. To mitigate environmental interference, the experiment is sited at the SarGrav Laboratories in Sardinia’s Sos-Enattos region, renowned for its exceptionally low seismic noise and selected as a candidate location for the next-generation Einstein Telescope gravitational wave observatory.

Relatore: Allocca, Annalisa (INFN)

18:05 GRINTA: a new probe for time-domain astrophysics

Recent observations of the transient sky at all wavelengths are increasingly revealing the importance of the multi-messenger and multi-wavelength approach. The GRINTA (Gamma-Ray INternational Transient Array Observatory) mission, to be launched at the middle of the next decade, is a small gamma-ray observatory with good sensitivity, excellent angular resolution and fast follow-up capability for studying transient sources at timescales from ms to hours and ensuring optimal integration with multi-messenger networks. The GRINTA mission will carry two complementary payloads to cover the 5-10,000 keV band, that will detect and localise gamma-ray bursts within a 8 steradian field-of-view and will be able to perform imaging surveys with sub-arcmin resolution. GRINTA will operate in synergy with the most powerful electromagnetic, gravitational wave and neutrino observatories foreseen to be operational in the 2030's.

Relatore: Dr. Natalucci, Lorenzo (Istituto Nazionale di Astrofisica (INAF))

18:20 An updated proto-neutron star neutrino emission model

We present an improved parametric model for neutrino emission from core-collapse supernovae that directly connects neutrino luminosity and average energy to stellar properties during the emission. Our model incorporates two critical physical processes: convection within the proto-neutron star (PNS) and the evolving dynamics of neutrinosphere radii during the early emission phase. Crucially, the evolution of the PNS radius is tied to its gravitational-wave signature, providing a stronger physical framework for joint neutrino and gravitational-wave searches of the next Galactic supernova.

Relatore: Ballelli, Matteo (GSSI)

20:30 → 23:50 Cena Sociale

La cena sociale si terrà in centro storico a L'Aquila presso il Ristorante "La Malandrina" il giorno Mercoledì 6 maggio 2026 alle ore 20:30.
il costo è incluso nella fee di registrazione.
Per insegnanti, studenti secondarie, non professionisti e accompagnatori che non pagano la quota di registrazione, la quota di 55 euro per la cena sociale va pagata separatamente presso il ristorante.

gio 7 maggio

08:45 → 10:00 Assemblea dei Soci

10:00 → 10:40 Assegnazione Premi SAIt

10:40 → 11:10 Coffee Break

11:10 → 12:20 Little Red Dots (dibattito scientifico)

Roberta Tripodi
INAF - Osservatorio Astronomico di Roma
New colors for black holes in the early Universe: spectroscopic insights from Little Red Dots
In this talk, I will focus on CANUCS-LRD-z8.6, one of the highest-redshift spectroscopically confirmed LRD at z = 8.6319, which hosts an accreting SMBH and shows broad Hβ, high-ionization UV lines (e.g., CIV, NIV), very low metallicity (Z < 0.1 Zsun), and a BH mass exceeding that expected from its host. These properties suggest accelerated SMBH growth relative to the galaxy (Tripodi+25, Nat. Comm., 16, 9830).
I will also introduce JWST/NIRCam+NIRSpec results on Bz5.3, a broad-line AGN at z = 5.3 behind the Bullet Cluster (Tripodi+25, ApJL,994, L6). Strong Fe II, O I, and Ca II triplet lines, along with broad Balmer emission, confirm the presence of a stratified broad-line region (BLR). Remarkably, we report the first high-redshift detection of the λ1304 bump (O I + Si II), commonly observed in local AGNs. I will also discuss the implications on the excitation mechanisms of the BLR based on low-ionization line diagnostics. Photoionization modeling also reveals multiple gas phases in the BLR with diverse densities and ionization states. Finally, I will discuss the potential role of environment in shaping the evolution of LRDs based on the latest available JWST observations, and I will present an empirical classification of the spectroscopic diversity of LRDs (Perez-Gonzalez, RT incl, 2026; arXiv:2602.20247).

