Recently, I've come to understand that authorship practices, such as the order of authors, can significantly impact job applications, particularly in astronomy-oriented fields. Therefore, I urge the need to clarify some important aspects related to these practices in my research papers.

Author ordering 

Author ordering in high-energy physics and gravitation is conventionally alphabetical, whereas in astronomy and astrophysics, it is based on contribution. Cosmology lies at the boundary of these fields, meaning that authorship practices are often mixed. 

In my works, different practices and ordering schemes have been adopted over the years, notably without following homogeneous rules, nor with guidelines being consistently implemented (whether for external collaborations or within the same research groups). 

To provide concrete examples, in rare cases, all authors contributed equally to the work, which is thus signed alphabetically. However, following the high-energy physics convention, papers have often been signed alphabetically despite a larger fraction of the work being carried out by one (or a subset of) author(s). Most times, a two-tier alphabetical ordering scheme (with two groups of people—those who contributed somewhat more to the work and those who contributed less) has been implemented, without weighting the individual contributions. In all these cases, my contributions could have been extremely relevant despite myself not being listed as the first (or among the first) author(s). Other times, none of these rules have been followed, and case-by-case decisions have been made regarding the author order. Fortunately, in these cases, I have never been listed before someone who contributed more than I did. However, I don't feel the reverse is necessarily always true. As I never cared much about author ordering, I never paid particular attention to ensuring this aspect was implemented consistently. 

As a result, I discourage inferring sensible information based solely on the author's ordering, as this can be a source of misunderstandings. Instead, I encourage referring to my contributions to each work, which are detailed on a paper-by-paper basis.

My Authorship policy

Unlike some author-ordering practices, my personal policy  (and ethics) for claiming authorship in papers has remained (and will remain) consistent over the years. It can be summarized by 3 simple rules, as follows:

1) I claim authorship only if I feel that my fractional contribution is of order 1/N, where N is the number of authors in the paper. Note that because of this rule, in the small N limit, the author's ordering becomes irrelevant. Conversely, in the large N limit, the rule itself becomes somewhat irrelevant, and I rely on the next two principles to decide whether to claim authorship or not.

2) I do not claim authorship without having actively worked on the paper (in the strictest sense).

3) I do not claim authorship based solely on sharing a code or a suggestion that can solve a problem, even when these are relevant for the paper to get done. Despite several invitations to be part of papers, in all cases when I was not able to actively work on the manuscript, I always declined authorship and opted to be included in the acknowledgments. 

The combination of these three rules has led me to be listed as an author only on papers where my contribution is real and relevant (and often larger than 1/N) — as any of the other authors involved can hopefully confirm. 

Important:  I would like to stress that this statement is not aimed at downplaying the importance of my collaborators. My intentions are
(a) - to clarify my contributions in the different papers to prevent other comments (aka feedback) from questioning my actual work;
(b) - to clarify my personal authorship policies as well as my past and future decisions concerning accepting/declining my authorship in papers.
Finally, I would like to conclude by thanking all my co-authors for the science we did together. From my point of view, science is and remains a collaborative effort, not an individual endeavor.

We study two parametric tests of gravity, the (μ, Σ) framework and the growth index γ, which modify aspects of the ΛCDM model's predictions for matter perturbation growth. These tests are motivated by results from the 2018 Planck-PR3 spectra, which suggest deviations from ΛCDM predictions at a 2.5σ significance. Using the updated Planck-PR4 spectra from NPIPE maps, we show that the latest data agree better with General Relativity, as constraints on Σ₀ and γ₀ fall within 1.5σ to 2σ of GR predictions. Alternative likelihoods (HiLLiPoP and LoLLiPoP) further confirm this, showing consistency with ΛCDM within 1σ. This improved consistency also corresponds with a reduction in the lensing anomaly, as Planck-PR4 data shows a reduced tendency for parameters to deviate from standard values.

My Contribution: I proposed and supervised the project, produced all figures, and contributed to the interpretation of the results. I made the primary contribution to writing the paper.

