collaborators

8 papers

astro-ph.GA2025

Compact Size, High SFR: Defining Morphological Features of Ly-Emitters

Keunho Kim, Anahita Alavi, Christopher Snapp-Kolas +7

The mechanisms of Ly photon escape are key to understanding galaxy evolution and cosmic reionization, yet remain poorly understood. We investigate the UV-continuum sizes of 23…

astro-ph.GA2025

Euclid Quick Data Release (Q1). Active galactic nuclei identification using diffusion-based inpainting of Euclid VIS images

Euclid Collaboration, G. Stevens, S. Fotopoulou +271

Light emission from galaxies exhibit diverse brightness profiles, influenced by factors such as galaxy type, structural features and interactions with other galaxies. Elliptical ga…

astro-ph.GA2025

A gradient boosting and broadband approach to finding Lyman-α emitting galaxies beyond narrowband surveys

A. Vale, A. Paulino-Afonso, A. Humphrey +5

In this work, we test whether gradient-boosting algorithms, trained on broadband photometric data from traditional Lyman- emitting (LAE) surveys, can efficiently and accurately…

astro-ph.GA2025

Euclid Quick Data Release (Q1). Exploring galaxy morphology across cosmic time through Sersic fits

Euclid Collaboration, L. Quilley, I. Damjanov +333

We present the results of the single-component Sérsic profile fitting for the magnitude-limited sample of \IE galaxies within the 63.1 deg area of the Euclid Quick Data R…

astro-ph.GA2025

Through the fog: a complementary optical galaxy classification scheme for 'intermediate' redshifts

Duarte Muñoz Santos, Cirino Pappalardo, Henrique Miranda +10

Understanding galaxy classification depends on our interpretation of their spectra. To date, the hydrogen Balmer lines remain the most consistent way to classify galaxies, but at '…

astro-ph.GA2025

Importance of modelling the nebular continuum in galaxy spectra

Henrique Miranda, Ciro Pappalardo, José Afonso +7

The neglect of modelling both stellar and nebular emission significantly affects the derived physical properties of galaxies, particularly those with high star formation rates. Whi…