Fabio Pacucci
Center for Astrophysics - Harvard & Smithsonian
THE LITTLE RED DOTS ARE DIRECT COLLAPSE BLACK HOLES
The discovery by JWST of a substantial population of compact "Little Red Dots" (LRDs) presents a major puzzle: their observed spectra defy standard astrophysical interpretations. Here, we show that LRD spectra are naturally reproduced by emission from an accreting Direct Collapse Black Hole (DCBH). Using radiation-hydrodynamic simulations, we follow the growth of the DCBH seed via a dense, compressionally heated, collisionally ionized accretion flow. The model self-consistently reproduces the screen responsible for the observed Balmer absorption, while allowing UV/optical emission to partially escape, along with reprocessed infrared radiation. Crucially, this structure is not a blackbody and requires no stellar contribution: the UV continuum originates entirely from reprocessed DCBH radiation, attenuated only by a small amount of dust with an extinction curve consistent with high-redshift galaxies. This single framework simultaneously explains the key observational puzzles of LRDs: (a) weak X-ray emission, (b) metal and high-ionization lines alongside absent star-formation features, (c) overmassive black holes, (d) compact morphology, (e) abundance and redshift evolution -- linking them directly to pristine atomic-cooling halos, (f) long-lived ($>100$ Myr), slowly variable phases driven by radiation pressure. Our findings indicate that JWST is witnessing the widespread formation of heavy black hole seeds in the early Universe.

Federica Loiacono
INAF - Osservatorio di Astrofisica e Scienze dello Spazio
THE ABUNDANCE OF LITTLE RED DOTS FROM COSMIC DAWN TO NOON
The James Webb Space Telescope discovered a class of active galactic nuclei (AGNs) missed by previous selections. A fraction of these sources, dubbed "little red dots" (LRDs), show properties that are at odds with “classical” AGNs, and their nature is matter of intense debate. Most of these objects have been found at z > 4. At cosmic dawn (z ~ 6) they are ∼ 1-2 dex more abundant than X-ray and UV-selected AGNs at z ∼ 5 − 7 with similar bolometric luminosity. According to some theories, LRDs may represent the early, rapid growth stages of newly formed black hole (BH) seeds. In this scenario, the abundance of LRDs rapidly decreases from cosmic dawn to cosmic noon, where it is expected to fall short of that of standard AGNs by ∼ 3 dex.
In this talk I will compare the number density of LRDs at cosmic dawn to that at z~2-3, with the latter based on a sample of spectroscopically confirmed LRDs. I will show that this population is still abundant at cosmic noon, with their space density being only a factor of 2-3 lower than that of UV-selected quasars with comparable luminosity. A similar trend is observed in terms of BH masses. This result suggests that the formation of BH seeds can be efficient from cosmic dawn down to cosmic noon.

Laura Bisigello
INAF - Osservatorio Astronomico di Padova
THE QUEST FOR LOW-z LRDs
Since its launch, the James Webb Space Telescope (JWST) has uncovered a puzzling population of sources characterised by a compact morphology, “v-shaped" spectra, and broad hydrogen emission lines. The nature of these "Little Red Dots" (LRDs) remains highly debated, largely due to the challenges of observing them at high redshifts (z > 4). Current theoretical models disagree, for example, regarding the host galaxy's contribution to the observed spectral energy distribution at different wavelengths. Identifying LRDs at lower redshifts (z < 4) is therefore critical to resolve their host galaxies, establishing stringent multi-wavelength constraints, and, moreover, to trace their cosmic evolution. I will provide an overview of the current search for low-z LRDs, highlighting also recent results from wide-area surveys such as Euclid.

Chair: Andrea Ferrara

11:10 New colors for black holes in the early Universe: spectroscopic insights from Little Red Dots

In this talk, I will focus on CANUCS-LRD-z8.6, one of the highest-redshift spectroscopically confirmed LRD at z = 8.6319, which hosts an accreting SMBH and shows broad Hβ, high-ionization UV lines (e.g., CIV, NIV), very low metallicity (Z < 0.1 Zsun), and a BH mass exceeding that expected from its host. These properties suggest accelerated SMBH growth relative to the galaxy (Tripodi+25, Nat. Comm., 16, 9830).
I will also introduce JWST/NIRCam+NIRSpec results on Bz5.3, a broad-line AGN at z = 5.3 behind the Bullet Cluster (Tripodi+25, ApJL,994, L6). Strong Fe II, O I, and Ca II triplet lines, along with broad Balmer emission, confirm the presence of a stratified broad-line region (BLR). Remarkably, we report the first high-redshift detection of the λ1304 bump (O I + Si II), commonly observed in local AGNs. I will also discuss the implications on the excitation mechanisms of the BLR based on low-ionization line diagnostics. Photoionization modeling also reveals multiple gas phases in the BLR with diverse densities and ionization states. Finally, I will discuss the potential role of environment in shaping the evolution of LRDs based on the latest available JWST observations, and I will present an empirical classification of the spectroscopic diversity of LRDs (Perez-Gonzalez, RT incl, 2026; arXiv:2602.20247).