I test whether the preference for evolving dark energy is confirmed by CMB experiments other than Planck, finding that it is generally weakened. The Atacama Cosmology Telescope and WMAP data, when combined with DESI BAO and Pantheon-plus Supernovae, yield independent constraints with precision comparable to Planck, recovering the cosmological constant within two standard deviations. However, a preference for Dynamical Dark Energy reappears when Pantheon-plus is replaced by distance moduli measurements from the Dark Energy Survey Supernova Program (DESy5). In contrast, no preference for dynamical dark energy is observed in the South Pole Telescope data. I argue that Planck temperature and E-mode polarization anisotropy measurements at large angular scales strengthen the shift toward evolving dark energy.

We explore the implications of Redshift Space Distortion (RSD) measurements, both alone and in combination with CMB, Type-Ia Supernovae, and DESI BAO measurements, for Interacting Dark Energy (IDE) models, where energy-momentum flows either from Dark Matter to Dark Energy or from Dark Energy to Dark Matter. We show that in the first case, RSD can be very constraining on the amount of energy-momentum that can be exchanged in the Dark Sector of the cosmological model. In contrast, in the second case, RSD supports a non-vanishing energy-momentum flow at a confidence level of about two standard deviations. In this latter case, structure formation data are found to be in agreement with CMB data concerning the value of S8, underscoring that the model can address or at least alleviate the S8 tension.

My Contribution: I contributed to the interpretation of the results and the writing of the paper.

We investigate the impact of post-DESI BAO measurements on neutrino mass cosmology by incorporating additional available cosmological probes. We quantify the preference for the normal mass ordering over the inverted one, as well as the tension between cosmological and terrestrial data. Depending on the dataset combination and the tension metric used, the tension between cosmological and terrestrial observations ranges from 2.5σ to 5σ. These findings are reinforced when allowing for a time-varying dark energy component with an equation of state within the physically motivated non-phantom regime, w(z) ≥ -1, confirming the intriguing synergy between the nature of dark energy and laboratory probes of the mass ordering. If these tensions persist and cannot be attributed to systematics, it will necessitate a reevaluation of either standard neutrino (particle) physics or the underlying cosmological model, or both. 

My Contribution: At the early stages of this project, I performed exploratory MCMC runs, fully accounting for the DH, NH, and IH scenarios in both ΛCDM and w(z)CDM, with w(z) both in the phantom and quintessence regimes. These runs were subsequently used to plan the final strategy for the results involving DESI data, which were performed by Jun-Qian Jiang. I contributed to the analysis and interpretation of the results and to the writing of the paper.

We confirm the robust preference for dynamical dark energy identified in DESI BAO data and distance moduli measurements for Type Ia supernovae when combined with CMB observations. We demonstrate that assuming a specific parameterization to describe the evolution of the dark energy equation of state (EoS) has minimal impact on the overall preference of these data, which favor a present-day quintessence EoS that crossed the phantom barrier in the past. We also present statistical analyses to assess which parameterization is more suitable to fit the data, finding that a linear CPL model is not necessarily the favored choice.

My Contribution: I contributed to the analysis and interpretation of the results. I made the primary contribution to writing the paper.

We explore combining early and late-time new physics to resolve the Hubble tension. Specifically, we investigate models that have been effective either before or after recombination: a spatially uniform, time-varying electron mass (with non-zero spatial curvature) and a sign-switching cosmological constant causing an AdS-to-dS transition within the CDM model. Analyzing data from the Cosmic Microwave Background (CMB), Baryon Acoustic Oscillations, and Type Ia Supernovae, we find that no combination of these models can solve the Hubble tension. The matter density parameter is crucial, affecting significant physical scales in opposing ways. Despite the overall failure, we offer insights into model-building to address the Hubble tension.

My Contribution:  At early stages, I independently proposed the idea (although suggesting different early and late time models compared to those analyzed in the paper) to some of the collaborators involved in the project. I contributed to the analysis and interpretation of the results. I produced Figure 7 and contributed to the paper writing.

We propose a consistency test for ΛCDM, potentially able to clarify the nature of the Hubble tension and confirm or rule out new physics prior to recombination with a statistical significance of ∼4σ. In particular, we argue that forthcoming surveys such as LISA GW standard sirens and DESI or Euclid angular BAO measurements can be combined to achieve a model-independent measurement of the sound horizon with a relative precision of 1.5% within the redshift range z ≲ 1.

