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<b>***Reminder for tomorrow’s seminar!***</b></div>
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If you would like to join us for lunch, please let me know. </div>
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Since Yuchen is staying in the evening, there will also be a dinner plan, anyone is more than welcome to join us. </div>
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Cheers,</div>
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Tutku</div>
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<b>From: </b>Astro <astro-bounces@lists.nottingham.ac.uk> on behalf of Tutku Kolcu (staff) <Tutku.Kolcu@nottingham.ac.uk><br>
<b>Date: </b>Friday, 28 November 2025 at 15:42<br>
<b>To: </b>Nottingham Astro Group <astro@nottingham.ac.uk><br>
<b>Subject: </b>[Astro] Astronomy Seminar, 3rd December 🎄<br>
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Dear all,</div>
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Next week's speaker will be Dr Yuchen Ding from Liverpool John Moores University. Please find below the title and the content of the seminar. </div>
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<span style="font-family: Aptos; font-size: 11pt; color: rgb(33, 33, 33);"><i>Probing the Assembly of Low Star-formation Galaxies via Population-Orbit Superposition Method</i></span></p>
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<span style="font-family: Aptos; font-size: 11pt; color: rgb(33, 33, 33);">Understanding the formation of low star-formation galaxies is key to unraveling the processes that drive galaxy evolution. My talk will mainly contain three parts:</span></p>
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<span style="font-family: Aptos; font-size: 11pt; color: rgb(33, 33, 33);">In the context of the Fornax3D project, we analyzed 21 galaxies in the Fornax cluster observed with MUSE/VLT by applying a novel population-orbit superposition method. By fitting the
luminosity distribution, stellar kinematics, age and metallicity maps simultaneously, we obtained the internal stellar orbit distribution and stellar population distributions. </span></p>
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<span style="font-family: Aptos; font-size: 11pt; color: rgb(33, 33, 33);">Based on the model, we decompose the dynamically cold disk (orbital circularity λz > 0.8) for each galaxy, and obtain its luminosity fraction, age and metallicity radial profiles. For
galaxies in the Fornax cluster, we find that the luminosity fraction of cold disk in recent infallers are consistent with field galaxies from CALIFA, while the cold disk fractions in ancient infallers with tinfall > 8 Gyr are a factor of ∼ 4 lower, with control
of stellar mass. Moreover, the stellar age of cold disk is highly correlated with galaxy infall time into the cluster, and we find positive age gradients in cold disks, with stars in the inner disk being younger than those in the outer disk, contrary to the
expectation of inside-out growth.</span></p>
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<span style="font-family: Aptos; font-size: 11pt; color: rgb(33, 33, 33);">We then directly compare our results with galaxies in Fornax-like clusters in TNG50 simulations, and find that they agree with each other remarkably well on cold disk fractions, stellar
age, age gradients, and their dependence on galaxy’s infall time to the cluster. In the simulations, we find gas in the outer disk was partly removed and partly compacted into the inner regions when falling into the cluster, which leads to quick stop of star
formation in the outer disk, but a long tail of star formation in the inner regions. The turnover of star formation radius from out to inner regions is highly correlated with the galaxy’s infall time. This process explains most of the above results. At the
same time, tidal shocking partially heats the cold disk formed before infall, which further reduces the cold disk fraction in ancient infallers which bear the strongest tidal effects.</span></p>
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<span style="font-family: Aptos; font-size: 11pt; color: rgb(33, 33, 33);">Finally, we analyzed one low star-formation S0 galaxy in the GECKOS survey - a VLT/MUSE large program targeting 36 nearby edge-on galaxies at Milky Way mass. We find an old, metal-poor
nuclear stellar disk, an extended main disk in this galaxy. It shows a strong negative age gradient in unclear disk and a strong positive age gradient in main disk. The presence of an old nuclear disk suggests the existence of an ancient bar structure. Furthermore,
we find that both the cold disk fraction and the age gradient align with those observed in galaxies from the Fornax cluster, implying that environment may play only a limited role in shaping the evolution of low star-formation galaxies.</span></p>
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<span style="font-family: Aptos;">The seminar will be in the <u>Physics Building C4 at 15:45</u>, followed by the
</span><span style="font-family: "Apple Chancery", Arial, Helvetica, sans-serif;">wine and cheese</span><span style="font-family: Aptos;"> in the usual place.</span></div>
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If you want to join us for lunch or want to arrange a meeting with Yuchen just let us know.</div>
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Best,</div>
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<span style="font-size: 11pt; color: rgb(33, 33, 33);">Jesse , Luke & Tutku </span>
<span style="font-size: 14.666667px; color: rgb(0, 0, 0); background-color: rgb(255, 255, 255);">🎄</span><span style="font-size: 11pt; color: rgb(33, 33, 33);"><br>
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