Relatore: Tripodi, Roberta (Istituto Nazionale di Astrofisica (INAF))

11:28 The Little Red Dots Are Direct Collapse Black Holes

The discovery by JWST of a substantial population of compact "Little Red Dots" (LRDs) presents a major puzzle: their observed spectra defy standard astrophysical interpretations. Here, we show that LRD spectra are naturally reproduced by emission from an accreting Direct Collapse Black Hole (DCBH). Using radiation-hydrodynamic simulations, we follow the growth of the DCBH seed via a dense, compressionally heated, collisionally ionized accretion flow. The model self-consistently reproduces the screen responsible for the observed Balmer absorption, while allowing UV/optical emission to partially escape, along with reprocessed infrared radiation. Crucially, this structure is not a blackbody and requires no stellar contribution: the UV continuum originates entirely from reprocessed DCBH radiation, attenuated only by a small amount of dust with an extinction curve consistent with high-redshift galaxies. This single framework simultaneously explains the key observational puzzles of LRDs: (a) weak X-ray emission, (b) metal and high-ionization lines alongside absent star-formation features, (c) overmassive black holes, (d) compact morphology, (e) abundance and redshift evolution -- linking them directly to pristine atomic-cooling halos, (f) long-lived ($>100$ Myr), slowly variable phases driven by radiation pressure. Our findings indicate that JWST is witnessing the widespread formation of heavy black hole seeds in the early Universe.

Relatore: Pacucci, Fabio (Center for Astrophysics | Harvard & Smithsonian)

11:46 The abundance of little red dots from cosmic dawn to noon

The James Webb Space Telescope discovered a class of active galactic nuclei (AGNs) missed by previous selections. A fraction of these sources, dubbed "little red dots" (LRDs), show properties that are at odds with “classical” AGNs, and their nature is matter of intense debate. Most of these objects have been found at z > 4. At cosmic dawn (z ~ 6) they are ∼ 1-2 dex more abundant than X-ray and UV-selected AGNs at z ∼ 5 − 7 with similar bolometric luminosity. According to some theories, LRDs may represent the early, rapid growth stages of newly formed black hole (BH) seeds. In this scenario, the abundance of LRDs rapidly decreases from cosmic dawn to cosmic noon, where it is expected to fall short of that of standard AGNs by ∼ 3 dex.
In this talk I will compare the number density of LRDs at cosmic dawn to that at z~2-3, with the latter based on a sample of spectroscopically confirmed LRDs. I will show that this population is still abundant at cosmic noon, with their space density being only a factor of 2-3 lower than that of UV-selected quasars with comparable luminosity. A similar trend is observed in terms of BH masses. This result suggests that the formation of BH seeds can be efficient from cosmic dawn down to cosmic noon.

Relatore: Loiacono, Federica (Istituto Nazionale di Astrofisica (INAF))

12:03 The quest for low-z LRDs

Since its launch, the James Webb Space Telescope (JWST) has uncovered a puzzling population of sources characterised by a compact morphology, “v-shaped" spectra, and broad hydrogen emission lines. The nature of these "Little Red Dots" (LRDs) remains highly debated, largely due to the challenges of observing them at high redshifts (z > 4). Current theoretical models disagree, for example, regarding the host galaxy's contribution to the observed spectral energy distribution at different wavelengths. Identifying LRDs at lower redshifts (z < 4) is therefore critical to resolve their host galaxies, establishing stringent multi-wavelength constraints, and, moreover, to trace their cosmic evolution. I will provide an overview of the current search for low-z LRDs, highlighting also recent results from wide-area surveys such as Euclid.