My Contribution: I proposed the project and conceptualized the methodology and analytical tools to implement it. I realized the different forecast data and likelihoods underling the study, performed the MCMC analyses, and produced Figure 1, Figure 2, Figure 5, and Figure 6. I made the primary contribution to writing the paper.

We explore the implications of Baryon Acoustic Oscillation measurements from the Dark Energy Spectroscopic Instrument (DESI) for Interacting Dark Energy (IDE) models, where energy-momentum flows from Dark Matter to Dark Energy. Combining Planck-2018 and DESI data, we find a preference for interactions beyond the 95% confidence level, leading to a present-day expansion rate of H0 = 71.4 ± 1.5 km/s/Mpc, perfectly aligned with SH0ES. This preference persists when including expansion rate measurements derived from the relative ages of massive, early-time, and passively-evolving galaxies, as well as distance moduli measurements from Type-Ia Supernovae in the Pantheon-plus catalog, calibrated using SH0ES Cepheid host distances. Overall, our findings suggest that high and low redshift data can be equally or better explained within the IDE framework compared to ΛCDM, while also yielding higher values of H0, in closer agreement with the local distance ladder estimate.

My Contribution: I proposed the project and conceptualized the methodology and analytical tools to implement it.  I implemented the DESI likelihood in Cobaya[*] and performed the MCMC analyses. I produced Figure 1 and Figure 2. I made the primary contribution to writing the paper.

[*] I cross-check I could reproduce all the results provided by the DESI collaboration in Tab.III of [arXiv:2404.03002]. Additionally, all the results in this paper have been independently cross-checked by Miguel A. Sabogal and Rafael C. Nunes using an independent likelihood for MontePython.

I review and discuss the possible implications for inflation resulting from considering new physics in light of the Hubble tension. I show that models with ΔNeff ≈ 0.3-0.4 (that could bring the tension down to 3σ while being moderately disfavored compared to ΛCDM) drastically change the constraints on inflation so that the most accredited scenarios (e.g., Starobinsky inflation) would no longer be favored by data. I then focus on Early Dark Energy, arguing that an EDE fraction of 0.4-0.6% (only able to mildly reduce the H0-tension down to ∼3σ) could already require a similar change in perspective on inflation. Performing a full joint analysis of EDE and Starobinsky inflation, I find that the two models can hardly coexist for f_EDE ≳ 0.06.

We present model-marginalized limits on the six standard ΛCDM cosmological parameters by considering three independent Cosmic Microwave Background experiments: the Planck satellite, the Atacama Cosmology Telescope, and the South Pole Telescope. We also consider low redshift observations in the form of Baryon Acoustic Oscillation data from the SDSS-IV eBOSS survey and Supernovae distance moduli measurements from the Pantheon-Plus catalog. We prove that marginalized errors are stable against the different fiducial cosmologies making irrelevant the choice of different possible cosmological scenarios once both high and low redshift probes are fully accounted for.

My Contribution: I performed all the MCMC analyses, computed the Bayesian Evidence and derived the parameter posteriors. I contributed to writing the paper.

We offer a thorough review of Interacting Dark Energy (IDE) cosmology, which explores models involving a non-gravitational interplay between Dark Matter (DM) and Dark Energy (DE). We expand the dark sector physics by considering two scenarios: one with a constant DE equation of state and another with a dynamic equation of state given by a CPL parameterization. In both cases, we identify two distinct physical regimes based on whether the equation of state resembles phantom or quintessence behavior. We examine various IDE models in light of Cosmic Microwave Background data from the Planck satellite and the Atacama Cosmology Telescope, both independently and combined with data from Supernovae and Baryon Acoustic Oscillations. Our analysis refines previous studies, narrowing down the parameter space for these models and indicating challenges in resolving cosmological tensions solely within the IDE framework.

My Contribution: I proposed the project and conceptualized the methodology and analytical tools to implement it.  I implemented the dynamical Dark Energy Equation of State for IDE and developed a novel sampling methodology that allows us to explore the quintessence and phantom regimes in the dynamical case properly. I implemented the different updated likelihoods in cobaya (Pantheon-Plus and updated BAO). I performed the vast majority of the MCMC analyses and created all figures. I made the primary contribution to writing the paper.

