Deciphering the internal composition of Earth-like planets and the architecture of their planetary systems with PLATO (Giampaolo Piotto, Luca Malavolta)

ESA's mission PLATO (PLAnetary Transits and Oscillations of stars) will discover hundreds of small planet candidates that transit bright, nearby stars, some of them possibly in the Habitable zone of their host star. While PLATO can provide precise radii and orbital periods for many Earth-size candidates, follow-up observations with groundbased telescopes are pivotal for confirming their planetary nature and, ultimately, for constraining their internal composition when mass is obtained via the radial velocity (RV) technique. For the first time in an exoplanetary mission, ground-based follow-up is a fully integrated part of the PLATO space mission, within the Ground Observation Program (GOP).

PLATO will be launched in early 2027, and the first scientific data will become available to the PLATO Consortium only a few months later, in an ideal timeframe for a PhD thesis for a LVII cycle student. Several members of Exoplanet team in Padova hold key leadership responsibilities within the PLATO mission, including the target selection and the development of the planet detection pipelines. As such, we have priority access to PLATO early-science data and GOP observations of the PLATO prime sample targets. Collecting data, however, is not enough. The presence of spots and faculae on the stellar surface can introduce spurious signals in the spectroscopic time series and hamper our ability to weigh small planets, while cyclic variation in the magnetic field of the star may hinder the detection of massive long-period planets, making it difficult to identify the actual architecture of the planetary system.

We propose a PhD projects, focused on Earth-sized candidate planets in multi-planet systems identified by PLATO, in which the student will develop and implement new models to disentangle the planetary signals from stellar activity while taking advantage of the exquisite photometric precision of PLATO and spectroscopic data gathered by the GOP with state-of-the-art instruments, such as ESPRESSO at the Very Large Telescope. The student will combine PLATO photometry, GOP spectroscopy, and Gaia DR4 astrometry in a Bayesian framework, developed within our research group, to measure planet masses, robustly assess the architectures of planetary systems, constrain the densities of transiting planets, and unveil their internal compositions by comparison with theoretical models in the mass-radius diagram.

The student will become familiar with the most recent experimental techniques for modelling stellar interference in light-curve and RV datasets, and will become expert in state-of-the-art statistical tools applied to exoplanet science, including Bayesian analysis and Gaussian Processes. As part of this project, the PhD candidate will become part of the PLATO Mission Consortium and have the opportunity to conduct observations at the most important observatories at ESO and in the Northern hemisphere

  Exoplanets with PLATO (Giampaolo Piotto, Domenico Nardiello, Tiziano Zingales)

The ESA/PLATO mission (Rauer+2025) will revolutionize exoplanet research by discovering thousands of new transiting planets, with a particular attention to Earth-sized worlds in the habitable zones of Sun-like stars. Equipped with 26 wide-field optical cameras optimized for ultra-high-precision photometry, the mission will observe its first long-duration field (LOPS2) continuously for at least two years (Nascimbeni et al. 2025), delivering more than 200,000 light curves for a carefully selected stellar sample.

PLATO will be launched in early 2027, and the first scientific data will become available to the PLATO Consortium only a few months later. The exoplanet research group at the University of Padova is deeply involved in the mission at the highest level, with its members holding leading roles and major responsibilities in PLATO. This prominent involvement will provide the group with early access to the first scientific data obtained during the initial months of observations, well before these data become publicly available and to data reserved to PLATO Consortium.

A student starting the PhD programme  from the XLII cycle will be ideally positioned to contribute to the PLATO mission, as the arrival of the first data will coincide with the early stages of the PhD. This timing will offer a unique opportunity to  be inserted into the PLATO European Consortium and to play an active role in the analysis and scientific exploitation of the mission’s observations. 

Given the strong involvement of the UNIPD exoplanet group in the PLATO mission, together with the internationally recognized expertise of its members, several PhD projects focused on the exploitation of PLATO data are proposed, matching student interests and capabilities. Some examples are:

• Analysis of early science data (first six months of the mission unique access) for the finding and validation of transiting exoplanets.

• Analysis of the light curves of young stars for the stellar characterization and the search for exoplanets.

• Development of tools of analysis of light curves with machine learning techniques.

• Studies of the Transit Time Variations for the analysis of planetary systems with dynamical methods.

• others.

  Counter rotation in disk galaxies (Alessandro Pizzella)

Counter-rotating disk galaxies are galaxies, either spiral or S0,
characterized by a stellar disk composed of two components, one
rotating in the opposite direction to the other. They represent no
more than about 5% of disk galaxies. Several mechanisms have been
proposed to explain the origin of this peculiar structure, the most
relevant being the acquisition of external material by a pre-existing
stellar disk. The study of counter-rotating galaxies therefore
provides important clues about the formation and evolution of disk
galaxies.

The advent of integral field spectroscopy has given a significant
boost to the study of this phenomenon. Extended databases and archival
data are now available for thousands of galaxies, and detailed
analyses of stellar kinematics and populations will make a substantial
contribution to understanding how gas acquisition in disk galaxies
occurs.

  Memory in Chaos: Reconstructing Cluster Histories from Gravitational-Wave Phase Space (Alessandra Mastrobuono Battisti, Elisa Bortolas)

This PhD project explores a novel question: do gravitational-wave sources retain a measurable “memory” of the dynamical environments in which they formed?
The student will investigate whether chaotic few-body interactions imprint detectable structures in the phase space of merging binaries.
The project will use controlled N-body and scattering experiments to generate libraries of dynamical interactions under varying cluster conditions.
A key objective is to identify invariants or statistical fingerprints (e.g. correlations in mass ratios, spins, eccentricities) that survive dynamical processing.
The student will develop new phase-space and information-theory diagnostics to quantify this “dynamical memory.”
Machine-learning tools will be used to classify formation pathways directly from synthetic GW observables.
The project will test whether different environments (young clusters, globular clusters, nuclear clusters) occupy distinct regions of observable parameter space.
A central challenge will be disentangling degeneracies between initial conditions and stochastic evolution.
The outcomes will provide a new conceptual framework to interpret GW data as probes of underlying dynamical processes.
This project opens a pathway toward “inverse stellar dynamics,” where observations constrain the chaotic physics of dense stellar systems.