Relatore: Bisigello, Laura (Università di Padova)

12:20 → 13:30 Tavola rotonda: Obiettivi, Strategie, Risorse

Patrizia Caraveo
Presidente della Società Astronomica Italiana

Sara Lucatello
Presidente della European Astronomical Society

Roberto Ragazzoni
Presidente dell'Istituto Nazionale di Astrofisica

Eugenio Coccia
Vice-Presidente della Società Italiana di Fisica

13:30 → 14:30 Pranzo

14:30 → 16:00 Eliofisica e Space Weather

14:30 Il Sole, l'eliosfera e oltre: le sfide per il futuro

Lo scorso decennio ha visto una trasformazione radicale della nostra visione dell'eliosfera: da una serie di fenomeni isolati a un sistema unico e interconnesso, una macchina complessa di cui il Sole è il motore centrale.
Questo cambio di paradigma è stato favorito e accelerato da una nuova generazione di strumenti, tra cui la missione Solar Orbiter e il Daniel K. Inouye Solar Telescope (DKIST), che hanno aperto finestre osservative inaspettate sui processi fisici alla base dell'attività solare e della formazione e propagazione del vento solare nell'eliosfera.
In questo intervento delineo le nuove prospettive e le sfide aperte emerse con questa nuova visione dell'eliosfera, accennando a come future missioni spaziali e strumenti da terra, uniti a progressi nei metodi e modelli teorici, potranno contribuire ad affrontarle.

Relatore: Andretta, Vincenzo (Istituto Nazionale di Astrofisica (INAF))

14:55 Space Weather e Space Climate: l'impegno italiano nelle sfide future

Negli ultimi decenni, lo studio dello Space Weather (SWE) e dello Space Climate (SC) ha assunto un ruolo centrale nel panorama scientifico internazionale, per via dell’impatto dell’attività solare e dei raggi cosmici sulle infrastrutture tecnologiche e sulle attività umane. Questi temi sono al centro del programma internazionale COURSE (Cross-scale cOUpling pRocesses in the Solar-tErrestrial system) promosso da SCOSTEP (Scientific Committee on Solar Terrestrial Physics), che definisce le priorità di ricerca per il periodo 2026–2030 nell’ambito delle relazioni Sole–Terra.
Le principali sfide per il futuro nei campi dello SWE e SC riguardano: 1) la comprensione completa e dettagliata dei processi fisici sottostanti all’attività solare; 2) la caratterizzazione dell’intero intervallo della variabilità solare, inclusi gli eventi estremi; 3) la valutazione accurata degli effetti sulle infrastrutture spaziali e terrestri e sulla salute umana; 4) il salto di qualità nella capacità di prevedere in modo tempestivo i fenomeni di SWE; 5) lo sviluppo di servizi operativi sempre più affidabili ed efficienti per garantire un’efficace mitigazione e la protezione del pianeta.
In questo contesto, la comunità italiana svolge un ruolo rilevante, anche attraverso il partenariato esteso Space It Up!, finanziato da ASI e MUR, che integra ricerca fondamentale e applicazioni operative. Il contributo italiano include lo sviluppo di nuove missioni spaziali, il potenziamento delle infrastrutture osservative, lo sviluppo di modelli fisici avanzati e tecniche di analisi dati e di previsione innovative, anche basate sull’intelligenza artificiale. Il rafforzamento delle collaborazioni e delle infrastrutture di ricerca sarà cruciale per consolidare il ruolo dell’Italia in questo settore strategico.

Relatore: Dr. Laurenza, Monica (INAF-Istituto di Astrofisica e Planetologia Spaziali)

15:15 Mapping the Origin of the FIP Effect: High-Resolution Insights from IBIS and Hinode/EIS

The chemical composition of solar plasma remains largely unchanged as it travels along open magnetic fields from the chromosphere and corona into the heliosphere. While the solar corona is expected to have a chemical composition similar to the solar photosphere, it often exhibits a peculiar enrichment of elements with low First Ionization Potential (FIP), the so-called FIP effect. Understanding the mechanism of this fractionation is crucial for many reasons, including recostructing the origin of the solar wind.

In this talk, I will present recent breakthroughs in identifying the physical driver of this phenomenon. By combining high-resolution spectropolarimetric high-resolution spectropolarimetric ground-based observations from the IBIS instrument with EUV spectroscopic data from the HINODE/EIS mission, we provide the first direct evidence of a magnetic link between chromospheric wave reflection and coronal FIP fractionation. Our analysis allows us to disentangle upward and downward propagating waves, confirming the presence of wave reflection within the chromosphere. These findings provide a robust observational validation of theoretical models involving the ponderomotive force.