We investigate scale-invariant inflation, addressing the dynamics by solving the two-field trajectory to yield effective dynamics resembling that of a single field. This results in vanishing entropy perturbations and protects the model from destabilization effects. We establish stringent upper limits on the non-minimal coupling strength, excluding conformal coupling at a high significance level.  We demonstrate the model's robustness against initial conditions. We argue that the model predicts a minimal level of primordial tensor modes, well within the detectable range of upcoming CMB experiments.  

My Contribution: I contributed to the data analysis by applying the methodology that some of us developed in [arXiv:2306.12414]. I realized Fig.2, Fig.3, and Fig.4.  I significantly contributed to the paper writing.

We generalize the calculation of the spectrum of gravitational waves in a cyclic Universe, making no assumptions about the vacuum state of the theory and including the contribution of tensor modes produced during the dark energy phase of the previous cycle. We show that these modes have minimal impact on the spectrum observed in the current cycle, while avoiding backreaction effects sets restrictive constraints on deviations away from the Bunch-Davies vacuum during this phase, limiting the overall freedom to consider alternative vacua in the cyclic Universe.

My Contribution: I proposed the project. I contributed to the calculation. I gave the main contribution to the paper writing

We test α-attractor quintessential inflation in light of Cosmic Microwave Background measurements from the Planck satellite, the Atacama Cosmology Telescope, and B-mode polarization data from the BICEP/Keck collaboration – both alone and in combination with low-redshift observations. The model can provide equally good fits as ΛCDM for a broad range of parameter values.

My Contribution: I proposed the project and conceptualized the methodology and analytical tools to implement it.  I implemented the model and performed the MCMC analysis. I made the primary contribution to writing the paper.

We test alternative cosmological perturbation histories in light of the preliminary James Webb Space Telescope (JWST) data. We argue that models with a larger matter component and/or a larger scalar spectral index can substantially improve the fit to JWST measurements. In this regard, phenomenological extensions related to the dark energy sector of the theory are appealing alternatives, with Early Dark Energy emerging as an excellent candidate to explain (at least in part) the unexpected JWST preference for larger stellar mass densities.

My Contribution: I performed the MCMC analysis of Early Dark Energy and Interacting Dark Energy. I contributed to the JWST data-analysis. I made the primary contribution to writing the paper.

We study the possibility of measuring the optical depth at reionization without relying on large-scale Cosmic Microwave Background (CMB) polarization and obtain competitive measurements that can validate the state-of-the-art constraints on this parameter.   Within the ΛCDM model, our most constraining result is τ=0.080±0.012, obtained by combining Planck temperature and polarization data at ℓ>30, the Atacama Cosmology Telescope (ACT) and Planck measurements of the lensing potential, Baryon Acoustic Oscillations (BAO), and Type-Ia supernova data from the Pantheon+ catalogue. Notably, using only ACT temperature, polarization, and lensing data in combination with BAO and supernovae, we obtain τ=0.076±0.015, which is entirely independent of Planck. 

My Contribution: I performed the MCMC analysis for all the different combinations of datasets, realized all figures and tables. I made the primary contribution to writing the paper.

We study scatter-like interactions between neutrinos and dark matter in light of different combinations of temperature, polarization and lensing data released by three independent CMB experiments: the Planck satellite, the Atacama Cosmology Telescope, and the South Pole Telescope. We apply two different statistical methodologies and, alongside the usual marginalization technique, we cross-check all the results through a Profile Likelihood analysis. Both methods confirm a mild preference for non-vanishing interactions from small-scale CMB data both when neutrinos are considered massless or massive particles. The Profile Likelihood analysis also confirms that interactions are not disfavoured by Planck.

My Contribution: I performed the MCMC analysis for all the different combinations of datasets. I made the primary contribution to writing the paper.

This contribution aims to present a comprehensive and up-to-date overview of the situation emerging from the most recent analyses of the Cosmic Microwave Background temperature anisotropies and polarization angular power spectra examining the key elements underlying current discrepancies and the challenges that must be addressed to restore cosmic concordance.

