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<span style="caret-color: rgb(0, 0, 0); color: rgb(0, 0, 0); font-size: 14px;">Hi all,</span>
<div><span style="caret-color: rgb(0, 0, 0); color: rgb(0, 0, 0); font-size: 14px;"><br>
</span></div>
<div><span style="font-size: 14px;">This week’s lunch talk will be given by Yannick Bahé, and will take place on Thursday 4th December at 1pm in A113. Title and abstract below.</span></div>
<span style="font-size: 14px;"><br>
<span style="caret-color: rgb(0, 0, 0); color: rgb(0, 0, 0);"><b>Title:</b> Star formation quenching in z ~ 0 groups and clusters</span><br style="caret-color: rgb(0, 0, 0); color: rgb(0, 0, 0);">
<br style="caret-color: rgb(0, 0, 0); color: rgb(0, 0, 0);">
<span style="caret-color: rgb(0, 0, 0); color: rgb(0, 0, 0);"><b>Abstract:</b> Isn’t this a solved problem? As it turns out, no. Even though we are now probing group/cluster environments out to z > 2, there is still much we do not know even in the local Universe,
including how commonly star formation is actually shut down in group and cluster galaxies - the quenched fraction. In my talk, I will give an update on this topic from a combined observation and simulation perspective. On the observational side I will present
a new analysis of the GAMA survey to quantify the quenched fraction over two orders of magnitude in stellar and halo mass, based on from full spectrum fitting (for star formation rates) and detailed matching to the FLAMINGO simulations (for halo masses). I
will then compare these quenched fractions to predictions from the new COLIBRE simulations to test whether our theoretical expectations agree with reality.</span></span>
<div><span style="font-size: 14px;"><font color="#000000"><span style="caret-color: rgb(0, 0, 0);"><br>
</span></font>Thanks,</span></div>
<div><span style="font-size: 14px;">Joe</span></div>
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