Relatore: Murabito, Mariarita (Istituto Nazionale di Astrofisica (INAF))

15:30 IBIS 2.0: Interferometric BIdimensional Spectrometer 2.0 at the THEMIS Solar Telescope

The IBIS2.0 project aims to upgrade the INAF Interferometric BIdimensional Spectrometer, originally operated at the Dunn Solar Telescope of the National Solar Observatory from 2003 to 2019, for its installation and operation at the THEMIS solar telescope at the Teide Observatory. The refurbished instrument integrates the original dual Fabry-Perrot etalons with a new polarimetric unit, interference filters, new scientific cameras, and a fully modernised instrument control and data-handling system. IBIS2.0 is designed to preserve the spectral coverage of the original system (580-860 nm) while offering automatisation of the instrument's operations and enhanced operability. The integration of the instrument at THEMIS is currently underway. In this contribution, we present the IBIS 2.0 instrument, the status of its installation at the new telescope, as well as the new observational capabilities that it will offer.

Relatore: Sant, Kamal

15:45 Gnevyshev Gap and Forbush decrease frequency over five Solar Cycles: Insights from the Rome Neutron Monitor

The galactic cosmic ray (GCR) intensity is modulated by solar activity and represents indirect probe of the heliospheric conditions. For instance, the GCR intensity follows the approximately 11-year solar cycle, exhibiting a well-known anti-correlation with solar activity. At short-term time scales, Forbush decreases (FDs), i.e. GCR intensity ranging from hours to days are driven by transient solar wind structures, such as interplanetary coronal mass ejections (ICMEs).
Understanding the link between long and short-term variations is essential for a comprehensive description of solar activity, heliospheric environment and space weather–space climate coupling. A particularly interesting feature emerging at solar maximum is the temporary decrease in solar activity known solar cycle double-peak or Gnevyshev gap (GG).
We investigated the specific relation between the occurrence of FDs and the solar activity cycle characteristics, including GG, over the course of five solar cycles. The GCR intensity data are provided by the SVIRCO (Studio delle Variazioni dell’Intensità dei Raggi COsmici) Observatory, i.e. the neutron monitor located in Rome (Italy), having a geomagnetic cutoff of 6.27 GV.
We perform a statistical analysis of the occurrence of CME and geoeffective ICME as a major driver of FDs, showing similarities and differences with respect to FD occurrence during the different phases of the solar cycles. We discuss how the frequency and magnitude of FDs evolve in response to the structuring of the solar cycle. Our results confirm the existence of the GG in the FD occurrence and highlight a dependence on the odd-even parity of the solar cycles[M.

Relatore: Recchiuti, Dario (Istituto Nazionale di Astrofisica (INAF))

16:00 → 18:30 Visita ai Laboratori Nazionali del Gran Sasso dell'INFN (ingresso riservato)

(ingresso riservato)

21:15 → 22:30 Perché torniamo sulla Luna? (Conferenza divulgativa aperta al pubblico)

(Conferenza divulgativa aperta al pubblico)
A oltre 50 anni dalla fine del programma Apollo, la Luna ha riconquistato l’attenzione del pubblico. Dopo che la Cina ha dichiarato che porterà i suoi taikonauti sulla Luna entro il 2030, è partita la corsa degli Stati Uniti per arrivare prima. In una direttiva presidenziale dello scorso dicembre, alla NASA è stato ordinato di fare allunare i suoi astronauti entro il 2028, ultimo anno della Presidenza Trump. Stiamo assistendo ad una nuova corsa alla Luna e ci chiediamo chi vincerà?

Patrizia Caraveo: Annoverata nella lista dei ricercatori e delle ricercatrici che hanno pubblicato il maggior numero di articoli più citati nel mondo scientifico, Caraveo è stata nominata Commendatore dell’Ordine al Merito della Repubblica Italiana. Dal 2025 è Presidente della SAIt. E stata inserita tra le 100 donne contro gli stereotipi e, con il suo stile diretto e coinvolgente, porterà a L'Aquila uno sguardo autorevole e appassionato sui grandi temi dell’astronomia e della geopolitica spaziale.

Relatore: Caraveo, Patrizia (Istituto Nazionale di Astrofisica (INAF))

SAIT 2026 Caraveo LUNA.pdf

ven 8 maggio

09:00 → 11:05 Calcolo, Archivi e Intelligenza Artificiale

09:00 AI: come preparare gli archivi dell’era del Big Data per lo sfruttamento scientifico di ampio spettro

L’astronomia nell’era digitale ha cambiato radicalmente l'approccio sia osservativo che di analisi delle osservazioni. Una seconda rivoluzione nel modo di fare scienza sta avvenendo ora grazie all'uso intensivo dell’AI nelle sue declinazioni di Machine Learning e Deep Learning. In questo talk presenterò il punto di vista dell’archivista, di chi si occupa della categorizzazione dei dati osservati e simulati, della preparazione delle collezioni all’esplorazione in ML e DL, approcci che sono diversi ma richiedono entrambi una cura del dato quanto più possibile precisa per evitare i ben noti problemi di allucinazione degli algoritmi. In particolare si farà un excursus sui principi FAIR, sulle forme di standardizzazione esistenti per la formattazione dei dati, sulla metadatazione e sui protocolli di pubblicazione dei dati che aiutano soprattutto nell’utilizzo del Machine Learning, mentre alcuni accenni verranno fatti per quanto riguarda gli accessi e l’utilizzo dei dati di archivio per il Deep Learning.