This paper investigates the current limitations on the equation of state for dark energy. We specifically focus on the apparent inclination towards phantom dark energy observed in Planck Cosmic Microwave Background (CMB) data alone. We thoroughly examine the origins of this inclination and attribute it to various physical and geometrical factors. To establish a reliable conclusion, we combine data from Planck CMB, Baryon Acoustic Oscillations, Type Ia Supernovae, and Cosmic Chronometers, which yields a consensus dataset consistent with the cosmological constant value. In summary, although there are a few sporadic indications, we do not find any compelling evidence that steers us away from the cosmological constant.

My Contribution: I realized half of the MCMC analyses based on the CMB data in Table 2. I conducted the MCMC analyses for various combinations of CMB and local probes data as presented in Table 3. I produced all the plots from Fig. 1 to Fig. 7. I actively participated in the writing of the paper.

This study explores late-time hot relic mass constraints using lensing data from the Atacama Cosmology Telescope, combined with data from the Planck Satellite and other local probes such as Baryon Acoustic Oscillations measurements, shear-shear, galaxy-galaxy, and galaxy-shear correlation functions from the Dark Energy Survey, as well as distance moduli measurements from Type Ia Supernovae. The tightest bounds obtained are stronger than laboratory neutrino mass searches, reaffirming the reliability of extracting thermal relic properties using cosmological observations. Finally, we present a discussion concerning the implications of the results on cosmic tensions. 

My Contribution: I proposed the project. I performed the MCMC analysis and realized all plots and tables. I contributed to the paper writing. 

This paper introduces a numerical method for investigating multifield models of inflation. The algorithm solves the field equations throughout the entire inflationary period, predicting observable quantities such as scalar perturbations and gravitational waves. It incorporates the transfer matrix formalism to track the behaviour of modes on super-horizon scales and entropy transfer. The algorithm is integrated with Boltzmann codes to compute the full cosmology, including CMB anisotropies and polarization. A novel sampling algorithm efficiently explores the parameter space, enabling Monte Carlo analysis. The method is tested on a specific model, deriving constraints on its parameters.

My Contribution: I proposed the project and conceptualized the approach to implement it. I contributed to the theory code, interfaced it with Boltzmann integrator codes,  and developed the sampler and the data analysis pipeline. I contributed to the paper writing. 

The standard model of cosmology is largely successful in describing many observations, including precise measurements of the Cosmic Microwave Background (CMB) radiation. However, some intriguing anomalies remain currently unexplained within this theoretical framework. Such discrepancies can be broadly categorized into two groups: those involving CMB-independent probes and those within different CMB experiments. Examples of the former category include the  Hubble tension between the value of the present-day expansion rate of the Universe inferred by CMB observations and local distance ladder measurements. The latter category involves anomalies between the values of cosmological parameters obtained by different CMB experiments and their consistency with the predictions of ΛCDM. In this chapter, we primarily focus on this second category and study the agreement among the most recent CMB measurements to d the limitations and uncertainties underlying both the current data and the cosmological model. Finally, we discuss the implications for the Hubble tension and its proposed solutions.

Note: Invited chapter for the edited book "Hubble Constant Tension" (Eds. E. Di Valentino and D. Brout, Springer Singapore, expected in 2024)

The absence of a definitive detection of B-mode polarization and the emerging discrepancies among different CMB experiments present a challenge in determining precise predictions for the inflationary models that best explain the observed data. In this work, we further explore this difficulty and conduct a case study by analyzing four well-known inflationary potentials in light of the most recent CMB observations released by Planck and ACT, along with B-modes polarization data from the BICEP Collaboration, and measurements of Baryon Acoustic Oscillations (BAO) and Redshift Space Distortions (RSD) from BOSS DR12 and eBOSS DR16. We show that the most typical models such as Starobisnky and α-attractors are in disagreement with the ACT small-scale CMB measurements, particularly when combined with B-modes polarization data. On the other hand, these potentials are in perfect agreement with the Planck measurements at larger angular scales. This dichotomy makes it challenging to identify a single model or a group of models that can be universally considered as the preferred choice based on all available CMB observations.

My contribution: I proposed the project and conceptualized the approach to implement it. I performed the data-analysis of the different potentials; I realized figure 1. I made the primary contribution to writing the paper.