  Reconstructing the Milky Way Assembly through Globular Cluster Dynamics (Alessandra Mastrobuono Battisti)

This PhD project will investigate the assembly history of the Milky Way using globular clusters as dynamical tracers.
The student will be trained in high-resolution N-body simulations to model the evolution of globular clusters in realistic, time-dependent Galactic potentials.
These simulations will be combined with cosmological galaxy models to link cluster orbital properties to specific accretion events.
A central objective is to identify observable signatures of past mergers encoded in the phase-space distribution of clusters.
The student will analyse Gaia and spectroscopic datasets to constrain and validate the models.
Particular focus will be placed on distinguishing in-situ from accreted cluster populations through kinematics and chemical properties.
The project will involve the development of analysis tools to associate clusters with their progenitor galaxies.
Through this work, the student will reconstruct the timing and mass spectrum of past merger events.
The PhD will provide training in computational astrophysics, Galactic dynamics, and data–model comparison.
The expected outcome is a dynamically calibrated reconstruction of the Milky Way assembly, bridging stellar dynamics and Galactic archaeology.

  Early Activity in Pristine Comets: Spectroscopic Diagnostics from the Near-UV to the Near-Infrared in Support of Comet Interceptor mission (Monica Lazzarin, Fiorangela La Forgia)

Recent observations of dynamically new comets and of the interstellar object 3I/ATLAS have
revealed unexpected activity and emission features at large heliocentric distances,
challenging traditional models of cometary outgassing and coma chemistry. Understanding
how cometary activity begins and evolves as a comet approaches the Sun is therefore a key
open problem, and one that is directly relevant for the Comet Interceptor mission of the
European Space Agency, which will encounter a dynamically new or interstellar comet
during its first passage through the inner Solar System.
This project will investigate the spectroscopic evolution of cometary activity across a wide
wavelength range. Visible spectroscopy obtained from Asiago telescopes will enable the
study of major molecular emissions such as CN, C2 and C3, as well as atomic and alkali
species, and their spatial distributions within the coma. These observations will also support
the identification and long-term monitoring of particularly interesting targets, including newly
discovered comets from next-generation surveys such as Vera C. Rubin Observatory
(LSST), which are expected to dramatically increase the discovery rate of distant and
dynamically new comets. The visible observations will be complemented by near-infrared
spectroscopy obtained with the Telescopio Nazionale Galileo using the NICS instrument,
extending the spectral coverage to 2.5 μm. This range allows investigation of additional CN
bands, molecular features of C2 and C3, and possible absorption signatures of amorphous
and crystalline water ice in cometary dust.
The project will also include preparatory studies for future observations with CUBES, which
will open the near-UV window (3000–4000 Å) at high spectral resolution, enabling detailed
studies of CN and key isotopic tracers such as OD/OH. By combining multi-wavelength
spectroscopy with systematic monitoring of newly discovered comets, the project aims to
identify diagnostics of early activity and contribute to the ground-based framework
supporting the selection and characterization of potential targets for the Comet Interceptor
mission.

  Visible Spectroscopy of Near-Earth Asteroids: Surface Properties, Taxonomic Classification, and Space Weathering Constraints (Monica Lazzarin, Fiorangela La Forgia)

Near-Earth Asteroids (NEAs) are among the most accessible small bodies in the Solar
System and represent key targets for both planetary science and planetary defence. Their
surface composition, inferred from visible reflectance spectroscopy, provides crucial
information on their origin, collisional history, and space weathering history — the process by
which solar wind irradiation and micrometeorite bombardment progressively alter the optical
properties of asteroid surfaces, making them spectrally different from their presumed
meteoritic analogues. European observational programmes such as NEOROCKS and
NEOPOPS have built extensive spectral databases combining observations from multiple
telescopes across Europe. In this project, we exploit spectra acquired within NEOPOPS,
obtained with the 1.22m Galileo Telescope and the 1.82m Copernico Telescope at the
Asiago Astrophysical Observatory and the Large Binocular Telescope (LBT), complemented
by an independent dataset of spectra acquired with the Very Large Telescope (VLT). The
standard Bus-DeMeo taxonomic framework provides a well-established classification
scheme, but its PCA-based approach was built on a specific dataset and is not directly
transferable to spectra from different instruments and surveys, limiting the ability to combine
heterogeneous databases in a consistent way. This PhD project aims to overcome this
limitation by developing a unified spectral analysis framework that allows datasets from
different facilities to be compared and classified consistently, without being tied to a single
instrument or survey. The project will also include the acquisition of new visible-NIR spectra

of NEAs, together with the reduction and calibration of the observational data following
standard spectroscopic pipelines. The resulting spectra will be analysed in terms of spectral
slope, taxonomic class, and key spectral features, and compared statistically with existing
datasets to identify systematic trends across the NEA population. Applied to the combined
NEOROCKS, NEOPOPS, and VLT datasets, this approach will enable a statistically sound
comparison between NEAs and Main Belt Asteroids, providing new observational constraints
on the role of space weathering and surface rejuvenation processes in shaping the spectral
diversity of the NEA population.

  Surface Composition and Space Weathering of Apophis: Hyperspectral Observations with ESA Ramses/HAMLET and Cross-Calibration (Monica Lazzarin, Fiorangela La Forgia)

The ESA Ramses (Rapid Apophis Mission for Space Safety) spacecraft will rendezvous with
the near-Earth asteroid (99942) Apophis ahead of its exceptionally close flyby of Earth in
April 2029, at a distance of approximately 32,000 km — well within the geostationary belt.
Apophis is classified as an Sq-type asteroid, spectrally analogous to LL ordinary chondrites,
with a moderately space-weathered surface that may be substantially resurfaced by tidal
forces during the encounter, potentially shifting its spectral signature toward a fresher
Q-type. Among its instruments, Ramses carries HAMLET (HyperScout for Apophis

MultispectraL Exploration and Taxonomy), an advanced hyperspectral imager operating
across two channels — 650–950 nm and 900–1700 nm — enabling mineralogical mapping
including key absorption features of olivine, ortho- and clinopyroxene, as well as hydrated
phases, with significantly broader spectral coverage than its predecessor HyperScout-H
aboard Hera. This PhD project addresses three interconnected scientific and technical
challenges. First, the extended spectral range of HAMLET requires a rigorous
cross-calibration strategy with respect to HyperScout-H, in order to ensure photometric and
spectral consistency between the two datasets and to anchor HAMLET's Channel 2 (NIR
beyond 960 nm) to well-characterised laboratory and in-flight references. Second, leveraging
the spectral dataset acquired by Hera at Didymos–Dimorphos — both S-type bodies sharing
taxonomic affinity with Apophis — we will develop a machine learning transfer learning
framework, based on spectral domain adaptation, to simulate and predict the hyperspectral
response of HAMLET at Apophis prior to arrival, enabling the pre-definition of optimal
observing strategies and data reduction pipelines. Third, the HAMLET data cubes will be
analysed to map spectrally distinct surface units and track spatial variations in key spectral
parameters — including spectral slope, band depth, and olivine-to-pyroxene ratios — across
the surface of Apophis. By comparing the spectral state of Apophis before and after the
closest approach, this project aims to provide the most direct observational test to date of
the role of planetary encounters in refreshing the surfaces of near-Earth asteroids and
driving the Sq-to-Q spectral transition — one of the key open questions in asteroidal space
weathering.