Relatore: Knapic, Cristina (Istituto Nazionale di Astrofisica (INAF))

09:25 Enabling Italian Astrophysics at Scale: Achievements and Future Directions from the National Centre for HPC, Big Data and Quantum Computing

The National Centre for High-Performance Computing, Big Data and Quantum Computing has represented a major opportunity to advance the computational and data-intensive capabilities of Italian astrophysics. Within this framework, Spoke 3 on Astrophysics and Cosmos Observations has delivered an integrated programme of activities across HPC code enabling and GPU acceleration, advanced algorithms for exascale-oriented applications, machine learning and Bayesian methods for large astrophysical datasets, remote visualization, and FAIR-compliant data management and archive services. These activities have produced not only optimized codes, innovative workflows, and interoperable infrastructures, but also a broader ecosystem connecting software development, data services, scientific applications, and community expertise.

An important outcome of this experience is the demonstration that astrophysics can serve as an extreme and fertile laboratory for the development of advanced digital technologies with impact beyond the scientific domain. This has already been shown by several innovation and cascade-funding projects, where methodologies originally developed for astrophysical challenges were successfully extended to applications such as environmental monitoring, seismic risk assessment, financial analytics, and interoperable data platforms.

Starting from these results, we are proposing a long-term framework to consolidate and extend this trajectory: a Deep Tech Living Lab (DT-Lab). The Lab is conceived to integrate HPC, artificial intelligence, EOSC-aligned FAIR data infrastructures, advanced visualization, and exploratory quantum computing in a co-design environment involving research institutions, industry, and public stakeholders. Its goal will be to transform the extreme requirements of next-generation astrophysical infrastructures and missions, including SKA, CTA, Euclid, LSST, and LISA, into drivers for technological innovation, technology transfer, and high-level training.

Relatore: Taffoni, Giuliano (Istituto Nazionale di Astrofisica (INAF))

09:45 La Ricerca Scientifica nell'era degli Agenti Autonomi: prospettive per l'Astrofisica

Le metodologie basate sull'Artificial Intelligence sono in rapidissima evoluzione. I modelli linguistici (LLM), sempre più potenti, non sono più limitati alla sola generazione ed elaborazione di testo, ma sono anche capaci di pianificare ed eseguire task complessi. Attraverso l'integrazione all'interno di agenti autonomi, possono accedere a strumenti e dati esterni (grounding), generare ed eseguire nuovi moduli software e implementare meccanismi automatici di verifica formale, mantenendo punti di controllo umani (human-in-the-loop). Questo consente di superare i limiti intrinseci dovuti alla natura stocastica e di aumentare la precisione dei risultati, fino a raggiungere, in casi specifici, l'affidabilità e il rigore richiesti dalla ricerca scientifica.

In questo contributo esploreremo alcuni esempi applicativi in ambito scientifico e le prospettive di utilizzo dell'A.I. generativa nel campo della ricerca astronomica (es. analisi dati multi-messenger, automazione di pipeline, interrogazione della letteratura scientifica, gestione di workflow complessi, ecc.)

Verrà inoltre discussa la sfida trasformativa per l’INAF, analizzando come l’adozione di queste tecnologie richieda un aggiornamento trasversale delle competenze, una infrastruttura tecnologica e organizzativa adeguata e un’attenta riflessione metodologica per garantire che l'automazione potenzi, senza sostituire, la valutazione critica del ricercatore.

Relatore: Capasso, Giulio (Istituto Nazionale di Astrofisica (INAF))

10:05 Fiber-fed wavefront sensing with machine learning: results from simulations to experimental laboratory setup

The synergy between astronomy and photonics is opening new perspectives in wavefront sensing for ground-based telescopes. In this context, a further integration of photonic devices with machine learning techniques represents a particularly promising approach.
This work investigates the use of multimode fibers (MMFs) as wavefront sensors, coupled with a properly trained Neural Network (NN). In an initial work phase, aberrated wavefronts were propagated through a simulated MMF with known characteristics, and the resulting intensity patterns were used to train a given network architecture, assessing its ability to recognize the input aberrations.
To experimentally validate the concept, an optical bench has been developed and operated under controlled laboratory conditions, following the same approach adopted in the simulation phase. In this presentation, the methodology and the results obtained so far will be discussed.