We present up-to-date limits on neutrino masses and abundances exploiting either the Data Release 4 of the Atacama Cosmology Telescope (ACT) or the South Pole Telescope polarization measurements from SPT-3G, envisaging different non-minimal background cosmologies and marginalizing over them. Our model-independent mass limits assess the robustness of current cosmological measurements of the neutrino mass scale as well as the consistency between high-multipole and low-multiple Cosmic Microwave Background observations measuring such scale. 

My contribution: I contributed to the data analysis for all the different cosmological models and to the bayesian model comparison. I made the primary contribution to writing the paper.

We extend our analysis of neutrino Dark Matter interactions with small-scale CMB measurements [arXiv:2303.16895] by further proving the robustness of a preference (at 1σ level) for a non-zero coupling between the two species obtained by ACT as well as its combination with Planck and BAO. Our results are confirmed both by assuming a temperature-independent and T-squared-dependent cross-section as well as by fixing and relaxing the effective number of relativistic degrees of freedom in the early Universe. When performing a Bayesian model comparison, the interacting scenario is mostly preferred over a baseline ΛCDM cosmology.  The preferred value of the interaction strength is used as a benchmark and the potential implications of dark matter's interaction with a sterile neutrino are discussed.

My contribution:  I performed the cosmological data analyses for the νDM interactions, and realized figures 1-4 & 8-11. I made the primary contribution to writing the paper.

We revisit the possibility of using cosmological observations to constrain models that involve interactions between neutrinos and dark matter.  We show that small-scale measurements of the cosmic microwave background with a few per cent accuracy are critical for uncovering unique signatures from models with tiny couplings that would require a much higher sensitivity at lower multipoles, such as those probed by the Planck satellite.  We analyze the high-multipole data released by the Atacama Cosmology Telescope, both independently and in combination with Planck and Baryon Acoustic Oscillation measurements, finding a compelling preference for a non-vanishing coupling which aligns with other CMB-independent probes. We illustrate how this coupling could be accounted for in the presence of dark matter interactions with a sterile neutrino. 

My contribution:  I performed the cosmological data-analyses for the νDM interactions, I realized figure 1 and figure 2. I made the primary contribution to writing the paper.

We analyze a cosmological model featuring an interaction between dark energy and dark matter in light of the measurements of the Cosmic Microwave Background released by three independent experiments:  the Planck satellite, the Atacama Cosmology Telescope, and WMAP (9-year data).  We show that different combinations of the datasets provide similar results, always favouring an interacting dark sector with a 95% CL significance in the majority of the cases. Remarkably, such a preference remains consistent when cross-checked through independent probes, while always yielding a value of the expansion rate consistent with the local distance ladder measurements.

My contribution: I contributed to the MCMC analyses for the different data-sets, I realized the bayesian model comparison, realized figure 1 and figure 2. I made the primary contribution to writing the paper.

We explore observational constraints on a cosmological model with an interaction between dark energy (DE) and dark matter (DM). By using a compilation of 15 measurements of the 2D BAO (i.e., transversal) scale in combination with Planck-CMB data,  we explore the parametric space of a class of interacting DE models (IDE) showing that Planck-CMB + 2D BAO measurements provide a strong statistical evidence in favor of IDE cosmologies, offering a potential solution  to the H0 tension.

My contribution: I contributed to the MCMC analyses for the different cosmological and astrophysical data-sets, I contributed to the bayesian model comparison, I realized figure 1 and contributed to the paper writing.

We present strong model-marginalized limits on both thermal neutrinos and thermal QCD axions. Novel aspects of our analyses are the marginalization over several background cosmologies and the inclusion of small-scale Cosmic Microwave Background observations from the Atacama Cosmology Telescope and the South Pole Telescope, together with those from the Planck satellite and Baryon Acoustic Oscillation data. 

My contribution: I contributed to a modified version of the code CAMB able to compute the thermal axion cosmology, I contributed to the data analysis for all the different cosmological models, I contributed to the bayesian model comparison, I realized figure 1 and figure 3. I made the primary contribution to writing the paper.