  Hyperspectral Surface Mapping of the Didymos–Dimorphos System: Compositional Analysis and Machine Learning Approaches from ESA Hera Mission Data (Monica Lazzarin, Fiorangela La Forgia)

The ESA Hera mission represents the first planetary defence spacecraft designed to
characterise in detail the near-Earth binary asteroid system (65803) Didymos–Dimorphos,
following the kinetic impact delivered by NASA's DART spacecraft in September 2022.
Scheduled to reach the Didymos system in late November 2026, Hera will carry out a
six-months proximity science campaign aimed at measuring the mass of Dimorphos,
characterising the DART impact crater, and investigating the surface and interior
composition of both bodies. Among its payload, the HyperScout-H (HS-H) hyperspectral
imager will acquire simultaneous spatial and spectral data in the 0.65–0.95 μm wavelength
range, providing key constraints on surface composition, space weathering effects, and the
potential presence of exogenous material deposited by the impact. This PhD project focuses
on the processing and scientific exploitation of the HS-H hyperspectral data cubes to
produce high-resolution compositional maps of the surfaces of Didymos and Dimorphos. The
analysis will include the derivation of key spectral parameters — such as spectral slope,
band depth, and reflectance — and their spatial distribution across both bodies, with
particular attention to the contrast between the fresh, unweathered crater material and the
surrounding space-weathered regolith. Since models of binary formation predict that
Dimorphos originated from Didymos, comparing the spectral properties of the two bodies
offers a unique opportunity to test this hypothesis and to constrain the resurfacing induced
by the DART impact. To handle the high dimensionality of hyperspectral data cubes,
dimensionality reduction techniques will be applied prior to clustering to mitigate the curse of
dimensionality. Unsupervised machine learning algorithms will then be used to identify
spectrally distinct surface units, while approaches that jointly exploit spectral and spatial
information will be explored to detect surface patterns not recoverable through spectral
analysis alone. The results will contribute to a deeper understanding of S-type asteroid
composition, impact-driven resurfacing processes, and the broader validation of kinetic
impactor deflection as a viable planetary defence strategy.

  Temporal variability of TeV blazars: timing and multi-frequency studies in the CTAO era (Elisa Prandini)

This PhD project aims to investigate the temporal variability of TeV blazars using very-high-energy gamma-ray data from current (MAGIC) and next-generation instruments (CTAO, ASTRI) as well as data in infrared to gamma-ray bands. Blazars exhibit strong variability across all wavelengths, and studying this behavior provides key constraints on particle acceleration and emission mechanisms. The project will focus on characterizing variability over multiple timescales, from intra-night to long-term trends. Advanced statistical techniques (e.g. power spectral density, structure function) will be applied to quantify variability properties. A multi-frequency approach will be adopted, combining TeV data with observations at lower energies. Cross-correlation analyses will be used to probe connections between emission regions. The results will be interpreted within different emission scenarios. 

This work will help constrain the physical processes in relativistic jets. It will also contribute to the development of analysis strategies for CTAO. Overall, the project lies at the intersection of high-energy astrophysics, time-domain astronomy, and statistical data analysis. 

  Measuring the bar pattern speed evolution across cosmic time with Euclid (Enrico Maria Corsini, Jairo Mendez Abreu)

The bar pattern speed is a key parameter characterising the dynamical state of galactic bars. Theoretical arguments and numerical simulations suggest that its time evolution is closely connected to dynamical friction and angular momentum exchange with the surrounding dark matter halo in which the bar forms. Observational measurements of bar pattern speeds as a function of redshift therefore provide important constraints on models of galaxy formation and the secular evolution of barred galaxies. In this thesis, we aim to investigate the evolution of bar pattern speeds with redshift by exploiting morphological measurements of low-inclination ringed galaxies from the Euclid First Data Releases. Deep neural networks will be used to identify the sample galaxies out to a redshift of 1, corresponding to the last 7 Gyr. Their optical images will be analysed to measure the ratio between the deprojected outer ring radius and the bar size, a quantity commonly used as a proxy for the dark matter fraction within the bar region. This will enable the first statistically significant investigation of the dynamical evolution of barred galaxies across cosmic time.

  Multi-messenger Studies of Active Galactic Nuclei (Elisa Bernardini)

Cosmic rays reach Earth with energies up to hundreds of EeV, but their production sites remain unknown. Multi-messenger astrophysics combines information from different "messengers" to solve this mystery. Neutrinos are particularly important as they are exclusively produced through hadronic interactions, making neutrino sources a "smoking gun" for cosmic ray origins. However, neutrino detection is challenging due to weak fluxes and high backgrounds. Multi-wavelength correlation studies help identify neutrino sources, as demonstrated by the 2017 discovery of the blazar TXS 0506+056 and the recent association of the Seyfert galaxy NGC 1068 with neutrino emission. Both sources account for only a small fraction of the total cosmic neutrino flux observed by IceCube, suggesting many sources remain undiscovered.

This project focuses on modeling the spectral energy distribution of Active Galactic Nuclei using leptonic and hadronic emission processes. The goal is to identify correlations between electromagnetic flux at different wavelengths and neutrino flux, and study their temporal evolution. The ultimate aim is to support targeted neutrino searches with telescopes like IceCube and KM3NeT, and guide electromagnetic follow-up campaigns by partner instruments.

  Physics of strongly magnetized neutron stars: theory and observations (Roberto Taverna, Roberto Turolla)

Summary: This PhD research project focuses on the theoretical and observational properties of X-ray emission from highly magnetized neutron stars: magnetars and XDINSs. Building on the landmark success of the NASA-ASI IXPE mission, which opened the era of X-ray polarimetry, the candidate will be tasked with advancing current numerical tools and developing innovative simulation facilities. A primary objective is to produce high-fidelity numerical models capable of interpreting existing IXPE data while providing predictive power for upcoming missions. Strong emphasis will be placed on the development of new simulations in preparation for the launch of the Chinese Academy of Sciences' eXTP observatory and other next-generation facilities like the ESA proposed mission EXPO. By bridging the gap between complex plasma physics in a strongly magnetized medium and polarimetric observables, the project aims at decoding the extreme environments of these compact stars within the evolving landscape of high-energy astrophysics.