Relatore: Di Francesco, Benedetta (Istituto Nazionale di Astrofisica (INAF))

10:17 Local AI Infrastructure for Agentic Workflows in Modern Astronomical Data Processing: Toward Domain-Specific Large Language Model Training

The exponential growth of astronomical datasets demands a paradigm shift in data analysis, with AI emerging as a critical enabler. We present a dedicated local AI infrastructure comprising five NVIDIA GB10 Grace-Blackwell Superchip nodes, each with 128 GB of unified memory, designed to deliver domain-specific AI capabilities while ensuring full data sovereignty. The system runs open-weight Qwen models optimized via Mixture-of-Experts (MoE) architectures for automated code generation, documentation, and agentic workflow orchestration—enabling dynamic pipeline development that keeps pace with scientific discovery. We argue that agentic AI workflows—capable of autonomous task orchestration, failure recovery, and adaptive reasoning—will become the dominant paradigm for complex astronomical pipelines. Key applications include automated flagging, calibration, imaging, and source extraction in radio astronomy, where LLM agents can integrate domain knowledge across heterogeneous data conditions, as required by the data deluge from next-generation observatories like the Square Kilometre Array (SKA). To scale these capabilities, we are planning to expand our infrastructure to support inference on larger LLMs (200B+ parameters) and will leverage this capacity to train a lightweight, domain-specific LLM tailored to astronomical workflows, using curated datasets of pipeline scripts, calibration logs, and peer-reviewed literature. This localized, sovereign approach ensures reproducibility, efficiency, and privacy—critical for next-generation data-intensive science. By embedding AI directly into the scientific workflow, we move beyond tool-assisted analysis toward autonomous, adaptive discovery, establishing a sustainable model for AI-augmented astronomy at scale.

Relatore: Lacopo, Giovanni (Istituto Nazionale di Astrofisica (INAF))

10:29 Quantum Computing and Quantum Machine Learning in Astrophysical Data Analysis: Methods and Current Limitations

The increasing complexity and volume of astrophysical data are motivating the exploration of novel computational paradigms beyond classical high-performance computing. In this context, quantum computing and quantum machine learning (QML) are emerging as potential complementary approaches for data analysis, although their practical applicability remains under active investigation.
This contribution presents an overview of recent research on the application of quantum computing techniques to astrophysical problems, with a focus on methodological developments and computational constraints. In particular, hybrid classical–quantum models will be discussed, including Quantum Convolutional Neural Networks for the classification of transient astrophysical signals, and Quantum Graph Neural Networks for the analysis of large-scale structure. Additionally, the integration of the Quantum Fourier Transform into cosmological data analysis pipelines, such as those used for Cosmic Microwave Background map processing, will be presented.
The discussion will concentrate on the key computational challenges that currently limit the performance of QML approaches in the noisy intermediate-scale quantum (NISQ) regime. These include data encoding overhead, limited qubit resources, and constraints on circuit depth, which together often dominate the overall computational cost.

Relatore: Farsian, Farida (Istituto Nazionale di Astrofisica (INAF))

10:41 Astrofisica multimessaggera e del dominio temporale: il supporto degli standard dell'IVOA.

Integrare e rendere interoperabili le informazioni fornite da infrastrutture distribuite, spaziali o terrestri, simulazioni e modelli numerici, richiede un approccio condiviso dalla comunità.
L'International Virtual Observatory Alliance (IVOA) è un'organizzazione aperta, guidata dalla comunità, il cui scopo è discutere e sviluppare standard di interoperabilità, per promuovere un ecosistema di servizi e strumenti (noto come Virtual Observatory - VO).
Gli standard IVOA coprono la maggior parte dei requisiti dei principi FAIR e forniscono una solida base per aderire ai principi FAIR in astrofisica. La visione dell'IVOA è che i dati e altre risorse in astrofisica debbano funzionare come un unicum volto a favorire la ricerca scientifica.
Il supporto per l'astronomia multimessaggera e del dominio temporale è uno dei motori scientifici per lo sviluppo degli standard IVOA.
Questo contributo descrive lo sviluppo degli standard di interoperabilità in questo ambito dell'astrofisica, li illustra inseriti nel contesto generale dell'IVOA e fornisce esempi di servizi e soluzioni.