We revisit the calculation of relic radiation from primordial gravitational waves discussing some caveats of the state-of-the-art analyses. Through a parametric investigation, we demonstrate that the calculation is dominated by the behaviour of the tensor spectrum on scales where the slow-roll dynamics break down and the production of gravitational waves becomes model dependent. Motivated by these results, we realize a theoretical Monte Carlo and, working within the framework of the Effective Field Theory of inflation, we investigate the observable predictions of a very broad class of models proving the calculation to be remarkably model-dependent. We, therefore, conclude that accurate analyses are needed to infer reliable information on the inflationary Universe.

My Contribution: I proposed the project and conceptualized the approach to implement it. I performed the parametric analysis; developed the algorithm for integrating the Hubble Flow Equations; contributed to derive the results from the theoretical  Monte Carlo, derived the updated bounds on inflation from the BBN; realised all the plots in the paper. I made the primary contribution to writing the paper.

We systematically explore the effects of adding curvature in extended cosmologies involving a free-to-vary neutrino sector and different parametrizations of Dark Energy showing that forcing the Universe to be flat can significantly bias the constraints on the equation of state of the DE component and its dynamical nature.

My contribution: I contributed to the analyses and interpretation of the results. I realized figures 17-22. I made the primary contribution to writing the paper.

We explore yet a new potential challenge for inflationary cosmology arising from Planck-independent observations of the cosmic microwave background. Namely the ∼ 2.7σ discrepancy in the value of the scalar spectral index measured by Planck (ns = 0.9649 ± 0.0044) and by the Atacama Cosmology Telescope (ACT) (ns = 1.008 ± 0.015).  We show that this discrepancy is neither alleviated with the addition of large-scale structure information nor with the low multipole polarization data. We discuss possible avenues to alleviate the tension relying on either neglecting polarization measurements from ACT or in extending different sectors of the theory

My contribution: I proposed the project. I performed the MCMC analyses, realized all the figures. I made the primary contribution to writing the paper.

We study the global agreement between the most recent observations of the Cosmic Microwave Background temperature and polarization anisotropies angular power spectra released by the Atacama Cosmology Telescope and the Planck satellite in various extended cosmological models. By using the Suspiciousness statistic, we show that the global "CMB tension" between the two experiments, quantified at the Gaussian equivalent level of ∼2.5σ within the baseline ΛCDM, is reduced at the level of 1.8σ when the effective number of relativistic particles  is significantly less than the standard value, while it ranges between 2.3σ and 3.5σ in all the other extended models.

My contribution: I wrote the pipeline for the suspiciousness , contributed to the data analysis , I realized figure 1. I made the primary contribution to writing the paper.

We present an updated data-analysis comparison of the most recent observations of the Cosmic Microwave Background temperature anisotropies and polarization angular power spectra released by four different experiments: the Planck satellite on one side, and the Atacama Cosmology Telescope (ACTPol) and the South Pole Telescope (SPT-3G), combined with the WMAP satellite 9-years observation data on the other side. We investigate in a systematic way many extended cosmological models providing several hints for anomalies in the CMB angular power spectra in tension with the standard cosmological model. This indicates that either significant unaccounted-for systematics in the data are producing biased results or that ΛCDM is an incorrect/incomplete description of Nature. 

My contribution: I contributed to the data analysis , I realized figures 13-18.  I made the primary contribution to writing the paper.

We revisit the joint constraints in the mixed hot dark matter scenario in which both thermally produced QCD axions and relic neutrinos are present.  In light of recent advances in literature, we recompute the cosmological axion abundance and improve the state-of-the-art analyses by avoiding approximate methods, such as the instantaneous decoupling approximation, and limitations due to the limited validity of the perturbative approach in QCD that forced to artificially divide the constraints from the axion-pion and the axion-gluon production channels.  Investigating the two most popular axion frameworks ( the KSVZ and DFSZ axion) we find robust and self-consistent limits on the QCD axion mass that are approximately a factor of 5 more constraining  with respect to the existing limits. 

My contribution: I contributed to a modified version of the code CAMB able to compute the thermal axion cosmology and address the new advances in literature; I contributed to compute the BBN predictions and to include them in CAMB; I contributed to the realization of the likelihoods for future CMB-S4-like and BAO DESI-like experiments; I contributed to the algorithms and the methodology used for the data analysis; I carried out the analysis of the BBN data; I contributed to the analysis of the CMB and BAO data (and the CMB-S4 and DESI forcasted data); I realized all the tables and figures. I was among the principal contributors in writing the paper.

