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A list of published articles I have contributed to
This study mapped dust, atomic gas, molecular gas, and metallicity across ten nearby spiral galaxies, on scales of roughly 0.6 to 2.3 kpc. We measured the dust-to-gas ratio (DGR) and the dust-to-metal ratio (DMR) as functions of metallicity.
Measuring molecular gas through carbon monoxide (CO) is the main uncertainty. The inferred DGR and DMR trends depend strongly on the assumed CO-to-H₂ conversion factor (αCO). No single αCO fits the whole sample, so we introduced a hybrid prescription that treats CO-bright and CO-dark galaxies differently, using both their metallicity and their position relative to the empirical CO luminosity–SFR relation.
Most molecular gas surveys target massive galaxies, because the CO (used to trace molecular hydrogen) is hard to detect in low-mass, metal-poor systems. The MaLHUCO survey addresses this with JCMT CO(J=2–1) line observations, in 42 star-forming disk galaxies of type Scd or later, drawn from the MaNGA survey.
We explored how molecular gas relates to the global properties of galaxies at the low-mass end of the star-forming population. The relation between molecular gas mass and star formation rate (the Kennicutt–Schmidt law) stays close to linear (slope≈1) at low stellar masses. Furthermore, the 12μm luminosity provides a promising tracer of molecular gas content.
Using a sample of 18 large, face-on spiral galaxies from the DustPedia project we explored the contributions of young and evolved stars to the dust heating.
We found that in 56% of the galaxies, Tdust shows a stronger correlation with ΣSFR than with ΣM*, indicating the dominant role of young stars in dust heating in star-forming regions. In ~72% of the sample young stars are not the unique contributors to dust heating, and other sources (e.g., evolved stars) can play a role (see correlation coefficients in figure).
We also found that the presence of a central AGN does not significantly influence Tdust radial profiles.
Using deep JWST imaging in the SMACS-0723 cluster field, we studied the mid-IR (MIR) emission of quiescent galaxies (QGs) at intermediate redshift (0.2 < z < 0.7).
We observed a scatter in the MIR spectra, especially at λrest > 5 µm, that can be attributed to different dust continuum levels and/or the presence of polycyclic aromatic hydrocarbon (PAH) features in QGs.
We used approximately 1000 X-ray sources in the COSMOSLegacy survey (within the UltraVISTA region) and compared their SFR with about 90000 non-AGN systems compiled by the HELP collaboration.
Our results showed that at low to moderate X-ray luminosities, AGN tend to have lower (or at most equal) SFRs compared to non-AGN systems with similar stellar mass and redshift. At higher x-ray luminosities, we observed an increase in the SFR of AGN for systems that have 10.5 < log [Mstar(Msol)] < 11.5.
In a Principal Component Analysis (PCA), we investigated how the shape of the FIR SED correlates with the galaxies' intrinsic stellar and dust properties.
We found that 95% of the variance can be described by two principal components (PCs). The first component controls the wavelength of the peak of the SED and the second characterises the width.
The physical quantities that correlate better with the coefficients of the first two PCs, and thus control the shape of the FIR SED are the dust temperature, the dust luminosity, the SFR, and fabs (i.e. the fraction of absorbed stellar luminosity by dust).
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