  Multi-wavelength catalogs and modeling for the CTAO extragalactic survey (Michele Doro)

The upcoming extragalactic survey of the Cherenkov Telescope Array Observatory (CTAO) will provide an unprecedented view of the high-energy gamma-ray sky. To fully exploit these observations, a comprehensive multi-wavelength (MWL) catalog of extragalactic sources is required. This project will contribute to the development of a “super-catalog” combining observational data and physical modeling across the electromagnetic spectrum. The student will use the Firmamento portal to collect MWL data and redshift information for candidate sources and integrate them into a standardized database. In parallel, the project will perform time-resolved spectral energy distribution modeling using the Markarian Multi-wavelength Data Center (MMDC). The final goal is to build tools and workflows to connect MWL observations, modeling results, and CTAO survey predictions. The project combines astrophysical data analysis, scientific programming, and multi-wavelength modeling, contributing to the preparation and scientific exploitation of the CTAO extragalactic survey.

Useful links for background
- Cherenkov Telescope Array Observatory (CTAO): https://www.ctao.org
- Firmamento multi-wavelength portal: https:/firmamento.space
- Markarian Multi-wavelength Data Center (MMDC): https://mmdc.am/

  Open tools for interpreting Dark Matter constraints from gamma-ray and multi-messenger searches (Michele Doro)

Astrophysical and laboratory searches for particle Dark Matter produce numerous experimental limits that constrain possible Dark Matter models. In particular, gamma-ray observations provide one of the most powerful probes, since annihilation or decay of Dark Matter particles is expected to produce high-energy photons observable from targets such as dwarf spheroidal galaxies or the Galactic Center. This project aims to develop open computational tools to collect, standardize, and interpret constraints from different Dark Matter searches. The student will contribute to expanding the gDMbounds open repository, building a database of experimental limits from gamma-ray experiments (including CTA) as well as from direct detection, collider, and other indirect searches. A key objective is to implement tools that allow recasting experimental limits: starting from published constraints from one experiment, the software will enable their reinterpretation for different Dark Matter models or the estimation of the expected sensitivity of future instruments. The project involves scientific programming in Python, open-source development on GitHub, and data visualization, ultimately transforming the repository into an open platform where Dark Matter constraints can be explored, compared, and recomputed interactively.

Useful links for background:
- gDMbounds repository: https://github.com/micheledoro/gDMbounds

- Cherenkov Telescope Array Observatory: https://www.ctao.org

- Example CTA Dark Matter study: https://academic.oup.com/mnras/article/544/3/2946/8293234

  Relativistic effects in galaxy surveys (Daniele Bertacca)

Maps of the Universe based on galaxy redshifts are distorted by several relativistic effects. LIGER takes a (N-body or hydrodynamic) Newtonian simulation as an input and outputs the distribution of galaxies in comoving redshift space, e.g. see Borzyszkowski, Bertacca & Porciani (2017),  Elkhashab, Porciani & Bertacca (2022, 2025).
This result is achieved by making use of a coordinate transformation and simultaneously accounting for lensing magnification. The calculation includes both local corrections (i.e. peculiar velocities, dipole velocity and Sachs Wolfe effect) and terms that have been integrated along the line of sight (e.g. integrated Sachs Wolfe effect, lensing convergence, magnification and time delay).
In general, in a wide-angle survey, peculiar-velocity and dipole effects are not accurately described by the Kaiser limit at very large scales. The aim of this project is to measure the impact of redshift-space distortions, both the local and non-local terms, on the monopole of the galaxy power spectrum that will be measured in a Euclid-like survey.

  Multi-messenger studies of Active Galactic Nuclei (Elisa Bernardini)

Cosmic rays are protons and nuclei reaching Earth with energies up to hundreds EeV, while their production sites remain today an unsolved mystery. Multi-messenger astrophysics aims to solve this puzzle by combining information from different ”messengers”. Among these, neutrinos play a fundamental role, being produced exclusively in astrophysical processes involving the interactions of hadrons. The identification of sources of neutrinos represents therefore a “smoking gun” of production sites of cosmic rays. Detecting neutrinos is however challenging, due to weak fluxes underneath overwhelming backgrounds, but the identification of sources of neutrinos is effectively aided by correlation studies using multi-wavelength data. This approach was proven by the discovery of the first astrophysical source of neutrinos in 2017, the blazar TXS 0506+056, found in a flaring state in gamma-rays. More recently, an astrophysical source of a different class, the Seyfert galaxy NGC 1068, also classified as a starburst, was associated by IceCube to the emission of cosmic neutrinos. In both cases the observed fluxes accounts for a negligible fraction of the total diffuse flux of cosmic neutrinos observed by IceCube since 2013, leaving significant room for new discoveries. This project focuses on the modelling of the spectral energy distribution of Active Galactic Nuclei using both leptonic and hadronic emission processes. The main goal is to identify global correlation features in the electromagnetic flux at different wavelengths and the associated neutrino flux and to study their temporal evolution. The ultimate goal is to aid targeted searches of neutrinos signals from selected astrophysical targets using neutrino telescopes like IceCube and KM3NeT and guide observation strategies for follow-up electromagnetic campaigns by partner astronomical instruments.

  Constraining the Dust Attenuation Curves of Galaxies at 2 < z < 12 with JWST (Giulia Rodighiero, Paolo Cassata, Benedetta Vulcani, Laura Bisigello)

This PhD project aims to investigate the shape and evolution of dust attenuation curves in galaxies across cosmic time (2 < z < 12), using rest-frame UV-to-optical spectra from JWST/NIRSpec and JWST/NIRCAM-WFSS obtained through archival programs and from various surveys in which the supervisors are involved (e.g. CEERS, POPPIES). The candidate will build a homogeneous galaxy sample spanning wide ranges in stellar mass, star formation rate, and redshift. By applying and extending methods from local studies (e.g., Balmer decrements and UV slopes), the project will derive selective attenuation curves and study their dependence on galaxy properties. A key objective is to determine whether the Calzetti-like attenuation law holds at early epochs or if significant deviations emerge with redshift or galaxy environment. Statistical techniques will be used to control for stellar population age and geometry. The project offers opportunities for collaboration with JWST team members and for incorporating deep learning methods to optimize attenuation modeling. Results will provide critical constraints on galaxy SED modeling and dust evolution in the early Universe.