Snowmass Collaboration paper on cosmological tensions and anomalies. 

My PhD Thesis

We make use of the Etherington reciprocity theorem, or distance duality relation (DDR), to build a consistency check for extended cosmological models.  We provide the first joint measurement of the Hubble constant (H0) and DDR to percentage accuracy and find a mild 2 sigma discrepancy between the latest SH0ES measurement of H0 and the validity of the DDR.  Then, we outline our consistency check methodology for extended cosmological models, finding that models with non-zero spatial curvature show a preference for DDR violation at the level of 1.5 sigma.

My contribution: I contributed to the codes used for constraining H0 and DDR, I contributed to outline the consistency check methodology and I analyzed the different models discussed in Sec. IV.2. I realized Fig3.  I contributed to the paper writing.

We study how the improvements expected by future Cosmic Microwave Background and Baryon Acoustic Oscillation measurements can be translated into constraining power for well motivated extensions of the Standard Model of elementary particles that involve axions thermalized before the QCD phase transition by scatterings with gluons in combination with neutrinos and primordial BBN elements. 

My contribution: I proposed the project and conceptualized the approach to implement it. I implemented the code for axion-gluon interactions inside CAMB, I contributed to the realization of the likelihoods for future CMB-S4-like and BAO DESI-like experiments; I contributed to the modification of CAMB to include all the BBN primordial  elements. I analyzed the simulated data and realized Figs. 2 and 3. I made the primary contribution to writing the paper.

In light of the most recent cosmological observations, we provide new updated constraints on the slow-roll inflation in different extended scenarios beyond the ΛCDM cosmological model.  We interpret the results under the framework of the different inflationary models proposed in literature, showing how the differences in the datasets can change the compatibility among the different models, sometimes leading to discordant conclusions.

My Contribution: I analyzed the different datasets, realized the triangular plots. I made the primary contribution to writing the paper.

In light of the most recent cosmological observations we analyze a realistic mixed hot-dark-matter scenario which includes axions and massive neutrinos as additional thermal species.  For the axion thermalization in the early Universe, we consider both the axion-gluon scattering and the axion-pion scattering.  For the latter process we remain in the range of validity of chiral perturbation theory and we don't assume any specific model for axion interactions.

My contribution: I implemented the code for axion-pion and axion-gluon interactions inside CAMB,  l  realized Figs. 1 and 3. I made the primary contribution to writing the paper.

We study the effects of a coupling of the inflaton field to higher-curvature tensors in models of inflation with a minimal breaking of conformal symmetry. We show that an observable violation of the inflationary consistency relation(s) from higher-curvature tensors implies also a relatively large scale dependence of the tensor tilt. We discuss the implications for the observational constraints.

My contribution: I proposed the project and conceptualized the approach to implement it. I developed the theoretical model and performed the theoretical calculations. I contributed to the data analysis and I realized Figs. 1 and 3.  I made the primary contribution to writing the paper.

We study the effects of a non-trivial gravity propagation during inflation. We discuss the implications for the stochastic background of inflationary gravitational waves both from the theoretical side and on the data analysis perspective. 

My Contribution: I proposed the project and conceptualized the approach to implement it. I developed the theoretical model and performed the theoretical calculations. I contributed to the data analysis. I made the primary contribution to writing the paper.

We show that due to the huge difference in the scales probed by CMB and GW experiments, higher-order terms in the primordial tensor spectrum, albeit negligibly small on the CMB scales, may give non-negligible contributions on the scale probed by direct gravitational observations.  We discuss the implications for the constraints on the tensor tilt.

My Contribution: I proposed the project. I derived the results, realized the figures. I made the primary contribution to writing the paper.

We investigate the higher-order slow-roll consistency relations among scalar and tensor parameters. We show that a set of slow roll consistency relations can be derived at any order in the power-law expansion, discussing the implications both from a theoretical point of view and on a data analysis perspective.

My contribution: I derived the results, analyzed the data, realized the figures. I made the primary contribution to writing the paper.