Relatore: Molinaro, Marco (Istituto Nazionale di Astrofisica (INAF))

10:53 Un nuovo codice parallelo per risolvere l’interazione tra particelle e radiazione col formalismo della Matrice di Transizione

La diffusione e l’assorbimento di radiazione ad opera di particelle irregolari ricopre un’importanza fondamentale in moltissime applicazioni scientifiche e tecnologiche, spaziando dall’analisi di campioni di laboratorio al monitoraggio di inquinanti atmosferici e oceanici, fino allo studio degli effetti di estinzione da mezzo interstellare. Nonostante l’importanza del problema, una completa trattazione è resa difficoltosa dalla complessità teorica inerente la risoluzione del formalismo sottostante, che ammette soluzione analitica in pochi casi semplificati. In situazioni più realistiche, bisogna ricorrere a metodi numerici, come il formalismo della matrice di transizione (T-matrix). Tale formalismo descrive le particelle come operatori lineari che, applicati ad un generico campo di radiazione incidente, determinano univocamente il campo risultante, fornendo una descrizione completa della fisica del problema. Ciò rappresenta un vantaggio rispetto a metodi alternativi, quali l’approssimazione a dipoli discreti (DDA), che richiede un calcolo separato per ogni direzione di radiazione incidente e diffusa, o la teoria modificata dei campi medi (MFT), inadeguata a descrivere particelle molto disomogenee, che, tuttavia, sono più semplici da affrontare e sono stati per questo impiegati più diffusamente. In questo contributo presentiamo una nuova implementazione del metodo della matrice di transizione, basato sul formalismo sviluppato da Borghese, Denti & Saija, che, traendo vantaggio da risorse di calcolo distribuito e parallelo, sfrutta le potenzialità di moderne architetture di calcolo per risolvere con maggiore efficienza modelli ad elevata complessità. Concludiamo la trattazione illustrando come l’applicazione di modelli realistici di particelle influenza l’interpretazione degli spettri di assorbimento nel mezzo interstellare e nello studio delle atmosfere planetarie.

Relatore: Dr. La Mura, Giovanni (INAF - Osservatorio Astronomico di Cagliari)

11:05 → 11:30 Coffee break

11:30 → 13:00 Dibattito scientifico: Gravitational Waves e Multimessenger Astronomy del prossimo decennio

Maria Grazia Bernardini
INAF - Osservatorio Astronomico di Brera

Monica Colpi
INAF - Osservatorio Astronomico di Brera

Francesco Vissani
INFN - Laboratori Nazionali del Gran Sasso

Andrea Possenti
INAF - Osservatorio Astronomico di Cagliari
TO TRIGGER OR TO BE TRIGGERED: THE TWO FACES OF THE PULSAR TIMING ARRAYS IN THE MULTIMESSENGER CONTEXT
The rotational stability of a subset of the “recycled” pulsars opens the possibility to exploit them as components of a galactic scale gravitational wave detector, known as Pulsar Timing Array (PTA), in turn providing a unique instrument to search for gravitational waves (GWs) in the ultra-long period range, nicely complementary to the frequency range of other current or future GW detectors. The PTA experiments have recently published intriguing results, showing the first evidences for a detection, yet to be supported by additional data and analysis. In this contribution it will be discussed how the PTAs can benefit of multi-messenger programs or will be able to trigger multi-messenger follow-ups with a special focus for the European Pulsar Timing Array (EPTA) case.

Luigi Piro
INAF - IAPS Roma

Paola Severgnini
INAF - Osservatorio Astronomico di Brera

Chair: Marica Branchesi

Relatori: Bernardini, Maria Grazia (Istituto Nazionale di Astrofisica (INAF)), Branchesi, Marica (Istituto Nazionale di Astrofisica (INAF)), Colpi, Monica (Istituto Nazionale di Astrofisica (INAF)), Piro, Luigi (Istituto Nazionale di Astrofisica (INAF)), Possenti, Andrea (Istituto Nazionale di Astrofisica (INAF)), Severgnini, Paola (Istituto Nazionale di Astrofisica (INAF)), Vissani, Francesco (Istituto Nazionale di Fisica Nucleare (INFN))

13:00 → 13:15 Chiusura dei lavori

13:15 → 14:00 Light lunch