  Revealing the Dust-Obscured Nature of High-Redshift Galaxies with MIRI-JWST (Giulia Rodighiero, Laura Bisigello, Andrea Grazian, Paolo Cassata)

This PhD project aims to characterize the physical properties of faint, dusty, high-redshift (2 < z < 12) galaxies using archival and collaboration-based JWST/MIRI observations. Building on recent dropout-based selections (e.g., F200W-dropouts from CEERS), the candidate will combine mid-IR MIRI photometry with NIRCam imaging and available NIRSpec spectroscopy to perform detailed SED fitting. The goal is to constrain stellar masses, dust attenuation, star formation histories, and AGN activity in extreme populations such as ultra-high-redshift candidates. The project will explore the prevalence and nature of dust in galaxies previously missed in UV/optical surveys and assess their contribution to the cosmic star formation rate density. Machine learning and stacking techniques may be employed. The candidate will contribute to large JWST collaborations and lead a unique effort in understanding dust-obscured galaxy evolution at early times.  The candidate will be also involved in ALMA collaborations that provide direct submillimeter counterparts to the dusty candidates (e.g. the recent CHAMPS survey).

  Galaxy Formation and Evolution with Euclid (Giulia Rodighiero, Paolo Cassata, Laura Bisigello, Andrea Grazian)

This PhD project will be developed within the Euclid Consortium to study galaxy formation and evolution using Euclid’s unprecedented imaging and spectroscopy over wide cosmological volumes. By combining photometric and spectroscopic data, the candidate will investigate how galaxy properties—such as mass, morphology, star formation, and quenching—are shaped by their environment, from dense clusters to cosmic voids. The project will leverage Euclid’s large-scale structure mapping and multi-wavelength synergies with ground- and space-based surveys. Depending on the candidate’s interests, the focus can range from statistical population studies to detailed modeling of galaxy physical parameters or machine learning techniques for classification. The student will become a formal member of the Euclid consortium and he/she will be  actively involved in the Euclid Galaxy Evolution Science Working Group, contributing to the  early science phases of the mission.

  Probing Atomic Gas in Galaxies in the local Universe and Beyond with HI Surveys (Giulia Rodighiero, Isabella Prandoni, Francesco Sinigaglia)

This PhD project aims to investigate the evolution of atomic hydrogen (HI) in galaxies in the Local Universe or beyond (z ≳ 0.2) using spectral stacking techniques and deep HI surveys such as MeerKAT/MIGHTEE, uGMRT, and VLA. The candidate will construct statistically significant galaxy samples by combining spectroscopic redshifts and multi-wavelength photometry to derive HI–stellar mass scaling relations. A key goal is to study how HI content varies with galaxy properties (e.g., stellar mass, SFR, morphology) and environment (e.g., groups, filaments). The student will use and further develop stacking pipelines to recover average HI masses where direct detections are not feasible. The project also involves reduction and analysis of proprietary HI data in the Euclid Deep Field South. Depending on interest, the project may include machine learning tools or simulations to interpret the gas dynamics and baryon cycle. This work will contribute to our understanding of cold gas evolution leading up to the SKA era.

  Probing Cosmic Microwave Background anomalies (Nicola Bartolo)

The Cosmic Microwave Background (CMB) radiation is a privileged laboratory to study the initial conditions of the universe, its composition and evolution. At present there are several hints of statistical anomalies in the properties of the CMB fluctuations w.r.t to the standard model of Cosmology, especially on the largest angular scales. Even though their statistical significance is not high, such anomalies are interesting in that they might reveal new physics beyond the standard cosmological model.  Systematics might be a possibility, still up to now all the explanations in this sense have not been satisfactory, and moreover such anomalies have been reported independently both by the WMAP and the Planck satellite, two instruments with different systematics. The aim of this PhD project is twofold. On the one hand an investigation of possible (cosmological) effects able to explain such anomalies will be developed. Possible scenarios to be analyzed include both early universe conditions and low redshift evolution.  On the other hand, we aim at investigating alternative observables able to better characterize the nature of these anomalies (e.g., fully exploiting the CMB polarization information, also in view of future CMB experiments) or observables related to future galaxy, radio, and gravitational-wave datasets, such as Euclid, SKA, Lisa and ET.

  Cosmic Microwave Background (CMB) birefringence: theory and observations (Nicola Bartolo)

In the last 5 years there has been an increasing evidence of what is called CMB birefringence, namely a rotation of the linear polarization of CMB photons while they propagate, from their emission (at the last scattering surface) up to observation. Such a non-vanishing polarization rotation angle is at present detected at the level of up to 3.6 sigma. Such an effect can be the tracer of new physics,  e.g. parity-violating extensions of standard electromagnetism and could probe the existence of a new cosmological field acting as dark matter or dark energy. It has become customary to employ Cosmic Microwave Background (CMB) polarised data to probe such a phenomenon. Future CMB surveys (like the next CMB satellite LitBIRD, devoted to CMB polarization) will have the capacity to dramatically improve the sensitivity to such an effect.  The PhD project thesis will deal with both theoretical and phenomenological/observational aspects of such a phenomenon.

  Investigating the primordial stochastic gravitational wave background (Nicola Bartolo)

Two years ago various international collaborations, exploiting pulsar timing arrays, have measured for the first time a stochastic gravitational wave background. Its origin is still to be precisely defined and besides supermassive black holes, a cosmological origin is at present compatible with data. The PhD thesis will focus on both theoretical and phenomenological aspects  that can further open the way to distinguish between different types of stochastic backgrounds of gravitational waves, focusing in particular on their primordial origin. Various observables can be investigated, as well their specific imprints over an enormous range of frequencies, from their possible imprints on Cosmic Microwave Background polarization, to Pular Timing Arrays, and direct future interferometric measurements (Einstein Telescope and LISA). 

