TODDLERS 2.0: Stellar feedback and observables across diverse IMFs, binary populations, and cloud environments

Abstract

Modeling the feedback-driven evolution of star-forming regions and their multi-wavelength emission is essential for interpreting galaxy observations across cosmic time. TODDLERS couples 1D shell dynamics with Cloudy photoionization to predict UV-to-mm observables. The original framework assumed instantaneous star formation, uniform cloud density, a fixed IMF with single-star evolution, and fixed dust properties. We present TODDLERS 2.0, extending the framework to broader stellar populations, birth-cloud conditions, and dust physics. Stellar feedback and input spectra are modeled using pySTARBURST99 (arbitrary IMFs, upper mass limits up to 500 M$\odot$) and BPASS (binary evolution, upper mass limits up to 300 M$\odot$), including stochastic IMF sampling for low-mass clusters (M$* \lesssim 10^4$ M$\odot$) and constant star formation. The 1D evolution includes non-uniform cloud density profiles and dynamic cloud density evolution driven by escaping ionizing radiation. Cloudy post-processing includes modified grain size distributions and diffuse ionized gas. Cloud density profile and star formation mode regulate fragmentation timescales and shell extent: centrally concentrated profiles fragment earlier, while constant star formation delays fragmentation relative to bursts. Top-heavy IMFs generate stronger feedback and earlier fragmentation than a Kroupa IMF. Dynamic cloud density evolution introduces an additional feedback channel, strongest at low metallicity where unswept cloud density decreases by up to three orders of magnitude. For low-mass clusters, stochastic sampling produces order-of-magnitude feedback variations, demonstrating breakdown of the fully sampled IMF approximation. TODDLERS 2.0 models diverse stellar populations, cloud structures, and star formation modes as a standalone tool or sub-grid emission model for galaxy simulations.