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Gentle reminder of this at 1pm today.</div>
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Joe</div>
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<div id="divRplyFwdMsg" dir="ltr"><font face="Calibri, sans-serif" style="font-size:11pt" color="#000000"><b>From:</b> Joseph Butler <Joseph.Butler@nottingham.ac.uk><br>
<b>Sent:</b> Monday, November 3, 2025 4:38:30 PM<br>
<b>To:</b> astro@nottingham.ac.uk <astro@nottingham.ac.uk><br>
<b>Subject:</b> Lunch Talk - 6/11/25</font>
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<div><span style="font-size:14px">Hi all,</span>
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<div style="color:rgb(0,0,0)"><span style="font-size:14px">This week’s lunch talk will be given by Candela Zerbo, and will take place on Thursday 6th November at 1pm in A113. Title and abstract below.</span></div>
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<div><span style="font-size:14px"><b style="color:rgb(0,0,0)">Title</b><span style="color:rgb(0,0,0)">: Minding the Gap Between Scales: Insights from Simulations on the Role of Local Density and the Cosmic Web on Galaxy Evolution</span><br style="color:rgb(0,0,0)">
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<b style="font-size:14px; color:rgb(0,0,0)">Abstract</b><span style="font-size:14px; color:rgb(0,0,0)">: The evolution of galaxies is strongly influenced by their surrounding environment, from the local density of neighbouring systems to their position within
the cosmic web. In this work, we aim to disentangle the relative importance of these factors using simulated galaxies. Building on the observational framework of O’Kane et al. (2024), we classify simulated galaxies into six environmental categories to explore
how their baryonic properties and star formation activity vary with local density and cosmic-web location. As a first step, we focus on two test clusters from </span><i style="font-size:14px; color:rgb(0,0,0)">The Three Hundred</i><span style="font-size:14px; color:rgb(0,0,0)"> project.
We examine the spatial distribution of their galaxies and the stellar mass function in each environment. We will later incorporate star formation rates and compare different density estimators. Future stages will include contrasting results between hydrodynamical
(GIZMO–SIMBA) and semi-analytic (SAG) models, and evaluating the impact of different filament identification methods. This ongoing work will provide new insights into how local and large-scale structures jointly drive galaxy evolution.</span></div>
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<div><span style="font-size:14px; color:rgb(0,0,0)">Thanks,</span></div>
<div><span style="font-size:14px; color:rgb(0,0,0)">Joe</span></div>
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