  Towards fully simulating the variability of stellar populations (Michele Trabucchi, Leo Girardi, Diego Bossini)

Stellar variability, either due to stellar oscillations or binary processes, is an extremely valuable tool to study the structure and evolution of stars and galaxies. Measuring the period of pulsating stars allows a determination of their intrinsic brightness, thereby providing a way of characterising the distance and age of the stellar population they belong to. Solar-type and red giant stars, as well as some compact stellar remnants, display rich spectra of low-amplitude radial and non-radial oscillations that can be exploited to probe their interior structure. The variability of binary stars can provide information on the history formation, evolution and mass transfer in multiple stellar systems. Many distinct theoretical and empirical models exist to describe the variety of stellar variability phenomena that we observe, but a tool homogeneously incorporating their predictions does not currently exist. It will be the PhD student’s task to gather such models from the literature, complementing them with new calculations through state-of-the-art public software for the simulation of stellar oscillations. Then, the student will implement these models into the TRILEGAL code developed within the Stellar Physics group, a tool for the simulation of stellar populations in galaxies and clusters. Finally, the student will compute such simulations and compare and constrain the novel results against observations from the most recent time-domain astronomical surveys, such as OGLE, Gaia, ZTF, LSST, Kepler, TESS.

  The role of stellar rotation on stellar population models (Guglielmo Costa, Leo Girardi, Alessandro Mazzi)

Hubble Space Telescope data for star clusters in the Magellanic Clouds made crystal clear that rapidly rotating stars are much more common than previously thought. However, most interpretative tools of stellar populations (e.g. age estimates based on the HR diagram or on the integrated spectra of galaxies) completely ignore the presence of rotating stars. To fix this situation, our team has started a deep revision of the PARSEC database of stellar models, with the consideration of rotation on the stellar evolution, on the stellar spectra, and in the surface chemical abundances. In this PhD project, we will complete the transition to stellar population models that fully include the impact of rotation, hence providing an extremely useful database to the astrophysical community. There is plenty of public and proprietary data on which our models can be calibrated, including HST imaging and spectra of Magellanic Cloud star clusters, Keck spectroscopy of giants in nearby galaxies, and the broadening of spectral lines from Gaia. Moreover, new data from JWST and EUCLID will possibly be available soon as well as asteroseismic inferences on the internal rotation from the Kepler and TESS satellites.

  Constraining Asymptotic Giant Branch models at solar and super-solar metallicity with resolved stellar populations in M33 and M31 (Michele Trabucchi, Leo Girardi, Giada Pastorelli)

The thermally-pulsing asymptotic giant branch (TP-AGB) is one of the most challenging evolutionary phases to model due to the complexity of physical processes such
as internal mixing episodes, mass loss, variability, and dust formation. To constrain stellar models, comparing predictions with observational data is necessary. Resolved stellar populations data has proven successful in providing critical constraints to the models. The Triangulum Galaxy (M33) and Andromeda Galaxy (M31) are ideal candidates to put stringent constraints to models at solar- and super-solar metallicity, with high-quality data from the Hubble Space Telescope already available (in the surveys PHAT, PHATTER, PHAST and their extensions). The project aims to perform accurate stellar population synthesis simulations of M31 and M33 using the TRILEGAL code, which incorporates state-of-the-art AGB models. The data-model comparison will inform the computation of new AGB models at solar- and super-solar metallicity able to reproduce the target galaxies. This project is part of an ongoing effort to provide the astronomical community with calibrated and well-tested stellar evolutionary tracks and stellar isochrones, used in many astrophysical applications (distance scale determination, interpretation of integrated light of high-redshift galaxies, chemical evolution of galaxies). The PhD student will be supported by members of the Padova research group, experts in stellar evolution and stellar populations modelling, and encouraged to work with and visit our collaborators in the USA (at STScI - Baltimore, CCA Flatiron - New York, University of Washington - Seattle).

  Refreshing stellar evolution in the light of new opacities (Guglielmo Costa, Leo Girardi, Diego Bossini)

Rosseland mean opacities are a fundamental ingredient of stellar models and stellar evolutionary codes. Several recent developments reveal that presently-available opacity tables and interpolation codes are not exactly “well established” and accurate. Even for the Sun, there is a long-standing discrepancy between solar models and the speed of sound revealed by helioseismology, which is possibly associated with inaccurate opacity tables. The situation becomes even more uncertain for stars that have significant changes in the chemical composition of their envelopes, like for instance fast-rotating stars and the products of close binary evolution. In this project, we will leverage the available tools for the fast computation of opacity tables, including our code AESOPUS at low temperatures, and TOPS tools at high temperatures, to explore the uncertainties associated with the opacity tables and their interpolation. The PhD student will make extensive use of the PARSEC stellar evolution code, aiming at a significant revision and extension of our present databases of stellar evolutionary tracks and isochrones.

  Supermassive Black Holes in the Early Universe: Physics and Rapid Cosmological Evolution (Eugenio Bottacini)

Constraining the physics of supermassive black holes (SMBHs) in the early Universe and understanding their rapid cosmological evolution to masses of the order of 10^9 Msun remains a major challenge. However, blazars that are galaxies with jets oriented toward the observer, offer valuable insight. Simulating the physical processes responsible for emission across the entire electromagnetic spectrum, from radio waves to gamma rays, enables constraints on SMBH physics. This, in turn, allows for modeling their cosmological evolution with updated physical parameters. The aim of this project is to constrain the physics of SMBHs in the early Universe and model their growth from a seed mass of M = 10^6 Msun at z = 30 to M = 10^9 Msun at z = 3–4. The ideal PhD candidate is expected to learn to use simulation software and contribute to a larger research project in SMBH science.

  Globular Clusters as Windows on Near-Field Cosmology (Antonino MIlone, Anna Marino)

Globular clusters are among the oldest stellar systems and serve as fossil records of the early Universe. Understanding their origin is key to major cosmological questions: How did they form? What role did they play in building the Galactic halo? Did they contribute to cosmic reionization?
This PhD project tackles these topics by investigating multiple stellar populations in globular clusters. Our group has developed powerful tools combining spectroscopy and multi-band photometry, which have transformed the field.
The candidate will apply these methods to analyze UV, optical, and IR data from  space telescopes and wide-field ground-based facilities. A key focus will be on new deep observations from James Webb Space Telescope Cycle 4 and 6 (Proposal ID #8960, PI: Milone), targeting low-mass stars to probe the origin of multiple populations.
This research will shed light on star formation at high redshift, the assembly of the Milky Way, and the role of globular clusters in early cosmic evolution—advancing our understanding of near-field cosmology with cutting-edge data. The project offers a unique opportunity to work at the frontier of near-field cosmology using the most advanced observational datasets available.

