Other Publications

A list of published articles I have contributed to

Tailor et al., 2025, The role of young and evolved stars to the heating of dust in local galaxies, A&A,forthcoming :

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.

Blánquez-Sesé et al., 2023, Uncovering the MIR emission of quiescent galaxies with JWST, A&A, 679, L2 :

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.

Mountrichas et al., 2022, Star-formation of X-ray AGN in COSMOS: The role of AGN activity and galaxy stellar mass, A&A, 661, A108 :

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.

Nersesian et al., 2021, Probing the pectral shape of dust emission with the DustPedia sample, MNRAS, 506, 3986 :

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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