  Binaries, Extended Turn-Offs, UV-Dim Stars, and Other Exotic Phenomena in Star Clusters (Antonino Milone)

In recent years, a series of groundbreaking discoveries has revolutionized our understanding of the formation and evolution of stars and stellar populations. These include the detection of split main sequences and extended main sequence turn-offs in young star clusters, as well as the identification of UV-dim stars, blue plumes, zig-zag patterns along the main sequence, and other exotic phenomena that challenge the predictions of standard stellar evolution models.
The candidate will investigate these phenomena using data from our extensive surveys of globular and open star clusters in the Milky Way and the Magellanic Clouds, complemented by additional imaging datasets. The project will involve applying state-of-the-art data reduction and analysis techniques and will include collaboration with leading experts in the field. A central component of the research will focus on new observations from the James Webb Space Telescope, obtained through the Cycle 4 program "The Missing Link for Understanding Multiple Populations in Star Clusters" (ID #9012, PI: Milone).

  Dynamics of Milky Way Satellites and Their Stellar Populations (Antonino Milone)

This project aims to investigate the dynamics of star clusters and dwarf galaxies orbiting the Milky Way by exploiting high-precision stellar astrometry from Gaia, the Hubble and James Webb Space Telescopes, and wide-field facilities from both ground-based and space-based observatories.
The candidate will develop expertise in advanced techniques of image analysis and data reduction, focusing on the measurement of stellar proper motions. This includes both relative motions within individual stellar systems and absolute motions of Galactic satellites. By combining astrometric data from multiple observatories and applying innovative analysis methods, the candidate will constrain the orbits of Milky Way satellites as well as the motions of stellar populations and peculiar stars within clusters.
Key goals of the project include:
– Investigating the internal kinematics of multiple stellar populations in globular clusters to gain insights into their origin, evolution, and role in Galactic assembly and cosmic reionization.
– Studying the velocity distribution of stars in Milky Way satellites to understand their dynamical evolution. Proper motion data will also be used to search for signatures of dark compact objects, including stellar-mass and intermediate-mass black holes.

  Validation and ranking of exoplanetary candidates from space-based missions (Giampaolo Piotto, Giacomo Mantovan, Domenico Nardiello)

The advent of photometric, large-scale, space-based surveys like TESS and the upcoming PLATO is dramatically increasing the number of known exoplanets and exoplanetary systems, as well as planet candidates and false positives.
To efficiently prioritize candidates for follow-ups and further characterization, we need to validate and rank them using statistical analyses that compare their properties with known exoplanets. Validation is an essential tool that allows us to
identify the most promising candidates and optimizes the use of observing time. The student will analyze planetary candidates with state-of-the-art software and develop algorithms based on AI capable of untangling planetary signals from false positives.
The student will apply these software tools to TESS and PLATO data, including additional information from different sources (e.g., Gaia). The student will also be actively involved in the follow-up activities our group promotes, including
observations at the telescope.

  Exoplanet search using TESS in preparation of the PLATO mission (Domenico Nardiello, Valerio Nascimbeni (INAF), Giampaolo Piotto)

This is a thesis to exploit TESS data to search for transiting exoplanets and variable stars. The space mission TESS has discovered thousands of candidate exoplanets by surveying over 95% of the sky and many other discoveries are expected.
In this context, the student will develop tools for photometric extraction, correction, and analysis of TESS stellar light curves, particularly for PLATO targets within the LOPS2 field. These tools will also make use of AI routines, to optimize the required results. Key tasks of the project include identifying planetary transit signals and variable stars, vetting high-confidence planetary candidates, and determining accurate parameters of TESS planetary candidates and their star hosts. Most promising newly-discovered planets would be also proposed for observations with CHEOPS (an operating ESA mission in which our group is deeply involved), and for radial velocity follow-ups with HARPS-N. This research is crucial for the preparation of the PLATO mission (launch end-2026), which will search for habitable rocky planets and in which our group is deeply involved. The thesis will contribute to the detailed characterization of PLATO targets and the detection of TESS long-period mono-transit candidates that will be confirmed by PLATO.

  Exoplanets around young stars (Domenico Nardiello, Luca Malavolta, Giacomo Mantovan)

The accurate knowledge of the ages of stars hosting planets allows us to know in detail how planetary systems form and evolve. Accurate and precise age estimates of the stars in the Milky Way can be only possible for (coeval) members of stellar systems like open clusters, associations and co-moving groups. Looking for exoplanets around stellar cluster members has two advantages: (i) the stellar (and consequently the planet) parameters are well constrained (ii) looking to exoplanets around stars with different ages (from few Myr up to some Gyr) allows us to follow the evolution of the exoplanetary systems in different environments.
The PhD project aims to identify, validate, and characterize exoplanetary systems around young stars (&lt;1 Gyr) using over seven years of TESS data and complementary datasets. The student will identify young stars using updated
astrophotometric catalogues (e.g., Gaia), analyse light curves, detrend stellar activity, and discover new transiting exoplanets by using machine learning techniques. The goal is to analyze young planetary systems, compare them to older systems, and develop tools for the PLATO mission. The student will join an international collaboration with significant involvement in PLATO and ground-based follow-up facilities.

  Artificial Intelligence to discover new exoplanets (Tiziano Zingales, Luca Malavolta, Giampaolo Piotto)

Around 7500 exoplanets have been discovered in the Milky Way, and this number continues to grow. The rapid expansion of astronomical data in recent decades has driven the exoplanetary community to develop increasingly efficient analysis tools.
With the PLATO space mission set to launch in 2026, tens of thousands of new exoplanets are expected to be found, many within the habitable zone. To fully exploit the scientific potential of this mission, the development of an advanced artificial intelligence algorithm is proposed. This AI will simulate realistic transit light curves using the PLATOsim tool, process and clean the resulting data, and be trained to detect planetary signals buried in noise and stellar variability. Using state-of-the-art machine learning and deep learning techniques inspired by computer vision, the algorithm will be optimized for accuracy and efficiency. Designed for scalability and minimal human intervention, the final product will automate the exoplanet discovery process. Once validated on PLATO data, the tool can be extended to other missions
such as Kepler, TESS, and CHEOPS, broadening its impact across the field.

  Population study on exoplanetary atmospheres - Towards a deeper understanding of planetary existence (Tiziano Zingales, Valerio Nascimbeni -INAF-)

Atmospheric characterisation of exoplanets is key to understanding their composition and formation history. The James Webb Space Telescope (JWST), with its cutting-edge capabilities, is revolutionising this field through numerous successful transit observations, with many more expected. This project aims to deepen our understanding of atmospheric diversity, crucial to refining planetary formation models, and explore habitability. During this project, the candidate will extract and standardise all available JWST transmission spectra to ensure a uniform dataset free
from instrumental biases. Next, atmospheric retrievals will be performed using the TauREx code, applying varied models to identify key gases such as water vapour, CO₂, and methane. Finally, a comparative population analysis will reveal patterns and shared features across planetary atmospheres. The results will offer crucial insights into atmospheric processes and help constrain theories of planetary evolution.

  Exoplanet search and characterization using the TTV method (Valerio Nascimbeni -INAF-, Luca Borsato -INAF-, Giampaolo Piotto)

The transit time variation (TTV) technique probes planetary masses and orbits through gravitational interactions in multi-planet systems. We lead an ongoing program combining data from TESS, CHEOPS, and ground-based telescopes, supported by dedicated software for TTV modeling. The PhD project will build on this framework, focusing on the analysis of TTV signals from CHEOPS and TESS, in preparation for PLATO and Ariel. The student will gain hands-on experience with observations and join an international team leading TTV efforts for several space missions.

  Super-Eddington Accretion onto Supermassive Black Holes (Mauro D'Onofrio, Paola Marziani)

In recent years, a growing body of observational evidence suggests that supermassive black holes may undergo phases of super-Eddington accretion which seems necessary to explain their rapid  growth at early cosmic times.  A first goal of the  thesis is therefore to define multi-frequency selection criteria (involving  spectral energy distributions, emission line properties, and variability patterns) to make it ossible the reliable identification of super-Eddington candidates in large surveys such as SDSS and DESI. The student will afterwards focus on three key aspects of  super-Eddington accretion: (1) the accurate estimation of accretion parameters — refining black hole mass and Eddington ratio estimates through multi-component spectral fitting and empirical correlations, with particular attention at viewing angle effects; (2) the dynamics of the wind — using velocity shifts and profiles of optical and UV emission lines  to characterize outflows driven by radiation pressure; (3) the chemical composition of the line-emitting gas — investigating metallicity-sensitive diagnostics to infer enrichment and evolutionary status, in connection with recent scenarios proposing nuclear star formation in the outskirts of an advection dominated accretion flow. The student will work on a gold sample of several tens of super-Eddington candidates for which proprietary, dedicated observations were obtained (VLA, ESO/VLT XSHOOTER, GTC/Osiris) as well as on survey data. Depending on the student background and interest, the  analysis might be purely observational or more oriented toward dynamical and photoionization modeling, or modelization of accretion-modified stars. The student will benefit from a steady collaboration of the supervisors with astronomers at Gemini/NoirLab, Belgrade Observatory and University, Instituto de Astrofísica de Andalucía, the Instituto de Astronomía of UNAM, among others.

  The environment and the morphology of Active Galactic Nuclei Hosts along the Eigenvector 1 sequence (Mauro D'Onofrio, Paola Marziani)

This thesis will explore the host galaxy morphology and  environment of a spectroscopically selected sample of AGN organized along the Eigenvector 1 (E1) sequence. The project focuses on the physical link between the nuclear properties of quasars — such as Eddington ratio, occurrece and power of relativistic ejections,  chemical enrichment and the large-scale features of their host galaxies and surroundings. A particular emphasis will be placed on the interaction between radio jets and the ambient interstellar medium (ISM). The student will examine how radio morphology, jet orientation, and feedback signatures appear in special classes of type-1 AGN, and correlate with position along E1, using archival radio maps (e.g., VLA FIRST) and spectroscopic indicators of outflows or shocks, part of them already available from SOAR dedicated observations.  In parallel, the host galaxy morphology and color will be investigated across the E1 sequence using multi-band imaging data (e.g., SDSS, Pan-STARRS). Tricolor composite maps will be used to trace dust lanes, star-forming regions, and structural asymmetries, helping to infer merger signatures, tidal features, or gradients in stellar population. A dedicated survey might be planned as part of the Ph.D. project.  The project is oriented toward image analysis and classification, as well as toward interpreting physical correlations across the AGN parameter space. The thesis will contribute to understanding how AGN activity — especially radio-mode feedback, due to weakly active supermassive black holes — is shaped by and shapes its galactic environment. 

  Exploring the low-surface brightness universe with new generation all-sky surveys (Enrico Maria Corsini, Enrichetta Iodice - INAF-)

The new generation of all-sky surveys provided by Euclid and Vera C. Rubin Observatory will explore the structures in the Universe down to the faintest surface brightness levels, where the relics of the galaxy mass assembly reside and allow to constrain their build up within the Lambda Cold Dark Matter (LCDM) paradigm. Present deep imaging and spectroscopic surveys have largely enhanced the detection and characterization of the galaxy outskirts, intra-cluster light (ICL) and low-surface brightness (LSB) galaxies. The similarities between the present and planned surveys has valuable advantages: existing data provide a preview of the science that will soon be delivered by the new surveys and represent test beds for building up the knowledge required for managing the upcoming massive data-sets, also with the aid of tailored numerical simulations. Our main science goal is to study the galaxy mass assembly in different environments, by extensive analyses of the light and color distributions of the stellar halos, ICL and LSB galaxies. This PhD project is part of larger scientific program, named VST-Early-type Galaxy Surveys (VEGAS, https://sites.google.com/inaf.it/vegas/home), which aims at studying the mass assembly of galaxies in groups and clusters using the deep imaging surveys at VST. The acquired know-how, tools, and scientific developments will be immediately transferred to explore the data of the new generation all-sky surveys boosting the study of galactic structures down to the LSB regime.

  Multi-phase galaxies in the primordial Universe (Cassata, Rodighiero)

Understanding the multiphase nature of galaxies in the early Universe is key to unveiling the processes that govern galaxy formation and evolution. In this PhD project, the candidate will combine high-resolution near-infrared imaging from JWST/NIRCam, spatially resolved spectroscopy from JWST/NIRSpec IFU, and submillimeter observations of the [C II] 158 μm line with ALMA to investigate the complex interplay between stars, ionized gas, molecular gas, and dust in galaxies at high redshift (z ≳ 4). NIRCam imaging provides detailed rest-frame optical morphologies and stellar mass distributions, while NIRSpec IFU data trace the ionized gas and nebular emission properties, allowing for independent estimates of recent star-formation activity. Complementary ALMA observations of [C II] allow us to probe the cool interstellar medium at sub-kiloparsec scales, offering crucial insight into the distribution and dynamics of the cold gas and its relation to star-forming regions. By integrating these multi-wavelength, multi-phase diagnostics, this work aims to constrain the physical mechanisms driving star formation, feedback, dust growth, and structural assembly in the first few billion years of cosmic history.